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SP-1288
SP-1288
Research and Scientific Support Department
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Contact: ESA Publications Division
c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands
Tel. (31) 71 565 3400 - Fax (31) 71 565 5433
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SP-1288
June 2005
Report on the activities of the
Research and
Scientific Support
Department
2003 – 2004
Scientific Editor
A. Gimenez
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ESA SP-1288
ISBN
ISSN
Scientific Editor
Editor
Published and distributed by
Copyright
Price
Report on the Activities of the Research and Scientific
Support Department from 2003 to 2004
92-9092-963-4
0379-6566
A. Gimenez
A. Wilson
ESA Publications Division
© 2005 European Space Agency
€30
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CONTENTS
1. Introduction
5
4. Other Activities
95
1.1
Report Overview
5
4.1
95
1.2
The Role, Structure and Staffing of RSSD
and SCI-A
5
Symposia and Workshops organised
by RSSD
4.2
ESA Technology Programmes
101
Department Outlook
8
4.3
Coordination and Other Supporting
Activities
102
1.3
2. Research Activities
11
2.1
Introduction
13
2.2
High-Energy Astrophysics
14
2.3
Optical/UV Astrophysics
19
2.4
Infrared/Sub-millimetre Astrophysics
22
2.5
Solar Physics
26
2.6
Heliospheric Physics/Space Plasma Studies
31
2.7
Comparative Planetology and Astrobiology
35
2.8
Minor Bodies
39
2.9
Fundamental Physics
43
2.10
Research Activities in SCI-A
45
3. Scientific Support Activities
53
3.1
Astrophysics Missions Division
56
3.2
Solar and Solar-Terrestrial
Missions Division
64
3.3
Planetary Missions Division
70
3.4
Fundamental Physics Missions Division
78
3.5
Space Telescope Operations Division
80
3.6
Science Operations and Data Systems
Division
83
3.7
Science Payload and Advanced Concepts
Office
89
Annex 1:
Manpower Deployment
107
Annex 2:
Publications
(separated into refereed and
non-refereed literature)
113
Annex 3:
Seminars and Colloquia
149
Annex 4:
Acronyms
153
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introduction
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1. INTRODUCTION
1.1 Report Overview
This report on the activities of the Research and
Scientific Support Department (RSSD) covers the 2-year
period of 2003-2004. It is prepared as input to the
Department’s Advisory Committee, a group of
independent external scientists invited by the Director of
ESA’s Scientific Programme to review the Department’s
activities. It forms the basis of the oral reports made to
ESA’s Space Science Advisory Committee and the
Science Programme Committee every second
year. Through the publication of the report as an ‘SP’
(Special Publication) by the ESA Publications Division,
the activities of the Department are brought to the
attention of the scientific community and to a broader
audience.
These Biennial Reports have been produced since 1980.
In this volume, a number of changes introduced in the
last report have been kept. The report also covers the
activities of the Science Payload and Advanced Concepts
Office (SCI-A) owing to its close links with many
activities in RSSD and its history as the previous Science
Payload Technology Division.
The report is divided into four Chapters plus four
Annexes. Chapter 1 deals with the Department’s role and
organisation. A brief summary is given because its
mandate and structure did not change significantly
during the reporting period. Reference should be made to
the previous report (ESA SP-1268) for further
information. The names of staff, their locations, their
functional duties and scientific research interests are
given in Annex 1.
Chapter 2 addresses the scientific research of the
Department’s staff, broken down according to
‘discipline’ rather than divisional structure. A complete
listing of the scientific papers published in the literature
is given in Annex 2. Some 340 refereed papers were
published during 2003 and 2004, and more than 350
conference papers and other publications appeared.
Chapter 3 provides a top-level summary of the missionrelated activities at Divisional level. For the four
Missions Divisions, the prime contributions to the
scientific support of the various elements of the Science
Programme are summarised. For the two Operations
Support Divisions, special mention is also made of postoperational and archiving phases. The activities of SCI-A
are included.
Finally, Chapter 4 addresses a variety of activities carried
out by RSSD in its support role to the community. The
Chapter summarises important scientific symposia and
workshops organised by the Department, support to the
Directorate’s science communication activities, and
various other activities.
While this Biennial Report provides perspective on the
breadth and quality of the activities of the staff, both in
their research and functional work, it is not intended to be
comprehensive. Up-to-date information on the Department’s activities can be obtained at http://www.rssd.
esa.int and for SCI-A at http://sci.esa.int/science-e/
www/area/index.cfm?fareaid=65
1.2 The Role, Structure and Staffing of RSSD
and SCI-A
RSSD, one of the two Departments of ESA’s Scientific
Directorate, provides the direct interface to the scientific
community throughout all mission phases. Following
in-orbit checkout and commissioning, it is also responsible for the management of the missions. In addition, the
Department plays its part in the dissemination of
scientific knowledge to the public and for educational
purposes.
In essence, the role of RSSD is to ensure the best possible
scientific performance of ESA’s Scientific Programme
missions. To this end, the Department is responsible for
the implementation of all science management aspects of
the missions in the Science Directorate throughout their
study and operations phases.
In particular, the Department is responsible for providing
scientific expertise to studies and projects in all phases,
and for ensuring that maximum scientific return within
practical technical and budgetary constraints is
maintained as a target through all phases of a scientific
mission. The Department also manages, through its study
or project scientists, the activities of each mission
science team.
RSSD is responsible for all aspects of science operations
(definition, development, implementation and execution)
through all phases of missions and manages the
operations phases of missions following in-orbit
commissioning, supported, as necessary, by system
engineering expertise from the Scientific Projects
Department.
In very close coordination with SCI-A, RSSD provides
scientific and payload expertise within the Agency in all
phases of scientific missions, including to other
directorates of the Agency (e.g. on International Space
Station payloads). It works with external science teams
to define the science requirements for future mission
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introduction
Head of Research and
Scientific Support
Department
SCI-S
Chief Scientist
SCI-SR
Astrophysics Missions
Division
SCI-SA
Science Operations and
Data Systems Division
SCI-SD
Planetary Missions
Division
SCI-SB
Space Telescope
Operations Division
SCI-SN
Solar & Solar-Terrestrial
Missions Division
SCI-SH
Fundamental Physics
Missions Division
SCI-SP
Figure 1.2/1: The structure of RSSD.
studies and associated payloads and passes these to
SCI-A for follow-up.
It is, of course, very important that the scientific staff of
both RSSD and SCI-A maintain their scientific
proficiency by undertaking personal research.
In order to discharge its responsibilities and tasks in an
efficient manner, the Department is structured into four
Missions Divisions:
—
—
—
—
the Astrophysics Missions Division;
the Planetary Missions Division;
the Solar and Solar-Terrestrial Missions Division;
the Fundamental Physics Missions Division;
and two Operations Support Divisions:
— the Science Operations and Data Systems Division;
— the Space Telescope Operations Division.
The Office for Science Payload and Advanced Concepts
(SCI-A) is under the direct authority of the Director of
the Scientific Programme. This Office is responsible for
the assessment phase and the strategic approach for
Figure 1.2/2: The structure of SCI-A.
future missions as well for new payload technologies in
support of the Cosmic Vision long-term Scientific
Programme. The Office works, in close liaison with the
RSSD study scientists and the science community, to
determine the science and technological needs of this
programme. In addition, SCI-A provides payload
support/expertise to missions under development, both to
RSSD Project Scientists as well as the Science Projects
Department. The Office is also responsible for laboratory
support throughout the Directorate, including those
RSSD research activities requiring such support.
The organigram of RSSD is shown in Fig. 1.2/1. In
addition, the office of the Department Head is supported
by a budget control group including three integrated
project controllers from SCI-M. The role and functions
of the six Divisions, and those of SCI-A, are described
further in Chapter 3.
The staff of the Department (37 at the end of 2004) and
of SCI-A (21, including 2 advanced recruitments) hold
posts within the overall ESA staff complement. Staff
associated with Science Operations Teams are generally
supernumerary positions. By the end of 2004, there was
a complement of 68 supernumeraries (3 in SCI-A).
Fig. 1.2/2 depicts the structure of SCI-A. It should be
noted that, in these teams, many contractors and often
staff from Principal Investigator (PI) institutes work
together in an integrated structure. An overview of the
staff in post at the end of 2004 is given in Table 1,
integrating personnel from RSSD proper and SCI-A.
Figure 1.2/3 gives the distribution of staff according to
functions within RSSD.
Department staff are located not only at ESTEC, close to
the Science Directorate’s project teams and the Technical
Directorate, but also in Villafranca (ISO and XXMNewton science operations teams), in Garching and
Baltimore (Space Telescope Operations Division) and
Greenbelt (SOHO Project Scientist Team at NASA
Goddard Space Flight Center). During 2004, the Villafranca facilities were integrated into the European Space
Astronomy Centre (ESAC). Figure 1.2/4 shows the
distribution according to location of personnel from
RSSD.
While not formally on the ESA staff complement,
Internal Research Fellows, on contracts of maximum
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introduction
7
Table 1: RSSD Staff in Post at end of 2004.
Head of Department: A. Gimenez
Assistant Administrator: C. Bingham
Divisional Assistants: S. Ihaddadene, B. Schroeder, C. Villien
Chief Scientist: B.H. Foing
Astrophysics Missions Division
J. Clavel (Head)
M. Fridlund
T. Boeker
A. Heras
J. de Bruin
P. Jakobsen
F. Favata
R. Laureijs
S. Leeks
A. Marston
Project Controller: R. Fontaine*
R. Davis*
G. D’Aquino*
*seconded from SCI-M
A. Parmar
M.A.C. Perryman
G.L. Pilbratt
T. Prusti
J. Tauber
R. Vavrek
H. Laakso
R.G. Marsden
L. Sanchez Duarte*
T.R. Sanderson
R.M. Schulz
L.H. Svedhem
K. Wirth
O. Witasse
A. Clampin-Nota
H. Jenkner
I. Kamp
J. Maiz-Apellaniz
M. Miebach
B. Mobasher
N. Panagia
M. Robberto
M. Sirianni
E. Villaver
T. Wiklind
M.J. Szumlas
D. Texier**
G. Thoerner
A. Toni
C. Winkler
J.J. Zender
Integral Science Operations
L. Hansson (Head)
P. Barr
L. O’Rourke
A. Orr
J. Sternberg
ISO Data Centre (ESAC)
A. Salama (Head)
R. Lorente
E. Verdugo
M. Arpizou
M. Ehle
J.C. Gabriel
M. Guainazzi
J. Hoar
M. Kirsch
Solar and Solar-Terrestrial Missions Division
H. Opgenoorth (Head)
C.P. Escoubet
B.G. Fleck*
S. Haugan*
*located at SOHO/EOF, NASA Goddard Space Flight Center
Planetary Missions Division
G. Schwehm (Head)
A. Chicarro
D.V. Koschny
J.-P. Lebreton
P. Martin
Fundamental Physics Missions Division
R. Reinhard (Head)
L. Cacciapuoti
O. Jennrich
Space Telescope Operations Division
D. Machetto (Head)
M.R. Rosa
D. Sforna
ST-ECF (Garching)
STScI (Baltimore)
R. Albrecht
R.A.E. Fosbury
A. Aloisi
A. Micol
S. Arribas
Science Operations and Data Systems Division
M.F. Kessler (Head)
F. Jansen
C. Arviset*
N. Schartel*
K. Bennett
*located at ESAC **located at Geneva
P. Garcia Lario
XMM-Newton Science Operations (ESAC)
L. Metcalfe (Head, Science Support)
J. Munoz Peira (Head, Instrument Operations)
B. Altieri
A. Pollock
M. Santos-Lleo
Herschel Science Operations Development
J. Riedinger
S. Ott
Science Payload and Advanced Concepts Office (Science Payloads Technology Division)
A. Peacock (Head)
T. Beaufort
P. Falkner
D. Klinge
S. Andersson
J.F. van der Biezen
Ph. Gondoin
D. Lumb
T. Appourchaux
B.A.C. Butler
J. Heida
D. Martin
H.J. Arends
A. van Dordrecht
B. Johlander
N. Rando
M. Bavdaz
C. Erd
J. Romstedt
L.C. Smit
U. Telljohann
J. Verveer
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introduction
Figure 1.2/3: Distribution of RSSD staff according to
prime function.
Figure 1.2/4: Distribution of RSSD staff according to
location.
2 years and funded by the Agency’s Education budget,
play a major role in the Department’s research activities.
Typically, some 15 Research Fellows were in post at any
one time during the reporting period. The Department
and SCI-A also hosted several Young Graduate Trainees
on 1-year contracts, and offered numerous opportunities
for trainees and stagiaires.
1.3 Department Outlook
Highlights for the Department in the reporting period
include:
— the successful launches of Mars Express, SMART-1,
Rosetta and Double Star, and the very promising first
data from all their instruments;
— the successful arrival of Cassini-Huygens at Saturn
and the release of the Huygens probe towards Titan;
— the excellent scientific results from Mars Express
during its first year in orbit around the Red Planet;
— RSSD and SCI-A contributions to the planning of
ESA’s long-term Scientific Programme ‘Cosmic
Vision’, covering the decade 2015-2025;
— the completion, testing and delivery of
Co-Investigator contributions to Rosetta and
SMART-1 instruments;
— the continued excellent science return from the HST,
Ulysses, SOHO, Cluster and XMM-Newton
missions in orbit;
— maintaining a high level of research with a significant number of publications in spite of the increasing
pressure of the scientific support activities;
— the active organisation of a number of symposia and
workshops for the space science community;
— transfer of the BepiColombo mission to Mercury
from the assessment phase to implementation phase.
In 2004, RSSD achieved an all-time record of missions
in orbit under its responsibility. A total of 11 space
missions (comprising 14 spacecraft) were being
operated, with an impact on the Department’s efforts in
the area of science operations despite the frozen level of
complement.
During the past 2-years, time was devoted to
consolidating the reorganisation of the Department in
line with its new role and goals. In addition, some
refinements in the internal working procedures of the
Directorate were found necessary. The next 2 years are
expected to see a review of the effectiveness of the
structure in place and the performance of the staff at all
levels, with the possibility of more changes if required
for the achievement of the overall goals of the
Department. Moreover, further discussions are expected
within the Directorate to improve interfaces with the
Projects Department and other Offices, and new areas of
cooperation with other Directorates, such as the newly
created programme for Exploration, will need to be
expanded.
At the level of the Scientific Programme, the challenges
of the coming years are clearly dominated by the
definition of the new Cosmic Vision plan for the decade
2015 to 2025. Many discussions and evaluations will
have to be done in close cooperation with the scientific
community and our Advisory Bodies to define the
themes, and then the missions to be implemented, to
achieve the selected scientific goals. While the last
2 years were devoted to implementing a previously
approved programme under increasingly difficult
budgetary circumstances, we can now look into the
future for new targets and science. Of course, we are still
not clear of the problems with the current programme,
but we certainly have to start the discussion on what
missions should be launched in little more than 10 years
from now, in order to keep a stable European
contribution to space science.
The way to define and implement missions is also
changing considerably. For example, the use of themes,
rather than the usual call for ideas, is allowing us to study
new technologies not constrained by existing studies or
projects and to look for the actual scientific needs in the
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introduction
reference decade instead of trying to just do ‘more of the
same’. In particular, SCI-A is responsible for the
assessment of all future missions within the Directorate
and is therefore closely linked to RSSD and the
technology development activities. In the implementation of missions, lessons learnt have been introduced
together with a more systematic risk analysis for each
mission. In particular, for the Department’s domain, the
design and implementation of science operations has
become more pro-active and new ideas will have to be
implemented in the next years to ensure a more efficient
performance of the operation of planetary missions.
Concerning the research activities in the Department, the
coming years will focus on the increasing recognition,
and evaluation, of the results achieved by the staff.
Another point of importance is the rapidly increasing
need to devote time to functional activities to the
detriment of the time available for research – a dangerous
situation that should be avoided. Nevertheless, research
cannot be dictated and an average allocation of 20% of
the time may not be enough for competitive science. It is
important to see how these activities develop and
whether further adjustments will be necessary in the light
of experience.
Our opportunities for the analysis of data provided by
missions in orbit are now enhanced by those offered by
SMART-1, Mars Express, the arrival of Cassini at Saturn
and the very recent entry of the Huygens probe into the
atmosphere of Titan. In astronomy, the data exploitation of
successful missions such as Integral, XMM-Newton and
HST or ground-based observatories continues, as well as
that of data archives from previous missions like ISO that
are currently being enhanced through the development of
virtual observatories. In the area of the Solar System,
research flourishes, in close collaboration with partners in
the scientific community, thanks to Ulysses, SOHO and
Cluster data. New flight instrumentation is under
development through contributions to the COROT and
STEREO missions. Finally, we have seen in the past
2 years the beginning of an effort in the area of
Fundamental Physics research that should develop further.
Scientific support activities to missions under
development or study will require close attention.
Continued efforts will be devoted to the preparation of
Herschel and Planck, which are entering critical phases
of their development, as well as to the European
contribution to JWST. On the other hand, Gaia will begin
its implementation phase and the preparation of the very
demanding science operations will require special
attention. The gravitational wave observatory LISA and
its technology mission LISA Pathfinder will require
special efforts in this emerging area of space science. In
the Solar System domain, our activities will focus on
Venus Express, to be launched in 2005. Equally, the
preparations for BepiColombo, travelling to Mercury,
and of Solar Orbiter will need to be intensified.
9
One of the important responsibilities of RSSD – the
science operations of the various scientific missions –
continues to require our full attention as well as the
further development of skills and tools to cope with an
increasingly demanding activity. The availability of
properly processed scientific data, to the full satisfaction
of the scientific community at large and valid for both
observatory-type missions, with its high pressure from
the scientific community, and PI-type missions, is a clear
objective.
For SCI-A, one of the key tasks is the technical
assessment of all future missions within the Directorate
coupled to long-term planning, both at mission level and
for technology development. Such technology planning
is assisted by a parallel Technology Research and
Development Programme.
To conclude, while the need to maintain and, where
necessary, to improve the links with the research
institutions in Member States through active cooperative
programmes remains a prime goal of the Department,
other aims for the future include the continued provision
of properly processed scientific data to the community
and support to the development of science communications and science education activities in ESA.
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2.
RESEARCH ACTIVITIES IN RSSD AND SCI-A
2.1
Introduction
2.2
High-Energy Astrophysics
2.2.1
2.2.2
2.2.3
2.2.4
Stellar coronae and star-formation regions
X-ray binaries
Galaxies and active galactic nuclei
Ground-based photon-counting studies
2.3
Optical/UV Astrophysics
2.3.1
2.3.2
2.3.3
2.3.4
2.3.5
The Helix Nebula: when opportunity knocks
Central stars of planetary nebulae
Identifying core-collapse SN progenitors
Metals in the dwarf starburst galaxy NGC 1705
Luminous IR galaxies: a key galaxy population
2.4
Infrared/Sub-millimetre Astrophysics
2.4.1
2.4.2
2.4.3
2.4.4
2.4.5
Solar System studies
Interstellar medium studies
Star formation
Stellar studies
Extragalactic studies
2.5
Solar Physics
2.5.1
2.5.2
2.5.3
2.5.4
Chromospheric oscillations
Dynamics of transition region blinkers
Comparison of blinkers and explosive events
Coronal magnetic fields
2.6
Heliospheric Physics/Space Plasma Studies
2.6.1
Energetic particles from the October/November
2003 solar events
Energetic particles in the high-latitude, highspeed solar wind
Acceleration of electrons in the auroral region
Magnetospheric observations
Examples of other associated activities within
SCI-SH
2.6.2
2.6.3
2.6.4
2.6.5
2.7
Comparative Planetology and Astrobiology
2.7.1
2.7.2
2.7.3
2.7.4
2.7.5
2.7.6
Mars research
Lunar studies
Cassini-Huygens data analysis preparation
Ground-based observations of Titan winds
Earth comparative planetology
Astrobiology
2.8
Minor Bodies
2.8.1
2.8.2
2.8.3
2.8.4
2.8.5
The MIDAS instrument on the Rosetta mission
Determination of isotopic ratios in comets
Characterisation of the new Rosetta target comet
Comet modelling
Ground-based observations of comets
2.9
Fundamental Physics
2.9.1
2.9.2
2.9.3
Interferometer design for LISA Pathfinder
A phasemeter for LISA Pathfinder
Frequency stabilisation for LISA
2.10
Research Activities in SCI-A
2.10.1
2.10.2
2.10.3
2.10.4
Development of superconducting cameras
Advanced semiconductor sensors
Development of advanced optics
Advanced instrumentation research for
planetary missions
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research activities
13
2.1 Introduction
contracts, as well as Portuguese and Spanish Trainees on
2-year grants funded by their respective nations. The
Department also hosted a number of Stagiaires for
durations of up to 6 months, as part of their research or
graduate engineering studies, as well as externally
supported research students. The scheme for Internal
Research Fellows, Trainees and Stagiaires, besides
offering training and experience at RSSD, permits a
continuous exchange and collaboration with their
institutes of origin or with their future destinations. A
number of Master or PhD theses were co-supervised by
RSSD and SCI-A staff scientists and colleagues from
academic institutes.
Research in RSSD and SCI-A is an integral part of the
activities of the scientific staff, needed to maintain and
develop its scientific skills, peer recognition and handson experience in space science. Active involvement in
research is necessary for Staff Scientists to remain part of
the community when performing their mission-related
duties.
The overall research programme is organised in thematic
research groups covering different areas in astrophysics
(high-energy, optical/UV, IR/sub-mm); solar physics,
heliospheric and space plasma physics; comparative
planetology and astrobiology; minor bodies; fundamental physics; development and exploitation of
superconducting cameras for astronomy. These topics
reflect the breadth of the Cosmic Vision programme
within the different fields related to ESA science
missions. The results of these research activities, as well
as new proposals for the following year, are reviewed
annually, and the overall RSSD research programme is
assessed by an external visiting committee every 2 years.
The activities have been influenced by the opportunities
given by the ESA Science Programme, but are
constrained by the limited time available to scientists
owing to increased workload on projects, studies and
other functional activities. In addition, in support of
future missions and long-term planning, SCI-A conducts
an independent laboratory-based Technology Research
and Development Programme in close coordination with
other Programmes of the Agency.
RSSD and SCI-A staff undertake research collaborations
with external institutes from all the Member States and
with the international community, both in instrument
development and data exploitation for ESA and
international space science missions. External
researchers have also contributed to the scientific output
of the department in the form of extended visits to RSSD
and SCI-A.
The Research Groups provide a basis for the integration
and daily research activities of Research Fellows and
Trainees, with the Chief Scientist responsible for their
overall supervision. ESA Internal Research Fellows, on
post-doctoral contracts of up to 2 years, play a major role
in the Department’s research activities. On average, some
15 internal Research Fellows are in post at any one time,
covering the large range of topics in RSSD. They are
recruited through the standard ESA process of
interviews. The excellence and publication record of
candidates, their research programme matching RSSD
research priorities, and the training opportunities at
RSSD for their future career prospects are prime
selection criteria. RSSD is also hosting a Post-Doctoral
Researcher funded through the EU European Network
collaboration scheme. The Department, together with
SCI-A, hosts Young Graduate Trainees on 1-year
Mention should also be made of the role of 20 ESA
external post-doctoral Research Fellows, funded to work
1 or 2 years in ESA Member States’ institutions. They
contribute in the building of research networking in
support of ESA missions. There are two calls per year
(applications due end of March and end of September)
covering all aspects of post-doctoral research related to
ESA activities in space science as well as Earth
observation, microgravity and human spaceflight and
space technologies.
RSSD and SCI-A scientists publish, on average, some
180 refereed papers per year (those published or accepted
in 2003 and 2004 are listed in Annex 2). They still
manage to maintain a leading role in more than a third of
their research papers, despite the functional workload in
scientific support to projects, thanks to their commitment, collaborations within research groups and with the
outside community, and the contributions by Research
Fellows.
RSSD staff organised Workshops or Symposia in support
of ESA science missions or in relation to scientific
themes or collaborative research topics (Section 4.1).
They also contributed to several coordination and
supporting tasks (Section 4.3), as well as science
communications and education activities (Section 4.4). A
programme of seminars for the Department (also open to
other interested scientists) invites external scientists to
present results or reviews over a wide range of space
science topics (Annex 3). The successful colloquia
programme presenting prestigious speakers to all ESTEC
staff continued during the reporting period (Annex 3).
Also, within a programme of internal seminars, RSSD
scientists report on their ongoing research activities or
give tutorials for their colleagues across disciplines.
The following Sections are arranged according to the
individual research lines.
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2.2 High-Energy Astrophysics
The High-Energy Astrophysics research group uses
primarily XMM-Newton observations coupled with
extensive ground-based facilities to address a wide range
of issues. Topics such as stellar physics and accretiondriven objects are the focus of the group’s attention.
2.2.1 Stellar coronae and star-formation regions
Using XMM-Newton data, Favata et al. (2004) reported
the first clear evidence for an X-ray cycle in a star other
than the Sun. During the 11-year solar cycle, the X-ray
luminosity of the Sun varies in the 0.7-2.5 keV band by
some 2 orders of magnitude, yet the X-ray luminosity of
most active stars (which have X-ray luminosity 100-1000
times greater than the Sun) is remarkably constant,
within a factor of 2 or so, across several years. A
dedicated programme has been set up to monitor, at
6-month intervals, the X-ray luminosity of the solar
analogue HD 81809, which has an X-ray activity level
comparable to the Sun (thus much lower than the typical
targets of X-ray spectroscopic observations). The results
of the first 3 years of the programme are given in
Fig. 2.2.1/1; they show that the X-ray luminosity of
HD 81809 has varied by more than one order of
magnitude in the last 2 years, and, according to the phase
of the known chromospheric cycle observed in the Ca II
H&K lines, is expected to bottom out between 2005 and
2006. The XMM-Newton observing programme
Figure 2.2.1/1: Three years of XMM-Newton
observations of HD 81890 (square symbols), together
with the Mt. Wilson observations of the Ca II
chromospheric activity index of the same star
(crosses). The very large long-term variation in X-ray
luminosity, with a maximum in mid-2002, is easily
seen. (From Favata et al., 2004).
Figure 2.2.1/2: The coronal abundances of λ And,
plotted with its measured photospheric abundances.
Note how both differ in a similar way from the solar
photospheric composition (from Sanz-Forcada et al.,
2004).
continues throughout 2005 and will be re-proposed for
each future AO, aiming to observe at least one complete
cycle (HD 81809 has a chromospheric cycle duration of
8.2 years).
Chemical abundances of the coronal plasma in active
stars are an ongoing subject of debate. The discovery
from early ASCA spectra that the coronal plasma does
not have the composition of the solar photosphere (with
generally lower abundances reported) sparked a long
discussion about the actual abundance patterns and the
possible fractionation mechanisms. Progress has,
however, been hampered by the lack of photospheric
abundances for most active stars – the only stars
sufficiently X-ray bright for their high-resolution X-ray
spectrum to be observed and coronal abundances
derived. A long-term programme to determine both the
photospheric and coronal chemical abundances of
individual active stars is being carried out in RSSD in
collaboration with a number of institutions. The most
recent results (Fig. 2.2.1/2) come from the analysis of
XMM-Newton and Chandra high-resolution spectra of a
number of active stars (Sanz-Forcada et al., 2004). This
has shown that, in a number of specific cases, the coronal
abundances, which would be very different to solar
photospheric abundances, are actually very similar to
their stellar photospheric abundances. However, these
RS CVn-type active binary stars have themselves rather
strange photospheric abundances (Morel et al., 2004).
The structures of the coronae in active stars and their
comparison with the solar corona, the only spatially
resolved corona we can observe, have been open
questions since the beginning of imaging X-ray
astronomy. The advances in both collecting area and
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spectral resolution brought by XMM-Newton and
Chandra have allowed new statistics to be exploited,
namely the rotational modulation of spectral Doppler
shifts and of the global X-ray luminosity. Hussain et al.
(2005) studied the prototypical young main sequence star
AB Dor with a long Chandra LETG observation, and
found significant modulation in both the Doppler
velocity of the O VIII coronal line (with an amplitude of
about 60 km/s) and in the X-ray luminosity (at the 1015% level). This implies a highly non-homogeneous
corona, with the X-ray emission dominated by a small
number of compact emitting regions located at high
latitudes. These observations also rule out a corona
composed of very big magnetic loops (significantly
larger than the star itself), which were in the past thought
to be present on very active stars.
The origin of the observed strong X-ray activity in
intermediate mass young stars (Herbig Ae/Be stars,
HAeBe in short) remains a puzzle: these stars are not
expected to have a convective zone sustaining a dynamo,
and their winds are thought not to be energetic enough to
generate the observed X-rays through a wind shock
mechanism (thought to be the origin of the X-ray
emission observed in the more massive O and early B
stars). In a number of cases, low-mass companions have
been discovered to be the origin of the observed X-rays;
however, there remains a significant number of
apparently single HAeBe stars. Combining XMMNewton and Chandra data, Giardino et al. (2004) have
for the first time detected flaring activity from an
apparently single HAeBe star, V892 Tau. The
characteristics of the flares, one of which has a peak
temperature of around 90MK, require the plasma to be
magnetically confined, ruling out classical wind shock
models (in which the plasma is essentially unconfined).
While the origin of the magnetic field is still unclear,
detailed analysis of the flares constrain the magnetic field
at around 500 G.
15
Figure 2.2.2/1: XMM-Newton EPIC pn residuals
when the best-fit model is fitted to XB 1254-690
spectra for observations when a deep dip is present
(2001 Jan) and no dipping is evident (2002 Feb). The
absence of any overall change in absorption line
properties indicates that their presence is not related
to the presence, or absence, of dips.
from MXB 1659-298, GX 13+1 and 4U 1624-49. In the
last 2 years, these results have been extended by
observations of two more dip sources, XB 1254-690
(Boirin & Parmar, 2003) and XB 1916-053 (Boirin et al.,
2004). Ongoing analysis of all the dip sources observed
by XMM-Newton is allowing their global properties to
be investigated.
2.2.2 X-ray binaries
During Exosat observations, the LMXB XB 1254-690
exhibited irregular dips in X-ray intensity that repeated
every 3.88 h. The dips are almost certainly due to
obscuration in the thickened outer regions of an
azimuthally structured accretion disc. One of the
peculiarities of this source is that, during some
observations, deep (up to 80%) dipping is present but in
others it is completely absent, while the overall X-ray
intensity is unchanged. During an XMM-Newton observation in January 2001 a deep X-ray dip was seen while,
true to form, in a second observation a year later no dips
were evident. The 0.5-10 keV EPIC spectra from both
non-dipping intervals were very similar, being modelled
by a disc-blackbody and a power-law continuum with
additional structure around 1 keV and narrow absorption
features at 7.0 keV and 8.2 keV that are identified with
the K-alpha and K-beta absorption lines from H-like Fe.
The low-energy structure may be modelled as a 175 eVwide emission line. The absorption line properties show
no obvious dependence on orbital phase and are similar
in the two observations (Fig. 2.2.2/1), suggesting for the
first time that the occurrence of such features is not
directly related to the presence of dipping activity.
The outstanding spectral resolution and sensitivity of
XMM-Newton continues to be exploited to investigate
narrow absorption features in low-mass X-ray binaries
(LMXBs). In the previous report, results were reported
The discovery of narrow Mg XII, Fe XXV and Fe XXVI
K-alpha X-ray absorption lines in the persistent emission
of the dipping LMXB XB 1916-053 during an XMMNewton observation in September 2002 has been
References
Favata, F., Micela, G., Baliunas, S.L. & Schmitt,
J.H.M.M., 2004, A&A 418, L13.
Giardino, G., Favata, F., Micela, G. & Reale, F., 2004,
A&A 413, 669-679.
Hussain, G.A.J., Brickhouse, N.S., Dupree, A.K. et al.,
2005, ApJ 621, 999.
Morel, Th., Micela, G., Favata, F., Katz, D. &
Pillitteri, I., 2004, A&A 412, 495.
Sanz-Forcada, J., Favata, F. & Micela, G., 2004, A&A
416, 281.
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consistent with a decrease in the amount of ionisation, as
dipping activity progresses. This implies the presence of
cooler material in the line of sight during dipping,
consistent with the decrease in energy of the Fe feature as
dipping becomes more intense (Fig. 2.2.2/2). The
discovery of a 0.98 keV absorption edge in the persistent
emission spectrum is also reported. The edge energy
decreases to 0.87 keV during deep dipping intervals. The
detected feature may result from edges of moderately
ionised Ne and/or Fe, with the average ionisation level
decreasing from persistent emission to deep dipping.
This is again consistent with the presence of cooler
material in the line of sight during dipping.
References
Boirin, L. & Parmar, A.N., 2003, A&A, 407, 1079.
Boirin, L., Parmar, A.N., Barret, D., et al., 2004, A&A
418, 1061.
2.2.3 Galaxies and active galactic nuclei
The X-ray emission from advection-dominated accretion
flows in the elliptical galaxy NGC 3226 has been studied
(Gondoin et al., 2004)). The continuum can be described
by a bremsstrahlung model absorbed by neutral material.
The absence of variability suggests that the emission
originates from regions relatively far from the nucleus.
Based on luminosity considerations, the mass of the
central accreting black hole is be constrained to be 1.750x107 solar masses.
Figure 2.2.2/2: The variation in the Fe absorption
feature seen from XB 1916-053 during dipping
intervals. The energy of the feature is indicated by
vertical tick marks. The mean energy of the feature
decreases with increasing dip depth, consistent with
the presence of increasingly cooler material.
reported (Boirin et al., 2004). Such absorption lines from
highly ionised ions are now observed in a number of
high-inclination (close to edge-on) LMXBs, such as
XB 1916-053, where the inclination ranges between 60°
and 80°. This, together with the lack of any orbital phase
dependence of the features (except during dips), suggests
that the highly ionised plasma responsible for the
absorption lines is located in a cylindrical geometry
around the accretion disc. Using the ratio of Fe XXV and
Fe XXVI column densities, the photo-ionisation
parameter was estimated to be 103.92 erg cm/s. Only the
Fe XXV line is observed during dipping intervals and the
upper-limits to the Fe XXVI column densities are
The first systematic investigation of magnetic fields in
barred spiral galaxies is now complete (Harnett et al.,
2004; Beck et al., 2002). The radio surface brightness is
found to be highest in galaxies with a long bar. The
derived regular magnetic fields are significantly different
from those in non-barred galaxies, allowing new
constraints to be placed on dynamo-models. Individual
follow-up studies (including a comparison with X-ray
observations) are continuing.
XMM-Newton observations of nearby star-burst galaxies
have been analysed as part of a multi-wavelength
investigation of all phases of the extra-planar interstellar
medium (Ehle et al., 2004; Dahlem et al., 2003). This
study was conducted in order to assess the importance of
haloes as repositories of a metal-enriched medium and
their significance in terms of galactic chemical evolution.
The common goal of the multi-wavelength (X-ray, radio
continuum, H I and optical) project is to obtain a better
understanding of star-formation related outflows. The
galaxy NGC 4666 (Fig. 2.2.3/1) is an example of the
observed interplay between X-ray and optical filaments,
star-formation regions in the underlying disc, and the
magnetic field structure.
Analysis of XMM-Newton’s observation of the Seyfert 1
galaxy ESO 141-G55 has revealed, in addition to an Fe
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Newton observation of Mkn 304 (Piconcelli et al., 2004),
it seems likely that such absorbers are characteristic of
X-ray weak quasars in general. They are different from
the warm absorbers found commonly in AGNs that show
much lower column densities and ionisation parameters.
The X-ray spectrum of PG 1535+547 shows a relativistic
Fe K-alpha disc line from fluorescence emission and is
therefore only the second X-ray weak quasar with such
an unusual characteristic. The occurrence of a variable
relativistic Fe K-alpha fluorescence line in two out of the
five well-studied X-ray weak quasars may indicate that
such features are more common in these systems.
Figure 2.2.3/1: A pn-MOS 0.5-0.9 keV image of NGC
4666 overlaid on an H-alpha and N II optical narrowband image. In the halo, the most extended optical
emission line filaments, which form an X-shaped
structure, reach out to distances above the plane by
up to ~7.5 kpc. Vectors mark the orientation of the
magnetic field observed at 4.89 GHz with the VLA;
their lengths are proportional to the polarised
intensity.
K-alpha fluorescence line (equivalent width of ~40 eV),
an absorption edge at 7.6±0.1 keV (Gondoin et al.,
2003a). Similar results have been obtained for the
Seyfert 1 galaxy NGC 3227 by Gondoin et al. (2003b).
At soft energies, the spectrum of NGC 3227 shows
strong continuum absorption of 6.5x1022/cm2.
XMM-Newton spectra of 40 quasars with redshifts
< 1.72 from the Palomar-Green Bright Quasar Survey
sample have been analysed (Piconcelli et al., 2005;
Jimenez-Bailon et al., 2004). The hard X-ray continuum
emission > 2 keV can be modelled by a power-law with
mean 2-12 keV photon index of 1.89±0.11. Below 2 keV,
a strong broad excess is present in most spectra, for
which it is impossible to find an universal spectral shape.
Warm absorber features are present in around half of the
sources, in contrast to their rare occurrence (~5-10%) in
previous studies. The XMM-Newton view of opticallyselected bright quasars therefore suggests that there is no
significant difference in their X-ray spectral properties
when compared with low-luminosity Seyfert 1 galaxies.
Three X-ray weak quasars observed with XMM-Newton
have been studied (Schartel et al., 2004). All three
objects are absorbed by ionised material with high
column densities and ionisation parameters. In
combination with the similar result from the XMM-
The discovery of two new occurrences of extreme
variations in the column density obscuring nearby AGN
has been reported (Guainazzi et al., 2004). The typical
timescale of these phenomena is ~50 yr. This provides
further support to a scenario in which gas associated with
the host galaxy, or with dense regions of enhanced star
formation, is responsible for obscuration in 50% of the
AGN in the nearby Universe, which is inconsistent with
the predictions of the standard AGN Unification model.
The ongoing investigation of the star-formation
processes in the nuclei of spiral galaxies has been
expanded. Following up on the previous Hubble Space
Telescope survey of nuclear star clusters, Boeker and
collaborators (Boeker et al., 2002) have used an isophotal
analysis to demonstrate that many late-type spirals are
indeed ‘pure’ disc galaxies in that they show no evidence
for a spheroidal bulge component. The team has then
used the IRAM 30 m telescope to search for molecular
gas in the central kpc of 47 bulge-less spirals in order to
measure the fuel reservoir available for nuclear star
formation. The results demonstrate that a large fraction
of galaxies contain enough gas in the vicinity of the
nucleus to sustain at least a few modest (about 105 solar
masses in new stars) star-burst episodes. This is
consistent with scenarios that invoke nuclear cluster
growth through repetitive star-bursts. The challenge then
is to explain how the gas can lose its angular momentum
and be funnelled to within a few pc of the galaxy nucleus.
In order to advance observations at this level of detail,
Boeker and collaborators have performed a detailed case
study of IC342, a nearby, late-type spiral with a
prominent nuclear star cluster. Their observations with the
Owens Valley Radio Interferometer revealed a molecular
disc that coincides with the nuclear star cluster and has a
radius of only 15 pc. This demonstrates that molecular gas
can indeed accumulate on such scales, making repetitive
nuclear star-bursts a plausible scenario.
References
Beck, R., Shoutenkov, V., Ehle, M. et al., 2002, A&A
391, 83.
Boeker, T., Laine, S., van der Marel. R. et al., 2002, AJ
123, 1389.
Dahlem, M., Ehle, M., Jansen, F. et al., 2003, A&A 403,
547.
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Ehle, M. & Dahlem, M., 2004, Mem. S.A.It. 75, 515.
Gondoin, P., Orr, A. & Lumb, D., 2003a, A&A 398, 967.
Gondoin, P., Orr, A., Lumb, D. & Siddiqui, H., 2003b,
A&A 397, 883.
Gondoin, P., Orr, A. & Siddiqui, H., 2004, A&A 420, 905.
Guainazzi, M., Rodriguez-Pascual, P., Fabian, A.C.,
Iwasawa, K. & Matt, G., 2004, MNRAS 355, 297.
Harnett, J., Ehle, M., Fletcher, A. et al., 2004, A&A 421,
571.
Jimenez-Bailon, E., Piconcelli, E., Guainazzi, M. et al.,
2004, A&A, in press.
Piconcelli, E., Jimenez-Bailon, E., Guainazzi, M., et al.,
2004, MNRAS, 351, 161.
Piconcelli, E., Jimenez-Bailon, E., Guainazzi, M. et al.,
2005, A&A 432, 15.
Schartel, N., Rodriguez-Pascual, P.M., Santos-Lleo, M.
et al., 2005, A&A 433, 455.
2.2.4 Ground-based photon-counting studies
The SCI-A technology development programme in
superconducting detector arrays is being exploited within
RSSD. This technology allows for optical photon
counting with high efficiency, high time resolution, and
photon energy determination, and has been under
development for several years. It was last used at the
William Herschel Telescope on La Palma in October
2000, resulting in several publications mainly related to
the determination of light curves and physical conditions
in magnetic Cataclysmic Variables. Papers dealing with
temperature determination, and quasar redshift determination, both using the energy-resolved capabilities of the
device, have also been published over the last 3 years.
The array was recently upgraded from a 6x6 array
(S-Cam2) to a 10x12 array (S-Cam3), and operated again
at the WHT for six nights in July 2004.
The datasets arising from the S-Cam instrument are
complex to analyse and interpret. In addition to the issues
of photometric stability and calibration of normal CCD
cameras (e.g. atmospheric extinction and zenith angle
variations) access to the photon arrival times means that
the resulting datasets include time-dependent effects
(seeing and sky background variations, as well as timedependent differential atmospheric refraction, small
amplitude telescope oscillations during short periods of
high wind speed, etc) which must be calibrated as part of
the pipeline processing. Detector and electronics
enhancements made in the development from S-Cam2 to
S-Cam3 have resulted in a very stable instrument.
A number of different observing programmes, granted
through the Netherlands time allocation panel, have been
undertaken. Eclipse mapping of three CVs was carried
out in a programme led by P. Groot (Nijmijgen). Twelve
successive cycles of the 12-min period ultra-compact
binary RX J1914+24 were obtained (in a collaboration
with G. Ramsay and M. Cropper at MSSL), showing
research activities
Figure 2.2.4/1: The amplitude of the 10-min orbiter
binary RX J1914+24, observed with S-CAM3 in July
2004. Immediately apparent in the colour ratio
(bottom panel) are not only the amplitude variation
with orbital phase but also the colour dependency of
the amplitude. Observations were made in
collaboration with Cropper & Ramsey, MSSL (UK).
very nice amplitude and colour modulation at the
expected period. A series of exploratory observations of
pulsating white dwarfs and polar QPOs were undertaken
with R. Kotak (Imperial College, London). The high time
resolution of the photon arrival time datation (of order a
few microseconds) makes the device well suited to the
long-running search for further optical counterparts of
radio pulsars: one millisecond pulsar and two normal
pulsars were observed, under good photometric
conditions, with good reference astrometry allowing the
expected position of the pulsar to be well centred on the
array. Preliminary estimates of the limiting magnitude of
these observations, assuming a 10% pulsar duty cycle,
are at around V = 26.
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2.3 Optical/UV Astrophysics
The optical/UV astrophysics research group has relied
primarily on HST observations complemented by
ground-based facilities to study a wide range of objects,
including classical nebulae, the central stars of planetary
nebulae, star formation in starburst galaxies and
luminous IR galaxies.
2.3.1 The Helix Nebula: when opportunity knocks
The Helix Nebula (NGC 7293) lies about 600 ly away in
Aquarius and has a diameter of about 2.4 ly, thus
spanning as much as 14 arcmin. A substantial portion of
the Helix has been imaged in two colours, using both
ACS and WFPC2 by N. Panagia and collaborators.
Fig 2.3.1/1 shows an image made by combining the new
images from the HST-ACS and wide-angle images from
the Mosaic Camera on the WIYN 0.9 m Telescope at Kitt
Peak National Observatory. This is one of the largest and
most detailed celestial images ever made.
These HST observations were made possible by a
fortuitous combination of events. One of the most
prominent meteor showers is the Leonids each
November. The shower in 2002 was predicted to be
especially rich and since those meteoroids pose a nonzero risk to spacecraft, HST had to carry out a special
procedure to minimise the risk and any consequences. As
in the past several years, HST was required to point in a
particular direction during the meteor shower in order to
keep the telescope’s aft end towards the stream, while
minimising the cross-section of the solar arrays. This
stand-down period was from 0 h to 14 h UT on 18
November 2002. In preparing for this special effort, it
was noticed that just outside the nominal pointing region
lay the Helix Nebula, which had been imaged by Hubble
in some small areas but never in its entirety. This was too
good an opportunity to miss! The HST Project at
Goddard Space Flight Center was immediately contacted
and their concurrence in using HST slightly beyond its
nominal pointing area was secured. Thus, it became
possible to devote nine orbits of HST observing time to
imaging a substantial portion of the large Helix Nebula in
two colours, using both ACS and WFPC2, obtaining the
most detailed image ever of it. Apart from its outstanding
beauty, such an image is also extremely valuable because
it is a high-quality first-epoch dataset that is ideally
suited for later work on measuring the motions of the
tight knots immersed in the nebula.
2.3.2 Central stars of planetary nebulae
Stellar evolution predicts that stars in the range 1-8 solar
masses will lose most of their stellar envelopes through
mass-loss as they ascend the Asymptotic Giant Branch
(AGB) phase. It is the mass-loss that establishes the mass
Figure 2.3.1/1: The Helix Nebula seen by combining
the new images from the HST-ACS and wide-angle
images from the Mosaic Camera on the WIYN 0.9 m
telescope at the Kitt Peak National Observatory.
boundary between those stars that will evolve off the
AGB phase into Planetary Nebulae (PNe) and ultimately
fade into white dwarfs, and those that will end their lives
as type II Supernovae.
Studies of Central Stars (CSs) of PNe in the Galaxy are
hampered by the poor knowledge of their distances, a
problem that can be overcome by observing PNe in the
Magellanic Clouds (LMC and SMC; Fig. 2.3.2/1). From
ground-based observations, the unresolved nature of the
nebula has, however, so far prevented us from taking full
advantage of a known distance in the determination of
the CS parameters. As a result, most ground-based
studies have had to rely heavily on photoionisation
modelling of the nebula in order to derive these CS
parameters.
HST offers a unique opportunity to study the CSs of PNe
in the Magellanic Clouds with unprecedented accuracy,
largely because the stellar continuum can be measured
directly. Villaver and collaborators have determined
accurate masses of CSs of PNe for the two largest
samples of extra-galactic PNe ever studied, and have
explored the connections among the fundamental
properties of the stars and the physical properties of the
host nebulae (Villaver et al., 2003; 2004). Similar
average masses in the LMC and SMC have been
established as well as an indication of a difference in the
mass distribution of the two samples that cannot be
explained by a mass-loss rate dependency with
metallicity. As the immediate precursors of white dwarfs,
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Figure 2.3.2/1: A sample of HST (50 CCD STIS bandpass) images of LMC Planetary Nebulae. From left to right:
SMP 4, SMP 10, SMP1 8, SMP 102. The field of view is 3 arcsec and the intensity scale is logarithmic.
the study of the mass distribution of the CSs of PNe
should help to constrain the initial-to-final mass relation
within environments of differing metallicity.
2.3.3 Identifying core-collapse supernovae
progenitors
With the only exception of type SN Ia, theory predicts
that all other types of supernovae arise from the collapse
of the core of a massive evolved star that exhausts its
nuclear fuel and cannot generate enough energy to
support itself. After the explosion of one of these corecollapse supernovae, a neutron star or a black hole is all
that remains of the progenitor star. However, there are
very few observations of the SN progenitors that can be
used to confirm the theoretical predictions regarding
their nature. Until 2003, only two SN had had their
progenitors unambiguously identified: SN 1987A and
SN 1993J. The situation changed that year, when HST
played a decisive role in the identification of two new
progenitors and in the gathering of new information on
one of the previous two.
A combination of pre-explosion HST/WFPC2 and
Gemini/GMOS images and post-explosion HST/ACS
images have been used to identify the progenitor of the
Figure 2.3.3/1: Three-colour ACS/HRC mosaic (red:
F330W, green: F250W, blue: F220W) of the region
around the cluster Sandage 96 in NGC 2403, where
SN 2004dj took place, obtained 2 months after the
explosion. The field is 90 pc on each side, with north
towards the top. The central extended object is the
cluster itself (blue owing to the blue giants and
supergiants) while the reddish point source is the SN
located about 1 pc to the south of the centre of
Sandage 96.
type II-P SN 2003gd (Smartt et al., 2004). They found
that the star was an 8 solar-mass red supergiant, which is
consistent with the models of single stellar evolution.
Ground-based data from several telescopes have
identified that the type II-P SN 2004dj took place in a
14 Myr-old, 24 000 solar-mass stellar cluster that
included a number of red and blue supergiants (MaizApellaniz et al., 2004). Post-explosion HST/ACS images
obtained by Filippenko et al. were able to resolve the
supernova and the surrounding cluster (Fig. 2.3.3/1).
Images of the location of SN 1993J with HST/ACS have
been obtained that allowed the identification of a bright
blue star that could have been the companion of the
previously red supergiant that exploded (Maund et al.,
2004). The existence of such a companion had been
predicted by the theoretical models that had been
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advanced to explain the peculiar evolution of the SN,
which started out as a hydrogen-rich type II to later
transform into a helium-rich type Ib.
2.3.4 Metals in the dwarf starburst galaxy
NGC 1705
NGC 1705 is one of the most intriguing nearby objects.
At a distance of 5 Mpc, it is a dwarf galaxy that is
experiencing intense star formation, a so-called starburst.
As a result, it hosts in its centre a compact and massive
young star cluster and shows evidence of a spectacular
large-scale outflow triggered by the simultaneous
explosion of a myriad of SNe II. The extreme physical
conditions of starbursts like NGC 1705 must have been
much more common in the past, making them crucial
targets against which observations of higher-redshift
galaxies must be compared.
21
the starburst environment. What we observe could thus
be the result of either chemical pollution of the medium
closely surrounding the starburst or a metallicity gradient
from the inner metal-rich galaxy to an outer metal-poor
halo. The metal offset between the neutral and ionised
ISM has important implications for the chemical
evolution of dwarf starburst galaxies, since it implies that
widespread enrichment episodes have preceded the
current burst that dominates the bolometric luminosity of
these systems. A potential scenario is one where star
formation dates quite far back in the past, allowing the
metals to be produced in the most central regions and
efficiently dispersed in the surrounding neutral gas of the
halo. The ISM non-homogeneity may also imply a larger
loss of metals via galactic winds than previously thought,
thus favoring ‘bursty’ over low-level quasi-continuous
star formation.
2.3.5 Luminous IR galaxies: a key galaxy population
Dwarf starburst galaxies are characterised by a large
reservoir of neutral gas. This is a fundamental ingredient
for the star-formation onset, but it is also the place where
most of the baryons may hide. A. Aloisi and
collaborators have studied the neutral ISM of NGC 1705
by analysing the absorption lines detected in highresolution UV spectra of its central cluster. The synergy
between the complementary spectral ranges of the
HST/STIS and FUSE data used in this project has
allowed for the first time the issues involved in this type
of analysis (e.g., saturation, ionisation and depletion) to
be tackled. The study shows that the metals abundance in
the neutral gas of NGC 1705 are lower than in the ionised
gas of the H II regions probed via optical nebular
spectroscopy. This intriguing result unambiguously
indicates that the ISM in dwarf star-forming galaxies is
not homogeneous as previously suggested and usually
assumed in chemical evolution models, and may imply
the existence of a lower metallicity halo that surrounds
Luminous IR Galaxies (LIRGs) are believed to be very
common in the distant Universe, and are probably the
local counterpart of the sub-mm galaxies that give rise to
the far-IR background. The physical processes at work in
LIRGs (mergers of galaxies, dust-shrouded massive
starbursts, AGN formation, outflows, enrichment of the
intergalactic medium, etc) are likely to be the same as in
young galaxies in the early Universe. Therefore, they are
natural laboratories for understanding these processes in
detail, providing a local reference to high-z galaxy
population studies.
A project aimed at studying the internal structure and
kinematics of a representative sample of LIRGs is
underway. This study is based on Integral Field
Spectroscopy (IFS) using the 4.2 m William Herschel
Telescope and HST imaging (WFPC2 and NICMOS).
These two techniques are ideal and complementary to
study the complex physical and kinematics properties of
these objects. The analysis is mainly based on the rest
frame optical spectral diagnostic features (and near-IR
morphologies), which will be shifted towards longer
wavelengths in the high-z galaxy populations to be
studied with JWST. Furthermore, the linear resolutions to
be obtained with JWST for high-z populations are
coarsely of the order of those now obtained from the
ground for local LIRGs.
Figure 2.3.5/1: HST/NICMOS (K-filter) image of the
ultra-luminous IR galaxy IRAS 17208-0014, likely a
merging of two galaxies in its final dynamical phase.
The iso-contours indicate the ionised gas (H-alpha)
velocity dispersion map (top) and velocity field
(bottom) obtained with the fibre system on the 4.2 m
WHT.
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Figure 2.3.5/1 presents the ionised gas (Hα) velocity
dispersion map and velocity field of IRAS 17208-0014
(iso-contours), together with the near-IR image obtained
with HST/NICMOS (Arribas & Colina, 2003). It is
interesting to note that the peak of the velocity dispersion
map is centred on the near-IR continuum maximum,
which indicates that for this galaxy the velocity
dispersion seems to be a good mass tracer. Furthermore,
the velocity field has a pattern compatible with rotation,
with its kinematical centre in positional agreement with
the nucleus. This is a surprising result and differs from
those obtained for most of the objects studied so far,
where the velocity fields are rather dominated by tidal
induced forces. If velocity fields do not show rotation
they cannot be used for obtaining dynamical masses, a
key observational parameter for testing the hierarchical
models of galaxy formation and evolution – these models
predict an increase of galaxy masses over cosmic time. If
velocity fields cannot be used for inferring dynamical
masses, such models have to be tested by more indirect
techniques.
References
Arribas, S., Colina. L., 2003, ApJ 591, 791.
Maiz-Apellaniz, J. et al., 2004, ApJL (10 November 2004
issue).
Maund, J.R. et al., 2004, Nature 427, 129.
Smartt, S.J. et al., 2004, Science 303, 499.
Villaver, E., Stanghellini, L. & Shaw, R.A., 2003, ApJ
597, 298.
Villaver, E., Stanghellini, L. & Shaw, R.A., 2004, ApJ
614, in press.
research activities
2.4 Infrared/Sub-millimetre Astrophysics
The research group continues to utilise the ISO archive
extensively to further its research interests in a wide
range of astronomical topics, ranging from Solar System
studies to analysis of deep fields.
2.4.1 Solar System studies
Salama, together with Coustenis et al., has continued the
analysis of the ISO Titan data taken by the SWS
instrument. The near-IR spectra of Titan show several
weak CH4 absorption regions, in particular centred near
2.75 µm. Owing to interference from telluric CO2
absorption features, only part of this region (2.9-3.1 µm)
has been observed from the ground. ISO observations
show the 2.75 µm window in its full shape for the first
time. Using a detailed microphysical model of Titan’s
atmosphere, information on the atmospheric parameters
(haze extinction, single scattering albedo, tholin
refractive index, etc.) has been derived by fitting the
methane bands. From the derived surface albedo
spectrum around 2.75 µm, some constraints on Titan’s
surface composition were determined. ISO data appear to
be compatible with H2O and CO2 ices.
2.4.2 Interstellar medium studies
Work has progressed on the study of the dust emission of
the interstellar medium of our Galaxy with balloon-borne
sub-mm data (Dupac et al., 2003a) as well as with largescale space-borne measurements. In addition, the dust
emission of the NGC 891 galaxy was studied (Dupac et
al., 2003b). This research was performed in collaboration
with the Cold Universe group of CESR in Toulouse (F).
In addition, the analysis of the Archeops balloon-borne
experiment data, notably concerning the first detection of
polarisation of the submillimetre dust emission (Benoit et
al., 2004) and the measurement of the dust temperaturepolarisation spectrum is ongoing. This work includes the
measurement of the harmonic spectrum of the Cosmic
Microwave Background fluctuations. In addition, in
preparation for the Planck satellite operations phase,
simulations of different scanning strategies for the
cosmic microwave background is underway (Dupac &
Tauber, 2005). Studies continue with CESR (Toulouse)
into the gas/grain interaction in quiescent-dense interstellar medium (a filament in Taurus), using molecular
lines and continuum tracers.
Studies of the dust properties in nine interstellar regions
have also been fruitful, mostly from ISO observations at
60-200 µm (del Burgo et al., 2003), where an increased
far-IR emissivity was observed in big dust grains (15110 nm) towards low temperatures. The relative
abundance of very small grains (1.2-15 nm) with respect
to the big grains shows significant variations from region
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Figure 2.4.2/1: CVF observation of the M31 bulge.
Top: corrected images at 6 µm and 11.3 µm and, for
comparison, the uncorrected 11.3 µm image. Bottom:
spectrum of the M31 bulge obtained by linearly
correlating the smooth radial gradient of the bulge
emission at each wavelength with that measured at
6 µm (left), and the spectrum of the dust clouds that
can be seen in the images (right).
to region at low column densities. Along lines of sight of
higher column density, the data indicate the disappearance of small grains. These results can be interpreted in
terms of coagulation of dust. The larger size and porous
structure of grains could explain the increased far-IR
emissivity. The far-IR emission from large grains in
Taurus has been separated into warm and cold
components, from which the temperature and optical
depth of the components was determined and compared
with the properties of the molecular gas. In addition,
characterisation of the cirrus structure over the 90200 µm wavelength range continues (Kiss et al., 2003).
proto-Oort cloud at distances of several tens of thousands
of AU from the binary.
Improvements in the data reduction of the ISOCAMCVF have been made that were motivated by the goal of
analysing extended emission data in less excited regions
of the sky. The key features of the new data process are
the subtraction of the zodiacal emission and the
associated straylight, the improvement of the wavelength
calibration, and the astrometry. The scientific information that can be now extracted from the data is greatly
enhanced for the large number of observed fields with
extended emission fainter than the zodiacal light. Thanks
to all these corrections, reliable spectrum and spatial
structure of extended objects can be extracted. The
results of the improved pipeline have been made
available for public use in the ISO archive.
As part of the GLIMPSE legacy team of the NASA
Spitzer Space Telescope, a survey has been conducted of
parts of the Galactic Plane in four IR wavebands between
3.6 µm and 8 µm. The early results of protostars in the
Elephant Trunk Nebula and the discovery of a distant
star-formation region have been published by Reach et
al. (2004) and Mercer et al. (2004), respectively.
2.4.3 Star formation
The investigation of the star-forming system in L1551
has continued. It is now clear that the inner parts of this
proto binary (class 0/1) is surrounded by a massive
(> several solar masses) disc, from which the outflow
lifts off. Aspects of the shocks within the outflow are
being investigated, particularly with respect to the
recently discovered X-ray source. In addition – for the
first time – methanol from the outer edges of this disc has
been detected, which suggests that it could be due to a
Analysis of a sample of high-luminosity star-forming
regions observed by ISO LWS indicate they are
characterised by strong far-UV stellar fields causing
atomic ionisation. This work has shown how photoionisation models can explain the observed fine structure
line luminosities and where other components, such as
photodissociation emission and shock excitation by
outflows, have to be included to account for the observed
spectra.
Two research projects concerning low-mass brown
dwarfs and planetary-mass objects in star-forming
regions are also underway. The first is based on very
deep ISOCAM images of the Taurus molecular cloud.
The IR excess from the circumstellar disc of the forming
stars is commonly used to identify young stars. It has
been found that, in contrast to previous studies in which
the presence of galaxies in the field was not taken into
account, the galaxies dominate the detections at these
low flux-levels. These results have ramifications for the
interpretation of the deep images of star-forming regions
acquired by the Spitzer Space Telescope.
The second project compares two different methods for
identifying young stars. In general, mid-IR studies yield
a higher fraction of low-mass stars when compared to
optical and near-IR surveys. The questions addressed are:
‘What is the cause of this discrepancy?’ and ‘Which
method gives the best measure of the true fraction of
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low-mass objects?’. Highly embedded regions (i.e.
regions with very recent star formation) are best studied
in the mid-IR because of the large extinction. This
extinction may cause a strong bias in optical studies. For
older regions, optical surveys bring the advantage of
increased sensitivity and higher spatial resolution. The
Chamaeleon star-forming region is the ideal intermediate
in which both methods have been applied. The candidate
lists from both mid-IR (ISOCAM) and near-IR surveys
have been compared. They find that the effects of
extinction in the optical are minimal and only a few stars
in the very densest part are undetected in the near-IR
survey.
Investigations into aspects of the process of star- and
solar system-formation have continued. High-resolution
spectra have been obtained with the VLT/UVES
combination of the Beta Pictoris disc. The data maps the
gas distribution within the gas disc in more than 70
absorption lines, demonstrating the warping of the disc.
Gas can be traced from the inner parts out to more than
400 AU. The origin of the gas remains unclear; the
investigation clearly shows that the gas is not
accelerating outwards as it should do, given the radiation
pressure. An unseen molecular component may hold the
atomic gas in place.
2.4.4 Stellar studies
A local interface dynamo model has been developed in
order to reproduce the activity cycles of about 30 Suntype stars, which have been detected by monitoring,
since 1966, the photometric variation in two bands
centred in the Ca II H and K lines. The local model splits
the dynamo equations into two systems, the first for the
overshoot region where the strong toroidal field is
assumed to be produced by the internal differential
rotation, and the second for the base of the convection
zone where the so-called alpha-effect produces the
poloidal field. The model includes some new features,
such as the refraction of the magnetic waves from the
overshoot region to the convection zone, and the scaling
of the width of the shear layer where the differential
rotation is concentrated in the Sun. The observed trends
in the magnetic cycle and rotation periods are well
reproduced by the model. The dependence of the
magnetic intensites in the stellar interiors on the spectral
types, obtained with the model, agrees with that followed
by the observed surface magnetic fields.
Nova continue to be studied through the use of
observations made by ISO SWS. For CP Crucis (Nova
Crux 1996), abundance enhancements versus solar by
mass were found to be of 75, 17 and 27 for N, O and Ne,
respectively, from ISO and quasi-simultaneous groundbased observations. Additionally, the Mg abundance in
the ejecta is constrained to be approximately solar. The
nova appears to be an example of the ‘missing link’
research activities
between CO and ONeMg novae (Lyke et al., 2003). For
Nova V723 Cassiopae, the IR spectrum was dominated
in the first year by H and He recombination lines, and at
later times by coronal lines. From the H recombination
lines, electron temperature and an electron density were
derived. From the coronal lines abundance ratios of
S/Si ≈ 2.1, Ca/Si ≈ 1.6 and Al/Si ≈ 1.5 were found. The
ejected mass was also constrained (Evans et al., 2003).
ISO/SWS IR spectra of oxygen-rich AGB stars with
optically thin dust shells continue to be exploited (Heras
& Hony, 2005). The low mass-loss rate regime is of
particular interest because, owing to the low densities of
the outflow, dust condensation may not be complete and
it is possible to observe the intermediate steps in the
dust condensation sequence. The composition of the
dust and the physical conditions in the shells were
determined by modelling the SWS observations with
the radiative transfer code DUSTY. Through the
comparison with the CO observations found in the
literature, gas-to-dust ratios were calculated and the
mass-loss rates derived. The results show that, even in
the low-density environments studied, the dust
produced is enough to drive the stellar wind by
radiation pressure. The composition of the dust and its
dependence on the physical conditions at the inner shell
is consistent with the thermodynamic dust condensation
sequence. However, the temperatures derived for the
dust formation are lower than those estimated by
current theories.
ISO/SWS spectra of S stars are also now being
examined. These AGB stars have abundances between
the oxygen-rich and the carbon-rich AGB stars. Owing
to this intermediate composition pattern, the molecules
and solid components that form around such stars are
poorly known. In general, it is assumed that the solid
particles are predominantly silicates, i.e. oxygen-rich
dust. The new ISO spectra present the first-ever
detection of magnesium-sulphide grains around S stars.
Such grains are otherwise observed only in carbon-rich
environs. Furthermore, the spectra indicate that the
silicates present around these stars are systematically
different from those found around oxygen-rich AGBs.
A radiative transfer model has been developed in order
to derive physical parameters (size, distance, density) of
detached dust shells around carbon-rich AGB stars
based on their IR spectra (Hony & Bouwman, 2004).
This model was also applied to two well-studied stars
with good agreement with other methods (CO mapping
and imaging of light scattered from the dust). The new
method can be easily applied to more distant stars
where these other techniques fail. It is intended to apply
and test the new model extensively by using new
observations from the Spitzer Space Telescope in three
accepted programmes.
Studies of the dust shell around the peculiar post-AGB
object HD 56126 (Fig. 2.4.4/1) have also been
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merging of multiple observations of the same source,
about 16 500 mid-IR objects were confirmed with a
confidence level of the detection probability to better
than 99%. The catalogue will contain these sources and
associated flags like source characterisation, detection
quality and astrometric correction. The typical sensitivity
limit reached in this survey is about 1 mJy, with a median
of 3.9 mJy.
Figure 2.4.4/1: Multi-wavelength spectrum of the
post-AGB object HD 56126. The star is surrounded
by a shell of carbon-rich dust. The shell is easily
identified in the mid-IR image (top-left), while the
star itself (indicated by the star symbol) is hardly
detected. The spectrum is clearly divided in two
components; the star dominates the UV and optical
light, while all the IR radiation originates from the
dust in the shell roughly 2500 AU away. The various
dust components have been indicated.
conducted (Hony et al., 2003). From the detailed
radiative transfer modelling of the IR spectrum and
imaging, stringent constraints are placed on the
composition and physical parameters of the shell. It has
been found that the star has relatively normal dust
properties but has exhibited an atypically high mass-loss
rate.
The analysis of individual stellar sources evolving from
the AGB to the PN stage, using multi-wavelength
observations, has continued. In particular, in collaboration with A. Riera (U. Barcelona) and others, a detailed
analysis was made of the remarkable highly collimated
optical jets associated with the proto-PN Hen 3-1475
(Garden Sprinkler Nebula), interpreted as the result of
episodic mass loss by a precessing binary system. A
detailed chemical abundance analysis of the PN Me 2-1
was also carried out using a combination of ISO and IUE
data, with optical spectra taken from the literature.
Finally, two rare, new type I PNe belonging to the
Galactic Bulge population were identified as such and
studied in detail.
2.4.5 Extragalactic studies
The ISOCAM Parallel Mode observations continue to be
exploited. A 27 sq. deg. area was observed with LW2, a
broadband filter centred on 6.7 µm. The work on the
resultant point source catalogue is close to completion:
after statistical cleaning, astrometric corrections and
As a first scientific result derived from ISOCAM parallel
results, a collaboration led by Haas (Ruhr Universitaet
Bochum, D) discovered unique mid-IR excess sources.
Various arguments suggest that they likely contain an
AGN. The ongoing optical spectroscopy indicates 40%
of the sample to be classical AGN and the remaining part
to be dust-shrouded sources. A survey of mid-IR selected
AGNs was initiated to confirm this. In addition,
observing time was granted by Spitzer and TNG.
Improvements in the ISO calibration has led to further
work in the areas of the far-IR source count analysis and
luminosity function in the ELAIS fields (Heraudeau et
al., 2004; Serjeant et al., 2004) and cosmic far-IR
background (Rowan-Robinson et al., 2004).
A series of papers on the deep ISOCAM survey through
gravitationally lensing galaxy clusters has been
published. Metcalfe et al. (2003) presented the
catalogue of 7 µm and 15 µm observations of 148 midIR sources from the A370, A2218 and A2390 fields.
The fluxes of lensed background sources were
corrected for amplification to yield source counts
reaching three times deeper than other mid-IR surveys.
These counts confirmed and extended earlier findings
of a factor of ten excess of 15 µm galaxies compared to
models with no evolution. Most sources occur at
0.4 < z < 1.5 with median ~0.6, and resolve the bulk of
the cosmic mid-IR background.
Clusters of galaxies have also been studied (Biviano et
al., 2004; Coia et al., 2005a; 2005b) based on archival
and published data to investigate the properties of
clusters of galaxies over a range of redshift
(0.18 < z < 0.4). Clusters A2219, Cl0024+1654 and
A1689 were included, for a total sample of about 75
cluster sources, constituting a substantial fraction of the
ISO results on galaxy clusters beyond Virgo and Coma.
Comparing IR-based star-formation rates with optical
results shows up to 90% of cluster star-formation activity
hidden from optical spectra by dust. Clusters were
compared at 15 µm. Cl0024 has similar redshift to A370
but hosts ten times as many luminous IR galaxies
(LIRGs). No LIRGs were detected in A1689, A2218 or
A2390, while a total of three might have been expected
based on the results from Cl0024. The sources in Cl0024
are much more powerful than those in A1689 and A2218.
A2218 galaxies were fitted by models of quiescent
ellipticals. The 13 galaxies detected in Cl0024 are
strongly star-forming.
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References
Benoît, A., Ade, P., Amblard, A., et al., 2004, A&A 424,
571.
Biviano, A., Metcalfe, L., McBreen, B., et al., 2004, A&A
425, 33.
Coia, D., McBreen, B., Metcalfe, L. et al., 2005a, A&A
431, 433.
Coia, D., Metcalfe, L. McBreen, B., et al., 2005b, A&A
430, 59.
del Burgo, C., Laureijs, R. J., Ábrahám, P., Kiss, Cs.,
2003, MNRAS 346, 403.
Dupac, X., Bernard, J.-P., Boudet, N., et al., 2003a, A&A
404, L11.
Dupac, X., del Burgo, C., Bernard, J.-P., et al., 2003b,
MNRAS 344, 105.
Dupac, X. & Tauber, J., 2005, A&A 430, 363.
Evans, A., Gehrz, R.D., Geballe, T.R., et al., 2003, AJ
126, 1981.
Héraudeau, Ph., Oliver, S., del Burgo, C., et al., 2004,
MNRAS 354, 924.
Hony, S., Bouwman, J., 2004, A&A 413, 981.
Hony, S., Tielens, A.G.G.M., Waters, L.B.F.M., de Koter,
A., 2003, A&A 402, 211.
Heras, A. & Hony, S., 2005, A&A, in press.
Kiss, Cs., Ábrahám, P., Klaas, U., et al., 2003, A&A 399,
177.
Lyke, J.E., Koenig, X.P., Barlow, M.J., et al., 2003, AJ
126, 993.
Mercer, E.P., Clemens, D.P., Bania, T.M., et al., 2004,
ApJS 154, 328.
Metcalfe, L., Kneib, J.-P., McBreen, B., et al., 2003,
A&A 407, 791.
Reach, W.T., Rho, J., Young, E., et al., 2004, ApJS 154,
385.
Rowan-Robinson, M., Lari, C., Perez-Fournon, I., et al.,
2004, MNRAS 351, 1290.
Serjeant, S., Carramiñana, A., Gonzáles-Solares, E., et
al., 2004, MNRAS 355, 813.
research activities
2.5 Solar Physics
The research group continues to use SOHO observations
extensively to further its research interests in a wide
range of topics in solar physics, such as studies of the
chromosphere, transition region dynamics and coronal
magnetic fields.
2.5.1 Chromospheric oscillations
Investigations are underway to study the interaction of
the topographic structure of the solar chromospheric
plasma with the wave modes observed (McIntosh &
Fleck, 2004; McIntosh et al., 2003). A distinct correlation
between the inferred plasma topography and the phase
differences between and suppression of oscillations at
different levels in the solar atmosphere has been
established (Fig. 2.5.1/1). This can be interpreted as
evidence of interaction between the waves and the
extended magnetic ‘canopy’.
Coronal holes are the lowest density plasma components
of the Sun’s outer atmosphere. They are associated with
rapidly expanding magnetic fields and are the source
regions of the fast solar wind. The interfaces between
open and closed regions make them a topologically
interesting place. McIntosh et al. (2004) have therefore
studied the propagation characteristics of chromospheric
oscillations in and around an equatorial hole by applying
phase-difference and travel-time diagnostics to TRACE
time series in the 1700 Å and 1600 Å UV continua
bandpasses. Their results suggest a significant change in
atmospheric conditions at the base of the chromosphere
inside the coronal hole relative to its boundary and quietSun regions. Fig 2.5.1/2 shows a SOHO EIT 195 Å
context image from 2003 July 14, 00:08 UT. The TRACE
field-of-view is shown as the thick red rectangular
region. The coloured contour levels qualitatively indicate
the coronal hole boundary.
Figure 2.5.1/3 shows a travel-time map between the
1700 Å and 1600 Å signal. The travel-time (∆t) at any
frequency (ν) is computed by applying a Gaussian filter,
G(ν, δν), about ν with a width δν to each bandpass,
cross-correlating the two filtered sequences and
determining the shift of the cross-correlation function.
The 1700 Å continuum is formed a few tens of km below
the 1600 Å continuum. For upward travelling waves, the
1700 Å signal therefore leads the 1600 Å signal by a few
seconds (negative travel-time according to the
convention applied here).
There is a notable difference in travel-time between the
coronal hole interior and exterior (~4 s). Interpreting the
waves as being predominantly acoustic in nature, the
observed travel-time, ∆t ≈ ∆z/cs, is directly proportional
to the height difference between the two bandpasses,
where cs is the local sound speed in the lower
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Figure 2.5.1/2: SOHO EIT 195 Å context image from
2003 July 14, 00:08 UT. The red rectangular region
shows the TRACE field-of-view, while the yellow and
orange contours show the 100 DN and 200 DN
intensity levels in the image, respectively.
Figure 2.5.1/1: Upper left: spatial variation in the
altitudes at which the plasma-β is of order unity in the
TRACE field of view. Solid contours are added for
reference, each separated by 0.25 Mm. The map is
based on a potential field extrapolation of a timeaverage MDI longitudinal magnetogram. The
presence of the network elements, where the βtransition height is blue-violet in colour, is perhaps
the most striking feature. The other panels show one
example of the integrated oscillatory power in the 38 mHz band of the 1700, 1600 and 1550 Å TRACE UV
bandpasses, respectively. On each of these panels we
have overplotted the contours of the β-transition
height in the upper left. Note the clear correlation
between the reduced power and the contours.
chromosphere (~6 km/s). For a filter frequency of
7 mHz, the 4 s difference can therefore be approximated
to a difference in ∆z of 24 km between the coronal hole
interior and its boundary, a not insignificant fraction of a
scale height near the chromospheric temperature
minimum (~100 km).
This is a quite unexpected and confounding result: Why
would the largely hydrodynamic (high plasma-β) coronal
hole interior plasma at the base of the chromosphere care
Figure 2.5.1/3: Travel-time map at full TRACE
resolution between the 1700 Å and 1600 Å bandpasses. The coloured rectangles denote regions of
coronal hole interior (red), coronal hole
boundary/exterior (blue), and coronal hole arcade
(purple).
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about the fact that the magnetic field is open to the
interplanetary medium and stratify itself so?
Conventional thinking would assume that the
chromosphere should have little knowledge of the
topologically open coronal holes above. Follow-up
studies addressing a possible connection between the
mixture of field polarities, proportion of open/closed
magnetic structures, UV/EUV intensity/Doppler velocity
contrast, and in situ solar wind measurements are ongoing.
2.5.2 Dynamics of transition region blinkers
Blinkers are small-scale intensity enhancements
observed in the transition region of the solar atmosphere.
They were first detected by eye in SOHO/CDS data, but
automated methods have been developed more recently
to identify these events. Blinkers are best observed in
O V (which is formed at a temperature of 2.5x105K) and
have mean areas of 3x107 km2 and mean lifetimes of
16 min. They are either density enhancements or
increases in filling factor, but not temperature events.
They occur above regions where one polarity of
magnetic field dominates, including quiet Sun, plage
regions or sunspots.
Such blinkers can be further investigated by studying the
relative Doppler and non-thermal velocities of quiet-Sun
and active-region blinkers identified in O V with
SOHO/CDS. It has been found that O V blinkers have a
preference to be more redshifted than the normal
Figure 2.5.2/1: Three SOHO/CDS O V rasters taken
7 min and 8 min apart. The circled region shows a
blinker in the second frame.
research activities
transition region, but the range of these enhanced
velocities is no larger than the typical spread of Doppler
velocities in this region. The anticipated ranges of
Doppler velocities of blinkers are 25-30 km/s in the quiet
Sun (20-40 km/s in active regions) for O V.
Bewsher et al. (2003) also found that blinkers have
preferentially larger non-thermal velocities than the
typical background transition region. Again, the increase
in magnitude of these non-thermal velocities is no greater
than the typical ranges of non-thermal velocities. The
range of non-thermal velocities of blinkers in both the
quiet-Sun and active-regions are estimated to be 3045 km/s in O V.
There are more blinkers with larger Doppler and nonthermal velocities than would be expected in the whole
of the transition region. The results have been used to
help elaborate further the many mechanisms proposed to
explain blinkers.
2.5.3 Comparison of blinkers and explosive events
Blinkers (intensity enhancements) are predominantly
observed with the CDS instrument on SOHO and were
discussed in the subsection above.
Explosive events, however, are characterised by strong
non-Gaussian enhancements in the wings of spectral
lines, and have large velocities (50-250 km/s) associated
with them. Explosive events have recently been observed
with the SUMER instrument on SOHO but where first
observed using HRTS. They have a mean area of 1 Mm2
and mean lifetime of 1 min. They are associated with
regions of complex weak fields or on the edges of
unipolar. Models of the magnetic reconnection
configuration required for explosive events to occur have
also been presented.
There has been much speculation as to whether blinkers
and explosive events are the same phenomenon, but
observed differently with the CDS and SUMER
instruments.
Bewsher et al. (2004a) have analysed co-spatial and
co-temporal CDS and SUMER datasets and automatically identified both blinkers and explosive events in both
instruments data. They found that blinkers were
identified in the SUMER data if the temporal resolution
of the data was reduced to that of the CDS data,
otherwise short-lived localised intensity enhancements
were identified. Explosive events were identified in the
CDS data if the width of the spectral line was
significantly increased, and occasionally if an
enhancement in the wing was present. In 3.5 h of data,
they found only one case where a blinker and an
explosive event coincided, ten examples of lone blinkers
and seven examples of lone explosive events. This has
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(a)
29
Figure 2.5.3/1: (a) SUMER single slit image showing
an explosive event labelled S1; (b) CDS raster
showing blinkers labelled C1-3. The diamonds on the
CDS raster mark the locations of blinkers and the
vertical dashed line indicates the position of the
SUMER slit. (c-d) lightcurves of the explosive event,
S1 and blinker, C2 (which is closest spatially to the
explosive event). (e-f) spectral line profiles of the
explosive event S1 and blinker C2.
(b)
(c)
(d)
Figure 2.5.4/1: Highly twisted magnetic flux tube
inside an active region obtained from a non-linear
force-free extrapolation technique based on
photospheric vector magnetograms. The contours
characterise the vertical magnetic field strength on
the photosphere.
(e)
(f)
led to the suggestion that blinkers and explosive events
are not the same type of event. A theoretical statistical
model was presented in Bewsher et al. (2004b), which
hypothesised that blinkers and explosive events are
random and not physically connected in any way.
2.5.4 Coronal magnetic fields
To understand most of the phenomena in the solar
corona, such as flares, CMEs and filament eruptions,
knowledge of the 3-D magnetic field is required.
Considering that the observed solar region is in a forcefree equilibrium state, the coronal magnetic field can be
extrapolated from photospheric magnetic field measurements. Régnier and co-workers used vector magnetograph measurements to study magnetic structures inside
active regions (filaments or sigmoids) and their evolution
before and after flares.
Régnier & Amari (2004) have found that a filament and
a sigmoid can both be described by a twisted flux tube
with a number of turns less than 1 and opposite electric
current densities. They have also shown that the eruption
associated with the studied active region is most likely
due to a highly twisted flux tube with a number of turns
more than 1 (Fig. 2.5.4/1) different from the filament and
the sigmoid. Studying the dynamics of an active region
has also shown that the main progenitors of small flares
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identification of the source of the flare at a reversed-Y
null point in the low corona.
Figure 2.5.4/2: Characteristic magnetic configuration
of the active region where most of the flares of
October/November 2003 originate. Red field lines
describe the system of loops involved in the post-flare
phenomena. The background image is the
SOHO/MDI magnetogram at 10:00 UT Oct 28, 2003.
in an active region are the transverse photospheric
motions (sunspot rotation, magnetic flux emergence) and
the complex topology (separatrix surfaces, separators)
(Régnier & Canfield, 2004). The extrapolated coronal
magnetic configurations are used to construct the
synthetic X-ray and EUV emission maps by solving the
energy equation along each individual coronal loop
(Lundquist et al., 2004). The constructed maps are
compared with observed images recorded by Yohkoh/
SXT and SOHO/EIT, giving some constraints on the
coronal heating mechanism.
Vector magnetograms are also useful for determining the
flow field on the photosphere. By combining the
induction equation and the local correlation technique,
Welsch et al. (2004) were able to self-consistently derive
the three components of the flow field at the
photospheric level. The flow fields as well as the forcefree coronal magnetic configurations are the boundary
conditions of magnetohydrodynamic (MHD) evolution
codes.
Over 2 weeks in October/November 2003, the Sun
featured unusually strong activity, with 12 X-class flares
and two significant proton storms. Régnier & Fleck
(2004) studied the magnetic properties of AR 10486 (the
active region in which most of the events occurred)
before and after the X17.2 flare on 28 October. Two
methods were used: (i) the study of the active region
dynamics by determining the potential coronal field from
SOHO/MDI magnetograms with a high temporal
cadence, as shown in Fig. 2.5.4/2; (ii) the analysis of a
more accurate coronal magnetic configuration using a
non-linear force-free extrapolation from a vector
magnetogram taken before the flare, which led to the
References
Bewsher, D., Parnell, C.E., Pike, C.D., Harrison, R.A.,
2003, Solar Physics 215, 217.
Bewsher, D., Innes, D.E., Parnell, C.E., Brown, D.S.,
2004a, A&A, submitted.
Bewsher, D., Brown, D.S., Innes, D.E., Parnell, C.E.,
2004b, ESA SP-575, 465.
Lundquist, L.L., Fisher, G.H., McTiernan, J.M.,
Régnier, S., 2004, ESA-SP 575, 306.
McIntosh, S.W. & Fleck, B., 2004, ESA SP-547, 149.
McIntosh, S.W., Fleck, B., Judge, P.G., 2003, A&A 405,
769.
McIntosh, S.W., Fleck, B., Tarbell, R.D., 2004, ApJ 609,
L95.
Régnier, S. & Amari, T., 2004, A&A 425, 345.
Régnier, S. & Canfield, R.C., 2004, ESA-SP 575, 255.
Régnier, S. & Fleck, B., 2004, ESA-SP 575, 519.
Welsch, B.T., Fisher, G.H., Abbett, W.P., Régnier, S.,
2004, ApJ, 610, 1148.
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2.6 Heliospheric Physics/Space Plasma Studies
The scientists in SCI-SH have expertise in the observations of electromagnetic fields and plasma particles, as
well as in the detection of high-energy particles. Basically,
their studies deal with two major areas. Firstly, how the
solar wind originates and how it varies in the heliosphere;
the team has particular expertise in solar energetic
particles in the MeV range. Secondly, how the Earth’s
plasma environment (the magnetosphere and ionosphere)
is driven by the solar wind, particularly the transfer of
particles between different regions as well as how particles
are energised in the magnetosphere.
2.6.1 Energetic particles from the October/
November 2003 solar events
The research group has investigated heliospheric effects
of the intense solar activity that occurred in OctoberNovember 2003 using observations of the COSPIN/LET
instrument on the Ulysses spacecraft located near the
solar equator at 5.2 AU from the Sun. COSPIN/LET was
built by members of SCI-SH together with current
members of SCI-A.
Figure 2.6.1/1 (top panel) presents the proton/alpha ratio
for the 42-day period after 17 October (DOY 290).
Dashed vertical lines mark the times of forward (F) and
reverse I shocks identified in the magnetic field data at
Ulysses, where F-shocks labelled in red indicate
probable CME-driven shocks. The lower panel contains
heavy ion abundance ratios (1-day averages), all
normalised to the solar energetic particle (SEP)
composition. Shown for reference is the 1.2-3.0 MeV
proton intensity. The onset time and duration of a large
CME associated with the October-November 2003
activity is marked by an inverted triangle.
Solar wind conditions at Ulysses prior to the period of
enhanced solar activity were dominated by recurrent
high-speed/low-speed stream interaction regions (SIRs).
As a result of the increased activity, and the associated
CMEs, this pattern was temporarily disrupted. The
highest particle intensities occur at the time of the reverse
shock on DOY 314/10 November, although the
preliminary analysis does not allow us to determine
conclusively whether or not this is the result of local
acceleration of the pre-existing SEP population. With the
possible exception of He, which apparently shows a
typical corotating interaction region (CIR) enhancement
(decrease in p/He, increase in He/O), the composition
signatures suggest that the CIR reverse shock processed
the ambient SEP population (as evidenced by the SEPlike C/O ratio). If real, the enhanced He content within
the CIR is presumably the result of accelerated
interstellar pickup helium. The signature for Fe/O is
suggestive of CIR composition, but very large scatter in
daily values prevents a firm conclusion.
Figure 2.6.1/1: Energetic particle observations of the
COSPIN/LET instrument on Ulysses.
2.6.2 Energetic particles in the high-latitude, highspeed solar wind
A detailed study has been made of energetic particle
events observed by COSPIN/LET during the recent
second northern polar pass. For a short time during this
high-latitude pass, Ulysses was immersed in high-speed
solar wind from the newly formed northern polar coronal
hole. Four large SEP events were observed, permitting
significant conclusions to be drawn concerning the
propagation of the particles to high latitudes.
A topic of considerable debate triggered by Ulysses
observations is the role played by perpendicular diffusion
in the transport of charged particles in the heliosphere.
Based on the events studied here, no evidence has been
found for local transport across the magnetic field.
Indeed, the particle angular distributions at the onset at
all energies were considerably more isotropic than events
seen at lower latitudes, or even at 1 AU.
It must be stressed that the observations do not allow
conclusions to be drawn about particle propagation close
to the Sun. Even though, at the location of Ulysses,
particles were propagating along the magnetic field lines
and not across them, there may be cross-field diffusion
occurring close to the solar surface. Another possible
mechanism is the large-scale distortion of the magnetic
field connecting Ulysses to the Sun at lower latitudes by,
for example, an outward-moving coronal mass ejection.
Continuing the research group’s study of the relationship
between the Sun and the heliosphere, the group is
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involved in a new instrument for NASA’s STEREO
spacecraft. The instrument comprises a proton and
electron telescope. Staff from SCI-A designed, manufactured and tested the overall electronics for the SEPT
instrument for two NASA/STEREO satellites; the
electronics is highly miniaturised using ASIC components. The instruments have been delivered for final
testing at Caltech. The PI institute of the instrument is the
University of Kiel (D); SCI-SH Co-I’s are R. Marsden
and T. Sanderson.
2.6.3 Acceleration of electrons in the auroral region
One of the key issues in space plasma physics is the
acceleration of charged particles. In the auroral region,
electrons become highly accelerated before hitting the
Earth’s atmosphere and causing auroral emission. The
acceleration is often related to the occurrence of large
electric fields, either DC or wave electric fields, which
can be monitored with electric field instruments. The
NASA Polar satellite (1996-) carries such an instrument
that was in part built by the SCI-SH team together with
current members of SCI-A.
Figure 2.6.3/1, taken from Janhunen et al. (2004c),
provides one possible approach to the acceleration
processes occurring in the auroral region. It appears that
an island of density cavities (see the isocontours in the
figure) and enhanced electric field structures occur at 45 RE radial distance in the evening and midnight
magnetic local time (MLT) sectors in the auroral region
during disturbed conditions. At the same time, the ion
beam occurrence frequency changes at the same altitude
(these ions come from the Earth’s atmosphere). It is
proposed that the mechanism involved in the electron
acceleration is electron Landau resonance with incoming
Alfvén waves.
The auroral kilometric radiation (AKR) is the strongest
electromagnetic emission generated around the Earth and
it can be detected from large distances, even beyond the
heliosphere. Similar radiation can be observed from
other planets featuring auroral displays, e.g. Jupiter and
Saturn. A new type of AKR emission is Dot-AKR,
originating from 2-3 RE radial distance, has been found
to occur during substorm onsets. This is suggested to be
an effect of Alfvénic wave acceleration in a pre-existing
auroral cavity. In Fig. 2.6.3/1 panel a presents a lowaltitude auroral cavity associated with a stable auroral arc
in the atmosphere and maintained by ion Bernstein
waves. At the substorm onset (panel b), Alfvén waves
arrive from the magnetosphere, causing electron
acceleration (via a resonance between waves and
electrons) and possibly also Dot-AKR emission in the
low-altitude cavity; the Dot-AKR emission is usually
short-lived and probably requires strong transient Alfvén
waves. If Alfvén wave activity lasts for some time,
electron acceleration causes some ions to leave the
Figure 2.6.3/1: Plasma processes that Alfvén waves
cause in auroral regions.
resonance region as well, leading to another density
cavity at higher altitudes (see panel c) found by the
authors in the earlier studies. After the Alfvén wave
activity has stopped, the cavity fills up on the ion time
scale, so that it continues to exist for some time (panel d).
The low-altitude depletion is all the time maintained by
other processes that are independent of Alfvénic activity.
Normal AKR is emitted all the time near the lower
boundary of the cavity, although not shown.
2.6.4 Magnetospheric observations
Double cusp and reconnection hypotheses
Magnetic reconnection has been successful in explaining
the main features of mass, energy and momentum
transfers from the solar wind into the magnetosphere. A
key parameter ruling the magnetic reconnection process
and therefore the whole solar wind-magnetosphere
coupling is the interplanetary magnetic field (IMF)
orientation. For southward IMF, reconnection takes place
at the low-latitude magnetopause, between the two cusps.
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Figure 2.6.4/1: Statistics of cusp observations from
Cluster.
The signature of low-latitude reconnection is a strong
anti-sunward convection in the cusp as well as an energy
dispersion of ions (higher energies at lower latitudes).
For northward IMF, on the other hand, reconnection
takes place at higher latitude, poleward of one or both
cusps. This drives a sunward convection in the cusp and
the ion energy dispersion is then ‘reversed’ (higher
energies at higher latitudes).
An intermediate case appears when the IMF is dominated
by its Y-component (dawnward or duskward IMF). Then,
reconnection is thought to occur simultaneously at high
and low latitudes. The discovery of the double cusp and
the study of its consequences in the high-latitude
ionosphere makes the coupling processes between the
solar wind and the magnetosphere more complicated
than described above.
Prior to the study of the double cusp, F. Pitout and
C.P. Escoubet performed a statistical study of three
months of Cluster crossings of the mid-altitude (at 56 RE) cusp (Fig. 2.6.4/1). A few morphological features
of the cusp have been defined and then related to the
prevailing IMF. The double cusp, which is thought to
occur when the IMF is dominated by its Y-component, is
searched for throughout this study. The preliminary study
reveals, among others, that textbook cases of cusps with
nice ion dispersions do not occur that often. Instead,
numerous irregular and discontinuous cusps are found,
among which there are interesting cases of discontinuous
cusps occurring under stable IMF conditions. The latter
are also good candidates for stable double cusps, which
require further studies.
Banded hiss emissions in the plasmasphere
The inner part of the magnetosphere contains two
important regions: radiation belts that contain relativistic
electrons, and a plasmasphere that contains cold plasma
originating from the ionosphere. Plasmaspheric hiss (at
100-10 000 Hz) is observed throughout the Earth’s
Figure 2.6.4/2: WHISPER spectrograms
Cluster 1 (top) to Cluster 4 (bottom)
from
plasmasphere, particularly during high magnetic activity.
This emission cuts off suddenly at the plasmapause, the
outer boundary of the plasmasphere. Although the
generation of hiss emission is not yet understood, it is
believed that the decay of radiation belt electrons is
significantly controlled by the hiss phenomenon.
Using Cluster instrumentation (WHISPER, STAFF and
WBD), an investigation into plasmaspheric hiss was
initiated which established a previously unknown
phenomenon, banded hiss emission (BHE) (Masson et
al., 2004). It appears below the electron gyrofrequency,
Fce, but above the lower hybrid resonance, from 2 kHz
to 10 kHz. The waves were shown to propagate in the
whistler mode. Based on the first year of Cluster
observations, the following properties of the BHE waves
were identified: (i) the location is strongly correlated
with the position of the plasmapause; (ii) no MLT
dependence was found; (iii) the spectral width is
generally 1-2 kHz; (iv) the central frequency of their
emission band varies from 2 kHz to 10 kHz and
correlates with the Kp index. All these features suggest
that BHE is in fact mid-latitude hiss (MLH). The central
frequency correlation with Kp, found by this study, is a
new property of MLH. It suggests either that MLH is
generated in a given f/Fce range, or that there is a Kpdependent Doppler shift between the satellites and a
possible moving source of the MLH.
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Figure 2.6.4/2 shows an example of MLH as observed by
WHISPER on 2001 October 7, 14:45-18:30 UT. MLH
occurs at 16:25-17:04 UT, indicated by white arrows.
MLH is found to intensify with altitude and with time
(note that the four Cluster satellites fly in a string-ofpearls formation near perigee).
2.6.5 Examples of other associated activities within
SCI-SH
In addition to the analysis of Cluster data, the team is also
involved in the analysis of magnetospheric data from
Double Star. The Double Star TC-1 spacecraft carries an
ASPOC instrument that keeps the satellite potential near
zero with respect to the ambient plasma. The team,
through SCI-A, contributed both hardware and expertise
on ion emitter development and in-flight operations to
ASPOC. The ion emitter module was improved after
experience gained on the Cluster mission. After the
successful launch on 29 December 2003, ASPOC is
functioning very well with a very good high-voltage
ignition and very stable ion current. The PI institute of
the instrument is the Space Research Institute in Graz
(A).
Moving from the study of the Earth’s magnetosphere
through the Cluster and Double Star missions, the
research group is now turning its attention to the
magnetosphere of Mercury. The team is involved in the
challenging (owing to the very high temperature
environment) development of an electric field instrument
for the BepiColombo/MMO satellite. The team is
responsible for the thermal analysis of the overall
instrument, which is delegated to SCI-A personnel for
implementation. The PI institute of the instrument is the
Royal Institute of Technology in Stockholm (S). In
addition, the study of ions from the surface of Mercury
and their interaction with the planet’s magnetic field will
be explored through the group’s involvement in the
PICAM ion spectrometer on the BepiColombo MPO
(Co-I C.P. Escoubet). Here, the design of the analoguedigital hybrid ASIC electronics together with the MCP
detectors is the responsibility of SCI-A in support of the
Co-I.
Finally, the SMART-1 satellite carries the SPEDE
instrument that monitors the performance of the solar
electric propulsion (SEP) engine of the satellite. The
Division, together with SCI-A personnel, has been
involved in the design and manufacturing of the two
booms as well as the testing and calibration of the overall
instrument. Measurements have been obtained since
early October 2003, and currently the team is working
with in-flight calibration issues. The PI institute of the
instrument is the Finnish Meteorological Institute in
Helsinki. Such experience will be invaluable for the
BeppiColombo mission to Mercury, which also will use
an SEP motor.
research activities
References
Janhunen, P. et al. (inc. Laakso, H.), 2004, Ann. Geophys.
22, 2213-2227.
Masson, A. et al., 2004, Ann. Geophys. 22, 2565-2575.
Sanderson, T.R., Marsden, R., Tranquille, et al., 2003,
Geophys. Res. Lett. 30(19), 8036.
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2.7 Comparative Planetology and Astrobiology
Comparative planetology is an important study area in
RSSD, because it is a necessary element in the
preparation of ESA’s current and future planetary
missions, and it maximises the scientific exploitation of
these missions. Studies of the Moon, Mars, Venus, Titan
and Mercury provide unique opportunities to improve
our understanding of the processes and factors that have
shaped our own planet. Mars Express, SMART-1 and
BepiColombo have the potential for developing expertise
and knowledge in comparative planetology focused on
the terrestrial planets. Venus Express, to be launched in
2005, offers similar opportunities, in particularly for
climatology. Huygens will provide detailed information
on one of the most mysterious objects in the Solar
System, Saturn’s moon Titan.
2.7.1 Mars research
Geologic evolution of the Martian surface
Gusev Crater is the landing site of one of the NASA Mars
Exploration Rovers (MERs). During the early
commissioning period of Mars Express, the HRSC took
a number of images over the Gusev area. The study of
this area, including the neighbouring highlands to the
south and lowlands to the north, has been the subject of
a stagiaire project. Data from Mars Global Surveyor,
Mars Odyssey and the recent Mars Express image and
altimetry data have all been used to produce a geological
map and geological profiles of the region (Fig. 2.7.1/1).
The basis for these geological profiles was provided by
HRSC digital elevation models (DEMs) derived from the
HRSC stereo images. The resolution of these DEMs is
better than the available MOLA altimetry data (better
than 200 m for HRSC, compared to 600 m horizontal
resolution for MOLA). Geological mapping of the
surface combined with geometrical analysis of the
geological profiles make it possible to determine the
stratigraphic sequence, including estimates of the
thickness of the various units. This provides a much
enhanced insight into the geological evolution of this
terrain. Some of the main issues are: (1) a relative
stratigraphic sequence of 16 units, including sediments
and volcanic rocks; (2) mapping of tilted Noachian
terrains, indicating a dynamic early history of Mars;
(3) correlation of two potential sedimentary units in the
Gusev crater.
Figure 2.7.1/1: Geological map of the Gusev crater on
Mars. The landing site of Spirit, one of the MER
landers, is also shown. The map distinguishes various
rock units and is based on both image data and
topography data from HRSC on Mars Express.
— characterisation of surface morphology and textures
at high/super resolution;
— characteristics of present and future landing sites.
In addition, HRSC data have been used to study the
evolution of the Martian surface through time and
geological processes. Specific issues being addressed by
HRSC Co-I B. Foing and collaborators are:
HRSC has obtained new evidence for geological activity
on Mars. Calderas on five major volcanoes in the Tharsis
and Elysium regions have undergone repeated activation
and resurfacing during the last 20% of Martian history.
Caldera floors as young as 100 Ma and flank eruptions as
young as 2 Ma have been found. These results confirm
that the volcanic edifices are characterised by episodic
phases of activity and suggest that volcanoes are
potentially still active today.
— role of water and volatiles;
— impact craters processes;
— evolution of volcanism and hydrothermal activity;
HRSC images have provided convincing evidence of a
current frozen body of water, with surface pack-ice,
around 5°N/150°E in southern Elysium (Murray et al.,
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2005). The study of tropical to mid-latitude glaciation on
Mars shows evidence of snow and ice accumulation and
flow in Mars Express HRSC data (Head et al., 2005).
Finally, very young volcanic and glacial activity at
Hecates Tholus has been discovered in HRSC images.
In preparation for future missions to Mars involving a
potential lander, Mutual Impedance Probes have been
built for atmospheric and surface investigations
(Huygens, Philae). The measurement of the electric
properties of surface and subsurface materials is an
important issue for planetary missions. A prototype of a
subsurface MIP has been developed, which will allow the
measurement of the profiles of the electrical conductivity
and permittivity along the path of a drill or mole, and
generate 2-D images of the electrical properties of
materials along the walls of the borehole. The environmental parameters and requirements for applications on
Mars have been analysed. This will allow the investigation of otherwise invisible subsurface structures, and the
detection and localisation of subsurface water deposits.
Study of the upper Mars atmosphere
The research team is also closely involved in the study of
the Martian atmosphere. Specifically, the UV
spectrometer SPICAM aboard Mars Express is
performing a number of different scientific observations,
including limb measurement. These observations aim at
studying the airglow (natural emission) of the upper
atmosphere. From such data, information can be deduced
on the composition and thermal structure of the coupled
neutral atmosphere/ionosphere, on both the dayside and
the nightside, and on the interaction with the solar wind.
SPICAM has provided the first spectra of the upper
atmosphere since Mariner-9 in the 1970s. A number of
limb data spectra are being analysed in detail and show
emissions of O, CO, CO2+. A model of the ionosphere
(Morel et al., 2004; Witasse et al., 2003) is being updated
in order to model the lines and bands detected by
SPICAM.
2.7.2 Lunar studies
The Moon bears the scars of countless impact craters,
and holds the only accessible record of the conditions in
the Earth-Moon system over the past 4.5 billion years.
The recent Clementine and Lunar Prospector missions
provided the first views of global geochemistry. The
SMART-1 mission will add the first global IR dataset and
the first global measurements using X-ray fluorescence,
which will map elemental Mg, olivine and pyroxenes
across the surface. These are critical to understanding the
Moon’s crustal evolution and origin, which is intrinsically linked to the early evolution of the Earth, as well
as other geological process in the Solar System, such as
volcanism, tectonics, impact cratering and volatiles.
research activities
The research team (B. Foing, D. Koschny, M. Almeida et
al.) is therefore actively involved in SMART-1, specifically with the AMIE imaging and the D-CIXS X-ray
spectrometer teams. In particular, a new technique has
been developed for remote sensing determination of
lunar surface composition based on AMIE data. The
approach is based on spectral and composition data
derived from a Lunar Soil Characterization Consortium
for a few, particle-size, separates of lunar soils, mapping
the abundance of TiO2 and FeO, pyroxene content,
maturity degree (Is/FeO), and a characteristic size of
particles (Shkuratov et al., 2003).
2.7.3 Cassini-Huygens data analysis preparation
Preparations for the arrival of Huygens at Titan:
Huygens radar tests
The main objective of the Huygens Radar Altimeter is
the determination of the Probe altitude, which is very
important for an optimised operation of the payload. In
order to assess the performance of the radar at high
altitudes, and verify the characteristics for concurrent
operation of both radars, the research team supported a
series of radar tests on the ground and aboard
stratospheric balloons (HASI Sicily flight June 2003, sky
test; PEASMA balloon flight November 2004). The radar
signal reflected by Titan’s surface contains important
information about surface properties such as roughness
and electrical parameters. The signal is processed via the
PWA experiment, which is part of HASI. In addition to
verifying the altimeter performance, the balloon campaigns provided valuable datasets for the development
and test of data analysis software, which will be used for
processing the radar data returned by Huygens in 2005.
Preparations for the arrival of Huygens at Titan: the
HASI-PWA experiment
The PWA experiment will explore the atmosphere of
Titan during the Probe’s descent. It will measure the
electric field (AC, Schumann resonances and lightning),
the atmospheric conductivity (Relaxation Probe and
Mutual Impedance Probe), pressure variations (Acoustic
Experiment) and signals returned from the surface of
Titan by the Huygens Radar Altimeter. The preparations
for the processing and analysis of Huygens data are
progressing in cooperation with partner institutes in
Austria (IWF), France (CETP) and Spain (IAA). Final
hardware tests have been conducted in order to finalise
the calibration and validate various models required for
data calibration.
A recent series of tests was designed to investigate the
impact of the Huygens probe attitude on the measurement of electric fields (Fig. 2.7.3/1). Preparations at
ESTEC include logistics, finalising the calibration
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2.7.4 Ground-based observation of Titan winds
software and preparing for the initial data analysis during
the Huygens arrival event.
The study of winds on Titan is a scientific objective of
the Cassini/Huygens mission. Earth-based observations
are attempting to provide complementary information.
All Earth-based techniques employ various implementations of the Doppler measurement technique. The
technique used here, however, is based on the absolute
accelerometry method developed for the detection of
extrasolar planets. The reflected solar spectrum from a
rotating body (in Titan’s case, its atmosphere) observed
by a high-resolution spectrometer was analysed. The
rotating atmosphere induces a Doppler shift in the whole
spectrum. Observations of Titan were performed in
2001-2002, with the UVES spectrometer mounted on the
ESO VLT. However, the data reduction, analysis and
interpretation using the UVES pipeline data processing
tools have led to results difficult to interpret. As a result,
the approach was verified by applying the method to a
rotating body with no atmosphere: Io. In that case, the
method consists of retrieving the surface rotation
velocity, which is well known. Four observations of Io
performed in early 2003 were analysed, yielding a
rotation rate with an uncertainty < 2 m/s (Civeit et al.,
2005). With the improved pipeline processing the
method is being applied to analyse the observations of
Titan, plus some recent observations of Saturn.
Reconstruction of the Huygens trajectory
2.7.5 Earth comparative planetology
The Huygens Project Scientist Team supported the
scientific activities of the Descent Trajectory Working
Group (DTWG). This group was created to ensure an
orderly and efficient analysis, interpretation and delivery
of the Cassini/Huygens engineering and instrument data
necessary for reconstructing the the Huygens probe entry
and descent trajectory. One of the major activities of the
group was the implementation and testing of a numerical
tool that can reconstruct the trajectory. In this context, the
Project Scientist Team built a synthetic dataset of the
mission in order to test the algorithm. The philosophy of
the approach, the assumptions made and the limitations
of the method are described in Perez-Ayucar et al.
(2004).
Impact cratering studies
Figure 2.7.3/1: Huygens balloon model in the electric
field test chamber at Padua University, Italy.
Study of the upper atmosphere of Titan
The upper atmosphere of Titan has been investigated by
the Cassini Orbiter through two dedicated studies of the
ionosphere. The first is related to the ion production due
to electron impact (Lilensten et al., 2005a). The second
concerns the modelling of a doubly charged ion layer that
could be detected by the UVIS instrument (Lilensten et
al., 2005b). This paper is the last of a series of three
studies on comparative planetology devoted to the
doubly-charged ions in planetary atmospheres (Mars:
Witasse et al., 2003; Earth: Simon et al., submitted).
Impact craters are the most common geological feature in
the Solar System. All of the planets have been struck by
countless asteroids, comets and meteoroids since its
formation 4.6 billion years ago. Impact craters thus
represent a fundamental field of research in planetary
studies. The emerging view of planets as geological
objects makes the search for previously unknown impact
craters on Earth a fundamental element of planetary
exploration. Various potential methods for the automated
recognition of impact craters from remote sensing data
have been considered. As a result of the study, an
algorithm based on the Hough transform was selected,
implemented and demonstrated to be effective in
identifying known craters from sample images of the
Earth, Mars and the Moon. The study also showed that
the detection of new unknown impact craters requires the
exploitation and fusion of data from multiple remote
sensing missions and sensors, and therefore the
development of more sophisticated recognition
algorithms. Envisat data are being exploited in the
framework of this work, to be followed by potential
fieldwork of a few examples of identified structures. Of
course, such an approach can also be applied to Mars
craters and in particular Mars crater synthetic studies
using coordinate registration by automated crater
recognition.
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Geological expedition to Pilbara terrain (Australia)
The Pilbara terrain in Western Australia is one of the
planet’s oldest terrains – up to 3.5 billion years old.
Because of its unique record of early life and conditions
on Earth, it is the focus of an international research effort
organised by the NASA Institute of Astrobiology. A field
expedition to the Pilbara terrain was organised in August
2004 to collect rock samples for three projects:
— spectral analysis of Archean volcanic rocks as
potential analogues for Martian geological units.
This project is in collaboration with the Geological
Survey of Western Australia, CSIRO (Australia) and
Technical University of Delft, ITC (Enschede, NL);
— study of the early Earth magnetic field. The
behaviour of the Earth’s early magnetic field is
related to the formation of the inner core. Numerical
models of the geodynamo predict a weaker magnetic
field at times prior to the formation of the solid inner
core. So far, no record of the early geomagnetic field
has been found. Granitic rocks in the Pilbara granitegreenstone terrain have been sampled for isotopic
dating and paleomagnetic analysis to determine if
such an early record is preserved in this terrain. This
project is in collaboration with MIT and Caltech,
where the measurements will be done;
— sampling of units that possibly formed as a result of
meteorite impacts. A 5 m-thick spherule layer was
discovered in the Coongan Greenstone Belt.
2.7.6 Astrobiology
Large organics in space
Spectroscopy of large PAHs, including laboratory studies
and comparison with the Diffuse Interstellar Bands
(DIBs) have been performed by Foing and collaborators.
For the first time, laboratory spectroscopy of the UV-VisNIR absorption spectra were obtained for a representative set of large PAHs that have been selected for longduration exposure experiment aboard the International
Space Station and Foton/Biopan. The PAH charge
distribution and DIB carriers ware also studied. Physical
parameters such as density, ionisation and temperature,
constrained by observed atoms and molecules, have been
computed for the line of sight towards a single cloud
towards HD 147889. It has been established that
different wavelength regions in the DIB spectrum
correspond to different charge states depending in the
size distribution. The contribution of catacondensed
PAHs to the strong UV 200-300 nm absorption and to the
DIBs is constrained (Ruiterkamp et al., 2005).
The study of DIBs’ weak unidentified interstellar
absorption bands observed towards reddened stars has
continued. Their carriers are believed to be large
carbonaceous molecules (e.g. PAHs). The Large and
research activities
Small Magellanic Clouds (LMC and SMC) offer a
unique opportunity to link DIB behaviour to widely
varying environmental conditions (e.g. metallicity, UV
radiation field and star-formation activity). To this end,
the absorption spectra of reddened OB stars in the
Magellanic Clouds have been observed at unprecedented
high resolution (R = 100 000) and high S/N with
VLT/UVES. Analysis of the spectra of the LMC and
SMC targets indicates that a delicate balance must exist
for DIBs to be present. Noteworthy in this respect is the
30 Doradus region in the LMC, where these special
conditions seem to prevail. Of all the LMC stars
observed, only the two in the 30 Dor region have
detectable DIBs. This balance appears to be strongly
dependent on the UV radiation field, which is
represented by the shape of the extinction curve (i.e. the
presence of the 2200 Å bump and the steepness of the
far-UV rise).
The strongest diffuse interstellar bands ever were
measured using the VLT/UVES in the heavily reddened
line of sight towards the high-mass X-ray binary
4U1907 +09. More than 180 DIBS could be detected in
this source. The relation between the DIB carriers, and
other species such as neutral hydrogen and K, could be
studied.
An astronomical search coupled to laboratory
spectroscopy was conducted for C84: a prototype of
large fullerenes. For the first time, a UV/Vis spectrum of
a neutral and ionised fullerene (C84 isolated in Ne
matrix) was obtained. It shows absorption bands that
have been compared to the optical DIB spectrum.
Finally, the ORGANICS experiment on Foton/Biopan
has been prepared to study effects of UV and particle
radiation on selected PAHs and fullerenes, in order to
better constrain the destruction pathways of large organic
molecules in interplanetary and interstellar environments.
Complex organics on Mars
The behaviour of organic compounds in a simulated
Mars environment is under study. Viking Lander biology
and molecular analysis experiments were re-analysed
and possible reasons why no organic compounds could
be clearly detected were identified (Ten Kate et al.,
2003). The search for organic molecules and traces of life
on Mars has been a major topic of planetary science for
several decades. The search for extinct or extant life is
the future perspective for several missions. A set of
organic molecules has been selected for simulation
experiments. Laboratory experiments under simulated
Mars conditions are performed in order to determine
what those missions should be looking for. This research
has been developed as part of a Mars Express
Recognised Cooperating Laboratory (RCL).
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The Mars simulation chamber has been used to study thin
layers of glycine exposed to low ambient pressures and
UV lighting conditions similar to those on Mars. Scaling
times for sample alteration were determined for these
Mars-like conditions. A sequence of Mars chamber
studies is dealing with the Martian survival properties of
ice covered by or mixed with dust. This should provide
an understanding of the remnants of glacier and ice
deposits during the Mars obliquity cycles, as observed by
Mars Express/HRSC.
References
Civeit, T. et al., 2005, A&A 431, 1157.
Cox, N. et al., 2004, A&A, submitted.
Head, J. et al., 2005, Nature 434, 346.
Lilensten, J. et al., 2005a, Icarus 174, 285.
Lilensten, J. et al., 2005b, GRL 32(3).
Morel, L. et al., 2004, PSS 52, 603.
Murray, J. et al., 2005, Nature 434, 352.
Perez-Ayucar, M. et al., 2004, ESA SP-544.
Ruiterkamp, R. et al., 2005, A&A 432, 515.
Shkuratov, Y. et al., 2003, Sol. Sys. Rev. 37, 251.
Simon, C. et al., 2004, submitted.
Ten Kate, I. et al., 2003, LPI 1, 1313.
Witasse, O. et al., 2003, GRL 30, 12.
39
2.8 Minor Bodies
The Minor Bodies research group explores the physical
and chemical properties of some of the oldest objects in
the Solar System with a view to understanding how it
was formed and providing insight into the formation and
evolution of extrasolar systems. Both topics are key
aspects of current and future activities in the Agency’s
science programme through such missions as Rosetta and
Darwin. To this end, the research group uses a variety of
tools, spanning the development of key instruments and
observations from ground- and space-based observatories, both underpinned by a theoretical- and modellingbased programme.
2.8.1 The MIDAS instrument on the Rosetta
mission
The MIDAS Atomic Force Microscope onboard the
Rosetta Orbiter was developed in collaboration with
IWF, Graz (A). This instrument will collect, image and
characterise the geometry of dust particles when in orbit
around Comet 67P/Churyumov-Gerasimenko. Among
the key scientific goals is the 3-D characterisation of
cometary dust with a resolution of better than 10 nm and
the determination of dust flux variation and statistics of
particles in the size range 10 nm to 5 µm. The AFM will
study the morphology of dust grains around a comet
in situ rather than requiring a far more expensive
sampling and return mission.
After many years of development, manufacturing,
integration and testing, the long-awaited successful
launch of Rosetta came in March 2004. Since then,
MIDAS has undergone its initial deployment and has
been checked out in the majority of its operational
modes. The instrument carries samples that allow a
complicated but high-resolution in-flight calibration. The
imaging conditions and parameters during the early
commissioning phase are identical to those during the
final orbit around Comet Churyumov-Gerasimenko. The
data show that MIDAS is fully operational and its
performance not only fulfils, but exceeds, the scientific
requirements. Fig 2.8.1/1 shows an image of a calibration
sample taken during flight. Repeated imaging on the
same location confirms a reproducibility of the absolute
dimensions of the sample in the range of a few nm. This
result confirms the excellent mechanical performance of
the instrument as well as the favourable imaging
conditions aboard Rosetta. If all goes well with the
instrument and the mission as it journeys to the comet,
we shall for the first time be able to study the
morphology of dust grains at the nm level from one of
the early primitive bodies of the Solar System.
The interpretation of flight data and further optimisation
of instrument operational parameters are supported by an
intensive measurement programme using the flight spare
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Figure 2.8.2/1: A part of the CN R branch of the
average reduced spectrum of comet C/2000 WM1
(LINEAR) compared with the synthetic spectrum.
Top panel: synthetic spectrum (thick line) contains
only 12C14N. Bottom panel: the synthetic spectrum also
contains 13C14N and 12C15N, which result in an almost
perfect fit to the observed spectrum.
Figure 2.8.1/1: The MIDAS flight instrument shortly
before integration on the spacecraft. Below: the first
image taken in space during Rosetta’s commissioning
phase shows the cubed structure of an onboard
calibration sample. The 3-D view is rendered from
raw data.
Solar System. From the ground, such isotopic ratios can
in principle be determined by high-resolution
spectroscopy (R ≥ 700 000) of the resonancefluorescence bands of certain simple molecules
containing the relevant element. In the case of the 12C/13C
ratio, this has been done over the past two decades for a
few bright comets, whereby the observed molecules were
usually CN and C2, trace gas species typically present in
cometary comae.
model installed in a vacuum chamber within the SCI-A
laboratories. This model is used as a testbed for new inflight procedures as well as a tool for the scientific
interpretation of the flight data from the comet. For this
purpose, a large number of specific samples that
resemble different physical and chemical properties of
cometary dust were installed. Data and experience
gained during future studies will be collected and
inserted into a database. This includes the growing
knowledge of cometary materials from other space
missions. The PI-team supported by the RSSD Co-I
activity should be well-prepared to face the rigours of the
encounter in order to exploit and maximise the return
from this novel instrument.
The analysis of high-resolution spectra of comet C/1995
Q1 (Hale-Bopp) and C/2000 WM1 (LINEAR) resulted in
the optical detection of 12C15N, which permitted the
14
N/15N ratio in CN to be derived for the first time. The
14
N/15N ratios were determined to be 140±35 and 140±30,
respectively, which is significantly lower than the value
in Earth’s atmosphere, usually referred to as the Solar
System value of 272 (Arpigny et al., 2003a; b).
2.8.2 Determination of isotopic ratios in comets
It should be noted that, over the past 2 years, the 12C/13C
and 14N/15N isotopic ratios were determined in the CN
coma of 12 comets of different dynamical histories
(Jehin et al., 2004a). For all the comets studied so far, the
12
C/13C ratio is consistent with the Solar System value of
89, whereas the 14N/15N ratio is only half the Solar System
value. The results for two periodic comets have been
published (Jehin et al., 2004b).
Isotopic ratios of the light elements in comets are
important clues to the origin and early history of the
Although remarkably similar values have been derived
for the 14N/15N ratios in the CN coma of the different
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comets, this ratio is much lower than the ratio derived for
HCN from sub-mm measurements in comet Hale-Bopp
(323±46). HCN was generally believed to be the main
parent of CN. However, the observations of Hale-Bopp
indicate a discrepancy between the nitrogen isotopic
ratios in CN and HCN, which would suggest that here is
at least one additional, unknown parent of CN, with even
higher 15N excess. Organic compounds like those found
in interplanetary dust particles are good candidates
(Aléon et al., 2003). These new findings are under
detailed evaluation and sub-mm measurements have
been initiated to retrieve the nitrogen isotopic ratio in
comets from HCN.
41
vations on 11 February 2003, post-perihelion characterisation of this comet is now available, covering its
evolution along the orbit between 2.29 AU and 3.22 AU.
Broadband BVRI images and low-resolution long-slit
spectra have been obtained for morphological, colour
and compositional analysis of the coma and for studying
the comet’s activity along its orbit (Fig. 2.8.3/1). Various
observational techniques have been used to collect data
for the analysis of long-term and short-term variability,
from which conclusions on several nucleus properties
can be drawn (Schulz et al., 2004a, and references
therein).
Water production rates from SOHO/SWAN observations
2.8.3 Characterisation of the new Rosetta target
comet
Post-perihelion monitoring in 2003
A new target comet was identified for the Rosetta
mission after its launch to Comet 46P/Wirtanen, planned
for mid-January 2003, was cancelled. As soon as
67P/Churyumov-Gerasimenko became a likely new
target based on its classification and orbital parameters,
extensive monitoring of this comet began to determine a
number of basic properties. Starting with the first obser-
Figure 2.8.3/1: Structurally enhanced broadband R
images showing the evolution of the distinct features
in the coma of Comet 67P/Churyumov-Gerasimenko
between February and June 2003. The direction of the
Sun and the comet velocity vector are indicated.
MIDAS/AFM will provide the morphology of the
associated dust grains when orbit about the comet is
achieved in 2014.
Since January 1996, the SOHO/SWAN instrument has
been producing full-sky Lyman-alpha maps. The SWAN
images can be used to study the hydrogen coma of
comets down to a visual magnitude of ~12. After the
retargeting decision of the Rosetta mission, the SWAN
archive was searched for possible occurrences of
67P/Churyumov-Gerasimenko. The comet was identified
in Lyman-alpha images obtained during its 1996
apparition, and five values for the production rate of
neutral hydrogen were obtained. As cometary neutral
hydrogen comes predominantly from photodissociation
of water, SWAN observations can be used to estimate the
water production rate of a comet. The observations
suggest a perihelion water production rate of about
Figure 2.8.3/2: Colour-coded nucleus bulk density
(kg/m3) as a function of the spin axis obliquity, I, and
argument Φ. Black areas: prolate ellipsoidal model
nuclei cannot reproduce the observed light curve
amplitude. Dots: observed water production rates are
most closely reproduced. Solid-line areas: empirical
change in the longitude of perihelion is reproduced.
Dashed-line areas: empirical change in the longitude
of the ascending node is reproduced.
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8x1027 s–1 and a possible post perihelion increase of
activity (Mäkinen, 2004a).
Nucleus properties estimated from non-gravitational
force modelling
The nucleus size, shape, active area fraction, spin axis
orientation, mass and bulk density of Comet
67P/Churyumov-Gerasimenko have been estimated
using a sophisticated thermo-physical nucleus model.
The model has to reproduce simultaneously the empirical
nucleus light curve, water production rate versus time,
and non-gravitational changes of the orbital period,
longitude of perihelion, and longitude of the ascending
node (per apparition). The results suggest that the spin
axis argument is close to either 60° (obliquity 100-140°)
or 240° (obliquity 40-90°). Hence, the nucleus semi-axes
are likely to be roughly 2.5x1.9 km. The nucleus bulk
density is at most 500 kg/m3 and the active area fraction
is 4-11% (Fig. 2.8.3/2). If substantial deviations between
observed and calculated water production rates are
allowed (to account for uncertainties in the modelling
and observational errors), the spin axis orientation and
nucleus dimensions cannot be estimated, but a hard
upper limit on the nucleus bulk density of 600 kg/m3 can
be determined (Davidson & Gutiérrez, 2004).
2.8.4 Comet modelling
As a part of a project to study the cometary particle
environment, the research team has built a complex
particle simulator capable of producing fractal aggregates through collisional coagulation, and simulating
their evolution and dynamics in a cometary coma after
being expelled from the nucleus (Makinen, 2004b). This
self-consistent ballistic rigid-body particle colliding
simulator can be used to study the physical properties of
cometary particles, the particle environment of a comet,
and even the dynamics of a meteor in Earth’s atmosphere. It is capable of producing fractal aggregates of icy
particles modelled by hard or soft (metaball) spheres, to
be used for creating test particles in future statistical
studies of the cometary coma-particle interaction
(Fig. 2.8.4/1). Instead of a predefined sticking probability, actual surface interactions are modelled and a method
for calculating internal stresses and fragmentation of an
aggregate is described. Simulations suggest that taking
fragmentation into account has two major consequences:
increase in the fractal dimension of particles, and a
noticeable change in the mass spectrum of an ensemble.
The work continued on extracting the size distribution of
dust particles by using measurements of the scattered
light at a number of wavelengths. The method is based on
general light-scattering properties of particles with a
power-law size distribution and places no limitation on
particle shape or structure. A set of equations that relates
Figure 2.8.4/1: A slice through an irregular body
(outlined with solid grey at intersection surfaces) at
1 AU, depicting outgassing water molecule density.
The Sun is to the right.
five dust colours to five dust characteristics (power index
of the size distribution, the smallest and largest particle
sizes, scattering efficiency averaged over the size range,
and albedo ratio for the smallest and largest particles)
was applied to spectrophotometric observations of comet
C/1995 O1 (Hale-Bopp). The calculated solution
demonstrates how physical characteristics of comet dust
change with the distance from the nucleus and how they
vary for different dates of observations. The power of the
size distribution was found to exceed values found for
other comets and is quantitative evidence for the
overabundance of small particles in Comet Hale-Bopp
(Kolokolova et al., 2003).
2.8.5 Ground-based observations of comets
Comet 81P/Wild 2
The pre-perihelion monitoring of the coma morphology
of Comet 81P/Wild 2 revealed the presence of longlasting fan structures, which remained essentially
unchanged for at least 3 months. The compositional
coma analysis confirmed the depleted abundance of C2
with regard to CN in this comet. The results of the
observations led to the prediction that distinct coma
features were likely to be present at the time of the
Stardust flyby (Schulz et al., 2003); such features were
indeed detected by that spacecraft.
Comet C/2000 WM1 (LINEAR)
The gas and dust coma of comet C/2000 WM1 have been
characterised from the analysis of optical imaging and
long-slit spectroscopy. The gas coma showed a double jet
structure in CN and C2, which has no counterparts in the
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dust. The gas production rates, dust colour and particle
distribution in the coma have been investigated (Lara et
al., 2004). Near-IR observations led to the discovery of
two sublimating components in the coma, which possibly
originate from different kinds of organic material (Tozzi
et al., 2004).
2.9 Fundamental Physics
References
Aléon, J. et al. (inc. Schulz, R.), 2003, Lunar and
Planetary Science 34.
Arpigny, C. et al. (inc. Schulz, R.), 2003a, Science 301,
1522.
Arpigny, C., et al. (inc. Schulz, R.), 2003b, BAAS 35(4),
986.
Davidson, B.J.R., Gutiérez, P.J., 2004, BAAS, in press.
Jehin, E. et al. (inc. Schulz, R.), 2004a, presentation at
35th COSPAR.
Jehin, E. et al. (inc. Schulz, R.), 2004b, ApJ 613, L161.
Kolokolova, L. et al. (inc. Schulz, R.), 2003, J. Quantitative Spectroscopy & Radiative Transfer 79-80, 861.
Lara, L.M. et al. (inc. Schulz, R.), 2004, A&A 422, 717.
Mäkinen, J.T.T. in The New Rosetta Targets, 2004a,
Kluwer, The Netherlands.
Mäkinen, J.T.T., 2004b, Particle Accretion and Dissipation Simulator. I. Collisional Aggregation of Icy
Particles, submitted to Icarus.
Schulz, R., 2003a, Highlights of Astronomy, IAU, 13.
Schulz, R., 2003b, BAAS 35(4), 970.
Schulz, R., 2004, CNES Magazine No. 21.
Schulz, R. et al., 2003, A&A 398, 345
Schulz, R. et al., 2004a, in The New Rosetta Targets,
Kluwer, The Netherlands, 15-24.
Schulz, R. et al., 2004b, A&A 422, L19-L21.
Tozzi, G.P. et al. (inc. Schulz, R.), 2004, A&A 424, 325.
The LISA Pathfinder spacecraft will carry the European
LISA Technology Package (LTP) and a similar USprovided package (ST7). Both packages consist of two
free-floating test masses, each in capacitive sensor cages
(‘gravitational reference sensors’), which are the heart of
the drag-free control and an essential part of the LISA
mission. The purpose of both packages is to test a variety
of operational modes of the gravitational reference
sensors together with their associated µN-thrusters and
drag-free loops, and to verify their performance and
noise behaviour.
Research in Fundamental Physics is concentrated on
supporting the LISA Pathfinder and LISA missions,
particularly in the area of high-precision phase measurements and interferometry.
2.9.1 Interferometer design for LISA Pathfinder
The LTP interferometer is the diagnostic tool used to
monitor the test masses in all operating modes
continuously by measuring the distance between the two
test masses, the position of one test mass with respect to
the optical bench, the differential alignment of the two
test masses (with two sets of measurements: DC and
differential wavefront sensing), and the alignment of one
test mass with respect to the optical bench.
In the LTP, three heterodyne interferometers obtain these
measurements, two to measure the distance and the
alignment of the two test masses with respect to each
other and with respect to the optical bench, and one
interferometer to provide a reference signal (Fig. 2.9.1).
2.9.2 A phasemeter for LISA Pathfinder
To evaluate the change in optical path length, precise
determination of the phase of the heterodyne signal
(typically a few kHz) is needed. The implementation of
the phasemeter chosen for LTP is based on digitising the
datastream with a sufficiently high sampling rate (about
100 kHz). It obtains the in-phase and out-of-phase
components of blocks of input data with respect to a
reference signal derived from the nominal heterodyne
frequency. These components are then used to calculate
the phase of the interferometric signal with respect to the
reference signal. Data output occurs with a rate of 10 Hz.
A laboratory prototype of this phasemeter (Fig. 2.9.2/1)
has been employed successfully at the University of
Hannover (D), with the active involvement of the RSSD
reseach team, to measure the performance initially of a
breadboard prototype of the LTP interferometer (Heinzel
et al., 2004). The phasemeter, at that point still realised in
software on a standard PC, was used during the test
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Figure 2.9.1/1: The Engineering Model of the LTP
optical bench.
campaign of the Optical Bench EM for LTP to
demonstrate the compliance of the EM. In a later stage, a
full LTP phasemeter, with 12 channels, 16-bit A/D
converters, and the software implemented in an FPGA
has been realised.
Differential wavefront sensing
As LTP will use quadrant photodiodes (QPDs) for the
sensing of all the interferometric signals, it is possible to
obtain information regarding the alignment of the test
masses by comparing the relative phase of the
heterodyne signals coming from the four different
quadrants of the QPD.
During the test campaign for the optical bench EM, an
accuracy of better than 10 nrad/√Hz in the frequency
range relevant for LTP was achieved using this
technique.
Figure 2.9.2/1: Schematics of the
LTP phasemeter.
Figure 2.9.1/2: Layout of the LTP optical bench.
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2.9.3 Frequency stabilisation for LISA
2.10 Research Activities in SCI-A
One of the most critical issues for LISA is the need for a
laser that is stable enough in frequency to allow the
detection of gravitational waves. All of the current
strategies to achieve the required stability rely on a
combination of pre-stabilisation and numerical postprocessing of the data.
The Science Payloads and Advanced Concepts Office
performs research focused almost exclusively on the
needs of future ESA science missions, and specifically
on advanced payload technologies. Such technologies
are underpinned through a long-term coordinated
material science and micro-electronics programme
involving:
A particularly promising approach for a laser frequency
stabilisation is a control system in which the instantaneous laser frequency is compared to the laser
frequency; a round-trip time of about 33 s. Owing to the
long intrinsic delay, the ensuing control loop is nontrivial in design, and transients and the damping of the
initial conditions become important issues. García et al.
(2005) have successfully demonstrated the feasibility of
the stabilisation scheme, replacing the 5 million km
LISA arm by a 300 m delay line and the laser with a
voltage-controlled crystal oscillator. They were able to
demonstrate a noise suppression of about 40 dB up to the
frequencies comparable to the inverse delay. The initial
conditions on closing the control loop, i.e. the change of
the laser frequency during one round-trip time, were
predicted to be critical for the performance of the
stabilisation scheme. García et al. showed that the
influence of the initial conditions could be minimised by
a suitable time-dependence of the control loop’s gain
when closing the loop.
References
García, A. et al., 2005, Class. Quantum Grav. 22(10),
S235-S242.
Heinzel, G. et al., 2004, Class. Quantum Grav. 21(5),
S581-S587.
—
—
—
—
materials for advanced superconducting sensors;
novel semiconductor sensor materials;
materials for low-resource optics;
application-specific integrated circuits (ASICs).
2.10.1 Development of superconducting cameras
The superconducting sensor programme is one of the
longer-term advanced sensor development programmes
focusing on applications from the near-IR to the soft
X-ray band. It has considerable heritage and combines
basic research on the properties of novel superconducting
thin films with direct and immediate applications of more
traditional superconducting materials. Developments of
practical sensors are aided by proof testing on the ground
on astronomical telescopes, which provides RSSD and
community astronomers with the latest astronomy
instruments.
A considerable effort by SCI-AI in the Superconducting
Tunnel Junction (STJ) development programme was
focused on completing the next-generation optical
spectrophotometer, S-Cam3, for its first observation run
in July 2004. This system is capable of measuring
individual optical photon energy, position (imaging) and
arrival time (to ~1 µs). The improvements of the new
system over its S-Cam2 predecessor can be summarised
as:
— FOV increase from 4x4 arcsec to 11x9 arcsec. This
has major system-level implications as well as
bringing the S-Cam instrument closer to an
astronomical instrument with wider applications;
— optimised IR rejection filters, while extending the
‘red’ response;
— increased energy resolution;
— increased electronics readout speed and hence the
system’s photon rate capability;
— improved data-acquisition software robustness.
The first objective was met by a redesign of the detector.
The S-Cam3 detector is an array of 10x12 pixels, each
33x33 µm with 4 µm inter-pixel gaps. The increased
pixel size corresponds to ~0.8x0.8 arcsec on the sky. The
combined effect of a significant increase in pixel number
and slightly larger pixel size ensures uncompromised
photometry on point sources, even under poor seeing
conditions, and a more accurate background subtraction.
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Figure 2.10.1/2: Comparison of the overall detection
efficiency of S-Cam2 and S-Cam3. Future S-Cams are
intended to develop the read response beyond 1 µm.
Figure 2.10.1/1: The S-Cam3 array of 10x12 pixels
each of 33x33 µm. Note the large amount of wiring
required to connect yet isolate individual pixels
electrically.
Also, simultaneous imaging of more than one object
becomes possible, which is useful when observing
extremely weak objects. Fig. 2.10.1/1 shows a
micrograph of the S-Cam3 array and highlights the
complex photolithography involved in this technology.
The layup of the detectors is identical to the S-Cam2
arrays: 100 nm Ta with 30 nm Al trapping layers on
each side of a very uniform and thin oxide layer. The
best arrays show 100% pixel yield: all 120 pixels are
low-leakage STJs with typical leakage currents of
~30 pA. The responsivity (defined as the total collected
charge in electrons per eV of incident photon energy)
for the selected array is slightly increased from
~15000 e–/eV in S-Cam2 to ~18000 e–/eV in the current
devices.
For these kinds of detectors, the rejection of thermal-IR
photons is of crucial importance. The low energy gap of
Ta/Al STJs makes them sensitive to wavelengths up to
~1 mm. Since the detector is optically coupled to a 300K
environment, the IR-rejection filters have very tight
requirements. Simple calculations of attenuation factors
in the vicinity of the peak of the 300K blackbody
radiation could not, however, explain the excess in subgap current measured in S-Cam2. It was therefore
concluded that we were suffering from residual very
long-wavelength radiation. In order to optimise the
suppression of the longer wavelengths, while
simultaneously improving the throughput in the visible,
the filter glasses were changed and an additional filter
was added at 300mK. This, in combination with
improved baffling and shielding, reduced the IR load per
unit detector area by more than an order of magnitude.
Figure 2.10.1/2 is a comparison of the total efficiency of
S-Cam3 versus S-Cam2. These curves take into account
the measured transmissions of all optical elements as
well as the detector’s efficiency. The peak efficiency has
increased from ~22% in S-Cam2 to ~30% in S-Cam3.
The bandwidth (at 10% of maximum) has also increased
from 335-690 nm to 330-745 nm. With the combined
effect of reduced IR load and higher detector
responsivity, we have been able to measure a photon
wavelength resolving power R = 13 at 500 nm, up from
R = 8 in S-Cam2.
The electronic readout system for S-Cam3 was
completely redesigned. It allows in situ verification of
each individual pixel by means of I-V curve tracing.
Furthermore, the preamplifier signals are immediately
converted to the digital domain at up to 40 MHz
sampling rates. A Finite Impulse Response filter is
implemented for each channel in FPGAs, which can be
reprogrammed ‘on the fly’. This allows an optimisation
of the filter algorithm for either higher energy resolving
power or higher speed. After event detection, the data
stream is split in two. One is logged on a RAID system
for off-line post-processing, while the other will be
processed in the programmable hardware for quick-look
purposes. In this way, light curves and spectra are
displayed in real-time and updated every second without
compromising raw data logging or running the risk of
system failure due to computing or data-stream bottlenecks. Maximum count rates are > 8000 counts/s/pixel
and > 500 000 counts/s over the whole array. With such
a capability, astronomers now have an additional tool
with which to investigate very high-speed phenomena in
a wide range of objects.
In order to cool the detector to its operating temperature
of ~0.3K, a dewar in combination with sorption coolers
was used. This dewar can contain ~12 litres of liquid
helium. Contrary to S-Cam2, S-Cam3 uses a hybrid
4
He–3He sorption cooler combination. The hold time at
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Figure 2.10.1/4: Processed S-Cam3 image of a 16th
magnitude star showing the effect of differential
atmospheric refraction. With its intrinsic ability to
detect and measure the colour of every single photon
with a time resolution of below 1 µs, a wide range of
astronomical applications can be envisaged for this
technology.
Figure 2.10.1/3: S-Cam 3 cryostat (blue) with the four
banks of preamplifier units (32 channels per bank)
mounted. In the foreground are the relay optics and
filter wheel.
the base temperature of 285mK is in excess of 24 h. In
combination with ~18 h hold time of the helium bath,
this allows for uninterrupted stable operation throughout
the night and convenient recycling during daytime. The
complete system can be seen in Fig. 2.10.1/3.
S-Cam3 saw first-light during a 7-night observation
campaign at the 4.2 m William Herschel Telescope at La
Palma (E) in July 2004. The instrument performed
extremely reliably, with only 15 min of observation time
lost due to instrument problems. The observation
programme focused on the detection of temporal and
spectral variability in a number of targets. Data
processing and analysis is underway. Fig 2.10.1/4 shows
a processed image of a point source under fairly poor
seeing conditions. Using the detector’s intrinsic
wavelength resolution, the effect of differential
atmospheric refraction is clearly seen. Fig 2.10.1/5 is a
processed image of 9x11 arcsec in which five different
sources can be distinguished, including a galaxy in the
lower right part of the image. The star in the upper left
part is Mv = 19. Note that there is some distortion in this
image because some pixels were lost through
electrostatic discharge in the course of the S-Cam3 final
assembly.
S-Cam3 has taken the development and application of
superconducting sensors further along the road to
practical systems providing meaningful astronomical
data. Further developments focusing around far larger
fields of view (~1x1 arcmin) and closed-cycle cooling
are now underway. Such developments may mean that
Figure 2.10.1/5: A processed S-Cam3 image of a
9x11 arcsec field showing multiple points sources and
a single extended source, in this case a galaxy. Future
S-Cams will extend the field coverage to about
1 arcmin, allowing intrinsic multi-colour deep-field
imaging for extragalactic studies.
space-based applications in future science missions are
not so far away.
2.10.2 Advanced semiconductor sensors
While superconducting sensors will have serious
applications in future astrophysics missions, sensors
based on new semiconductor materials should also be
beneficial to not only astrophysics but also planetary
missions.
Long-term developments in semiconductor detector
research have included the production of pixellated
detectors fabricated from GaAs. Previous work on
monolithic diodes and small pixel arrays have shown
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Bump
Dedicated ASIC
Pixel
p-layer
Insulating I-Layer (40-400 µm)
Substrate N-Layer (2 µm)
X-ray Illumination
Figure 2.10.2/1: The approach to bump-bonding a
dedicated ASIC to a large-format GaAs array so that
each pixel can be read out independent of all others.
The inset shows an SnPb bump bond ~20 µm in
diameter.
Figure 2.10.2/3a: Left, the limiting energy resolution
achievable for a range of compound semiconductors
as a function of band-gap energy at 5.9 keV. For
completeness, included are the superconductors on
which S-Cam3 is based. Curves are given for average
values of the Fano factor: 0.22 for superconductors
and 0.14 for semiconductors. NBG and WBG show
the regions in which the narrow band gap and wide
band gap semiconductors lie. Materials science
research within SCI-AT/AI is covering the majority of
these materials.
Figure 2.10.2/2a: The Medipix GaAs array (64x64
pixels) together with the vias for the SnPb bumpbonds (inset).
unprecedented performance as X-ray spectrometers due
to the focus within SCI-AT on the fabrication of
extremely high-quality epitaxial GaAs material.
Spectroscopic performance approaches that of
conventional silicon detectors, but with important
advantages of higher temperature operation (owing to its
larger energy bandgap) and enhanced radiation damage
tolerance.
The most recent activity has centred on the production of
larger arrays that can be bump-bonded to readout ASICs
(Fig. 2.10.2/1). A method of thinning away the
supporting semiconductor substrate to expose the
detecting volume and processing the contacts to allow a
low temperature bonding to the readout chip matched to
the detector pixels has now been demonstrated.
Figure 2.10.2/2b: An X-ray image of a sardine taken
with the SCI-AT GaAs array coupled to a Medipx
ASIC (top). The optical image (bottom is shown for
comparison).
In lieu of a spectroscopic readout ASIC that is still in
development, an imaging system of the same physical
dimensions has been adopted from the medical imaging
community. A complete end-to-end demonstration of a
representative imager system has thus been possible, not
only demonstrating the necessary packing technology for
future space mission applications, but also affording a
significant spin-off in terms of improving existing
medical imager technology – GaAs can replace Si pixel
arrays with the benefit of improved spatial resolution and
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Figure 2.10.2/3b: Measured 241Am and 55Fe energy loss
spectra in (a) 1 mm2, 500 µm-thick Si detector; (b) a
1 mm2, 40 µm-thick GaAs detector; (c) a 3.142 mm2,
2.5 mm-thick CdZnTe detector; (d) a 7 mm2, 500 µmthick HgI2 detector. These wide-bandgap semiconductors are all suitable for applications in hard
X-ray and gamma-ray planetary physics and
astronomy.
lower patient dose through the enhanced detection
sensitivity (Fig. 2.10.2/2a, b).
This work is expected to continue with the transfer of the
same technology to the bump-bonding of a spectroscopic
readout ASIC. This will be concluded by the
demonstration of simultaneous imaging and spectroscopy at X-ray wavelengths. Such a technology would
then be suitable for a low-resource X-ray planetary
surface mapper, that in combination with suitable optics
(see Section 2.10.3) can map the surface distribution of
chemical elements. Indeed, this technology development
has already led the scientific community to want it to
form the baseline for the X-ray imaging spectrometer on
ESA’s BepiColombo mission to Mercury.
In addition to this specific development in GaAs,
research continues on a number of other materials
suitable for hard X-ray and gamma-ray astrophysics. The
study of imaging sensors based on the wide bandgap
semiconductors HgI2 and TlBr are particularly promising
(Fig. 2.10.2/3) for room-temperature operation in the
gamma-ray regime.
Finally, low-bandgap semiconductors are also now being
studied for the UV, EUV and soft X-ray part of the
spectrum as potential imaging photon-counting sensors
for astrophysics. Here the energy resolution would be
improved over Si-based sensors while the needs for very
low-temperature cryogenic cooling, such as required for
superconducting sensors, may be relaxed (Fig.
2.10.2/3a).
49
Figure 2.10.3/1: The improvements in the stacking
and orientation of fibres used in micro-channel plate
optics. On the left is the old technology with rounded
edges that impede stacking. At right is the current
improvement, together with a high-resolution image
of a few micro-channels, each ~10 µm in width.
2.10.3 Development of advanced optics
To enable future low-mass (hence lower cost) astrophysics missions, SCI-AT has been developing lightweight optics using a number of different technologies
for applications at X-ray and gamma-ray wavelengths.
Future developments include expanding this area of
research to optical and IR wavelengths in support of the
Cosmic Vision programme.
As an example of the power of this type of focused
research and development, consider the case of microchannel plate-based optics. Micro-channel plate glass
technology has been adapted for X-ray reflecting optics,
where square pore glass micro-channels efficiently
reflect X-rays up to a few keV in energy. When such a
glass plate is slumped to an appropriate shape, and two
plates located back-to-back, an approximation to
classical Wolter X-ray optics can be obtained. Recent
activities have centred on improving the metrology and
preparation of drawn glass fibres, together with
improvements in fibre stacking. Major improvement in
the quality of the micro-channels has allowed
improvements in performance (Fig. 2.10.3/1). Measurements made at synchrotron facilities confirm a
significant improvement in attainable resolution, to
~30 arcsec. The large open area factor guarantees a very
low density of the optics, such that a geometric area of
1 m2 will weigh only 25 kg. Clearly, such low-mass
optics have applications not only in astrophysics
missions but also as the optical part of an imaging X-ray
spectrometer for future planetary missions, such as the
BepiColombo mission to Mercury.
Notwithstanding this dramatic demonstration of
performance, a number of future applications in
astrophysics demand a much higher angular resolution in
order to resolve distant populations of galaxies forming
early in the Universe. For the XEUS mission, for
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(Fig. 2.10.3/3). This facilitates a mission concept for
XEUS that allows a 10 m2-class telescope to be
transportable to an L2 orbit.
It is through these types of developments, when coupled
with novel deployment techniques, that high-precision
low-mass optics may have serious applications on future
ESA science missions over a number of different
wavelengths. This may enable more demanding scientific
missions to be realised while still constraining costs.
2.10.4 Advanced instrumentation research for
planetary missions
Figure 2.10.3/2: An X-ray image of a point source
observed through the micro-pore optics. The
resolution is ~3 arcsec. Such a technology will have
wide applications for future ESA astrophysics
missions.
Figure 2.10.3/3: The low-mass micro-pore optics with
a resolution of ~3 arcsec and an area-mass density at
1 keV of 200 kg/m2 (left). At right is the full-sized
high-mass XMM optics, having a resolution of
~14 arcsec and an area-mass density of 2300 kg/m2.
example, a requirement (goal) of 5 (2) arcsec is necessary
to avoid confusion between faint objects. Another
technological solution has been developed to address this
need. With a long focal length, a conical approximation
to Wolter optics can be obtained with excellent
resolution. Such a conical approximation is realised with
silicon micropores that are fabricated by a chemomechanical ribbing of highly polished silicon wafers.
The structure is in principle light and self-supporting.
Prototype modules produced in the last year have been
measured at synchrotron facilities (Fig. 2.10.3/2) and
shown already to offer an angular resolution of
~3.5 arcsec FHWM, sufficient to meet the requirements
of XEUS. The area density of this technology allows a
significant area-mass density advantage over, for
example, the XMM-Newton replicated optics approach
The Planetary Exploration Studies Section is involved in
a wide range of research and development activities for
remote sensing and in situ instrumentation for planetary
applications of future missions. The aim is to develop
scientific instruments with reduced resource demands
(power, mass, volume, number of interfaces, etc) by
miniaturisation, integration and use of the most recent
technologies. This approach leads to sophisticated
instrument suites for smaller and less demanding science
missions and enables new mission profiles at reduced
costs. Breadboards of several key instruments and
instrument suites are under development to demonstrate
scientific performance under environmental conditions
and to allow a better understanding of the operational
needs of future missions and the associated scientific
instrumentation.
Exploitation of missions in orbit or under development,
such as SMART-1, Mars Express, Venus Express,
Rosetta and Huygens, is also supported to investigate
Figure 2.10.4/1: Refraction and total reflection at an
interface between two media with refractive indices
n1 and n2 (n1 < n2). The exponential decay of the
electric field in a layer close to the interface, in the
case of total reflection, is indicated and the symbol of
a water molecule on the surface is shown.
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current limitations, fields for further improvements,
applicability of technology development and to define
further needs of future enabling key technologies.
Listed below are the most important activities currently
under study. These developments are performed in close
cooperation with various scientific institutes, industrial
partners, national agencies and several ESA departments.
A summary of a few of these developments are also
provided below to complement the list. Note: FM =
Flight Model, LM = Laboratory Model; BB = breadboard; dev/ment = development..
Research & Development
Highly Integrated Payload Suites (HIPS)
Laser altimeter (surface topography
from orbit)
Atomic Force Laboratory,
metrology and MIDAS
Rover (surface science with mobility)
Mole (subsurface science)
Heat flow and physical properties
package (for the Mole)
Geochemistry package (for Rover)
[alternative to LMS]
Laser Mass Spectrometer (LMS)
LIBS-RAMAN spectroscopy
Attenuated Total Reflection
Spectrometer (ATR)
Luminescence surface dating
(sample age determination)
Melting probes (subsurface science)
3-axis fluxgate magnetometer
front-end ASIC
Subsurface & surface radar
(topography & subsurface science)
Status
Target
level
dev/ment
BB
study
BB
FM
BB
LM
study
LM,
FM
EM
BB
BB
LM
BB
BB
study
BB
BB
BB
study
BB
dev/ment
BB
FMASIC
& BB
BB
study
Attenuated Total Reflection (ATR) Spectrometer
Figure 2.10.4/2: The Nanokhod rover under
development within D/TEC. The payload cab can
accommodate the LMS together with a micro-camera
or an alternative geochemistry package under
development within SCI-AP, comprising an alphaproton-X-ray and Mossbauer spectrometer.
Figure 2.10.4/3: Laboratory prototype of a packetsized mass spectrometer. The oversized power
connector and lens holder would be eliminated for a
flight version.
The starting approach here has been to consider the
detection of water sublimations on subsurface soil grains
on Mars with a miniaturised spectrometer based on the
Fahrenfort principle (Fig. 2.10.4/1). Initial tests with
commercial equipment have led to promising results that
indicate the elemental composition of the grain itself may
also be derived. The goal for the instrument front-end is
a diameter smaller than 3 cm, so as to be accommodated
as part of the payload of the mole that isalso under
development for subsurface investigations.
Laser mass spectrometer (LMS)
This instrument is being developed together with the
University of Berne to be accommodated inside the
payload cab of a microrover (Fig. 2.10.4/2). Early results
Figure 2.10.4/4: LMS flight-like electronics for the
second prototype spectrometer (laser control
circuitry and high-voltage power supply).
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from the first rover prototype LMS, with dimensions of a
few cm, its total mass and a laser source similar to those
envisaged for the flight model are very promising
(Fig. 2.10.4/3). A mass resolution and transmission in
good agreement with simulations have been achieved.
The mass resolution is sufficient to resolve adjacent
isotopes clearly when used with laboratory dataacquisition hardware. Work is ongoing to improve the
hardware: final miniaturisation of the electronics and
optics, and setting up a laboratory testbed for
performance verification and further improvements
(Fig. 2.10.4/4).
3-axis flux gate magnetometer
An ASIC containing the complete front-end electronics
for a 3-axis fluxgate magnetometer is under development. An integrated sigma-delta converter is used to
sample the output of the three magnetometer coils. The
output is passed through an integrated decimation filter
unit. Up to four housekeeping data channels are
supported on chip. Data output and instrument control is
provided via a synchronous serial interface. All required
excitation signals are also provided by the ASIC.
Experience gained through the successful and completed
development and application of the Particle Detector
Front End (PDFE) ASIC, which is due to fly on the
NASA STEREO mission within the IMPACT instrument
suite, has been used to ensure that an instrument on a
single chip can be developed. The development, research
and verification of the magnetometer ASIC is expected to
be a leading example for further integration of instrument
front-ends on ASICs.
MIDAS
An atomic force microscope has been successfully
developed into a flight model and accommodated on the
Rosetta mission. Laboratory tests are beingperformed
with a commercial AFM and with the spare FM to build
a reference database. This experience may well lead to
the design of a much lower-resource instrument for
incorporation into the payload of future planetary
missions based around mini-satellites.
research activities
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3.
SCIENTIFIC SUPPORT ACTIVITIES IN RSSD & SCI-A
3.1
Astrophysics Missions Division
3.4
Fundamental Physics Missions Division
3.1.1
3.1.2
3.1.3
3.1.4
3.1.5
3.1.6
3.1.7
3.1.8
3.1.9
3.1.10
3.1.11
3.1.12
3.1.13
Introduction and overview
Herschel
Planck
Eddington
COROT
Gaia
JWST
Astro-E2
Darwin
XEUS
Lobster-ISS
ROSITA
EUSO
3.4.1
3.4.2
3.4.3
3.4.4
3.4.5
Introduction and overview
LISA Pathfinder
LISA
ACES
Microscope
3.5
Space Telescope Operations Division
3.5.1
3.5.2
3.5.3
3.5.4
3.5.5
HST observation programme
Special HST programmes
Instrument status
The European Coordination Facility
HST operational status
3.2
Solar and Solar-Terrestrial Missions Division
3.6
3.2.1
3.2.2
3.2.3
3.2.4
3.2.5
3.2.6
3.2.7
Introduction and overview
Ulysses
SOHO
Cluster
Double Star
Solar Orbiter
Solar-B
Science Operations and Data Systems
Division
3.3
Planetary Missions Division
3.6.1
3.6.2
3.6.3
3.6.4
3.6.5
3.6.6
3.6.7
3.6.8
Introduction and overview
ISO
XMM-Newton
Integral
Astro-F
Herschel Science Centre development
Information technology support activities
Archive and Virtual Observatory activities
3.3.1
3.3.2
3.3.3
3.3.4
3.3.5
3.3.6
3.3.7
Introduction and overview
Cassini/Huygens
Rosetta
Mars Express
Venus Express
BepiColombo
SMART-1
3.7
Science Payload and Advanced Concepts
Office
3.7.1
3.7.2
3.7.3
3.7.4
3.7.5
Science Payload Instrument Section (SCI-AI)
Science Missions Section (SCI-AM)
Planetary Exploration Studies Section (SCI-AP)
Advanced Technology Section (SCI-AT)
Darwin special project group
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55
Section 3 addresses the contributions of RSSD and
SCI-A staff to the mission-related activities of the
Department and Office. These encompass ESA’s science
missions in their orbital and post-operations phases, the
approved missions under or awaiting development, and
missions under study. ‘Europeanised’ missions led by a
national agency and potential International Space
Station (ISS) payload elements are also included.
The chapter is structured by Division, reflecting the
RSSD organisation at the end of the reporting period
(see Table 1). As stated in Section 1, RSSD has four
Mission Divisions (Sections 3.1-3.4) and two
Operations Divisions (Sections 3.5 and 3.6). The
responsibilities of the Science Payload and Advanced
Concepts Office, which are independent of RSSD
although closely associated, are summarised in
Section 3.7.
For astronomy missions (excluding HST), the
Astrophysics Missions Division has responsibility for
Project and Study Scientist support until in-orbit
commissioning. Responsibility for the development and
execution of science operations and, after completion of
the in-orbit commissioning phase, for the mission
management rests with the Science Operations and Data
Systems Division. Responsibility for mission management of Solar, Solar-Terrestrial and Planetary Missions
during operational phases remains, however, with the
respective Mission Division. The Space Telescope
Operations Division hosts the ESA staff supporting the
Hubble Space Telescope Science Institute (STScI) in
Baltimore (US) and the European Coordinating Facility
(ST-ECF) in Garching (D).
For the sake of brevity, the instruments, Principal
Investigators, mission or interdisciplinary scientists,
science team members etc. of the missions described are
not tabulated here. Such information may be found in
ESA’s Report to COSPAR, the most recent being ESA
SP-1276 (July 2004), produced by the RSSD Project
Scientists, and in the relevant Web pages (the addresses
are included here as footnotes with each mission
description).
Table 2: Research and Scientific Support Department 2004 – Projects and Studies.
Division
Astrophysics
Missions
Missions in
Operation or
Post-Operation/
Archive Phase
Solar &
Terrestrial
Missions
Planetary
Missions
Ulysses
SOHO
Cluster
Double Star
Cassini/
Huygens
Rosetta
Mars Express
SMART-1
Venus Express
BepiColombo
Missions in or
awaiting
development
Herschel
Planck
Eddington
JWST
Gaia
COROT
Solar Orbiter
Mission and
ISS Payload
Studies
Darwin
XEUS
ISS*
ILWS
Solar-B
* Lobster-ISS, EUSO, ROSITA
Fundamental
Physics
LISA
Microscope
LISA Pathfinder
ACES
Space
Telescope
Operations
Science Ops.
& Data
Systems
HST
ISO
XMM
-Newton
Integral
Astro-F
Herschel
science ops.
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Astrophysics Missions Division
Madrid, Spain, the location of the Herschel Science
Centre during operations.
3.1.1 Introduction and overview
The past 2 years brought their share of good and bad
news. On the sour side, the financial situation of the
Science Programme forced the cancellation of the
Eddington mission by the SPC at the end of 2003. This
was particularly sad given the strong scientific case of
Eddington and its wide support in the scientific
community. The latter is illustrated by the highly
successful Eddington workshop organised by the
Division in April 2003 in Palermo. The excellence of
Eddington was also reaffirmed in 2004 by the SPC, who
recommended that it should be the first mission to
implement if additional money could be found.
The Columbia Shuttle accident in 2003 and the US
decision to terminate the ISS and Shuttle programmes
soon after 2010 were serious drawbacks to various
projects under study in the Division. The Division’s
Study Scientist, supported by the D/HME Study
Manager, expended considerable effort in investigating
alternative launch scenarios for the EUSO high-energy
cosmic-ray payload. However, mostly due to its large
size and mass, it soon became clear that there would be
no credible transportation system to lift EUSO into orbit
and install it on the ISS. Irrespective of these
programmatic uncertainties, the AWG and FPAG jointly
re-examined the science case of EUSO during Spring
2004. Both working groups confirmed that the scientific
potential of EUSO was excellent but not among their top
priorities, and therefore did not recommend its
continuation into Phase-B.
The early retirement of the ISS was also potentially bad
news for XEUS because the original mission profile
foresaw assembling the mirrors in orbit at the Station.
Fortunately, a breakthrough in the development of light
X-ray mirror technology by SCI-A meant that the ISS is
no longer needed and that a 10 m2 mirror spacecraft can
be injected directly into an L2 orbit by an Ariane-5-type
launcher at a much reduced cost.
The gradual build-up of the Herschel Science Centre
(HSC) operations team continued throughout the period.
Members of the team spent extensive periods at the PI
institutes, working together with the PI teams to prepare
for the scientific operations of Herschel, and for the
calibration of its instruments. They were deeply
involved in the Instrument Level Tests (ILTs)
successfully carried out in Autumn 2004. The Herschel
Common Science System (development led by RSSD)
was used to support the ILTs and archive the test data.
This rather hectic period ended happily with the delivery
of the instrument cryo-qualification models to ESA in
late 2004. The HSC team is now busy preparing the first
call for observing proposals, which will be issued in
2006. In April 2005, the team will relocate to ESAC near
With five staff in place, the small team in the Planck
Science Office is now complete. The development is well
under way by RSSD of the software tool needed to
evaluate the quality and completeness of the survey data
and replan Planck operations if necessary. The
publication of the first WMAP results suggest that the
detection of the so-called CMB polarisation B mode by
Planck is a real possibility, thereby enhancing the
scientific case for the mission even further.
RSSD activities in support of Gaia have also picked up
momentum. Most prominent is the development, under
RSSD responsibility, of a prototype data-analysis system.
This Gaia Data Access & Analysis Study (GDAAS) is
intended to demonstrate the feasibility of reducing the
1000 TB expected from the 5-year mission and of
iteratively extracting the positions and proper motions of
~1 billion sources. A milestone was achieved in late
2004, with the processing of 18 months of simulated data
and the successful recovery of 200 000 stars.
RSSD activities in support of JWST have also gained
significant momentum over the last 2 years, as the
project transitioned from its definition phase into
implementation. In late 2003, one new staff member was
added to the Division to assist the JWST Project
Scientist. Both have been busy defining the scientific
capabilities and detailed technical specification of
NIRSpec, an instrument that is being developed and
financed by ESA. They prepared the JWST Science
Management Plan, which was subsequently approved by
the SPC. The NIRSpec Instrument Science Team was
later appointed, to provide scientific guidance to the
Project Scientist.
3.1.2 Herschel
The Herschel Space Observatory is a multi-user
observatory-type mission targeting the 57-670 µm range
in the far-IR and sub-mm, providing observation
opportunities for the entire astronomical community.
Herschel is scheduled for launch in mid-2007.
Herschel is designed to address the ‘cool’ Universe; it
has the potential of discovering the earliest epoch protogalaxies, revealing the cosmologically evolving AGNstarburst symbiosis, and unravelling the mechanisms
involved in the formation of stars and planetary system
bodies. A major strength of Herschel is its photometric
mapping capability for performing unbiased surveys
related to galaxy and star formation. Redshifted ultraluminous IRAS galaxies (with SEDs peaking in the 50100 µm range in their rest frames), as well as class 0
proto-stars and pre-stellar object SEDs, have their
maximum emission in the Herschel prime band. Herschel
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shared with Planck. It will operate from the vicinity of
L2, which is situated 1.5 million km away from the Earth
in the anti-sunward direction. It offers a stable thermal
environment with good sky visibility. Commissioning
and performance verification will take place en route to
L2. Once these crucial mission phases have been
accomplished, Herschel will enter routine science
operations for a minimum of 3 years.
The scientific operations of Herschel will be conducted
in a novel decentralised manner. The operational ground
segment comprises six elements:
— the Herschel Science Centre (HSC), provided by
ESA;
— three dedicated Instrument Control Centres (ICCs),
one for each instrument, provided by their PIs;
— the Mission Operations Centre (MOC), provided by
ESA;
— the NASA Herschel Science Centre (NHSC)
provided by NASA.
The HSC acts as the interface to the science community
and outside world in general, supported by NHSC for the
US science community. The HSC/NHSC provides
information and user support related to the entire lifecycle of an observation, from calls for observing time,
the proposing procedure, proposal tracking, data access
and data processing, as well as general and specific
information about using Herschel and its instruments.
Figure 3.1.2/1: An artist’s view of the Herschel
satellite as developed by Alcatel.
is also well equipped to perform spectroscopic follow-up
observations and further characterise interesting
individual objects.
Herschel’s telescope is passively cooled (to maximise
size), while the three focal-plane instruments are housed
inside a superfluid helium cryostat, on top of which the
telescope is mounted. The instruments are provided by
consortia led by PIs who get guaranteed observing time
in return. The Photodetector Array Camera and
Spectrometer (PACS) is a camera and low- to mediumresolution spectrometer for wavelengths up to 210 µm.
The Spectral and Photometric Imaging Receiver (SPIRE)
is a camera and low- to medium-resolution spectrometer
for wavelengths longer than 200 µm. The Heterodyne
Instrument for the Far-Infrared’ (HIFI) instrument is a
heterodyne spectrometer. It offers very high velocity
resolution for a single pixel on the sky.
Herschel (Fig. 3.1.2/1) will be launched on an Ariane-5
RSSD is responsible for building the science groundsegment infrastructure for performing these tasks,
together with the ICCs. One single system that evolves
over time, rather than having separate systems for
different mission phases, is being built. The initial
version of this system has been delivered to the
instrument teams and was successfully used to support
the instrument-level tests during Autumn 2004. The
observation planning subsystem is based on the NASA
Spot tool used by Spitzer. In this way, not only is the
effort that went into building Spot reused, but previous
Spitzer users will immediately feel at home, increasing
their scientific productivity. SCI-SA personnel are
deeply involved in providing scientific guidance and
supervision to the HSC software developers and
performing the usual user acceptance tests. In the course
of 2004, SCI-SA personnel in the HSC spent a large
amount of time collocated at the PI institutes together
with the instrument teams, first preparing and later
executing the ILTs. In this way, they not only provided
useful support to the PI teams, but they also acquired
first-hand experience with the Herschel instruments.
The HSC SCI-SA scientists have also been busy
preparing or upgrading the large amount of
documentation required for the scientific operations of
Herschel, in particular concerning the observation
scheduling, the calibration of the observatory and
support to the scientific community.
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In order to promote Herschel awareness in the scientific
community, SCI-SA personnel have also been busy
delivering talks and organising conferences related to
Herschel science. In 2004 alone, there have been:
Telescope
Instruments
— a special session on Herschel at American
Astronomical Society Meeting 204 in Denver, USA
on 3 June 2004;
— the Beyond Spitzer and Herschel conference in
Pasadena, USA on 8 June 2004;
— several Herschel presentations at the SPIE
conference on Astronomical Telescopes and
Instrumentation in Glasgow, UK on 21 June 2004;
— The Dusty and Molecular Universe: A Prelude to
Herschel and ALMA conference in Paris on
27 October 2004;
— a workshop dedicated to the calibration of Herschel
in Leiden, NL on 1-3 December 2004.
Shields
Solar array
Service Module
Interface
to Ariane
Figure 3.1.3/1: The current configuration of the
Planck satellite, as developed by Alcatel Space (F).
On request from the Astronomy Working Group
chairman, the Project Scientist also presented the status
of Herschel to the AWG twice during the reporting
period.
At the time of writing, all SCI-SA personnel in the HSC
are in the process of relocating to the European Space
Astronomy Centre (ESAC) near Madrid (E), from where
Herschel science operations will be conducted.
3.1.2 Planck
In late 1992, the COBE team announced the detection of
intrinsic temperature fluctuations in the Cosmic
Background Radiation Field (CBRF), observed on the
sky at angular scales larger than ~10°, and at a brightness
level ∆T/T ~ 10–5. In February 2003, the WMAP team
announced results on scales of about 15 arcmin with a
similar sensitivity (see http://lambda.gsfc.nasa.gov for
detailed descriptions of both COBE and WMAP). These
fluctuations have been interpreted as due to differential
gravitational redshift of photons scattered out of an
inhomogeneously dense medium. They thus map the
spectrum of density fluctuations in the Universe at a very
early epoch. This long-sought result established the
Inflationary Big Bang model of the origin and evolution
of the Universe as the theoretical paradigm. However, in
spite of the importance of the COBE and WMAP
measurements, many fundamental cosmological
questions remain open. Building on the pioneering work
of COBE and WMAP, the main objective of the Planck
mission is to map the fluctuations of the CBRF with an
accuracy that is set by fundamental astrophysical limits,
allowing us to address these fundamental questions.
Planck was selected in late 1996 as the third Medium
mission (M3) of ESA’s Horizon 2000 Scientific
Programme, and is now part of its ‘Cosmic Vision’
Programme. The observational goal is to mount a single
http://www.rssd.esa.int/planck/
space-based experiment to survey the whole sky with an
angular resolution as high as 5 arcmin, a sensitivity
approaching ∆T/T ~ 10–6, and covering a frequency range
wide enough to measure and remove all possible
foreground sources of emission. The main scientific
result of the mission will be an all-sky map of the CBRF
fluctuations and their polarisation. In addition, the sky
survey will be used to study in detail the very sources of
emission that ‘contaminate’ the cosmological signal, and
will result in a wealth of information on the dust and gas
in both our Galaxy and extragalactic sources.
The Planck payload consists of a 1.5 m-diameter offset
telescope, with a focal plane shared by clusters of
detectors in nine frequency bands covering 30-900 GHz.
The three lowest bands (up to ~70 GHz) are covered by
HEMT-based receivers actively cooled to ~20 Kby an H2
sorption cooler. The higher frequency bands are handled
by arrays of bolometers cooled to ~100mK; the H2
sorption cooler provides pre-cooling for a JouleThomson 4K stage, to which a dilution refrigerator is
coupled.
Since 2002, the instrument development has intensified.
The qualification models have been largely
manufactured and are now undergoing test. The first
delivery to ESA was made in late November 2004, for
integration into a full qualification satellite. This model
will be tested in early 2005 in a specially designed cryochamber at the Centre Spatial de Liege (B). The flight
models are under manufacture and will be delivered to
ESA in mid-2005. After long and complex testing, the
satellite will be launched from Kourou in mid-2007.
At RSSD, activity in the past 2 years has concentrated on
the build-up of the Planck Science Office (PSO), which
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is in charge of overall scientific coordination, survey
planning, archiving of the final data products and their
distribution to the community. Support scientists and
engineers have recently joined the group, which will
move in late 2006 to its final location at ESAC. Many
new documents have been written by PSO staff during
the reporting period, among which the Calibration
Requirements document, the Planck Science Operations
plan and the Calibration and Performance Verification
Phase Science Operations Plan. PSO scientists have also
defined the baseline Planck scanning strategy as well as
the requirements on the Planck Survey Planning and
Performance evaluation Tool, and they continue to
provide scientific guidance and supervision to its
software developers. As for Herschel, the PSO scientists
have spent long periods at the HFI and LFI institutes to
support the ILTs.
The cancellation of the LFI 100 GHz channel by ASI in
2002 was a severe blow to the Planck scientific
capability because it removed the possibility to measure
the CMB polarisation at this critical frequency, where
contamination by foreground sources is minimal. The
Project Scientist successfully sought a resolution from
the AWG stressing the scientific importance of 100 GHz
polarisation measurements. This resolution helped the
HFI PI to convince NASA to provide the extra funds
required to finance the development by JPL of polarisation-sensitive bolometers at this critical frequency.
The Project Scientist, assisted by the Planck Science
Team, has updated the scientific case for the Planck
mission. The revised document, which takes into account
the exciting results obtained by WMAP, will be released
in mid-2005. Far from weakening the case for Planck, the
WMAP data actually enhance it. In particular, the
tentative detection of a very early re-ionisation epoch
makes it much more likely that Planck will be able to
detect the so-called polarised B-mode signal of the CMB
that carries information about primordial gravitational
waves generated during the inflation era. The Project
Scientist also updated the Science Management Plan, the
highest-level document governing the implementation of
the Planck mission. The revised document was approved
by the SPC in early 2004. The most important
modification is the introduction of an Early Release
Compact Source Catalogue (ERCSC), to be published
9 months after the completion of the first all-sky survey.
The idea behind the ERCSC is to allow follow-up
pointed observations with Herschel of the many compact
millimetric sources that Planck will discover, including
several hundreds clusters of galaxy.
SCI-SA personnel have also organised several
conferences and workshops to promote awareness of the
Planck mission in the scientific community, including the
Second Planck Symposium Setting the Scene, held in
Orsay (F) in January 2004 and attended by more than 200
scientists.
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3.1.4 Eddington
The Eddington mission has two main scientific goals:
— the detection of habitable planets orbiting other stars,
and the determination of their frequency of occurrence and characteristics in different environments;
— the understanding of the formation and evolution of
stars across a wide range of key stellar characteristics (age, chemical composition, mass).
While planets will be detected by looking for the small
but measurable decrease in a star’s light caused by a
planet’s transit, stellar structure and evolution science
will make use of asteroseismic techniques. These will
study stellar oscillations, as has been done with the Sun
for a number of years. Both techniques require long-term
very high-accuracy photometric time series (which can
be obtained only from space) and thus can naturally be
carried out by the same payload.
The original Eddington proposal, submitted in response
to the 2000 call for the F2/F3 missions, was based on a
monolithic 1.2 m-diameter telescope with a large-area
CCD mosaic. In May 2002, Eddington was approved as
an element of the Science Programme by the SPC, with
a 2009 launch date. Two parallel industrial definition
studies were conducted, with Astrium Germany and
Alcatel as prime contractors. These involved the
complete space segment, including the payload, which is
baselined to be ESA-procured. Both contractors
converged to a similar payload design, involving three
identical, parallel telescopes with a total collecting area
of ~0.7 m2 and a six-CCD focal plane. Each telescope has
a different filter, so that the resulting light curves offer
colour information (a unique characteristic of
Eddington).
In parallel, a development activity carried out with E2V
as prime contractor resulted in the development of the
CCD chips for the Eddington focal plane, with the first
CCD chips produced and qualified. These are based on
an existing design but are produced in a large, custom
format tailored to the Eddington focal plane.
Organised by RSSD, the second Eddington workshop
took place in Palermo (I) in April 2003, attracting more
than 150 scientists. The new instrumental configuration
was presented to the community, and significant progress
was made in the selection of the candidate fields for the
3-years planet-finding observation. This resulted in the
selection of the Lacerta field announced a few months
later. Later in 2003, an AO for the Eddington Science
Team was run, and resulted in the selection by AWG of
eight scientists.
Unfortunately, at the end of 2003 the financial situation
of the Science Programme required deep cuts in the
programme. Notwithstanding the high scientific rating
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given to it by the ESA advisory structure, it was decided
to remove Eddington from the programme, and to stop
all development activities. At a meeting in 2004, the SPC
reaffirmed the scientific interest of Eddington, and
recommended that, should fresh resources become
available to the Science Programme, Eddington would be
the first mission to be implemented.
3.1.5 COROT
COROT is a CNES-led mission for high-accuracy
photometry, with both asteroseismology and extrasolar
planet-finding among its science goals. With its 27 cmdiameter telescope and 2.8x2.8° FOV, COROT will
concentrate on a limited number of relatively bright
targets, and will be the first mission to perform a spacebased search for exoplanets with the transit method.
In return for its contribution to the telescope optics and to
the payload test and integration, the ESA Science
Programme has negotiated data rights for scientists based
in ESA member countries. To this effect, an AO was
issued in 2002, which drew a large response from the
European astronomical community, and which has
resulted in the selection of a number of teams that have
since then become significantly involved in the
development of the mission.
As a member of the COROT steering committee, the
SCI-SA Study Scientist oversees the scientific aspects of
the project, in particular the definition of the observing
programme. His role is also to protect the scientific
interests of the European teams involved in COROT.
COROT is on track for launch in the third quarter of
2006.
3.1.6 Gaia
Since June 2002, Gaia has been a confirmed mission
within the ESA Cosmic Vision 2020 science programme,
with a target launch date of mid-2011. Gaia will build on
the observational principles of Hipparcos to measure
detailed properties of the brightest 1 billion stars.
Astrometric accuracies of 10 microarcsec at 15th
magnitude should lead to 20 million stars measured with
distance accuracies of better than 1%, and more than 100
million better than 5%. Tangential velocities will be
measured astrometrically at better than 1 km/s for about
100 million stars, while the dedicated radial velocity
spectrometer will gather radial velocities to 1-10 km/s to
16-17 magnitudes, depending on spectral type. Gaia will
provide multi-colour (in 11 medium and 5 broad bands),
multi-epoch (of order 100 epochs over 5 years)
photometry for each object to 20th magnitude, with great
care being invested in devising the photometric bands to
maximise their astrophysical diagnostic power. Scientific
http://sci.esa.int/corot
Figure 3.1.6/1: Artist’s impression of the Gaia
satellite.
preparations for the mission involve the participation of
some 15 working groups, taking responsibility for
(amongst other aspects) the accuracy modelling, the
radial velocity instrument optimisation, preparation of
simulated data, and the development of a data processing
framework to handle the complex and large (of order
1 Petabyte) Gaia data set.
The status of the satellite and payload was presented to
ESA and the Gaia science team at the mid-term
presentations of the definition phase, held in September
2004 at ESTEC. The two industrial teams, Alenia/Alcatel
and EADS-Astrium, separately presented the status of
their detailed studies into all aspects of the Gaia satellite.
These definition studies will run until mid-2005.
Technical prototypes of many parts of the Gaia satellite
are now under development, including the silicon carbide
primary mirror, and engineering models of the
astrometric focal plane with flight-representative CCDs.
The final catalogues resulting from the Gaia mission are
not expected to become available until at least 2-3 years
after the end of mission operations, i.e. in about 2018
according to current planning. However, early release
catalogues of astrometry and photometry are foreseen
from early on in the mission phase.
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The Project Scientist interfaces with the ESA Gaia
Project Team, chairs the Gaia Science Team, which takes
overall responsibility for all aspects of the scientific
development of the mission, including coordination of
the scientific working groups, and leads a small team in
ESTEC supporting the community in developing plans
for the analysis of the huge quantity of data that will
result from the mission. At the science team level, this
involves monitoring and contributing to the satellite and
payload design through analysis and independent
modelling, and directing and coordinating the work of
the 14 scientific working groups. These cover payloadrelated aspects (such as accuracy modelling, on-board
detection, photometric system instrument definition,
radial velocity instrument definition); in-depth studies of
specific classes of objects that present particular
problems during the observations or data analysis phase
(such as binary stars, double stars, Solar System objects,
and reference frame definition), and aspects related to the
data analysis (database design, prototype reduction
system development, Grid-related studies and algorithm
coordination). Altogether, some 250 member-state
scientists are participating in these Gaia activities.
The RSSD Project Scientist support team, under
direction of the Project Scientist, supports the scientific
community in this coordination effort, and takes a lead in
the accuracy analysis, parameter database definition,
CCD performance and calibration, telemetry definition
and coordination of the data analysis prototype.
The status of the scientific contributions and preparations
for the Gaia mission were presented at The Three
Dimensional Universe with Gaia, a major symposium
held at the Observatoire de Paris, Section de Meudon (F),
during 4-7 October 2004, and attended by 240
participants.
Details at http://www.rssd.esa.int/Gaia include up-todate news, meetings of the working groups, information
sheets, presentation material, and outreach features.
61
perpetual shadow by means of a large deployable
sunshade. Further cooling of the mid-IR instrument is
achieved by a dedicated solid-hydrogen cryostat.
ESA’s participation in the mission was formally
approved by the SPC in October 2000, and consists of
four components:
— provision of NIRSpec, the Near-IR Multi-Object
Spectrograph covering 1-5 µm;
— provision of 50% of MIRI, the Mid-IR combined
Camera/Spectrograph covering 5-28 µm (through
special funding from the ESA member states);
— provision of the Ariane-5 launcher that will carry the
observatory to L2;
— contributions to JWST operations.
In return for its contributions, ESA will gain a ~15%
partnership in JWST and secure for astronomers from its
member states full access to the JWST observatory on
identical terms to those enjoyed today on HST: they will
have representation on all advisory bodies of the project
and will win observing time on JWST through a joint
peer-review process, backed by a guarantee of a
minimum ESA share of 15%.
Over the reporting period, the JWST observatory and its
instruments successfully transitioned from the definition
phase to the implementation phase. Following the NASA
selection of Northrop-Grumman Space Technologies as
the US Prime Contractor, the observatory underwent an
extended ‘re-plan’ exercise, the outcome of which
resulted in the present 16-element 6.55 m-diameter
telescope design and 4-instrument payload suite
(NIRCam, NIRSpec, MIRI and FGS-TF).
On the European side, the highlights and major
achievements of the period included:
NASA, ESA and CSA have, since 1996, collaborated on
the successor to the Hubble Space Telescope, the James
Webb Space Telescope (JWST). JWST is scheduled to
launch in 2011 and consists of a passively cooled,
6.55 m-diameter telescope, optimised for diffractionlimited performance at near-IR (1-5 µm) and mid-IR (528 µm) wavelengths.
— final approval of the inter-agency agreement
governing the European consortium that will provide
the Optics Module of MIRI;
— successful completion of the MIRI System
Requirements Review;
— initiation of the MIRI PDR;
— selection of EADS/Astrium GmbH as the Prime
Contractor for NIRSpec;
— initiation of the NIRSpec PDR;
— selection of the external members of the NIRSpec
Instrument Science Team;
— approval of the ESA JWST Science Management
Plan.
The JWST telescope proper and its three instruments are
to be cooled in bulk to < 50K, a temperature determined
by the operating temperature of the HgCdTe detector
arrays employed by the near-IR instruments. Cooling is
to be attained passively by placing the observatory at L2
and keeping the telescope and its instrumentation in
During 2003 and 2004, ESA’s participation in JWST was
supported by RSSD through the ESA Project Scientist,
joined by the Deputy Project Scientist starting in late
2003. Like the Faint Object Camera on HST before it, the
NIRSpec instrument is being built by European industry
to ESA’s specifications and under ESA project
3.1.7 JWST
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leadership. Hence, considerable effort by RSSD staff
went into defining the capabilities and detailed technical
specifications of NIRSpec. These specifications served
as a basis for the contractual negotiations with industry.
The JWST Project Scientist proposed a list of members
for the NIRSpec Instrument Science Team (IST) and got
it approved by the AWG at its meeting in May 2004.
Through an AO, he later recruited the IST whose main
role is to provide scientific guidance to the project. The
Project Scientist also drafted the JWST Science
Management Plan, which was approved by the SPC in
February 2004. He also obtained a recommendation from
the AWG for the addition of an Integral Field Unit to
NIRSpec, which considerably enhances the scientific
return of the instrument and provide a back-up in case of
failure of the Micro Shutter Array.
3.1.8 Astro-E2
Astro-E2 will be Japan’s fifth X-ray astronomy satellite.
The mission is being developed at the Institute of Space
and Astronautical Sciences, which is now part of the
Japan Aerospace Exploration Agency (JAXA), together
with a number of US and Japanese institutes. The
planned launch date is 2005. Astro-E2 will cover the
energy range 0.4-700 keV with capabilities highly
complementary to those of XMM-Newton and Integral.
Following an interval when the data belong to the
Astro-E2 Science Working Group, a Guest Investigator
Programme will begin. JAXA has kindly offered to
allocate part of the Japanese time to proposals led by
European astronomers. RSSD coordinated this
participation and an ESA AO was prepared. Following its
release, ESA established a Time Allocation Committee to
review the received proposals; the highest ranking have
been forwarded to JAXA for inclusion in the Japanese
part of the observing programme.
3.1.9 Darwin
The Darwin mission and its potential precursor
experiment GENIE (Ground-based European Nulling
Interferometer Experiment) have continued development. Darwin is ESA’s mission to search for and study
Earth-like planets orbiting nearby (25 pc) stars. It relies
on the technology of nulling or destructive interferometry, where the appropriate phase-delays are applied to
the beams from telescopes separated by many tens or
hundreds of metres, thereby accomplishing destructive
interference along the optical axis. This extinguishes the
light from the star – which is 10 orders of magnitudes
brighter than an Earth-like planet – while enhancing the
light from the planet. Darwin is now projected to consist
of three 3 m-class telescopes based on the Herschel
telescope, each on a separate spacecraft, with a beam
combiner and detector assembly on a separate satellite.
Two Soyuz-Fregats will launch the four spacecraft to L2.
http://www.rssd.esa.int/index.php?project=ASTROE2
Mid-IR spectroscopic observations will be able to detect
and measure ozone, carbon monoxide, water and
methane absorption lines, which together constitute the
best possible tracers of biological activities.
Since Darwin relies on the new technology of nulling
interferometry, ESA and ESO are jointly studying the
potential GENIE precursor instrument. This is a nulling
interferometer, using the infrastructure at VLTI, ESO’s
interferometer at Paranal in Chile. This instrument is
planned to achieve first-light some time after 2008, and
will study the Darwin target stars in detail in order to
determine the dust level in the exosystems, as well as
attempt spectroscopic observations of a number of the
known ‘hot Jupiter’ exoplanets.
In late 2003, both the GENIE Science Team and the
Terrestrial Exo-Planet Science Advisory teams were
appointed via a standard AO. Their role is to provide
scientific advice to ESA and the Study Scientist for the
definition, implementation and operation of the GENIE
and Darwin projects. The two industrial GENIE Phase-A
studies are progressing satisfactorily. The Study Scientist
is closely involved in the on-going large R&D
programme that is designed to develop the challenging
new technologies required for Darwin.
3.1.10 XEUS
XEUS (X-ray Evolving Universe Spectroscopy) is the
potential successor to XMM-Newton. The goals of
XEUS are to detect massive black holes in the earliest
AGN and estimate their mass, spin and redshift through
Fe line and continuum variability studies, to study the
formation of the first gravitationally bound, dark matterdominated groups of galaxies and trace their evolution
into today’s massive clusters, to study the evolution of
metal synthesis to the present epoch using observations
of hot intra-cluster gas and to characterise the mass,
temperature and density of the intergalactic medium
using absorption line spectroscopy.
The original intention was to launch two separate
detector and mirror spacecraft into low-Earth orbit with a
mirror area of 6 m2. The two satellites would fly in
formation, separated by the 50 m focal length of the
optics. The mirror area would be then expanded to 30 m2
by the addition of further mirror segments, delivered to
the ISS by the Shuttle. With the early retirement of the
Shuttle resulting from the Columbia tragedy, it became
apparent that this approach was no longer realistic.
Instead, a revised mission concept is being examined.
This consists of direct injection of separate spacecraft to
L2 by an Ariane-5 or similar, and a mirror area of around
10 m2 with a spatial resolution of 2-5 arcsec. XEUS will
use SCI-A’s new high-precision micro-pore optics, which
provide higher performance and lower mass than the
nickel replication used for XMM-Newton. RSSD has
http://sci.esa.int/darwin
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been closely involved in ensuring that the revised
mission scenario fulfils the scientific goals of the
mission, defining a possible payload, coordinating study
activities with the Japanese partners, and holding
discussions with other potential partners.
3.1.11 Lobster-ISS
Lobster-ISS ESA is a sensitive all-sky monitor under
study as a potential external payload on the ISS. LobsterISS will use a novel form of wide-FOV micro-channel
plate X-ray optics, and will be the first true imaging
X-ray all-sky monitor. Lobster-ISS will locate X-ray
sources to within 1 arcmin with a limiting sensitivity of
0.1 mCrab in a day. As well as providing an alert facility,
the outstanding sensitivity will allow many topics to be
studied using Lobster-ISS data alone. Lobster-ISS
recently completed an industrial Phase-A study. RSSD
staff ensured that the scientific capabilities of the payload
were maintained while producing a design that fulfils the
requirements of the Columbus External Payload Facility
on the ISS.
the handful seen so far from ground observatories. The
Phase-A study, jointly conducted by the Human
Spaceflight and Science Directorates, was recently
completed and the final report provided to the ESA
Science Advisory Structure. Unfortunately, EUSO was
not identified as one of the scientific priorities for
implementation in the foreseeable future. Activities are
continuing to investigate alternative implementation
scenarios. RSSD has supported the Phase-A study by
providing coordination between the separate instrument
and payload studies, and ensuring that the advice of the
independent Science Study Team is properly utilised.
3.1.12 ROSITA
ROSITA (Roentgen Survey with an Imaging Telescope
Array) is a proposal to perform the first imaging 0.511 keV all-sky survey using an array of telescopes on the
ISS. The main scientific goals are to detect obscured
accreting black holes, to study the hot intergalactic
medium in clusters and the hot gas in cluster filaments,
to find distant clusters of galaxies and to investigate the
galactic X-ray source populations. Following an initial
feasibility study, additional activities are on hold until the
outcome of the ‘Dark Universe Observatory’ NASA
SMEX proposal is known in 2005. DUO would perform
X-ray scans of limited regions of sky, whereas ROSITA
would perform an all-sky survey; the science goals of the
two missions are somewhat similar. RSSD has provided
support to the initial feasibility study and to subsequent
discussions with D/HME on future activities.
3.1.13 EUSO
Understanding the origin of cosmic rays with energies
> 5x1019 eV is one of the primary challenges in
astrophysics. At such extreme energies, cosmic rays
interact with the cosmic microwave background and the
distance that a cosmic ray can travel is limited to our
galactic neighbourhood. Intriguingly, all the astronomical objects that could produce such energetic cosmic rays
are likely to be much further away. The Extreme
Universe Space Observatory (EUSO) will observe the
light produced when such a cosmic ray interacts with the
Earth's atmosphere. Looking down from the ISS, EUSO
could detect around 1000 events per year, compared to
http://www.rssd.esa.int/LOBSTER
http://www.rssd.esa.int/ROSITA
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3.2
scientific support activities
Solar and Solar Terrestrial Missions Division
3.2.1 Introduction and overview
The Solar and Solar Terrestrial Missions Division
provides scientific support for all ESA missions in solar,
heliospheric and solar-terrestrial science. The present
missions in operational phase are Ulysses, SOHO,
Cluster and Double Star. Solar Orbiter is in its study
phase within SCI-A. Apart from providing science
support to these missions, the Division is also
responsible for their management once in their
operational phases.
Staff members of the Division are located at ESTEC,
with the exception of the SOHO team, who reside at the
SOHO Experiment Operations Facility at the NASA
Goddard Space Flight Center, Greenbelt, USA.
Ulysses has now been in orbit for over 14 years and is
presently on its way towards a third set of polar passes in
2006-2007 (south) and 2007-2008 (north), following the
decision by SPC to extend the mission to March 2008.
Ulysses has also completed a distant encounter with
Jupiter, where the scientific highlights were observations
of quasi-periodic radio bursts and distant observations of
Jupiter dust streams. Ulysses also observed cometary
ions in a coronal mass ejection. As in the past, Ulysses’
results continue to feature prominently at international
meetings and workshops, and the science team maintains
an exceptionally high publication record (over 120
papers during 2003-2004). Such activities are
coordinated by the RSSD Project Scientist Team and
extend to data dissemination, archives and long-term
calibration issues.
formations, the Cluster mission continues to deliver
outstanding results of small- and large-scale physical
processes in near-Earth space. As expected, Cluster has
now provided both evidence and direct in situ
observations of reconnection in the magnetic tail and the
dayside high-latitude magnetopause. It has furthermore
confirmed the existence of large-scale boundary waves
and vortices at the magnetopause, found filamentary
structures in the aurora, the cusp and the tail current, and
explicitly measured the extreme thinness of the bowshock and the cross-tail current just before substorm
onset. It appears that the number of results from Cluster
is still growing at an exponential rate, promising an
exciting future. Both SSWG and SSAC have recently
taken a positive stand towards plans for a further mission
extension to late 2009, allowing a number of new
adaptive or multi-scale configurations to be exploited
and new magnetospheric regions to be visited (in
particular, the important sub-solar magnetopause and the
near-Earth tail around 10 RE). An important step in the
direction of even more effective Cluster data exploitation
was the ESA SPC decision to fund the Cluster Active
Archive, an open approach to delivering high-resolution
Cluster data to the worldwide community.
ESA’s first collaboration with China, the Double Star
Project, got underway with successful launches into
equatorial (December 2003) and polar (July 2004) orbits.
The orbits are designed to support the Cluster mission,
and most of the European-provided instruments are
identical to the Cluster payload. In spite of some
problems with boom deployment and attitude computers,
both missions are now operating nominally, and will
provide important data complementary to Cluster for at
least the mission baseline period of 1 year.
The SOHO mission remains the flagship of solar and
heliospheric research, continuously supplying scientists
and, increasingly, space weather experts, through the
RSSD Project Science Operations Team, with data from
the Sun. A dramatic incident occurred in mid-2003, when
a problem with the high-gain antenna motor resulted in
some data loss, which sent a shockwave through the
scientific community. Using on-board data storage and
clever roll manoeuvres of the satellite, the SOHO RSSD
Project Scientist team was able to keep the damage from
the malfunctioning motor to a minimum, rescuing
continuous helioseismology data even during periods of
low-gain antenna contacts. Apart from such problems,
SOHO operations and science exploitation have run
smoothly throughout the reporting period. As usual, the
SOHO RSSD team has been extremely active in science
outreach and communications. The most spectacular
highlight was the coverage of the extraordinary solar
outbursts in Autumn 2003, which are still under scientific
study via a large number of spacecraft such as Cluster.
After reconfirmation following the reassessment of the
Cosmic Vision programme in 2003, Solar Orbiter is
under assessment in the Science Payload and Advanced
Concept Office, with support from the Study Scientist
concerning science issues and contacts with the
international scientific community. During 2003, the
Solar Orbiter Science Definition team reviewed the
scientific goals of the mission, resulting in a wellbalanced and highly focused mission.
Probing different key regions of the magnetosphere and
solar wind at variable scales using a variety of spacecraft
Following the restructuring of the Science Directorate in
recent years, no new hardware commitments have been
Several instruments built in previous years by members
of the Division and SCI-A personnel continue to deliver
good data. The instruments presently operative in orbit
are COSPIN on Ulysses, LOI on SOHO and EFW and
ASPOC on Cluster. For NASA’s STEREO mission, parts
of the SEPT/IMPACT instruments were delivered by
SCI-A during the reporting period. The SEPT instrument
built by SCI-A with science guidance from division staff
is the most recent link in a very successful series of
energetic-particle instruments from the Division.
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taken on during the reporting period. However, it is
hoped that staff of the Division will be involved in
providing the science requirements and guidance to SCIA for the thermal design and testing of hardware for the
ion and electric field instrument on BepiColombo’s MPO
and MMO, respectively.
Besides the primary occupation of the Divisional staff in
supporting the missions in orbit, almost all staff members
have pursued their own scientific research. In the
absence of new hardware projects, other than those listed
above, such activities have now concentrated on data
analysis. The prime research fields of the divisional staff
are in solar physics (Section 2.5), heliospheric physics
(Section 2.6) and space plasma physics (Section 2.6).
The combined effort of RSSD staff in scientific data
analysis has been supported by an active research fellow
programme.
Figure 3.2.2/1: An example of quasi-periodic
(~40-min period) radio bursts from Jupiter, detected
by URAP on Ulysses in October 2003. (Courtesy
R.J. MacDowall)
3.2.2 Ulysses
Ulysses is an exploratory mission being carried out
jointly by ESA and NASA to study the properties of the
interplanetary medium and solar wind in the inner
heliosphere as a function of heliographic latitude and
solar activity. The mission also focuses on the dust and
gas components of the local interstellar medium that gain
access to the heliosphere inside the orbit of Jupiter. The
European-built Ulysses spacecraft was launched by the
Space Shuttle on 6 October 1990, and a Jupiter gravityassist in February 1992 deflected it into its final highinclination heliocentric orbit. Major mission milestones
to date include the south and north polar passes at solar
minimum (1994/95) and again at solar maximum
(2000/01). Following a distant encounter with Jupiter in
February 2004 and aphelion passage in June 2004,
Ulysses is now heading south prior to the third set of
polar passes, in 2006/07 (south) and 2007/08 (north).
Scientific highlights during the reporting period included
observations of quasi-periodic radio bursts from Jupiter,
the most distant observations to date of dust streams from
Jupiter (Fig. 3.2.2/1), observations of the effects of the
October/November 2003 violent solar outbursts at the
orbit of Jupiter, and remote observations of cometary
ions trapped in a CME (Fig. 3.2.2/2).
A joint ESA-NASA Mission Operations Team at JPL
conducts spacecraft operations. A major priority during
the reporting period was to ensure that critical elements
of the hydrazine system used for attitude control
remained above freezing. The low temperatures were the
combined result of the diminishing power available from
the RTG power source and the large distance from the
Sun. The ensuing power and thermal constraints required
the introduction of a power-sharing plan for the scientific
payload whereby a core set of instruments is operated
continuously and a subset of the remaining payload is
http://helio.esa.int/ulysses
Figure 3.2.2/2: Ulysses observes ions from Comet
McNaught-Hartley trapped inside a CME. Earth’s
orbit is shown for reference. (Courtesy G. Gloeckler)
switched on on a rotating basis. Starting in October 2004,
the nominal ground station coverage via NASA’s Deep
Space Network was reduced from 70 h to 35 h per week.
This reduced coverage, introduced as a result of the 2003
Sun-Earth Connections Senior Review in NASA, will
last for 2 years. Within these constraints, the spacecraft
and payload are operating very well.
On the programmatic side, a major achievement was the
approval by ESA’s SPC in February 2004 of funding to
continue spacecraft operations until March 2008. This
mission extension, the third for Ulysses, will enable
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measurements to be acquired up to and including a third
set of polar passes. The scientific rationale for this is the
desire to have out-of-ecliptic observations covering as
much as possible of a complete Hale (22-year) solar
magnetic cycle. Furthermore, the launch in 2006 of
NASA’s twin STEREO probes will create a unique
opportunity for multi-spacecraft observations during
Ulysses pole-to-pole transit in 2007. Funding on the
NASA side for 2007-2008 will be decided at a Senior
Review in 2006.
During the reporting period, the ESA RSSD Mission
Manager, together with his JPL counterpart, provided
scientific advice to the operations team on all mission
aspects and co-chaired the Science Working Team
(SWT) meetings. In addition, the Mission Manager cochaired the corresponding ESA-NASA Joint Working
Group (JWG) meetings at which the overall policy issues
related to the mission are discussed. Four JWG/SWT
meetings were held in 2003-2004, two in Europe and two
in the USA. A major topic of discussion at recent SWT
meetings has been the implementation of payload powersharing. As part of his Project Scientist duties, the
Mission Manager assisted in the organisation of special
sessions related to heliospheric research at international
scientific meetings. Two collections of papers and a
major review article, all focusing on the results from the
recent solar maximum solar passes, appeared during the
reporting period. Individually, the Ulysses investigators
continued to publish prolifically, with more than 120
papers appearing in 2003-2004.
The Ulysses Data Archive is maintained at ESTEC by a
small RSSD Ulysses team and is mirrored at JPL.
Ulysses data are also archived by NASA at the National
Space Science Data Center (NSSDC), and form part of
the Planetary Data System (PDS) archive. During the
reporting period, key activities included the acquisition
of additional sets of high-resolution time data, and the
porting of the archiving software from the current VMS
system to Windows and UNIX platforms.
3.2.3 SOHO
SOHO is a mission of international cooperation between
ESA and NASA to study the Sun, from its deep core to
the outer corona, the solar wind and its interaction with
the interstellar medium. SOHO has provided the first
images of structures and flows below the Sun’s surface
and has identified the source regions and acceleration
mechanisms of the fast solar wind. It has revolutionised
both our understanding of solar-terrestrial relations as
well as our space weather forecasting capabilities by
providing a continual stream of images of the dynamic
solar atmosphere, extended corona and activity on the far
side of the Sun.
In September 2003 the SOHO Team was presented with
Figure 3.2.3/1: Cover of the July 2004 issue of
National Geographic, which includes the 32-page
story ‘The Sun: Living with a Stormy Star’.
the prestigious Laurels for Team Achievement Award of
the International Academy of Astronautics (IAA). The
award recognises both the outstanding achievements in
designing, building and operating the mission, as well as
the science it has performed.
SOHO is a busy observatory, with many coordinated
observations (covering well over half the observation
time) involving different instruments as well as groundbased observatories and other spacecraft.
The coordination of science operations by the RSSD
Project science team focuses on maximising the science
output of the mission on both short and long time scales,
serving current interests as well as possibilities for future
analysis by facilitating requested and ad hoc collaborations. It also involves identification and resolution of
technical issues under a variety of operational situations.
After showing signs of degradation in May 2003, the
azimuth drive of the high-gain antenna was parked in an
optimal position in June 2003. Coupled with 180°
spacecraft rolls twice per 6-month orbit, the parking
position introduces keyhole periods of 2-3 weeks every
3 months, when the low-gain antenna must be used with
34 m or 70 m DSN stations. Low availability of such
stations causes about 40% loss of telemetry during such
keyhole periods. Careful planning to take full advantage
of all on-board recording capabilities has still made it
possible to ensure near-continuous time series for the
GOLF and VIRGO instruments during the last three
keyholes (winter 2003 – autumn 2004), thanks to their
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doubly redundant telemetry streams. Concurrently, an
onboard software patch was developed by Saab Ericsson
Space to record only selected telemetry packets. The
patch was successfully tested during the last keyhole and
will be used for future keyholes, hopefully ensuring
continuous helioseismology data from the GOLF,
VIRGO and MDI instruments.
The Internet-based approach to science operations
coordination and data dissemination that SOHO has
pioneered since 1994 is still the cornerstone of the SOHO
information and data system, and it continues to grow: an
average of almost 16 million requests were received, and
more than 2700 GB of data were transferred from the
SOHO servers every month during the last 2 years (up
from 7 million requests and 950 GB during the last
period). Over the mission lifetime, the SOHO web
servers have received a total of 617 million requests and
have delivered > 91 TB of data.
Anticipating a reduction in the on-site staffing, emphasis
has been placed by the RSSD Project Science team on
streamlining all data-handling processes for automation
and ease of maintenance. The system encompasses
processing, archiving, cataloguing, searching and
distribution of level-zero telemetry, ancillary data sets
and science processed data, as well as real-time products
and general web pages for the public.
The SOHO teams have set a new standard in providing
images and results through the World Wide Web,
capturing the imagination of the science community and
the general public alike, and inspiring students of all ages
to seek more information about the Sun. SOHO images
have become stock footage for news organisations
around the world.
SOHO maintains its high profile in the international
media thanks to continued efforts to improve the SOHO
web pages and by expanding the network of personal
media contacts. SOHO images were featured on the front
covers of many popular science magazines, including the
cover of the July 2004 issue of National Geographic,
which featured a 32-page story on recent developments
in solar science and space weather. Members of the
SOHO RSSD Project Scientist Team worked closely
with National Geographic staff, reviewing the article and
consulting on the artwork and images.
67
and embassy staff, and several film crews making
documentaries on the Sun (e.g. Discovery Channel) were
supported.
3.2.4 Cluster
The four Cluster satellites were launched in pairs on two
Soyuz rockets in July and August 2000, into a polar orbit
targeting some of the most important near-Earth regions:
solar wind, bow shock, magnetosheath, cusp, magnetopause, plasmapause and magnetotail. By providing
unique 4-point measurements in the Earth’s magnetosphere, Cluster is revolutionising our understanding of
the dynamics of space plasmas. Originally funded to
operate for 2 years, and now in an extended mission
phase until December 2005, the spacecraft and payload
continue to perform well and are expected to do so for
several years to come. In order to fully realise the
potential of the mission, a second extension will be
proposed to the SPC early in 2005.
Discoveries made by Cluster have demonstrated the
critical importance of making measurements on different
spatial scales. For example, the substructure of the
magnetopause reconnection layer on electron scales of
~20 km; filamentary structure within the cusp over scales
of only 100 km; density irregularities at the plasmapause,
including plasmaspheric plumes, over scales from
100 km to several 1000 km; observations of a tail current
Figure 3.2.4/1: 3-D cut-away view of Earth’s
magnetosphere. The curly features sketched on the
boundary layer are Kelvin-Helmholtz vortices
observed by Cluster. They originate when the two
adjacent flows travel at different speeds; in this case,
the magnetospheric flow on one side and the solar
wind flow on the other. (Courtesy H. Hasegawa,
Dartmouth College)
Several special showings of the IMAX film Solarmax
were arranged by the RSSD Project Science team, e.g. at
the meeting of the American Metrological Society in
Seattle and the International Astronautical Congress in
Vancouver, Canada. The latter supported ESA’s
education support programme at this conference. We
have also supported ILWS exhibits at the United Nations
in Vienna and New York with SOHO materials, models
and real-time images. Numerous VIP tours to the SOHO
operations facilities were hosted for European ministers
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sheet only ~0.1 RE thick; the scale of the quasiperpendicular shock transition on the ion gyroradius
scale; propagating wave modes in the magnetotail with
wavelengths of several RE; and huge vortices on the
flanks of the magnetosphere.
During the last 2 years, the RSSD Project Scientist team
has devoted a large part of its time to the operations of
the Cluster mission and the distribution of data to the
scientific community. It chaired seven Cluster Science
Operations Working Group meetings and four Science
Working Team meetings. Five Cluster workshops were
organised between October 2002 and October 2004, to
discuss Cluster data and prepare the plan for the
spacecraft separation strategy. A special issue of Annales
Geophysicae was published in July 2004 with Cluster
results presented during the 5th Cluster workshop in
Orleans (F). A special ISSI book is being finalised on
Cluster results on the dayside boundaries of the
magnetosphere
The Cluster Science Data System (CSDS), which has
been specially developed to allow fast easy access to the
Cluster physical parameters measured by the
instruments, has been running smoothly since February
2001. Nine national data centres, in Austria, China,
France, Germany, Hungary, Netherlands, Sweden,
United Kingdom and the United States constitute the
CSDS. They are funded by their national agencies; ESA
through the Project Scientist team coordinates the system
and provides the user interface to allow a scientific user
to query, retrieve and manipulate the data coming from
all instruments. User access to the data system is
gradually increasing every month. The average
download by scientific users over a recent 3-month
period was > 5.8 Gbytes/month. The physical parameters
database contains more than 30 Gbytes.
A Joint Science Operations Centre (JSOC), at the
Rutherford Appleton Laboratory (UK), was established
to support the Project Scientist in coordinating the
complex science operations of the mission. Its five main
tasks are payload commanding, payload health
monitoring, planning and information dissemination,
data management system delivery and maintenance, and
the CSDSweb (quicklook) delivery and maintenance.
The Cluster quicklook plots are available at
http://www.cluster.rl.ac.uk/csdsweb/. JSOC has performed its tasks successfully since the beginning of the
mission. A very active period for JSOC is during the
constellation manoeuvres, when instruments have to be
switched-off during thrusters firing and switched on
again afterwards. Constellation manoeuvres consist
typically of 50 thruster firings from a few seconds up to
more than 1 h during a 1.5-month period and take place
once a year.
The importance of Cluster data to space physics is
underlined by the development of the Cluster Active
scientific support activities
Archive (CAA), funded by ESA, NASA and member
states. From early 2005, this archive will provide free
access for the entire scientific community to the full,
calibrated, high-resolution Cluster data set (CSDS
contains only low- and medium-resolution data). CAA
will be a unique research tool for the worldwide
magnetospheric science community for many years to
come. It consists of a core RSSD team with four people
that will prepare and populate the database at ESTEC,
and one person in each of the 10 European PI teams to
calibrate and deliver the data to the archive. The first
CAA data were delivered before the end of 2004 and then
2 years’ worth of data will be delivered annually.
3.2.5 Double Star
The two Double Star satellites were launched on
29 December 2003 and 25 July 2004 aboard Chinese
Long March 2C rockets. Double Star is a China-ESA
programme to study the effect of the Sun on the Earth’s
environment. The Chinese National Space Administration built, launched and is operating the two satellites.
ESA provided eight European instruments, the support
for their integration in Europe, their science operations,
and the acquisition of 4 h of data per day using the ESA
VILSPA II ground station. The orbits are designed to
maximise collaboration with Cluster such that both
small-scale and large-scale observations of the
magnetosphere are collected simultaneously.
The satellites and instruments are working well although
a few anomalies occurred shortly after the launches. On
TC-1, one solid boom holding the STAFF (magnetic
wave detector) did not deploy owing to a problem with a
pyro-actuator. STAFF observations are contaminated by
a strong background noise. Special software techniques
are being developed to minimise this effect. In addition,
a strong magnetic disturbance from the spacecraft solar
array is observed by the FGM (magnetometer). The FGM
software has been modified to limit the effect.
On TC-2 the boom pyros were exchanged and the solar
panel cabling modified, precautions that avoided the
problems encountered with TC-1. Unfortunately, both
the main and redundant attitude orbit control computers
failed within 2 weeks of launch. This lost the attitude
control capability on the polar satellite; however, the
attitude can be determined using the European- provided
magnetometer data. Spin axis pointing and spin rate are
nominal. Although the spin rate is expected to remain
stable over the mission, the spin axis is expected to drift
slowly. Present drift predictions indicate that at least a
1-year mission lifetime can be achieved for TC-2 without
problems.
During the last 2 years, the RSSD Project Scientist team,
which shares its time with the Cluster project, has
devoted a large part of its effort in preparation for the
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3.2.6 Solar Orbiter
The key mission objectives of the Solar Orbiter mission
are: to study the Sun from close up (48 solar radii, or
0.22 AU), permitting investigation of the solar surface at
high spatial resolution; to study the links between the
solar surface, the corona and inner heliosphere during
perihelion passes that are matched to the Sun’s rotation;
and to provide images of the Sun’s polar regions from
heliographic latitudes in excess of 30°. Solar Orbiter was
selected as an ESA Flexi-mission in 2000, and
reconfirmed in 2004 to be implemented as a common
development with the BepiColombo mission to Mercury.
Launch is foreseen for either October 2013 or May 2015.
Figure 3.2.5/1: Launch of the second Double Star
TC-2 satellite on 25 July 2004 from Tai Yuan.
mission, including the science operation of the European
instruments and preparation of the data system. The
Science Working Team is co-chaired by the Chinese and
ESA Project Scientists. The RSSD Project Scientist
co-chaired four DSP SWT meetings and four data system
implementation working group meetings between
October 2003 and October 2004.
Since the European contribution to Double Star consists
of Cluster spare or duplicate instruments, it was decided
to re-use as much as possible the data system developed
for Cluster. The European Payload Operation Centre
(adapted from Cluster JSOC) updated the data
management system for Double Star and coordinates the
commanding of the European payload. Similarly, the
Double Star Data System (DSDS), a subset of the Cluster
data system, distributes data to the user community. The
national data centres involved in the distribution of data
are in Austria, China, France, The Netherlands and UK.
The quicklook plot system has also been adapted to
display the data from all instruments, European and
Chinese, a few days after data acquisition and is running
at the Austrian data centre (http://edds02.iwf.oeaw.ac.at/
dsdsweb). TC-1 operations began in March 2004 and for
TC-2 in early October 2004. The coordinated dual
satellite mission is planned to last at least until July 2005.
The second Double Star workshop took place in Beijing
on 8-10 November 2004. More than 50 papers, the
majority combining both Double Star and Cluster data,
were presented during the 3 days. Very promising results
emerged on magnetic reconnection, bow shock structures
and surface waves on the magnetosphere.
The model payload comprises the following state-of-theart packages of heliospheric in situ and solar remotesensing instruments: Plasma Package (ion and electron
solar wind analysers); Fields Package (radio and plasma
wave analyser, magnetometer); Particles Package
(energetic particle detectors, interplanetary dust detector,
solar gamma-ray and neutron detector); Solar Remote
Sensing Package (visible-light imager and magnetograph, EUV full-Sun and high-resolution imager, EUV
spectrometer, X-ray spectrometer/telescope, coronagraph).
In 2003, the Study Scientist formed a Science Definition
Team (SDT) that was given the task of reviewing and
refining the scientific goals to achieve a well-balanced
and highly focused mission. SDT meetings were held in
ESTEC in May and September, resulting in a Solar
Orbiter Science Requirements Document (Sci-RD),
issued in December 2003. Throughout 2004, the Study
Scientist supported the assessment activities lead by
SCI-A, in particular with respect to payload-related
issues, and maintained the interface to the external
scientific community. Other activities included presentations at international meetings, and coordination efforts
in the framework of NASA’s Living With a Star
programme (specifically, Solar Probe and Sentinels), and
the International Living With a Star initiative.
3.2.7 Solar-B
Solar-B is a solar physics mission, led by ISAS, intended
to follow on from the highly successful Yohkoh
(Solar-A) mission. The payload comprises a coordinated
set of optical EUV and X-ray instruments to investigate
the interaction between the Sun’s magnetic field and
corona. The final goal is to reach an improved understanding of the mechanisms leading to solar variability
and ultimately controlling the energy output. These
processes are the main driving forces behind what is
generally referred to as space weather. Solar-B is
scheduled for a launch in August 2006.
After having received an invitation to collaborate with
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ISAS on Solar-B, particularly on data analysis and
operational ground support from a polar station, ESA
received SPC approval in early 2003 to invest > 7 Meuro
in providing an additional Norwegian ground station on
Svalbard. This station, because of its high latitude, will
be able to provide downlink for almost all Solar-B passes
in its Sun-synchronous low-altitude polar orbit. Closely
linked to the provision of the station, ESA is also
negotiating with Norway for a European data centre for
the full Solar-B database, supplying Europe’s solar
physics community with rapid access to the huge
amounts of data expected from this mission.
ESA’s involvement in Solar-B can be considered as an
initial ESA contribution to the International Living With
a Star Initiative (ILWS), which aims to increase our
understanding of how the variability of the Sun affects
the terrestrial and other planetary environments, in the
short- and long-terms. In particular, the effects of solar
variability on mankind and society are being
investigated.
B. Fleck acts as the prime ESA contact person with
respect to JAXA/ISAS, and R. Marsden and H. Opgenoorth represent ESA in the ILWS steering committee,
which has been chaired by the latter for the last 2 years.
scientific support activities
3.3
Planetary Missions Division
3.3.1 Introduction and overview
The past 2 years were probably the most exciting period
for planetary science in Europe, and the staff of the
Division played a major role in supporting the
community to contribute to this success. Three missions
were launched: Mars Express, SMART-1 and Rosetta.
Huygens was released from Cassini and completed its
mission to study Titan’s atmosphere and surface on
14 January 2005. Venus Express, which was approved
end-2002, is in its final stages of testing and will be ready
for launch in November 2005. It was a demanding time
for the Project Scientists and their teams, supporting the
project reviews, monitoring the payload development
and testing, and preparing the commissioning activities
jointly with the Experiment Teams and the Mission
Operations Team at ESOC.
The Division is responsible for the coordination of all
payload operations for Mars Express, Rosetta and
SMART-1. The supporting facilities for these missions
have been developed and the various teams have taken
over responsibility for planning the operations of their
specific mission. In addition to Huygens, the Division
took over the responsibility for the mission management,
during the exploitation phase, of Mars Express, Rosetta
and SMART-1.
The launch delay of Rosetta required an additional effort
to define the new mission scenario, monitor the new
target comet and demonstrate, in a unique team effort
with the Project Team and the Rosetta Science Working
Team, that we had defined a viable mission to the new
target, 67P/Churyumov-Gerasimenko. In addition, the
RSSD Project Scientist team had to support a long launch
campaign for the second time.
The successful redefinition of the baseline mission
scenario for BepiColombo by SCI-A was supported by
the Project Scientist. Unfortunately, the Mercury Surface
Element had to be dropped for programmatic reasons. A
successful mission profile involving two orbiters (one
ESA and one Japanese) was developed that ensured a
major science return could be maintained. The RSSD
Project Scientist was heavily involved in maximising this
science return from the low-resource model payload
designed within SCI-A, as well as in the payload
selection process and the accompanying negotiations to
secure payload funding.
In close collaboration with the Science Operations and
Data Systems Division, the ESA Planetary Science Data
Archive was created using the tools developed for the
archives for ESA’s astrophysics missions. The first data
sets ingested were the results from Giotto and the Giotto
Extended Mission and from the ground-based
observation campaign of the Rosetta targets. The archive
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is operational and waiting for the data sets from the first
6 months in Martian orbit from the Mars Express
instruments.
3.3.2 Cassini/Huygens
The Cassini-Huygens mission is a joint undertaking
between NASA, ESA and ASI. It is designed to explore
the Saturnian system and all its elements: the planet and
its atmosphere, rings and magnetosphere, and a large
number of its moons (icy satellites), in particular Titan,
Saturn’s largest moon. The Cassini-Huygens spacecraft,
launched in October 1997, was placed in orbit around
Saturn on 1 July 2004. The interplanetary voyage of
6.7 years included gravity-assists at Venus (April 1998
and June 1999), Earth (August 1999) and Jupiter
(December 2000). Results obtained during the cruise
phase and the planetary flybys have appeared regularly in
the scientific literature.
Saturn approach science started in early 2004. It included
a coordinated set of observations of Saturn’s auroras by
HST while Cassini monitored the solar wind conditions.
Remote sensing observations of the entire system during
the approach phase allowed the study of what already
appears to be a highly variable and dynamic system
where all elements are interacting (Saturn and Titan
atmosphere, rings, moons, magnetospheric plasma, dust).
Nineteen days before Saturn Orbit Insertion (SOI), a
2000 km flyby of the large outer moon Phoebe was
performed. Spectacular observations indicated that
Phoebe is most likely a captured object from the outer
Solar System. During SOI, Cassini-Huygens went
through a gap between the F- and G-rings. Unique ring
observations were obtained by several remote-sensing
instruments, including the Imaging Science Subsystem
(two cameras) and various optical spectrometers
covering the UV to the far-IR. The fields & particles
instrument complement has begun to study the global
morphology of Saturn’s magnetosphere. Lightning was
detected in Saturn’s atmosphere by the plasma wave
sensors, indicating some change in its characteristics
since the Voyager observations.
By the end of 2004, Cassini had performed three Titan
flybys: 2 July (300 000 km closest approach),
26 October (1174 km) and 13 December (1200 km)
(Fig. 3.3.2/1). The surface of Titan, ‘seen’ by three
remote-sensing instruments (camera, VIMS, radar) is
revealing itself to be more complex, exotic and
geologically diverse than ever anticipated. The
atmosphere’s thick haze is a challenge for the optical
remote-sensing instruments in reaching their best
resolutions. Remote observations by the Composite
Infrared Spectrometer (CIRS) and the Visual Infrared
Mapping Spectrometer (VIMS) on 2 July and
26 October, and in situ measurements in the upper
atmosphere by the Ion and Neutral Mass Spectrometer
http://sci.esa.int/huygens
Figure 3.3.2/1: The Cassini-Huygens trajectory on
arrival at Saturn. The Huygens mission was carried
out on the third revolution around Saturn. Three
Titan flybys were achieved before Huygens’ mission:
T0 (2 July, closest approach 300 000 km); Ta
(26 October, 1174 km); Tb (13 December, 1200 km).
The probe mission was carried out on Tc on
14 January 2005. More than 40 Titan flybys are
expected to follow Huygens’ mission before the
orbiter’s mission ends in mid-2008.
(INMS) on 26 October, as well as the two stellar
occultation data sets on 13 December by the UV Imaging
Spectrometer (UVIS), allowed, in combination with the
ground-based data set obtained during the Titan
occultation in mid-November 2003, the upper
atmosphere model of Titan’s atmosphere to validated and
updated, a key step in the validation of the performance
of Huygens mission.
During the reporting period, the RSSD Mission
Manager/Project Scientist, supported by the Huygens
Mission Team which is distributed across ESTEC,
ESOC, NASA/JPL and Industry, assumed the overall
responsibility for the implementation of the Huygens
recovery mission, which was completed in December
2003 when the required Probe onboard software patches
were uploaded and validated. In 2004, the work
concentrated on preparation activities for the Huygens
mission itself. Three major Huygens reviews were
conducted in 2003-2004. An Agency-wide Delta Flight
Acceptance Review was conducted on the recovery
mission from December 2003 to February 2004. The
review identified the need to consolidate the entry heat
flux and heat load calculations, because recent work on
radiation flux during entry into a methane-rich nitrogen
atmosphere had raised questions on the work done in the
early 1990s. A special effort began in April 2004 with the
Huygens industry team, NASA and Ecole Centrale de
Paris, where there is unique expertise high-temperature
plasma radiation spectroscopy. The work concluded in
late November 2004, allowing the latest methane
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Figure 3.3.2/2: Updated Titan atmosphere profile
after the T0, Ta, Tb flyby data set. The update profile,
represented by he thick purple line, falls within the
envelope of the engineering model used for the
Huygens mission design.
concentration in Titan’s atmosphere derived from the
early Cassini observations to be taken into account
(Figs. 3.3.2/2 & 3.3.2/3).
An ESOC-led Delta Ground Segment Readiness
Review was held in September 2004. The
recertification of the entry performance was one of the
major topics addressed in a Joint ESA/NASA Mission
Risk Review (MRR), which was conducted from midOctober to mid-December 2004. The MRR gave the
green light, on 16 December, to proceed with
preparations for the probe’s release. Huygens was
successfully released from Cassini on 25 December
2004 at 02:00 UTC. Thanks to excellent pointing and
performance of the Spin and Eject Device, Huygens
was targeted at the nominal entry angle of –65º. A series
of optical navigation images of the probe was obtained
by the two Cassini cameras, which contributed to
refining the probe trajectory and to confirming that the
entry ellipse uncertainty was only 0.8º (3º requirement).
At the end of 2004, it was known that Huygens was
well on its way to Titan for an entry on 14 January 2005
at 09:06 UTC (Fig. 3.3.2/4).
Following an initial study within the ESA General
Studies Programme (GSP) in mid-2003, initiated by the
Technical Directorate, a project was developed for
tracking the probe using Very Long Baseline
Interferometry (VLBI). The objective of the study was
to investigate synergies available between large
effective apertures for radio astronomy and the needs of
space applications like data downlinks (MARS/Venus/
Mercury landers and/or small orbiters) and monitoring
scientific support activities
Figure 3.3.2/3: VIMS image of Titan after Ta
observations. The expected Huygens landing site is
shown.
space debris. In order to arrive at a realistic concept, the
study focused on the tracking of Huygens during its
descent to Titan. The initial study was closely followed
by the RSSD Project Scientist. It demonstrated that the
tracking of Huygens was achievable. Following the
positive outcome of the initial study, further work was
done jointly by the Technical and Science Directorates
to develop a project for Huygens VLBI observations.
The ESA studies were led by the Joint Institute for
VLBI in Europe (JIVE), in Dwingeloo (NL). The main
goal was to measure the position of the probe during its
descent and on the surface to an accuracy of the order
of 1 km with a time resolution of a few seconds. At the
initiative of JIVE, radio telescope time was applied for
and obtained as part of the regular AO process in the US
and in Australia through peer-review proposals, which
were highly ranked during the evaluation process.
Altogether, 18 telescopes in the USA, Australia, Japan
and China were involved in the observations. Two test
observations were conducted in late August 2004 (using
Cassini transmitting in the X-band as the RF source),
and in mid-November 2004 (using Cassini’s Radio
Science S-band transmitter and Mars Express’ S-band
transmitter). Those test observations allowed the
Huygens team to debug and coordinate the complex
observation plan and were key to preparing for the real
Huygens observations.
Huygens successfully landed on Titan on 14 January
2005. All science instruments performed well, yielding a
data set of the moon’s physical and chemical properties.
The amazing descent panorama and superb pictures from
the landing site can be found on http://saturn.esa.int or
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Operations Centre (RSOC) and have a fully
operational system ready for the payload
commissioning that started shortly after
launch. It is responsible for consolidating the
command sequences for the operation of the
science payload. These command files are
submitted to the Rosetta Mission Operations
Centre (RMOC) at ESOC. In addition, the
Project Scientist Team team supported all
Project Reviews and the official RSOC
Reviews as part of the Rosetta Ground
Segment validation and commissioning.
Figure 3.3.2/4: Huygens Entry, Descent and Landing
scenario.
3.3.3 Rosetta
On 2 March 2004 Rosetta was launched from Kourou
on an Ariane-5G+. After the delay from early 2003
owing to the failure of the new Ariane-5ECA, the
Project and the RSSD Project Scientist team, in close
collaboration with the Rosetta Science Working Team,
studied alternative mission scenarios. These had to
meet three basic requirements: preserve the scientific
objectives of the mission, minimise the technical risks,
and minimise the financial impact on the overall
Science Programme. A mission to comet 67P/
Churyumov-Gerasimenko was finally identified that
met these requirements. The RSSD Project Scientist
team, in collaboration with the scientific community,
mounted an observing campaign to characterise the new
target in support of defining the new mission scenario.
In parallel, technical activities proceeded at an
increased pace in order to meet the new launch date of
February 2004. Fortunately, the Rosetta orbiter did not
require changes to cope with the new mission scenario.
However, considerable effort was needed to
demonstrate the compatibility of the Philae Lander
design with the new target. Churyumov-Gerasimenko
has a radius of 2 km, in comparison to the 0.6 km radius
of the original target 46P/Wirtanen. The greater
gravitational attraction will produce a higher
touchdown speed on the nucleus. All these technical
hurdles were overcome and Rosetta was ready to be
launched at the end of February 2004. After two brief
launch delays due to bad weather and a technical
problem, respectively, Rosetta was finally launched.
The Project Scientist team used the 1-year delay to
improve the implementation of the Rosetta Science
http://sci.esa.int/rosetta/
The payload commissioning was split into
three periods – two periods immediately after
launch until early June – and the Pointing and
Interference Campaigns in September and
October 2004. For the last period, RSOC took
for the first time full responsibility for preparing the
payload operations. This required very close interaction
and collaboration with the Experiment Teams. The
system worked flawlessly and proved the readiness of
RSOC.
The Mission Commissioning Results Review on
3 December 2004 at ESOC concluded that all goals of
the spacecraft and payload commissioning had been
achieved and that the mission was operational. From
mid-October the spacecraft was in quiet cruise mode, the
next big event being the first Earth gravity assist on
4 March 2005.
Subsequently, for the operational phase of the mission
the management of Rosetta was transferred from the
Projects Department to RSSD.
3.3.4 Mars Express
Mars Express is ESA’s first planetary mission and was
launched on 2 June 2003 from Baikonur Cosmodrome
aboard a Soyuz-Fregat. Following a 7-month journey, it
was inserted into Mars orbit on 25 December 2003. The
Beagle 2 lander was released on 19 December and
should have landed on 25 December; it was considered
to be lost following extensive searches by the NASA
Mars Odyssey orbiter, terrestrial radio telescopes and
Mars Express itself.
The Mars Express orbiter is designed to achieve the
following science objectives:
—
—
—
—
global high-resolution (10 m) photogeology;
super-resolution imaging at 2 m/pix of selected areas;
global mineralogical mapping at 100 m resolution;
global atmospheric circulation and mapping of
composition;
— study subsurface structure at km-scale down to the
permafrost;
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scientific support activities
— study surface-atmosphere interactions;
— study interaction of the upper atmosphere with the
solar wind.
The RSSD Payload Support Team (PST) at ESTEC acts
on behalf of the RSSD Mission Manager, in consultation
with the Science Operations Working Group (SOWG).
The Mission Manager is advised by the Project Scientist
and the Science Working Team (SWT) on all matters
related to optimising the mission’s scientific return.
The SOWG is composed of PI team representatives
assigned to address all science operations issues. The
Payload Operations Service (POS) at RAL (UK) is
contracted to support the PST, the PIs and the Mission
Operations Centre (MOC) in conducting efficient
operations of the mission’s scientific instruments. The
POS develops, implements, tests and operates the system
and tools required to support Mars Express.
For the detailed planning and the transition to and
implementation of the commanding of each instrument’s
operations, POS interfaces with the MOC on one side,
and with the PI institutes on the other. The PST plays a
key role in coordinating all the required inputs,
respecting the mission constraints and safeguarding the
balance in the scientific return of the Mars Express
instruments.
Up to the launch, the PST focused on preparing for
mission science planning and operations. A large effort
was spent on preparing the Master Science Plan, a
document describing the full range of Mars Express
science goals and mission planning, from global
overview to full detail. Following launch, emphasis
shifted to understanding and coordinating the mission
and its constraints in order to arrive at an efficient and
optimised mission planning process. This also involved
the first example of ‘interplanetary networking’, in
which some data from the NASA Mars rovers were
routed through Mars Express to Earth.
The PST has also been active in preparing the
requirements for the Mars Express science archive. It
was decided that the best way to implement the archive
would be through the reuse of the technology and
software used for ISO (and later XMM-Newton). The
archive was expected to be online in early 2005.
3.3.5 Venus Express
The development of the Venus Express (Fig. 3.3.5/1)
mission is progressing well and is on schedule for a
launch on 26 October 2005. The spacecraft is based on
the Mars Express platform, with modifications to the
thermal control to handle the more challenging
environment around Venus. The solar panels have been
redesigned and now use modern-technology cells that
Figure 3.3.5/1: Venus Express in fully operational
configuration. As the solar input at Venus is about
twice that at Mars, the solar panels are shorter than
for Mars Express.
operate well at the high temperatures expected at Venus,
and the size of the panels has been halved. The payload
is composed of a selection of instruments from Mars
Express, Rosetta and two newly built instruments.
Venus Express will be launched from Baikonur
Cosmodrome by a Soyuz-Fregat into a direct transfer
trajectory to Venus. The journey to Venus requires about
150 days. The operational orbit is a highly elliptic 24 h
polar orbit, with a pericentre altitude of 250-350 km and
an apocentre altitude of 66 000 km. The observations
will be split between the pericentre region, where highresolution studies of small-scale features will be carried
out, and near-apocentre and intermediate observations,
where global features will be studied.
Activities within the Planetary Missions Division have
concentrated on three areas. The first is the organisation
and lead of the Science Working Team and the related
meetings, with, as an important result, the refinement of
the scientific objectives and the definition of principles
for selecting observations for the different phases of the
mission. The second is the definition and the set-up of the
Science Operations Centre within the Division. The third
is interfacing with the ESA project team, ESOC and the
industrial contractors to follow the development of the
different elements of the project closely.
A somewhat new top-down approach has been taken to
the formulation of the scientific objectives. The
objectives are formulated as a set of fairly wide fields of
interest or ‘themes’, where each theme is broken down
into several sub-themes. The sub-themes in turn, are
broken down into a set of observations to be made, where
the physical parameters to be observed are defined. The
observations are distributed over the different phases of
the mission based on the importance of the specific
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conditions like illumination, repetition rate, conjunctions, eclipses and available downlink capability. For
each phase, all measurements that address all aspects of
the defined observations, and the individual instruments
that make the measurements, are identified. In this way,
full traceability exists in both directions: it can be seen
directly which theme is addressed by a specific
measurement and it can be verified that each theme is
properly covered with an adequate set of measurements.
The following Science Themes have been defined,
—
—
—
—
—
—
—
Atmospheric Dynamics;
Atmospheric Structure;
Atmospheric Composition and Chemistry;
Cloud Layers and Hazes;
Radiative Balance;
Surface Properties and Geology;
Plasma Environment and Escape Processes.
The organisation of the Venus Express Science
Operations Centre (VSOC) has been defined and its
interfaces to ESOC and to the individual PI institutes are
in the final state of definition. Experience from previous
missions, in particular Mars Express, Rosetta and
SMART-1, is used to synthesise a design that is flexible
and maximises the efficiency of the limited resources
available. A generic software package, MAPPS
(Mapping and Planning for Payload Science) for
assisting in the planning process is under development
in-house. A first version was distributed to the PIs and
other potential users during a dedicated workshop. The
intention is that this package will contain all functions
needed for the planning the science observations. It reads
the individual instrument request files, analyses and
checks the required resources and produces the files that
are passed to ESOC for further transmission to the
spacecraft.
The project has been progressing at an unprecedented
pace since the start in 2002. The RSSD Project Scientist
team has interacted with the project team, ESOC and
industry by participation, mainly by the Project Scientist,
in numerous meetings and by closely following and
commenting on the progress. The areas of payload
development, accommodation and operation, and
spacecraft performance and operations have been
prioritised. In some cases, when of direct interest to the
science performance, the performance and characteristics
of spacecraft subsystems have been monitored.
Contribution has been made to all major agency-level
reviews for spacecraft and ground system, as well as to
all payload reviews.
3.3.6 BepiColombo
BepiColombo is an interdisciplinary mission to explore
Mercury through a partnership between ESA and JAXA.
The mission was selected and approved by ESA’s SPC in
Figure 3.3.6/1: An example of the MMO and MPO
forming part of the BepiColombo composite stack
together with the SEPM and CPM.
October 2000 as the 5th Cornerstone mission. The
Mission consists of two orbiters, the Mercury Planetary
Orbiter (MPO), which is 3-axis-stabilised and nadir
pointing, and the Mercury Magnetospheric Orbiter
(MMO), a spinning satellite. The MMO is being
provided by JAXA. ESA is responsible for the overall
BepiColombo mission design, including launcher,
spacecraft composite, propulsion modules, ground
segment and the delivery of both spacecraft into their
dedicated orbits, as well as for the MPO and its
operations. The severe reduction of the science budget
after the Ministerial Conference in November 2001
resulted in a mission reassessment process, which started
in October 2002 with the aim of maximising the
scientific performance through the optimisation of the
payload complement, while reducing costs and
programmatic risk. The reassessment was performed by
SCI-A in close cooperation with the Planetary Missions
Division (SCI-SB), and was completed in June 2003.
The mission scenario that emerged from the reassessment was to carry the MPO and MMO together on a
single launcher (Soyuz-Fregat 2-1B) in mid-2012
(Fig. 3.3.6/1). The transfer to Mercury will be based on
Solar Electric Propulsion with a travel time of about
4.6 years. Upon arrival, the Solar Electric Propulsion
Module (SEPM) will be jettisoned and the Chemical
Propulsion Module (CPM) will provide the required
thrust for Mercury capture and orbit insertion
(Fig. 3.3.6/2).
The orbiters are dedicated to the detailed study of the
planet and its exospheric and magnetospheric environment. The MPO investigations include high-accuracy
measurements of the planet’s interior structure and a
global multi-wavelength analysis of the surface at a
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Figure 3.3.6/2: MPO and MMO orbiting Mercury.
resolution of 500 m, providing its morphology as well as
elemental and mineralogical composition. Thus surface
morphology will be correlated with surface composition.
Together with the MMO, it will provide the detailed
structure of the magnetic field and a complete characterisation of Mercury’s exosphere. The MPO orbit produces
optimal coverage of the polar regions. Hence the material
of the radar-bright spots observed from Earth and
suspected to be either water ice or sulphur will be
identified. The detection of sulphur would strongly
support the presence of at least a partially molten core.
At the start of the reassessment the Project Scientist, in
close collaboration with the external Science Advisory
Group, formulated the detailed science requirements for
the MPO scientific payload. In cooperation with the
science community, these agreed requirements were then
translated by SCI-A personnel into requirements on
instrumentation, which served as the basis for the
development of the overall payload architecture. Specific
science teams coalesced around particular themes of
MPO measurements, such as imaging, IR-spectroscopy/
radiometry, laser altimetry, UV/X-ray/gamma-ray/
neutron spectroscopy, radio science, magnetic field and
particle measurements, in order to develop the scientific
thrust of the mission. This effort resulted in a rather novel
payload concept based on a high level of integration. The
resultant MPO reference payload no longer consisted of
individual instruments, but of the front ends of these
instruments (IFE), which share common subsystems
such as data processing, electronics and power. In
addition, advantage was taken of the fact that new
technologies and miniaturisation techniques have been
developed in recent years, which allow alternative
approaches in instrument design and increased performances with lower use of precious resources (mass, power,
etc.). This new payload concept led to a significant
reduction in the mass of the reference payload which in
turn allowed for the inclusion of additional instruments
(thermal-IR mapping spectrometer and radiometer,
scientific support activities
neutral and ion particle analyser, limb pointing camera,
magnetometer), thereby maximising the mission’s
overall science return. Considerable effort by the RSSD
Project Scientist team went into further optimising this
scientific return by ensuring that specific measurements
from individual instruments could be correlated and
would complement each other. An example of this
approach is the correlation of the surface morphology
based on the optical camera instruments with the
mineralogical and elemental composition of individual
surface features as derived from the IR and X-ray
imaging spectrometers. In addition, simultaneous
measurements from the MPO and MMO will resolve
spatial and temporal ambiguities in the exosphere and
magnetosphere that would arise from single-point
observations.
In November 2003 the SPC approved this new concept
for MPO payload procurement through the endorsement
of the BepiColombo Science Management Plan. As a
result, the Request for Proposals for IFEs was issued on
26 February 2004; 20 proposals for the MPO payload
were received. On 30 September 2004 the Payload
Review Committee recommended an MPO payload
complement for selection that reflects the Reference
Payload. Considerable effort by the Project Scientist was
required in support of the Payload Review Committee
and subsequent negotiations with national funding
agencies and potential instrument consortia. As a result,
with the payload selection process now complete and the
mission deep into its definition phase, BepiColombo is
now well placed for a launch in mid-2012. Arrival at
Mercury and the start of the science exploitation phase is
expected for early 2017.
3.3.7 SMART-1
SMART-1 was launched by Ariane-5 on 27 September
2003. The commissioning of the spacecraft, its ion
engine and instrument functional checks were completed
during the first few weeks after launch. SMART-1 had to
travel through the inner radiation belts, during which
very violent solar flares in October-November 2003
made the operation of the startrackers and the ion-driven
spacecraft very difficult. The instruments were
commissioned in February 2004 and the first images and
spectra from the Earth and the Moon were obtained.
After an eclipse period in March 2004, the spacecraft
expanded its spiral towards the Moon, until the lunar
resonant approaches on 19 August (when SMART-1 was
closer to the Moon than to Earth for the first time), on
27 September and again on 12 October 2004.
SMART-1’s science objectives include studies of the
chemical composition of the Moon, of geophysical
processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative
planetology, and high-resolution studies in preparation
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Figure 3.3.7/2: Images taken by SMART-1 during the
lunar approach phase. The right image shows a slice
of the Moon’s far side and north pole; this was seen
for only the second time in the history of lunar
exploration.
Figure 3.3.7/1: First image of Europe obtained by
AMIE, from 70 000 km in July 2004. This began a
series of synoptic Earth images for camera operation
validation and calibration.
for future lunar exploration. The results could provide
new insights into topics such as the accretion processes
that led to the formation of rocky planets, and the origin
and evolution of the Earth-Moon system
The SMART-1 science payload, with a total mass of
19 kg, features many innovative instruments and
advanced technologies such as a miniaturised highresolution camera (AMIE) for lunar surface imaging, a
near-IR point-spectrometer (SIR) for lunar mineralogy
investigation, and a very compact X-ray spectrometer
(D-CIXS) with a new type of detector and microcollimator that will provide fluorescence spectroscopy
and imagery of the Moon’s surface elemental
composition.
The cruise and lunar approach demonstrated a number of
technologies (spacecraft, navigation, operations and
instruments) that will be useful for the future. The
mission’s prime objective, to demonstrate Solar Electric
Propulsion, has been fulfilled. The RSSD Project
Scientist and support team, together with the Science and
Technology Operations Coordination (STOC) centre at
http://sci.esa.int/smart-1/
Figure 3.3.7/3: Mosaic view of crater Pythagoras
taken by AMIE on 29/30 December 2004 from an
altitude of 4000 km.
ESOC, have been planning payload operations for the
cruise phase and the first part of lunar phase.
The SIR IR spectrometer showed nominal performance
when it measured the first near-IR space spectra of the
Moon in the range 0.9-2.5 µm. It also measured, by
comparison, Earth reference spectra with atmospheric
absorption. The comparison between lunar spectra has
demonstrated the ability of the instrument to distinguish
the mineralogy of different areas on the Moon.
AMIE has achieved a number of Earth pointings
(Fig. 3.3.7/1) which have been used not only for
educational and outreach purposes, but also to measure
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scenes of planetary interest using various colour filters
(geologic features such as volcanic terrains). It has also
observed the Moon at different distances and phases to
validate the instrument performances and exposure times
(Fig. 3.3.7/2 & 3.3.7/3). The Project Science team has
been heavily involved in the planning and execution of
these operations during this early preparatory phase.
SMART-1 has been the only mission in lunar orbit since
it was captured by the gravity field on 15 November
2004. Beyond its remaining primary science objective,
the mission provides, both for ESA and Europe, an
excellent strategic position from which to contribute to
future international lunar exploration collaborations with
approved missions (Lunar-A, Selene, Chandrayaan-1,
Chang’E, Lunar Reconnaissance Orbiter, Moonrise), and
possibly within the framework of the new NASA
Exploration initiatives.
By the end of 2004, more than about 110 papers related
to SMART-1 had been published in the scientific
literature, including 23 refereed papers. There is a large
public interest, as indicated by the media response,
articles and the web presence that showed Europe-wide
visibility for SMART-1 science and technology.
scientific support activities
3.4
Fundamental Physics Missions Division
3.4.1 Introduction and overview
The main activities in the Fundamental Physics Missions
Division fall into three areas: direct detection and
observation of gravitational waves, high-precision tests
of the Equivalence Principle (EP), and fundamental
physics applications of laser-cooled atoms.
In the first area, two missions are supported by the
Division: LISA (Laser Interferometer Space Antenna)
and LISA Pathfinder (formerly SMART-2). LISA is a
mission to detect and observe gravitational waves, jointly
undertaken with NASA. LISA Pathfinder is a technology
mission, aimed at demonstrating and validating key
technologies for LISA. During most of the reporting
period both missions were supported by an RSSD Project
Scientist. In July 2004, ESTEC hosted the 5th International LISA Symposium, organised by the LISA
Project Scientist. Various other workshops and meetings
associated with LISA and LISA Pathfinder took place
during the reporting period.
In the second area, the Division supports the Microscope
mission. This is a CNES/ESA collaborative mission to
test the EP in space, with a launch by the end of 2007.
The third area includes the Atomic Clock Ensemble in
Space mission. ACES is under development for flight
aboard the ISS, led by the Directorate of Human
Spaceflight, Microgravity & Exploration (D/HME); the
Division provides support in the form of a Project
Scientist.
3.4.2 LISA Pathfinder (formerly SMART-2)
LISA Pathfinder (LPF) is primarily intended to demonstrate the key technologies for the LISA mission,
especially the performance of the inertial sensors that
cannot be tested on the ground. To this end, LPF will
accommodate a LISA Technology Package (LTP),
provided in large part by European institutes and
industry, and a Disturbance Reduction System (DRS)
that is very similar to the LTP and has the same goals but
is provided by US institutes and industry. LTP and DRS
will be accommodated on a single spacecraft, injected
into an L2 halo-orbit. The projected mission duration is
180 days, shared between LTP, DRS and a joint
operational mode. The mission goals for the LTP are:
— demonstrating drag-free and attitude control in a
spacecraft with two proof masses in order to isolate
the masses from inertial disturbances. The aim is to
demonstrate a performance on the order of
10–14 m/s2/Hz1/2 in the frequency band 1-100 mHz.
The corresponding requirement for LISA is
10–15 m/s2/Hz1/2;
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— demonstrating the feasibility of performing laser
interferometry in the required low-frequency regime
with a performance as close as possible to
10–12 m/Hz1/2 in the frequency band 1-100 mHz, as
required for LISA;
— assessing the longevity and reliability of the
capacitive sensors, thrusters, lasers and optics in the
space environment.
As the environment of the LPF spacecraft will be
comparatively noisy (in terms of temperature
fluctuations and magnetic disturbances) compared to the
LISA environment, the mission goal for LPF is to meet a
performance of the inertial sensor that is a factor of 10
more relaxed than is required for LISA. This will allow
validation of the models derived and extrapolated from
ground testing, and further extrapolation to the LISA
requirements.
The LTP represents one arm of the LISA interferometer,
the distance between the proof masses is shrunk from
5 million km to 20 cm. As in LISA, the proof masses
fulfil a double role: they serve as optical references
(‘mirrors’) for the interferometer, and as inertial
references for the drag-free control system. The drag-free
control system aboard the LTP consists of the inertial
sensor, a propulsion system and a control loop using
capacitive sensing in all six degrees of freedom, as well
as the interferometric readout system.
After completing the two parallel system-level industrial
studies in 2003, both of which were actively supported
by the Project Scientist. the implementation phase began
in May 2004. A major milestone was passed by the
successful completion of the System Requirement
Review (SRR) in November 2004.
3.4.3 LISA
The objective of the LISA mission is the detection and
observation of gravitational waves from super-massive
black hole coalescences and galactic binaries in the
frequency range 0.1-100 mHz. The mission includes
three identical spacecraft, located at the vertices of an
equilateral triangle with a baseline of 5 million km. The
centre of the triangle is in the plane of the ecliptic, 1 AU
from the Sun, and trailing Earth by about 20º. By
measuring the distance between the spacecraft
interferometrically, the effects of a passing gravitational
wave can be registered. The orbital motion of the
detector allows information about the position and
orientation of the gravitational waves’ sources in the sky
to be obtained. The scientific goals of LISA are:
— determine the role of massive black holes in galaxy
evolution;
— make precision tests of Einstein’s Theory of
Relativity;
http://sci.esa.int/lisa/
— determine the population of ultra-compact binaries
in the Galaxy;
— probe the physics of the early Universe.
LISA is an ESA/NASA collaborative mission with a
launch foreseen in the 2012-2013 timeframe. By the end
of 2004, the project had entered the formulation phase
(Phase-A), both in Europe and in the US. As a means of
ensuring good communication between the engineers
and scientists, regular meetings involving both sides take
place. They are held typically three times per year,
alternating between the involved centres, ESTEC, GSFC
and JPL. The RSSD Project Scientist and his US
counterpart coordinate this activity.
To develop the requirements and design for the mission
and oversee the definition and development, helping to
make trade-offs and mission design choices, NASA and
ESA formed a LISA International Science Team (LIST)
in early 2001. LIST has 11 European and 11 US
members, including the respective Project Scientists. As
the project entered mission formulation at the end of
2004, LIST met for the last time in December 2004
before being disbanded. The science team will be
reinstated with modified membership and charter in 2005
to support the mission formulation phase.
In July 2004, ESTEC hosted the biennial International
LISA Symposium, organised by the RSSD Project
Scientist. The Symposium attracted over 160 scientists;
about 80 papers and posters were presented.
3.4.4 ACES
The Atomic Clock Ensemble in Space (ACES) mission
consists of a caesium-atom clock and a hydrogen-maser
clock aboard the ISS, plus laser and microwave links to
ground stations. It is managed by D/HME; the RSSD
Project Scientist provides scientific support and SCI-A
has assisted in technical development and programmatic
issues.
The ACES atomic clocks will be used as high-sensitivity
sensors for experimental tests of general relativity. The
mission will contribute to fundamental physics
experiments in two distinct areas:
— an improved measurement of the redshift by
comparing ultra-stable clocks aboard the ISS and the
ground. The expected improvement over Gravitational Probe-A is a factor 25. A number of auxiliary
measurements, such as a high-precision test of the
Sagnac effect and the search for a possible
anisotropy of the one-way speed of light (the theory
of special relativity), can be performed with
significantly improved precision;
— the search for a possible drift of the fine structure
constant. This constant characterises the strength of
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the electromagnetic interaction. The principle of the
experiment is to compare the rate of atomic clocks
(using different elements) as a function of time.
Another test of relativity is to search for a possible
anisotropy in the one-way propagation of light. The
comparison of ACES clocks with ground clocks
distributed worldwide will involve propagation of
electromagnetic waves (both optical and microwave) in
very different directions.
3.4.5 Microscope
Microscope (MICROSatellite à trainee Compensée pour
l’Observation du Principe d’Equivalence) will be the first
mission to test the EP in space. The accuracy is 10–15, 2-3
orders of magnitude better than possible on the ground or
with lunar ranging.
The payload comprises two differential electrostatic
accelerometers, one testing a pair of identical materials
(to provide an upper limit for systematic errors), one
testing a pair of different materials (the EP test proper).
The test masses are freely falling concentric cylinders of
platinum and titanium, respectively. A violation of the EP
would manifest itself as a differential movement of the
proof masses with the orbital frequency of the satellite.
The 3-axis stabilised, 193 kg satellite is planned for
launch in November 2007 on a shared Dnepr rocket into
a Sun-synchronous, quasi-circular orbit at about 700 km
altitude. The drag by the residual atmosphere at orbital
altitude and solar radiation pressure will be compensated
by a drag-free control system using Field Emission
Electric Propulsion (FEEP) thrusters. The required dragfree performance is 3x10–10 m/s2/Hz1/2 in the measurement
bandwidth.
Microscope is a CNES/ESA collaboration: ESA’s share is
the procurement of the FEEP thrusters. In return, ESA
will have full access to all FEEP flight data, which will
provide a valuable technology test in space for a whole
suite of future astronomy and fundamental physics
missions.
3.5
Space Telescope Operations Division
The Space Telescope Science Institute (STScI) is
responsible for all aspects of HST operations and, in
particular, its scientific productivity. The Space
Telescope Operations Division of ESA contributes to this
effort with the assignment of 15 ESA staff scientists and
engineers. Some of the senior staff members have
achieved significant leadership roles within the
Institute’s structure and are influential in key areas of the
decision-making process. In addition, activities in
support of the Hubble programme are carried out at the
ST-European Coordinating Facility in conjunction with
ESO. The Division manages and leads these activities.
The Hubble programme is considered to be one of the
most effective science missions ever, as rated by citations
in science news media. It has one of the most recognised
names and it is routinely cited as a major reason for
increased worldwide interest in astronomy. The demand
for telescope time is at a record high: more than six times
as much time was requested in Cycles 12 and 13 than
was available.
Highlights of the HST programme include notable
enhancements in Hubble’s ability to produce world-class
science, along with several achievements that gained
worldwide attention. By every measure, HST has more
science capability now than at any time in its lifetime. It
has achieved a discovery power 10 times greater than at
the beginning of the reporting period; ESA staff
contributed to all phases of this improvement.
The year of 2003 began with the tragic loss of the Space
Shuttle Columbia and its crew of seven on 1 February. It
ended with Hubble returning data of unprecedented
quality and size as a result of the instrument upgrades
made by Columbia’s crew on its last mission before the
disaster, Servicing Mission 3B. In between, we saw the
continued growth of new ideas to use Hubble to
understand the cosmos, stimulated by its evolution as the
world’s only serviceable space telescope.
Hubble was designed for an entirely different set of
scientific problems than those it is solving now. Most of
the original problems were solved in Hubble’s first
decade, and it is now concentrating on the most
important topics of today, none of which was developed
or even imagined during Hubble’s design. Yet Hubble is
now a dominant force in these new topics, in some cases
uniquely so.
A primary responsibility of the Institute, and an activity
led by RSSD staff, is to optimise the HST science
programme. There are several major areas where the
Institute adds value to the Hubble science programme,
and these are naturally the focus of our improvement
activities. These include stimulating the best possible
science programme from the astronomy community via
http://ecf.hq.eso.org/
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the proposal selection process, achieving the highest
possible observing efficiency with the telescope,
providing timely and accurate calibration of the Hubble
data, stimulating the use of the Hubble data archive for
additional scientific results, and providing tools to
support the astronomical community’s use of the
telescope and the archive.
Programs were selected and some are already fully
completed. As an example, investigators from
programmes such as the Great Observatories Origins
Deep Survey have already published more than 30 papers
describing their results in prestigious journals. The high
quality of papers based on Hubble observations reflects
the high degree of competitiveness of the proposal
process.
3.5.1 HST observation programme
Another important change was the start of the Hubble
Theory Program, funded as part of the Hubble Archival
Research programme. The Theory Program stressed the
importance of promoting theoretical research in
conjunction with major observing facilities, in order to
improve the interpretation and understanding of the data
from these facilities.
2004 saw continued evolution in the process for selecting
the Hubble science programme. Major improvements
were made, starting with Cycle 12, by reducing the time
between submitting proposals and starting observations
in an observing cycle. The Phase I deadline was moved
from September to the end of January, with observations
starting in July. Shortening the time between proposal
deadline and cycle start helps to ensure that recent
findings have greater influence on new Hubble
observations, quickening the pace of scientific advance.
Observatory operations continued at high efficiency,
averaging 43.7% for prime science observations and
48.6% for prime plus snapshot observations. Almost 60%
of Hubble’s observing time in the current cycle uses the
Advanced Camera for Surveys (ACS), installed during
SM3B in April 2002. The science data rate increased by
more than a factor of two following the installation of the
new instruments and the ground system has been
upgraded to respond to this increase challenge. HST is
also becoming easier to use, thanks to the new tools
produced at the Institute; migration of the archive data to
magneto-optical media was completed in 2004. Several
new software tools in support of HST operations were
released: the Astronomer’s Proposal Tool (APT),
StarView and the Space Telescope Grant Management
Systems (STGMS) are fully operational. These activities
involved considerable effort by RSSD staff.
3.5.2 Special HST programmes
STSci and, in particular, the ESA staff have provided
leadership in several important science policy issues.
Two new programmes, Treasury and Theory, added
opportunities for scientists to do research with Hubble
and its data archives. The Hubble Treasury Program was
started in Cycle 11 to stimulate science that might not
naturally be encouraged by the existing process, and, in
particular, to promote the creation of important data sets
that one would regret not having obtained when Hubble
is ultimately decommissioned. Treasury programmes
address multiple scientific problems with a single,
coherent dataset. The data sets carry no proprietary
rights. Recently compiled metrics support the conclusion
that papers from larger programmes, such as the Treasury
Programs, have considerably higher scientific impact
than those from smaller programmes. Several Treasury
A successful policy-related topic has been the
implementation of the project to trade observing time
between Chandra and HST. Both the HST and Chandra
Time Allocation Committees and users are very
supportive of the concept.
3.5.3 Instrument status
With the demise of the imaging spectrograph (STIS),
there has been renewed interest in the slitless capabilities
of ACS, particularly in the UV. In-orbit calibration data
are being reduced and a further calibration programme is
being planned to ensure that users are able to obtain highfidelity spectra from these modes. Wide Field Camera 3,
planned to be installed in HST in the next servicing
mission, is undergoing ground testing and ECF is
involved in the testing of the three grisms, one for the
near-UV and two for the near-IR. The possibility of
applying the extraction software to FORS2 MXU data is
currently being investigated and some daytime
calibrations have been taken to determine the feasibility
of this approach.
Under the Extension of the NASA/ESA MoU on HST,
the Instrument Physical Modeling group continued the
work on upgrading the HST STIS calibration pipeline
(STIS-CE) with physical model-based modules. This
work is the consistent further development of the idea
that calibration should make use of all the a priori
information that is available from the physical principles
that are embedded in the instrument’s design and
construction. Earlier testimony to the advantages of this
concept is the stability of the ESO VLT UVES pipeline
and the several solutions provided for calibration
shortcomings of the HST FOS spectrograph.
3.5.4 The European Coordination Facility
The Hubble ESA Information Centre (HEIC), which was
established at ST-ECF, continued to supply material to
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the media and public. With a unique graphical expression
in all lines of products, high scientific quality and
innovative distribution methods, the group has received
international recognition for their achievements.
data flows through sophisticated applications will be
deomstrated, along with the use of ‘registries’ to harvest
astronomical databases.
On a yearly basis, HEIC receives more than 1000
requests from press, public, educators, scientists and
others for printed products, information and electronic
products. Apart from the production of news and photo
releases, innovative educational material, CD-ROMs,
brochures and posters, the HEIC has made important
contributions. With up to 16 million hits/month, more
than 125 000 individual visitors and up to 2 TB of data
delivered, the http://www.spacetelescope.org website
belongs in the top group of astronomical outreach web
sites. Production of PR images from raw data continues.
This work has been based on HST data, but also images
from ESA missions such as ISO, XMM-Newton and
Integral, as well as the ESO VLT and others, have been
produced. This work is the most advanced of its kind in
Europe, producing high-quality artist’s impressions in
2-D and 3-D using highly optimised, very sophisticated
software and hardware technique. High-quality video
material for news releases can be produced on timescales
of a few days. The online distribution of broadcastquality video material enables broadcasters to use the
HEIC material in the evening news on the same day.
3.5.5 HST operational status
Slitless spectroscopy from space is competitive with
ground-based spectroscopy with large telescopes in those
spectral regions where the atmospheric background is
high. HST has exploited this advantage and offers slitless
spectroscopy facilities on NICMOS and ACS. The ECF
has developed expertise in all aspects of slitless
spectroscopy through support of the HST slitless
spectroscopy modes. Through well-defined agreements
with the STScI, the ECF has undertaken full cover for
these instruments, from involvement in ground testing, to
provision of software to extract wavelength and flux
calibrated spectra, to user support. Currently, most effort
goes into support for the ACS slitless modes, which
cover the red grism for the WFC and HRC, a near-UV
prism for HRC and two prisms for the far-UV SBC.
The Virtual Observatory (VO) project is evolving
quickly. The current ECF archive development includes
the creation of a database layer to host ancillary
information (metadata, which fully describe the HST
products through VO-compliant interfaces), and a
database of instrumental characteristics (initially for
ACS and WFPC2). The next VO science demonstration
is scheduled for January 2005 at ESAC. The VO project
is driven by its strategy of regular scientific
demonstrations of VO technology, held on an annual
basis. The next, based on input from the Science Working
Group, will revolve around two science cases: ‘Rich
Clusters of Galaxies’ and ‘Asymptotic Giant Branch to
Planetary Nebulae Transition’. On the technical side, the
use of powerful, distributed workflow processes driving
The HST spacecraft is operating nominally, but 2004 saw
the demise of STIS on 3 August. To make up for the loss
of scientific programmes, an additional 45 proposals
have been approved. These had already been rankordered by the original Cycle 13 TAC. A number of
already-approved programmes that originally used STIS
are in the process of being converted to use other
instrument modes, most notably ACS/SBC. RSSD
institute staff were actively involved in these complex
replanning issues.
As the observatory ages, and in the event it has to operate
with only two gyros before a refurbishment can take
place, preparations and development for the Two-Gyro
Science Mode continue, involving a number of the RSSD
division staff. Extensive documentation and user
information is available at the STScI website, including
a Two-Gyro Handbook and a ‘movie’ showing target
availability under the somewhat more restrictive
scheduling opportunities with two gyros. Detailed
simulations show that the impact on image quality from
jitter is substantially less than originally assumed, so that
a voluntary entry into Two-Gyro Mode is now being
discussed in order to preserve the lifetime of the
currently operating four gyros. In support of this
decision, detailed studies are under way to determine
how many orbits per week can be scheduled in two-gyro
mode as compared to using three units. On-orbit tests are
planned for February 2005.
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3.6
Science Operations and Data Systems
Division
3.6.1 Introduction and overview
The Science Operations and Data Systems Division
(SCI-SD) is responsible for the development and
execution of science operations for astronomy missions.
After completion of the in-orbit commissioning phase,
the Division becomes responsible for overall project
management: a Mission Manager is put in overall charge
and must ensure that operations are performed in the
most efficient manner possible within the constraints; the
Project Scientist remains responsible for ensuring
maximum scientific return. The Division also provides
support in data systems to the entire Department and has
long-term responsibility for the science archives of the
Directorate. The staff of the Division is located at ESAC
and ESTEC. During much of the reporting period, there
was also one staff member collocated with the Integral
Science Data Centre in Versoix (CH).
3.6.2 ISO
The Infrared Space Observatory (ISO) was the world’s
first true orbiting IR observatory. With a pointing
accuracy at the arcsec level and four highly sophisticated
scientific instruments, ISO explored the Universe at
wavelengths of 2.5-240 µm with unprecedented
sensitivity and capabilities. During its highly-successful
in-orbit operational phase from November 1995 to April
1998, ISO made some 30 000 individual scientific
observations of all types of astronomical objects. All the
data are available to the community via the ISO Data
Archive – follow the links from the ISO home page at
http://www.iso.vilspa.esa.es. The ISO project is well into
its Active Archive Phase, which will run until December
2006. This final phase is designed to maximise the
scientific exploitation of ISO’s extensive IR database and
to leave behind a homogeneous archive with refined data
products, as a legacy to future generations of
astronomers.
RSSD has the cradle-to-grave responsibility for ISO
scientific operations and, from the end of the
commissioning phase, overall responsibility for the
project. The Division has a team of staff and contractors,
led by the Project Scientist, in ESAC. Activities of this
team include maintaining the central data archive,
providing expert support to the community across all
instruments, and coordinating activities with the various
national ISO centres.
Archive maintenance and improvement activities have
continued. Version 6 of the ISO Data Archive, released in
July 2003, upgraded the functionality associated with,
and visibility of, the Highly Processed Data Products (the
result of dedicated projects focused on cleaning the
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pipeline products from residual instrumental artefacts).
Dedicated projects were undertaken, mainly in
collaboration with the national centres, to reprocess
observations of selected observing modes. As of October
2004, the archive includes 19 such data sets, some also
obtained from the community, equivalent to 18% of the
archive scientific content. For version 7, released in June
2004, a new approach was defined in the assessment of
the data quality, upgrading from a small set of technical
quality flags to a well-structured quality report, based on
a total of 85 flags.
The astronomical community continues to use the ISO
archive intensively. There are now 1600 registered users
and new users are still registering at a rate of about 10-15
per month. In the first 6 years of use, the equivalent of
nearly nine times the total number of scientific
observations in the archive has been downloaded, an
average monthly retrieval rate of around 13%.
Another major activity has been the integration of the
ISO archive into the Virtual Observatory. The ISO
archive already incorporated many elements of
interoperability with other popular astronomical
archives. The ad hoc implementation of these functionalities has evolved into a system complying with the new
standards set by the VO international community. ISO
was one of the first archives to be part of the European
VO prototype, as demonstrated in January 2004.
Documentation has also been a focus of activity. The
legacy version of the five-volume ISO handbook, the
definitive standalone guide to the ISO mission and to its
data products, was published in early 2004 (as ESA
SP-1262) and distributed to the PIs of the ISO observing
proposals and to some 300 astronomical libraries
worldwide. The proceedings of two recent conferences
organised by the ISO Data Centre were also released in
the period, Exploiting the ISO Data Archive – Infrared
Astronomy in the Internet Age (SP-511) and The
Calibration Legacy of the ISO Mission (SP-481).
The ISO Active Archive Phase Mid-Term Review was
held in June 2004. The Board, composed of external data
providers and users, was impressed with the
achievements of the ESA and National Data Centres over
the previous 2.5 years. Their recommendations focused
on making ISO data and results as widely available as
possible, by (i) concentrating the activities during the
remaining 30 months on maximising the content and
visibility of the Highly Processed Data Products, (ii)
continuing with the integration of the ISO archive into
the VOs, (iii) ensuring prompt publication of the planned
special issue of ISO Space Science Reviews, a 400-page
book reviewing the results of ISO.
In the 2003-2004 period, around 250 papers based on
ISO appeared in the major refereed journals (1160 papers
are known in total and tracked in the ISO data archive).
http://www.iso.vilspa.esa.es
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With the ISO data archive having establishing itself as a
general astronomical research resource and as an
important tool for planning future missions, with
activities continuing on enhancing its contents and
functionality, many more astronomical surprises and
discoveries from ISO are still expected.
3.6.3 XMM-Newton
XMM-Newton is an X-ray astrophysics observatory,
launched on 10 December 1999 with a projected and
designed lifetime of over 10 years. It enables
astronomers to conduct sensitive X-ray spectroscopic
observations of a wide variety of cosmic sources. It is
specifically designed to investigate in detail the spectra
of cosmic X-ray sources down to a limiting flux of
10–15 ergs/cm2/s. It is able to detect X-ray sources down to
a few times 10–16 ergs/cm2/s; however source confusion
starts to play a role at these flux levels. The principal
characteristics of XMM-Newton, with its three
telescopes and suite of complementary instruments
(EPIC, RGS, OM used simultaneously), can be
summarised as follows:
— effective aperture of 4500 cm2 at 1 keV (12.4 Å) and
1000 cm2 at 10 keV (1.24 Å);
— almost constant angular resolution across the full
waveband of ~15 arcsec HEW;
— X-ray field of view ~30 arcmin;
— capability of performing sensitive mediumresolution spectroscopy with resolving powers 100700 over the wavelength band 5-35 Å (3502500 eV);
— broadband imaging spectroscopy from 300 eV to
12 keV (1-40 Å);
— simultaneous sensitive coverage of the wavelength
band 1600-6000 Å (~17 arcmin FOV) through a
dedicated optical monitor, co-aligned with the X-ray
telescopes;
— continuous coverage of a source for up to 42 h.
Further details, including access to the data archive, may
be found by visiting http://xmm.vilspa.esa.es.
The Division has overall management responsibility for
the project and is directly responsible for the execution of
science operations. Mission operations for XMMNewton are conducted from ESOC, while science
operations are conducted from ESAC, where the Science
Operations Centre is located. The main tasks of the SOC
are:
— monitoring payload operations in real time;
— performing mission planning and constructing an
optimally efficient schedule. This includes issuing
and processing announcements of opportunity;
— maintaining and updating all XMM-Newton
handbooks;
http://xmm.vilspa.esa.es/
Figure 3.6.3/1: These four images illustrate the
XMM-Newton observtion of GRB 031203. The ring
structures expanding around the point source are the
first time-dependent light echo seen in X-rays.
— tracking the maintenance and implementation of
change requests to the SOC operations subsystems
by external contractors;
— defining, implementing and tracking procedures for
operating the scientific instruments;
— implementing instrument calibration observations,
coordinating and participating in their analysis, and
delivering finalised calibration files to the community;
— co-developing, pre-release checking and distributing
the Science Analysis Software (SAS) and the
associated data products.
During the reporting period, the work still performed at
ESTEC (except for mission management) was
transferred to ESAC.
During Autumn 2003, the Division prepared the case for
extending mission operations and presented it to the
scientific advisory structure and to the SPC, which
unanimously approved the principle of an extended
mission up to 31 March 2008. With such an outlook,
efforts to streamline and reduce the cost of operations
continue. In this context, a reduction in (contractor) staff
has already been implemented without affecting the
overall performance of the observatory or the ground
segment. One of the other elements to ensure that an
extended, cost-effective future is possible has been the
decision to transfer the operating system for the mission
control systems from SCOS-1b to SCOS-2000. This
activity is nearing completion and will, inter alia, provide
a solid operating environment up to the end of the mission.
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A new general management structure for satellites in orbit
was introduced. For XMM-Newton, this meant a
separation of the role of Mission Manager and Project
Scientist. The Mission Manager continued to work 50% on
XMM-Newton and a new Project Scientist was appointed
at ESAC. This new set-up is working extremely well.
85
scheme has been running for almost a year now and is
under evaluation. There is a clear indication of increased
science output from the SOC team contributing to the
650 refereed XMM-Newton publications so far.
3.6.4 Integral
The XMM-Newton users’ group now meets on an annual
basis, instead of biannually, as it was felt the mission is
now routinely and reliably turning out all products
expected by the community. In general, it is very positive
about the status of the mission.
With the improved knowledge and experience both in
mission planning and schedule execution, the SOC can
now carry out the necessary replanning and get the
satellite repointed in response to a target of opportunity
alert in as little as 4 h 40 min after receipt of the alert.
This is well beyond what the mission was designed for,
and provides spectacular science results (Fig. 3.6.3/1).
The calls for observing proposals are now issued annually
by the SOC and the process has become routine. The
uptake by the community remains very high, with 692
proposals submitted in response to AO-3 and 657 in
response to AO-4. The oversubscription factor is around
5-6. There is a clear and continuing trend to go for longer
observations and multiple sources per proposal.
A number of new releases of the XMM-Newton Science
Archive (XSA) and the Science Analysis Software (SAS)
were made available to the community. The XSA has now
become the standard tool for the community for retrieving
(and searching) both proprietary and public data. A few
thousand public data sets are available through the XSA.
One of the major new components integrated into the
XSA was the first XMM-Newton source catalogue
(1XMM), generated by the Survey Science Consortium
(SSC, PI: M. Watson, Leicester, UK). Preparations for
generating a second, extended, source catalogue have
started inside the SSC, and ESAC is actively regenerating
data sets wherever new processing (attitude, timing, etc.)
provide improvements. The SAS (now at release 6.0) has
become the de facto standard for analysing XMMNewton data; it is a complete suite of tools, which now
contains the tools to analyse grism spectra from the
Optical Monitor.
The observatory has implemented support of COSPAR
regional education activities (New Delhi, 2003; Durban,
2004) and is routinely organising workshops at ESAC to
teach people how to use the XMM-Newton data analysis
system.
In order to support observatory staff in executing their
science research objectives, the concept of a ‘science day’
has been introduced. This is a fixed day in the week that
is set aside for research. On this day, in principle, no
meetings or other functional duties are scheduled. The
The Integral gamma-ray observatory is dedicated to
spectroscopy and imaging of celestial gamma-ray sources
in the energy range from 15 keV to 10 MeV. It was
launched on 17 October 2002 by a Russian Proton rocket.
The payload consists of two imaging gamma-ray
instruments, one optimised for spectroscopy (SPI) and one
for high-resolution imaging (IBIS). These are supported
by co-aligned X-ray (JEM-X) and optical (OMC)
monitors. All three high-energy instruments use coded
masks for imaging. Further information is available at
http://astro.estec.esa.nl/Integral. The majority of Integral
observing time is available to the general astronomical
community via calls for proposals, with a smaller amount
(currently 25%) used for survey-type Core Programme
activities such as deep exposures of the galactic centre
region and regular scans along the galactic plane. Integral
operations continue smoothly, with the spacecraft,
instruments and ground segment performing well. A major
milestone was reached on 17 July 2004 when the first
Integral observations entered the public domain. These are
available to the scientific community via the on-line
archive at the Integral Science Data Centre.
The Division has overall management responsibility for
the project and is directly responsible for the Integral
Science Operations Centre, handling uplink and coordination activities. During the reporting period, ISOC was
located at ESTEC but is being moved to ESAC.
Downlink science operations (data processing and
distribution) are the responsibility of the Integral Science
Data Centre (ISDC, Versoix, CH). Mission operations
are conducted from ESOC. The main tasks of ISOC are:
— to issue Calls for Observing Proposals and to process
the submitted proposals;
— to conduct the scientific mission planning, including
processing ToO requests;
— to operate, jointly with the ISDC, a web-based
helpdesk to support Integral users who have questions about any aspect of the mission, or their own
observations.
Additionally, in close collaboration with the Integral
Science Working Team, the ISOC works:
— to finalise the Core Programme of guaranteed-time
observations for each AO-cycle and implement them
into the ISOC scheduling system;
— to prepare and manage the instrument in-flight calibration during the nominal and extended mission
phases;
http://integral.esac.esa.int
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creation of the corresponding commands to be sent to the
spacecraft. The Integral observing schedules, both shortterm and long-term, are available on the web. The overall
observing programme is summarised in the exposure
map (Fig. 3.6.4/1), which includes all observations to
February 2005.
Figure 3.6.4/1: Integral exposure map covering
scientific observations from December 2002 (start of
the nominal mission phase) until February 2005 (end
of AO-2 observing programme).
— to support the instrument teams in instrument
configuration and operations (e.g. telemetry
allocation, annealing of the SPI detector unit).
During Autumn 2003, the Division prepared the case for
extending mission operations and presented it to the
scientific advisory structure and to the SPC, which
unanimously approved the principle of an extended
mission up to 31 December 2008, with a review of the
science foreseen in Autumn 2006. An element of the
mission extension is to move ISOC from ESTEC to
ESAC in order to increase synergy with XMM-Newton.
The Mission Manager is ensuring that this transition is
conducted in the most cost-effective way, while
maintaining full operational capabilities. A plan for the
evolution of the ISOC manpower has been developed by
the ISOC manager and the activities defined in the plan
are underway, with science operations transferring from
ESTEC to ESAC in February 2005.
During the reporting period, two Calls for Observing
Proposals (AO-2 in 2003, AO-3 in 2004) were issued and
processed. The response from the community remained
strong, with 142 and 108 proposals received, respectively, with over-subscription factors of 8 for AO-2 and 4
(equivalent to 6 if the duration of the AO is taken into
account) for AO-3. After each AO, the pointing directions of the approved observations are scanned by ISOC
staff for targets close together in the sky which can be
observed in a single pointing – hence saving observing
time through amalgamation of several independent
research proposals. This is particularly important for
Integral where the observations are, owing to the low
fluxes, generally long, but the fields of view of the
gamma-ray instruments are very large (the fully coded
fields of view are 16º for SPI and (9x9)º for IBIS). The
accepted proposals are processed at the ISOC into an
optimised observing plan consisting of a timeline of
target positions, together with the corresponding instrument configurations. These are then forwarded to the
Mission Operations Centre (MOC) at ESOC for the
The gamma-ray sky is highly variable and interesting
new targets can, and do, appear unexpectedly anywhere
in the sky. When this happens, a ‘Target of Opportunity’
(ToO) request may be made. The Project Scientist,
supported by the ISOC mission planners, evaluates the
request and decides on the basis of scientific merit and on
the impact of the rescheduling, whether to go ahead. If
the request is granted, the ISOC generates a new
observing programme for the interval concerned and,
inter alia, makes this available on the WWW to aid
astronomers planning coordinated observations. During
the reporting period, 36 requests for ToO follow-up
observations were received, out of which 16 were
accepted and successfully observed.
The achieved sensitivities of the Integral high-energy
instruments are now close to the statistical limits derived
from the background counting rates and effective areas.
The Mission Manager has coordinated the activities to
improve the achieved sensitivities through better
observing techniques, background modelling and
analysis software.
One of the few major payload anomalies has been the
loss of two of the 19 SPI detectors. Both of these losses
followed annealing, when the SPI detectors are ‘baked’
to recover the loss of energy resolution caused by
radiation damage. The Mission Manager has coordinated
the efforts to understand the failures, using both in-flight
tests, ground tests on flight spare hardware, and
computer modelling. Once the failures are understood, it
will be possible to decide on future annealing strategies.
The Project Scientist coorganised the 5th Integral Workshop (Munich, February 2004) and co-edited the proceedings (SP-552). Support is being provided to organise an
Integral workshop in January 2005 (ESTEC) and the 6th
Integral Workshop in 2006 in St. Petersburg (Russia).
Finally the Project Scientist, in coordination with the
ISWT, contributed to the definition of the terms of
reference for the new Integral Users Group and the
associated update of responsibilities for the ISWT as laid
down in the Science Management Plan.
3.6.5 Astro-F
Astro-F is a Japanese mission with the prime goal of
making a second-generation all-sky IR survey with
higher sensitivity and longer wavelength coverage than
IRAS. ESA is collaborating with JAXA to provide
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tracking support (use of a second ground station) and
assistance with the survey data reduction (pointing
reconstruction) in return for 10% of the observing
opportunities during the non-survey parts of the mission,
to distribute to the ESA community. The SPC approved
this collaboration in Autumn 2000. During the reporting
period, JAXA/ISAS have announced launch delays from
February 2004 to end-2005 or early 2006. The Division
has overall responsibility for all of ESA’s contribution to
this mission.
Implementation of tracking support has been delegated to
ESOC, who, during the reporting period, have designed,
implemented and tested the various upgrades and
customisations necessary to enable the Kiruna tracking
station to provide the required service. All equipment is
now in hibernation until launch preparations start
6 months before launch. Activities for pointing
reconstruction and community support are carried out by
the Division’s team in ESAC. Work on the input
reference catalogues, needed for the pointing reconstruction task, was completed as planned by end-2004. The
Pointing Reconstruction User Requirement Document
has been issued and the detailed software design is
underway. Planning for the European Call for Proposals
is based on issuing the call in the May-June 2005
timeframe, preceded by a call for letters of intent, once
the launch date has been finalised.
3.6.6 Herschel Science Centre development
The science ground segment of the Herschel Space
Observatory (Section 3.1.2) is being implemented as a
distributed architecture with the science community
being supported by an ESA-provided Herschel Science
Centre located at ESAC (US astronomers supported by
the NASA Herschel Science Center at IPAC, Caltech)
and instrument operations being carried out from three
Instrument Control Centres, located on the PIs’ premises.
The key software ‘glue’ holding these centres together is
the Herschel Common Science System (HCSS), being
built jointly by the above parties, under the leadership of
the Division’s Herschel Science Centre Development
Team.
Within RSSD, the Astrophysics Missions Division has
overall responsibility for the scientific integrity of the
mission, while the Science Operations and Data Systems
Division is responsible for implementing the science
operations in close collaboration with the instrument
teams. From the end of the in-orbit commissioning
phase, the latter Division will take over overall project
management responsibility.
The HCSS is an ensemble of services supplied in the
form of a single, coherent and mostly platformindependent software system. Its users include the
Herschel Science Centre, the Instrument Control
Figure 3.6.6/1: A month-by-month history of HCSS
software problem reports (SPRs) and software
change requests (SCRs) and the change in the
number of open SPRs/SCRs (pink line).
Centres, and observers using Herschel. Seen end-to-end,
these services include support for (i) proposal submission, (ii) proposal evaluation, (iii) helpdesk support,
(iv) generation of observing schedules compliant with
the interfaces agreed with the Mission Operations
Centre, (v) reception and archiving of telemetry, (vi)
instrument data processing software, (vii) data products
in the Herschel archive.
One of the top-level requirements driving HCSS
development is that it supports the concept of smooth
transition, in which a nucleus of the system that is to be
used for in-flight operations already supports InstrumentLevel Tests in the laboratories of the PI teams several
years before launch. Owing to this requirement, HCSS
development started in early 2000.
During the 2003-2004 reporting period, seven releases
were made, emphasising the consolidation of the
development and the software having matured from the
early prototypes into production-level code. The status of
the development is:
— the system is in daily use for Instrument-Level Tests
of the Avionics/Cryogenic Qualification Models in
the PI laboratories;
— the system has been integrated into the Instrument
EGSE for use in satellite-level tests;
— significant progress has been made in the development of a Herschel Interactive Analysis framework,
with a group of scientific end-users giving direction
to and providing priorities for this resource-limited
development;
— development of the next system release, which will
support submission and handling of Herschel
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observing proposals and a first implementation of
the scientific mission planning system, is well under
way for delivery in 2005.
Examining the trends of the software problem reports
(SPRs) and software change requests (SCRs) handled by
the HCSS Configuration Control Board gives a vivid
insight into the development of the system (Fig. 3.6.6/1).
Initially, until the end of third-quarter 2003, there was a
steady but slow trickle of inputs. Then, a steady rise
started as both the number of users at the PI institutes and
also the intensity of their use increased. In addition to the
increase in average flow, the submission rate shows
rather pronounced peaks, well correlated with dates of
user releases of the system. This indicates that the system
tests performed by the developers and acceptance tests
performed by the users do indeed detect software
problems that are not encountered during normal use of
the system. Note also that the difference in open SPRs/
SCRs from one month to the next remains almost
constant despite the monthly influx, showing that the
HCSS developers just about manage to keep up.
3.6.7 Information technology support activities
The Division provides support in data systems to the
entire Department. The focus is on consolidating and
optimising the various services with the needs of the
community, the cost-effectiveness of the infrastructure
and the requirements of remote users kept firmly in
mind.
The Department’s highly valued technical mail service
allows ease of e-mail access to the peripatetic staff. The
mail service is closely integrated with the LDAP
(Lightweight Directory Access Protocol) services set-up
on which is built the RSSD intranet. By sharing common
resources, we have created a virtual community of all the
RSSD outstations. The RSSD web portal has been
developed to offer secure Single-Sign-On access to
shared services, including contact and personal
information, documents, web-page creation and
maintenance, mailing lists, directory services, mailing
labels, publication lists, etc.
in the case of Rosetta, a valuable Knowledge Base to take
forward through the long mission.
Tools have been created to harmonise the working
methods; these include the Publication Data Base, a tool
for registering and approving the publications of staff
members. This tool is integrated with the web services
such that an accepted paper is available to the public on
line. The same database may be used, in connection with
the developed Hermes community contact system, to
distribute electronically (or by paper if no e-mail address
is available) staffs’ preprints, with the resulting saving in
secretarial effort, printing and postal charges.
The various RSSD web sites have been consolidated into
a unified RSSD site at http://www.rssd.esa.int. Here, all
the information needed by end users of a science mission
may be posted with the necessary protection of
proprietary data and personal information. All project
scientists have access to a tool for developing their web
pages; it is optimally designed for us using PHP methods
and My_SQL database. Although the site is not
completely finished, it means we have significantly
reduced the maintenance overhead for the web sites,
freeing up Project Scientist time.
The departmental computing architecture is SUN-Solaris
based – a highly reliable architecture. During the reporting period, numerous obsolete items have been replaced
by a small number of modern powerful file servers, with
obvious economic benefits in performance and maintenance. Where appropriate, Linux machines have been
introduced, keeping in step with the academic community’s tendency towards Linux. Windows is both the
Agency’s and the general public’s preferred platform and
the Solaris team has developed a close working
relationship with the Windows support team. Interoperability is the keyword and facilities are shared among
the office, laboratory, science, operations and research
users, such as software licences, storage and printers.
3.6.8 Archive and Virtual Observatory activities
These elements make up a software tool-box that enables
the establishment of virtual communities, not just for
RSSD at large but also the external project teams spread
around the world. Such virtual communities have already
been set up for Planck, Gaia and Huygens, and it is
expected that, with management support, more projects
will soon adopt this technology.
The Science Archives Group at ESAC has been
consolidated to provide horizontal support for archive
activities to many science projects, ranging from
astronomical missions to planetary missions. Development and maintenance of the various archives is done in
an efficient and cost-effective manner by using common
architecture, code and manpower. This is demonstrated
by the achievements of the group during the reporting
period, including:
The Department’s documents are centrally managed
using the Document Management system (based on
Livelink). This permits staff to access their assets
(document libraries) while on the road, publish
documents directly to the web and create, as for example
— the ISO Data Archive allows ingestion and access to
highly processed data products provided by expert
user groups, and now provides a more detailed
quality report for each ISO observation;
— the XMM-Newton Science Archive now includes
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powerful and friendly access to the XMM-Newton
point source catalogue as well as on-the-fly
processing capabilities to offer users the most up-todate data products;
— a mirror of the Integral Science Data Archive,
together with an updated user interface based on
those built for ISO and XMM-Newton, has been
developed to support calibration and monitoring
activities within ESA, offering powerful query and
automatic data distribution systems;
— work has started on the Herschel Archive Browser
for instrument-level and system-level test data.
3.7
Experience gained in the astronomy archives has been
reused to develop the Planetary Science Archive (PSA).
This will be the single portal to all ESA planetary
missions data. Giotto data have already been ingested;
Mars Express, SMART-1 and Rosetta data will be
incorporated from early 2005. Huygens, Venus Express
and BepiColombo data sets will come in the future. The
PSA also offers a data set validation tool to help the PI
teams to provide data sets compatible with the PSA/PDS
data sets standards.
2003-2004 saw the successful completion of a number of
flight hardware activities. After the March 2004 launch
of Rosetta, MIDAS, RPC-MIP, OSIRIS and SESAME all
successfully underwent their first commissioning.
SPEDE on SMART-1 and ASPOC on the two Double
Stars are also performing as expected.
Activities on the Virtual Observatory (VO) have been
expanded in the second year of the reporting period. VOs
are defined as a collection of interoperating data archives
and software tools that use the Internet to form a
scientific research environment in which astronomical
research programmes can be conducted. The ISO Data
Archive and XMM-Newton Science Archive have
already been updated to support existing VO protocols,
such as Simple Image and Spectra Access, and are,
currently, two of the few VO-compliant astronomy
archives worldwide. Following this success, ESA is
providing more VO-dedicated manpower in 2005 and
2006 to fully integrate our archives into the VO world, to
develop tools to support the VO community, to increase
ESA and member-state data centre involvement in worldwide VO activities, and to position ESAC as the Space
Astronomy VO centre in Europe.
Science Payload and Advanced Concepts
Office
The Science Payload and Advanced Concepts Office
(SCI-A) provides support to the Agency’s science
missions and technology programmes as well as the
research programme of RSSD. The various sections
focus their support in these three important areas as well
as being responsible within the Directorate for the
assessment of future science missions.
3.7.1 Science Payload Instrument Section (SCI-AI)
Two additional flight projects are nearing completion.
The first is the COROT Digital Processing Unit. The
Engineering Model was delivered to the project and is
undergoing integrated tests. The assembly and electrical
tests of the flight and flight spare models (three in total)
were completed at Astrium GmbH and were in the SCI-A
laboratories by December 2004.
The second project is the Solar Electron Proton
Telescope (SEPT) for the STEREO mission as part of the
IMPACT suite of instruments within the Solar Electron
Proton package. SEPT consists of two dual, doubleended magnet/foil solid-state detector particle telescopes
that cleanly separate and measure electrons in the energy
range 20-400 keV and protons of 60-7000 keV, while
Figure 3.7.1/1: Top view of the STEREO Flight Model
analogue board.
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Fig. 3.7.1/2 the complete system integrated in its housing
with the various detectors. The four SEPT Flight Models
(plus one spare) are assembled and have undergone final
environmental tests. They were formally delivered to the
project in December 2004 after completion of the
calibration campaign.
Figure 3.7.1/2: The assembled STEREO Flight Model
Models.
Figure 3.7.1/3 shows the first spectra obtained with the
instrument using the electron conversion lines of a 207Bi
source. The PDFEs were operated in full anticoincidence mode. The green curve is related to CS1, the
centre segment of D1. The red curve shows the fluence
observed on CS2, the centre segment of D2. The blue
curve is related to XT1, the cross-talk ring of D1. At top
right is a basic sketch of the position of the source with
respect to the detectors. The K conversion lines are
nicely resolved. The different lines are also visible on
CS2, shifted by ~110 keV, the average energy deposited
by electrons crossing D1. These results indicate that, by
focusing on a detailed design, an optimised low-resource
instrument can be developed without loss of overall
performance. This approach will continue to be
developed in SCI-A through the study of Highly
Integrated Payload Suites (HIPSs).
3.7.2 Science Missions Section (SCI-AM)
The Science Missions Section of SCI-A is responsible for
providing support to science missions in orbit, under
development and under assessment, and for planning
longer-term future mission developments.
Figure 3.7.1/3: The first spectra obtained with one of
the telescopes and the dedicated electronics, using the
electron conversion lines of a Bismuth-207 source.
providing anisotropy information through the use of
several fields of view. Two SEPT units (NS: North-South
direction, E: Ecliptic) are located on each STEREO
spacecraft.
The electronics were designed and fabricated by SCI-A
for RSSD, while the housing and sensors were provided
by the University of Kiel (D). The major challenge of
SEPT involves the growing need for compact and highly
integrated instruments. SEPT is based on the Particle
Detector Front End ASIC developed under ESA’s GSTP.
With 640 g and 600 mW per unit, the instrument
demonstrates the technological development that is
possible and which will have to be matured further to
respond to future, ever-more demanding space missions.
Fig. 3.7.1/1 shows the assembled analogue board and
Support to the external scientific community is provided
directly and indirectly. Directly, for specific requests
related to instrument development, to payload reviews
and to programmatic aspects or by performing dedicated
studies on the payload complement baselined for future
missions. Indirectly, by assessing new missions, thus
defining the requirements of future instruments and the
related technology development needs, and by
supporting missions already under development. As an
example, over the last few years, SCI-AM staff have
followed the development of the SMART-1 payload units
closely, supporting PIs and the Project Scientist
throughout the different mission phases, including
commissioning after launch and performance
verification.
In the 2003-2004 period, SCI-AM staff provided
technical payload support to both RSSD (SCI-S) and the
Science Projects Department (SCI-P) for a number of
missions under development, such as Planck and
Herschel (participating in project reviews) and Integral
(Instrument Final Acceptance Review and In-Flight
Performance Review). In 2004 SCI-AM contributed to
the Systems Requirements Review of NIRSpec and
MIRI, two major instruments provided by ESA to the
James Webb Space Telescope. SCI-AM staff also
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module, as well as to assess the needs of a mission aimed
at investigating the ‘Pioneer effect’ (deviation from the
gravitational theory at large distances from the Sun).
Another TRS is the Solar Polar Orbiter, a mission
exploiting solar sailing and aiming to observe the Sun
from very high heliospheric inclinations
Figure 3.7.2/1: The Solar Orbiter orbiting the Sun at
0.2 AU during the science mission phase
contributed to the Gaia Mid-Term Review (September
2004), providing payload and detector expertise,
including integrated support to the Project Scientist in
areas such as radiation damage and detector modelling.
Considerable support on technical and programmatic
areas has been provided for the BepiColombo
reassessment and the following AO and payload
selection process. As part of its duties, SCI-AM
contributed to the cost and risk assessments of several
missions (such as BepiColombo, Darwin, Solar Orbiter
and the MIRI instrument), including payload, flight and
ground segments, with the final goal of estimating the
Cost-at-Completion of these future ESA science
missions.
A major task under the responsibility of SCI-AM during
2003-2004 was the Solar Orbiter assessment study
(Fig. 3.7.2/1). Activities included the preparation of all
mission reference documents, the conduct of a dedicated
industrial study on the payload complement, the
completion of two parallel competitive studies at system
level, the preliminary mission analysis and mission
control study, and a complete mission cost-risk
assessment. With such an in-depth study of all these
mission elements Solar Orbiter is well placed to move
into the development phase in 2006.
Technology Reference Studies (TRS) in astrophysics,
fundamental physics and solar physics are also being
developed by SCI-AM, based on the ideas put forward
by the scientific community following the ESA Call for
Ideas and the Cosmic Vision workshop that took place in
September 2004. SCI-AM staff are performing a
preliminary study on a future Gamma-Ray Lens project,
as a potential post-Integral mission and targeting photon
energies even above 500 keV. Similarly, in fundamental
physics, work is under way to assess requirements for a
standard fundamental physics payload and spacecraft
SCI-AM staff are responsible for the Darwin Groundbased Nulling Interferometer Experiment (GENIE)
definition phase, which involves conducting two
industrial parallel competitive studies to establish the
feasibility, performance, preliminary design and cost.
GENIE may be installed at the VLT of ESO (Chile) as a
precursor to the future Darwin payload. GENIE has a
two-fold objective: to exercise, on the ground, nulling
interferometry in prospect of the Darwin mission; to
provide the scientific community with a sophisticated
instrument capable of obtaining valuable scientific data.
The industrial studies ran during 2004 and the definition
study will be completed at the end of March 2005.
Finally, SCI-AM personnel supported a number of space
science instruments being studied or developed for the
ISS. Examples of instruments under study are EUSO and
Lobster. Support to the instrument team has been
provided in the case of SolACES, a UV radiometer under
development.
3.7.3 Planetary Exploration Studies Section
(SCI-AP)
The principal effort of the section has been the execution
of the 9-month reassessment of the BepiColombo
mission to Mercury, with the aim of maximising the
scientific performance and optimising the payload
complement, while reducing costs and programmatic
risk. The change of the mission profile from a split
launch for MMO and MPO into a single SoyuzFregat 2B launch brought a major reduction in cost.
Coupled with a detailed cost and risk assessment, this has
allowed the mission to move into the definition and
development phases. The section now provides support
to the Project Scientist and project team in such areas as
payload architecture, and participated, in particular, in
the evaluation of instrument proposals after the Request
for Proposals in support of the Payload Review
Committee.
The section provides support to a number of planetary
missions such as Venus Express, where the external
magnetometer team was supported during qualification
of the instrument and its boom. In the case of Rosetta’s
MIDAS, a major effort went into the final design,
integration, testing and verification of the flight
instrument and flight spare. Commissioning of MIDAS
after launch was successfully performed by SCI-AP
personnel in collaboration with the PI team. Parallel
activities, supported by SCI-AI, are establishing a
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scientific support activities
Figure 3.7.3/1: The Europa Mini-Satellite Orbiter
with its ice-penetrating radar deployed. The lifetime
is about 60 days after entering polar orbit, sufficient
for two complete high-resolution mappings of the
surface.
reference database to determine the magnetic properties
of selected meteorites and prepare for the data return.
Support has been provided on specific instruments for
Solar System research to the Instrumentation Section
SCI-AI. For example, the ASIC development for STERO
and the major contribution to the development of the
DSP-based DPU for COROT, based on the experience
with the DPU of Rosetta’s OSIRIS.
Finally, in preparation for future technology planning as
well as for establishing potential feasible mission
scenarios at an early phase, the section has been
prominent in running a TRS series related to Solar
System science. These have included the following toplevel mission profiles:
— exploration of the Jovian system and specifically the
mapping of Europa using a series of mini-satellites
(Fig. 3.7.3/1);
— in situ exploration of Venus via an aerobot coupled
with a series of microprobes;
— a mini-satellite sample and return mission to the
Martian moon Deimos;
— a solar polar microsat orbiter using a solar sail to
raise the ecliptic inclination to 90º;
— a microsat to explore the boundary of the
heliosphere, heliopause and beyond through the use
of a large solar sail to achieve initial high velocities
(Fig. 3.7.3/2).
Such mission studies allow the section to contribute
Figure 3.7.3/2: The Interstellar Heliopause Probe
(IHP) with its high-gain antenna, RTGs and boom
system (top), and the conceptual design showing the
instruments’ field of views (bottom). The sail would
be shed at about 5 AU since no further major gain in
acceleration could be achieved. The science phase
would then begin using the plasma instruments. The
probe would reach the assumed heliopause (~200 AU)
in about 25 years.
meaningful technical data to the future technology plans,
as well as providing quantitative data for the future
science programme through the Cosmic Vision process.
3.7.4 Advanced Technology Section (SCI-AT)
The Advanced Technologies Section provides support to
the community in two ways: by developing basic
enabling technologies for future missions and instruments, and by offering specific technology support to
on-going activities or studies. The key areas are in the
technologies required for science payloads and, in
particular, in advanced optics and detectors. It is
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93
systems should be possible without recourse to the very
low temperatures required for current sensors based on
superconductors.
Finally, the section’s technology expertise has been used
to support ESA missions past and future including:
Figure 3.7.4/1: The Wolter 1 micro-channel plate
optics developed as a prototype a variant of which
will form part of the imaging X-ray spectrometer
instrument on the BepiColombo mission.
particularly considered that precision lightweight optics
will be a crucial enabling technology, allowing lowercost missions with much higher sensitivities.
Specific areas of development include lightweight X-ray
optics such as those based on glass microchannel plates
(Fig. 3.7.4/1) and silicon micro-pore optics. These
technologies have been studied in detail for future
mission applications such as Lobster, a wide-field X-ray
telescope, the X-ray surface fluorescence spectrometer
on BepiColombo, and the XEUS large effective area
X-ray mirror. In the case of XEUS, the section is also
handling all mission-related aspects, including payload
accommodation, system engineering, mission analysis
and mission profile optimisation, because the optics
technology drives all other issues. At a later stage, the
mission will be transferred to SCI-AM for further
mission development at system level. In addition to these
specific soft X-ray optics technologies, optics
requirements for the hard X-ray and gamma-ray regions
are under active study or development, and preliminary
studies of the needs at far-IR wavelengths have begun.
Essentially, the experience gained in the development
and deployment of low-resource optics at X-ray
wavelengths for astrophysics and planetary missions will
migrate across to other wavelengths and disciplines.
The second area of key expertise is in advanced detector
technologies, which have been studied and developed
over a wide range of wavelengths. A programme for the
development of solid-state neutron detectors for
planetary science has also been introduced. Of particular
note is the study of low band-gap semiconductors for the
EUV and soft X-ray domains, where photon-counting
— XMM-Newton in-flight instrument calibration;
— radiation damage annealing studies on Integral;
— radiation damage analysis for Gaia and BepiColombo;
— BepiColombo spectrometers and particle monitor
design;
— supporting the development of specific payload
technologies for BepiColombo;
— CCD design and systems analysis for the Eddington
focal plane camera;
— establishing the Solar Orbiter Technology Development Plan;
— system design studies for XEUS instruments and
mirrors;
— developing the XEUS micro-pore mirror;
— supporting the Darwin Technology Development.
3.7.5 Darwin special project group
Darwin, the near-IR nulling interferometer, is a special
project under study in SCI-A. This mission requires
multiple spacecraft to fly in formation at L2. The mission
objectives are to detect and determine the nature of
extrasolar terrestrial planets out to a distance of about
25 pc. This is achieved through nulling interferometry at
6-20 µm. The Darwin special project group has
concentrated on studying in detail the optical architecture
of the mission with the aim of maximising the scientific
return while controlling the cost, complexity and risk.
This has been achieved through the use of four
spacecraft: three identical spacecraft carry ~3 mdiameter mirrors pointed at the target star, while a fourth
spacecraft combines the three transferred beams under
accurate phase control, including achromatic phase
shifts. In this way, the light from the central on-axis star
can be effectively reduced by six orders of magnitude
while the transmission map has off-axis regions close to
the star, where terrestrial planets would be detectable
depending on the planet’s orbital period and observation
time. Rotation of the constellation coupled with multiple
observations would allow planets to be detected and their
orbital periods to be established. Longer observations of
any planet, once detected, would allow its atmosphere to
be characterised through broadband spectroscopy.
The Darwin team has been able to reduce the mission
complexity, and thereby its cost, by introducing a novel
way of beam combination. This technique is based on
multi-axial beam injection into a single mode waveguide.
Recognising that the waveguide injection losses would
also occur when using traditional beam combination
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techniques, such as beam splitter plates, where a
waveguide would be used for wavefront filtering, and
that the technique allows odd numbers of beam to be
efficiently combined, the team determined that an
efficient nulling interferometer, involving the minimum
number of beams, could be realised. The concept has
been developed and now forms the mission baseline. An
initial laboratory verification of the concept has been
completed and will be complemented by more refined
breadboards. The team continues its studies in nulling
interferometry by pursuing explorative work in system
design and modelling.
It is envisaged to place the four spacecraft in orbit around
L2 using a pair of Soyuz-Fregat launchers. The cruise
duration to L2 is of the order 100 days. The Darwin team
is looking further into the details of the payload and its
accommodation, together with the development of the
mission at the system level.
scientific support activities
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4. OTHER ACTIVITIES
4.1 Symposia and Workshops organised by RSSD
The proceedings were published in Nucl. Phys. B (Proc.
Suppl.) 132 (2004).
4th Cluster Workshop ‘1st Cluster Tail Workshop’, Graz,
Austria, 26-28 March 2003
About 60 people attended this workshop to discuss the
structure and dymanics of the Earth’s magnetotail. A key
topic was thin current sheets that are unstable to
magnetic reconnection processes that energise charged
particles, causing fast plasma flows and magnetic flux
ropes. These events lead to precipitation of particles into
the Earth’s atmosphere, triggering auroral displays.
‘2nd Eddington Workshop: Stellar Structure and
Habitable Planet Finding’, Palermo, Italy, 9-11 April
2003
While the programme of this workshop focused on some
specific aspects of the preparation of the Eddington
mission (the choice of planet-finding field and the data
processing approach), broad science topics in the fields
of planet-finding and asteroseismology were also
extensively covered. The workshop was attended by 150
scientists from most ESA Member States as well as
Canada, USA, Australia, Hungary and the Czech
Republic. One of the workshop’s key issues was the
selection of the region of the sky where Eddington would
have searched for habitable planets. The workshop
generated a broad interest in the media, resulting in
coverage in national newspapers in Italy as well as
national TV and radio coverage in some of ESA’s
Member States.
‘The Restless High Energy Universe’, Amsterdam, The
Netherlands, 5-8 May 2003
About 140 people attended this conference dedicated to
results from the BeppoSAX mission. The Italian-Dutch
X-ray astronomy satellite was launched in April 1996
and operated for 6 years. It revolutionised the study of
gamma-ray bursts (GRBs) by discovering long-lived
X-ray afterglows which, at long last, allowed the
redshifts of GRBs to be determined and confirmed their
cosmological distances. During the conference, these
results and their legacy were reviewed together with
BeppoSAX results on clusters of galaxies and supernova
remnants, active galactic nuclei and the X-ray
background, stellar-mass black holes and neutron stars. It
is clear that results from the broadband (0.1-300 keV)
instrumentation on BeppoSAX played major roles in
many areas of high-energy astronomy. The workshop
also examined the legacy of the mission, showing how
discoveries from the mission have helped to define the
scientific priorities of later missions such as Swift and
Integral.
‘5th Cluster Workshop’, Orleans, France, 12-16 May
2003
This workshop dealt with spatio-temporal analysis and
multi-point measurements with Cluster. About 100
participants attended, and the main topics were the
dayside plasma boundaries of the magnetosphere and the
local characterisation of the space plasma. The magnetic
reconnection that also occurs on the dayside
magnetopause was widely discussed: here the
reconnection causes the transport of energy, momentum
and particles from the solar wind into the magnetosphere.
The measurement of electric current was also discussed:
the measurement is based on Ampere’s Law and requires
four satellites that are properly separated in order to
derive the current flowing across the satellite
constellation.
‘New Perspectives for Post-Herschel Far Infrared
Astronomy from Space’, Madrid, Spain, 1-4 September
2003
With Herschel and its instruments well into their
development and construction phase, it was timely to
discuss the long-term future of far-IR space astronomy
and to design a development plan for the post Herschel
era. ESA has already created a framework plan (Cosmic
Vision) for future missions based upon discussions and
considerations from the Horizon 2000+ planning
exercise. However, these activities took place some time
ago, when ISO was beginning operations and before the
implementation of Herschel got underway. More
recently, in 2002, US astronomers considered the options
for future far-IR/sub-mm space astronomy and have
constructed a roadmap for technology and mission
development.
At this meeting, about 75 members of the European
(far-)IR astronomical community (both scientists and
instrumentalists) met to discuss the long-term scientific
goals requiring observations in space in the 50-600 µm
range, to review the instrumentation capabilities to be
developed and to discuss a strategy for implementation.
‘IAA/ESA Workshop on the Next Steps in Exploring Deep
Space’, ESTEC, 22-23 September 2003
This workshop, organised by ESA and the IAA, was
attended by more than 125 participants. It built on an
ongoing IAA cosmic study ‘Next Steps in Exploring
Deep Space’ in order to give a vision for the exploration
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of space by humans in the first half of the 21st century.
The purpose was to provide a roadmap for a systematic,
logical and science-enabled plan for exploration of the
Solar System and observation of the Universe, a
programme to gradually but systematically establish a
permanent presence and infrastructure at each outpost
along the way. The workshop considered prorities
established by various communities and space agencies
across the world, and discussed the spaceflight
infrastructure required to pursue these goals, including
the relevant policy, international aspects and public
engagement.
‘6th Cluster Workshop’, ESTEC, 29 September –
3 October 2003
About 100 participants attended this workshop,
consisting of three parallel splinter sessions on various
topics, including collisionless shocks, magnetopause,
cusps, inner magnetosphere and identification of plasma
wave modes. Owing to the supersonic nature of the solar
wind, a shock layer is formed in front of the Earth’s
magnetosphere. The understanding of the shock
essentially requires multisatellite observations. At the
shock, strong electric currents flow; a typical current
here is of the order of 106 A (note that this can be
measured only with Cluster).
13th SOHO Workshop, ‘Waves, Oscillations and SmallScale Transient Events in the Solar Atmosphere: A Joint
View from SOHO and TRACE’, Palma de Mallorca,
Spain, 29 September – 3 October 2003
The 13th SOHO Workshop was held jointly with the
TRACE team on waves, oscillations and small-scale
transient events in the solar atmosphere. Detailed
observational studies with SOHO and TRACE have
provided a strong stimulus to theoretical developments,
so much so that coronal seismology (the determination of
coronal parameters by using information from the waves
the medium supports) is rapidly developing and
providing insight into some of the physical parameters
and processes at work in the corona. Nearly 100
participants discussed 110 papers in seven sessions
covering MHD Waves and Oscillations in Photospheric
Structures, Waves in the Chromosphere, Topological
Changes and Magnetic Coupling, Waves and Oscillations
in Prominences, Transition Region Dynamics:
Transients, Jets, Wave Acceleration in Open Magnetic
Regions and Coronal Seismology.
The proceedings were published by ESA SP-547.
symposia and workshops
‘ILEWG5, International Lunar Conference 2003’,
Hawaii, USA, 16-22 November 2003
The International Lunar Conference ILC2003 was
organised under the auspices of the International Lunar
Exploration Working Group (ILEWG). This meeting
attracted lunar explorers at large, including Apollo
astronauts John Young and Harrison Schmitt, space
professionals and enthusiasts from all over the world.
Among the topics discussed were the exploration and
utilisation of the Moon, and issues such as exploration,
science, advanced technologies, lunar resources, robotic
and human expansion, lunar bases, commercialisation,
Moon/Mars synergies, lunar tourism and who owns the
Moon were addressed ( http://www.spaceagepub.com/
program.html). This conference was an opportunity to
hear the latest news from SMART-1, the first European
mission to the Moon.
37th ESLAB Symposium, ‘Tools and Technologies for
Future Planetary Exploration’, ESTEC, 2-24 December
2003
With various European space missions either on their
way to, or already in orbit around, exciting planetary
objects, it was felt timely to reflect on experiences
gained, and at the same time to set new focal points for
future activities. The currently active or planned
planetary missions reflect drastically different environments, ranging from a cold and dark world on a comet
through quite benign conditions in orbit at Mars to hot
environments around Venus and Mercury. Future
expeditions may lead us to exotic worlds such as the
Jovian icy moons or in situ analysis of Martian soils.
There are high demands on innovative methods and on
the technology needed to decipher the manifold
scientific questions. The meeting was well supported by
the scientific community and, as a result, a very balanced
and interesting programme could be accomplished.
As a warm up in the first session, an overview was
presented of ESA studies on reference exploration
scenarios, which are used to identify the technological
needs of future planetary space missions. The challenges
of spacecraft and scientific payload developments were
addressed equally. Starting from this inspiring exercise,
the symposium went on with innovative ideas and
technological highlights in remote sensing instruments.
Considerable interest was shown for in situ
measurement techniques for planetary surfaces. New
payload instrumentation was introduced as well as
carrier systems enabling exploration strategies on a large
scale. The detection of water (a prerequisite for the
existence of life) and the recognition of traces of life
itself are of substantial interest and were reflected in a
full session. The presented concepts and technologies
demonstrated the advanced level of expertise within
Europe.
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symposia and workshops
The symposium was concluded with the Director of
Science’s outlook on the future of the scientific
programme. Overall, the 37th ESLAB Symposium was a
great success, combining the efforts of the European
science community and ESA towards the future
exploration of our Solar System and beyond.
‘Moon-Mars Workshop’, Bremen, Germany, 26 28 September 2003; Vancouver, Canada, 1-8 October 2004
The Moon-Mars Workshop (MMW) was a recommendation from the Space Generation Summit (SGS) held at
the World Space Congress in Houston in 2002. The Space
Exploration workgroups from SGS decided that it is very
important to look at current Moon and Mars exploration
plans and to highlight their commonalities in order to
show how developments for one benefit the other. A
single roadmap is needed for Moon-Mars exploration,
and this should accelerate our pace in exploration and
colonisation of our near Solar System. The First MoonMars Workshop was held in Bremen in conjunction and
collocated with the Third European Mars Society
Conference (EMC3), in connection with the IAF.
The Second Moon-Mars Workshop was held in
Vancouver during IAF 2004 (http://moonmarsworkshop.
com/ and http://moonmars.org/)
‘3rd VILSPA SAS Workshop’, VILSPA, Spain, 8-10
October 2003, and ‘4th VILSPA SAS Workshop’, VILSPA,
Spain, 8-11 June 2004
The VILSPA Science Analysis System (SAS) Workshops
provide XMM-Newton users who have little or no
experience of XMM-Newton data analysis with an
introduction to the procedures and techniques for
reducing and analysing XMM-Newton data. No specific
knowledge of X-ray data analysis is in principle required
to attend the workshop. The 3-4 day workshops are
organised as half-days of presentations, and half-days of
practical training (hands-on) sessions. In the practical
sessions, the participants, supported by XMM-Newton
SOC scientists, can accomplish reduction tasks on
XMM-Newton public databases, belonging to the SAS
Scientific Validation or extracted from the public
archive. Attendance is strictly limited to 20 people, to
ensure proper individual support.
2nd Planck Symposium, ‘Setting the Scene’, Orsay,
France, 28-30 January 2004
The objective of these meetings is to update the many
individuals involved in all facets of Planck’s development, and to stimulate discussion across Planck-related
topics. This Symposium carried the title ‘Setting the
Scene’ because it was timely to take a detailed look at
97
what will be the state-of-the-art of the field at the time of
Planck’s launch.
The bulk of the Symposium was devoted to scientific
talks on the probable scientific return of Planck in view
of currently ongoing and planned experiments. These
talks covered the spectrum of Planck science, not only
CMB-based cosmology, but also extragalactic science, as
well as the study of the Milky Way. Critical issues of
instrument technology and data processing were also
addressed. Finally, a large number of high-quality posters
gave insight into many detailed aspects of Planck.
The discussions held in the various sessions confirmed
that the scientific potential of Planck remains of the
highest calibre, even in view of the recent release of
WMAP data, and of new and very powerful ground- or
balloon-based experiments that are planned in the
coming decade. Although it was clear that, in just 3 days,
it was impossible to cover all the potential scientific
return of Planck, the Symposium fulfilled its objectives
and served as a valuable milestone on the road towards
the satellite’s launch.
‘5th Integral Workshop’, Munich, Germany, 16-20
February 2004
230 participants from all over the world attended the 5th
Integral workshop. Many key results from Integral
observations were presented, including one very exciting
result from Integral’s Galactic Plane Scan (GPS)
programme: the discovery of a new type of highly
obscured X-ray binary sources that had so far escaped
detection with other instruments. These new sources are
located within the Norma spiral arm of our galaxy.
Integral also observed the centre of the Galaxy, which
contains a super-massive black hole and yet only shows
relatively faint emission. The discovery of a source, IGR
J17456-2901, coincident with the Galactic nucleus
Sgr A* to within 0.9 arcmin was reported. It is the first
observation of significant hard X-ray emission from
within the inner 10 arcmin of the Galaxy and a
contribution from the galactic super-massive black hole
itself cannot be excluded. Detection of 91 gamma-ray
sources towards the direction of the Galactic centre was
reported, of which 26 are new discoveries (Nature 2004,
428, 293). The sources detected by Integral account for
the vast majority of the Milky Way’s (‘diffuse’) emission
at soft gamma-rays observed for 30 years, leaving only a
minor role for diffuse processes.
After 1 year in orbit, a comprehensive survey of Integral/
IBIS Core Program survey data was presented
incorporating both the GPS and GCDE. A total of 124
sources has been detected, of which 40% are low-mass
X-ray binaries and 31% are of undefined nature; 14
sources are completely new.
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The last session was devoted to Gamma-Ray Bursts
(GRBs); 10 have been seen in the field of view so far. It
was shown that the Integral Burst Alert System currently
gives the best GRB localisations, in terms of speed and
accuracy, for follow-up observation of their afterglows.
‘2nd Cluster Tail Workshop’, Mullard Space Science
Laboratory, Dorking, UK, 3-5 March 2004
Some 40 Cluster scientists gathered to discuss in
particular the dynamical processes of the Earth’s
magnetotail. A main topic was magnetic reconnection
that occurs everywhere in the Universe, but our geospace
is the only place where we can monitor and investigate it
in detail. Many other issues were also discussed, such as
the characteristics of thin current sheets that precede the
reconnection; characteristics and existence of ion beams;
plasma flow reversals, flux robes, plasmoids and
vorticity in the magnetotail; effects of interplanetary
shocks on the magnetotail, and so on. More information
about the workshop can be found at http://www.mssl.ucl.
ac.uk/www_plasma/missions/cluster/7thworkshop/
‘Titan from Discovery to Encounter’, ESTEC, 13-17
April 2004
This international conference was held on the 375th
birthday of Christiaan Huygens (born 14 April 1629).
During the 17th century, Huygens was one of the most
respected European scientists; a highlight of his career
was the discovery of Saturn’s largest moon, Titan. The
aim of the conference was to bring together historians
and space scientists to discuss not only Huygens the
person, the scientist and his relationship with other
scientists of his time, but also observations of Saturn and
its moons since the 17th century, as well as coming up to
date with the Cassini-Huygens mission and the latest
observations on the way to encounter. The conference
was attended by about 120 space scientists and
historians, and the last day was open to the public,
attracting more than 100 people.
The proceedings were published as ESA SP-1278.
‘13th Cool Star Workshop’, Hamburg, Germany, 5-9 July
2004
The ‘Cambridge Workshop on Cool Stars, Stellar
Systems and the Sun’ is the major event of the cool stars
community. Organised every 2 years, it now traditionally
alternates between the USA and Europe. The 13th
workshop was coorganised by the University of
Hamburg and RSSD. The workshop was a big success,
with 293 registered participants from all over the world,
making it one of the best attended since the start of the
series in 1980. Among the major topics discussed were
symposia and workshops
the new insights into coronal physics obtained from highresolution XMM and Chandra spectroscopy, new results
on stellar and planetary formation, and the impact of IR
survey and spectroscopy on our understanding of lowmass stars, brown dwarfs and planets. Cool Stars 13
experimented with the format of the meeting, with the
organisation of splinter sessions left to individual
participants. This was a success, as all splinters were well
attended. The generous sponsorship by ESA allowed the
participation of a number of students and young
researchers.
The proceedings will be published as ESA SP-560.
38th ESLAB Symposium, ‘5th International LISA
Symposium’, ESTEC, 12-16 July 2004
The 5th International LISA Symposium was held jointly
with the 38th ESLAB Symposium. The Symposium
traditionally focuses on the science and technology of
LISA and is held every second year. The Symposium was
attended by about 180 participants who discussed about
90 papers covering all aspects of LISA, starting from the
state of the mission in ESA and NASA, leading through
the technological aspects of LISA and its technology
demonstrator LISA Pathfinder, finally coming to the
astrophysics of the sources.
The proceedings will be published in a special issue of
Classical and Quantum Gravity.
14th SOHO Workshop, ‘Helio- and Asteroseismology:
Towards a Golden Future’, Yale University, New Haven,
CT, USA, 12-16 July 2004
The 14th SOHO Workshop was held jointly with the
annual meeting of the Global Oscillation Network
Group. It focused on the study of the interior of the Sun
from a seismic perspective and the prospects for similar
study of Sun-like stars. Nearly 120 participants discussed
over 125 papers addressing a wide variety of topics,
including the observational status of low-, medium- and
high-degree p-mode characterisation, low-frequency gmode detection, solar structure and dynamics, mode
excitation and damping, advances in local
helioseismology, and the first results from the Canada’s
MOST asteroseismology mission.
The proceedings were published as ESA SP-559.
‘The Moon: Science, Technology, Utilization and Human
Exploration’, COSPAR 2004, Paris, France, 22-23 July
2004
This event included solicited and contributed
presentations, organised in topical sub-sessions such as
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symposia and workshops
99
Science of the Moon, A Keystone for Planetary
Research; Formation and Early Evolution of the Moon,
Earth and Terrestrial Planets; The Moon as a Laboratory
for Comparative Planetology; Current Lunar Missions:
SMART-1, Lunar-A, Selene, Chandrayaan-1, South Pole
Aitken Sample Return, Lunar Reconnaissance Orbiter;
Astronomy from the Moon; Life Sciences on the Moon;
Future Exploration and Resources Utilisation; and
Astrobiology, Living and Working on the Moon and
Mars.
giant planets, UV/X-ray output of stars, and chemistry of
nebular material.
‘Dust Disks and the Formation, Evolution and Detection
of Habitable Planets’, San Diego, USA, 26-29 July 2004
(Towards Other Earths (Darwin/TPF), Heidelberg,
Germany, 22-25 April 2003)
15th SOHO Workshop, ‘Coronal Heating’, University of
St. Andrews, Scotland, UK, 6-9 September 2004
The second joint Terrestrial Planet Finder/Darwin
conference was held in Mission Bay, San Diego,
California in July 2004. Attracting about 250 participants
from all over the world, it followed the very successful
Heidelberg meeting in April 2003. The main purpose of
this conference series is to provide a forum in which to
develop the field of extrasolar planet research with
respect to the two missions Darwin and TPF. NASA and
ESA have recognised two primary, near-term goals in
arranging these joint conferences: (1) involve the
community in establishing high-level goals for TPF and
Darwin; and (2) address key areas of research relevant to
these ambitious missions that are important to the design
and architecture of TPF and Darwin, respectively.
There were three major topics for this conference. The
first addressed recent results on exo-zodiacal (EZ) discs
from Spitzer and other space and ground observations.
Also predictions of expected and exciting new results
from Spitzer, HST/ACS, Keck/LBTI Interferometers,
Herschel and ground-based sub-mm telescopes on the
evolution, structure, composition and frequency of debris
discs in the near and more distant future were discussed.
Among the issues debated were how to extrapolate from
the outer zodiacal clouds (Kuiper belt) detectable with
Spitzer to the inner zodiacal clouds that will be
measurable with TPF or Darwin. What do the Spitzer
measurements of the outer zodiacal cloud tell us about
the presence or absence of planets?
Secondly, the link between the physical conditions in the
early solar nebula and astrobiology, e.g. how might
astronomical conditions in the Hadean/Archaen periods
affect the formation and evolution of life? New data
from, for example, GENIE and the Keck-nuller may
provide new information on the properties of zodiacal
discs in the first 500 million years of a planetary system’s
existence. What does a high level of exo-zodiacal
emission imply in terms of bombardment and infall?
What other astronomical properties of a star and
planetary system might be relevant to the formation of
stable, habitable planets, for example, the dynamics of
Finally, an updated discussion of TPF and Darwin
designs and plans was also provided by ESA and NASA.
This included science requirements and technology
advances as well as more generic choices recently made,
such as mid-IR interferometry being the current driver in
Europe, while visual coronography is the first choice of
NASA.
More than 130 participants presented and discussed over
140 papers addressing a wide variety of topics, organised
around eight sessions covering: what is the coronal
heating problem?, driving coronal heating, wave heating
of the corona, kinetic aspects of coronal heating, the role
of reconnection in the corona, the solar-stellar
connection, plasma strands and the determination of the
local heating function, and where next in the search for a
solution to the coronal heating problem?
The proceedings were published as ESA SP-575.
‘8th Cluster Workshop’, New Hampshire, USA, 29
September – 1 October 2004
One hundred and thirty Cluster scientists gathered to
discuss the most recent scientific achievements of the
Cluster mission and to chart out the next phase of the
mission. During the 3-day workshop, the scientists
discussed several hot-button topics in four working
groups:
— bow shock processes, structure, and dynamics;
— physics of the inner magnetosphere;
— reconnection processes at the magnetopause and in
the tail;
— cusp dynamics and structure and auroral processes.
More information about the workshop can be found at
http://atlas.sr.unh.edu/cluster8/
‘The Three-Dimensional Universe’, Paris, France,
4-7 October 2004
This major symposium, dedicated to the scientific
aspects of the Gaia mission, was held at the Observatoire
de Paris, Meudon, as ‘Les Rencontres de l’Observatoire
2004’. Attended by 240 delegates, the 4-day meeting was
an opportunity to present the status of the Gaia mission
to the scientific community, and to hear the results of
investigations carried out in the various areas of the
mission over the previous 4 years.
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Activities and overall progress of the 14 scientific
working groups (from relativistic aspects of the data
analysis to the quasar reference frame) formed a major
part of the symposium. Various reports on the massive
data analysis preparations gave a detailed perspective on
the complexities and challenges facing the on-ground
data treatment: the overall simulation chain, the current
prototype data analysis system, Grid-related studies, and
the photometric data analysis.
Five participants accepted the delicate challenge of
summarising the poster presentations in the various
categories. This effort contributed significantly to the
coverage of a large variety of topics in a limited time, and
was greatly appreciated by the participants. A highlight
of the Symposium was the award by the Paris
Observatory of the degree of Doctor Honoris Causa to
the Honorary Chair of the Scientific Organising
Committee, Adriaan Blaauw, who celebrated his 90th
birthday earlier in the year.
Generous financial support by various organisations
connected to Gaia permitted the attendance at the
symposium of an unusually large representation of
younger scientists (PhDs and post-docs), many of whom
are already playing a key role in the preparation of the
ambitious Gaia mission. Attendees also included
collaborators from Greece (a new Member State of ESA)
and some non-member countries (Slovenia, Lithuania,
Estonia, Australia).
The proceedings were published as ESA SP-576.
‘The Dusty and Molecular Universe – A Prelude to
Herschel and ALMA’, Paris, France 27-29 October 2004
symposia and workshops
in the optical (Hubble and large 8-10 m ground optical
instruments such as ESO’s VLT), in X-rays (Chandra,
XMM-Newton) and other wavebands and facilities.
The meeting was organised such that the various groups
working on this scientific preparation could meet and
exchange their ideas, orientate their work towards the
best strategies, and plan complementary goals for early
science with Herschel and ALMA. About 200
participants delivered a large number of oral and poster
presentations.
The proceedings were published as ESA SP-577.
‘6th International Conference on Exploration and
Utilisation of the Moon’, Udaipur, India, 22-26
November 2004
The 6th International Lunar Conference was hosted by
PRL and ISRO, and cosponsored by ILEWG and ESA.
The President of India, Dr. Abdul Kalam, addressed the
meeting and made some highly relevant recommendations for international activities in exploration of the
Moon, ‘for the benefit of human kind’. Discussions and
presentations by 200 scientists from 17 countries focused
on new and planned missions to the Moon as well as
roadmap concepts for long-term exploration of the Moon
and the utilisation of lunar resources. The programme
included key elements of science overview and
opportunities for young scientists. The programme can
be found on http://www.prl.ernet.in/~ILC6/ and the
conference declaration on Sci.esa.int/ilewg
‘Herschel Space Observatory Calibration Workshop:
Models and Observations of Astronomical Calibration
Sources’, Leiden, The Netherlands, 1-3 December 2004
The future sub-mm and far-IR facilities of Herschel and
ALMA will make a breakthrough in our knowledge of
star formation, the bulk of it occurring in dusty and
obscured regions, that can be revealed only at these
wavelengths. They will shed light on the physical
processes of galaxy formation, the formation of the first
stars after the dark age, starbursts in interacting and
merging galaxies, and the fuelling of black holes. The
physics and chemistry of the interstellar medium will be
known in unprecedented detail. The production of dust
and various elements in stars, supernovae and stellar
winds will be tackled by the observation of the
circumstellar medium. Knowledge of cometary and
planetary atmospheres will be considerably enhanced,
and their molecular abundances revealed.
The main purpose of the workshop was to provide an
overview of the state-of-the-art of models, observations
and laboratory spectroscopic studies associated with
Herschel calibration sources, and to facilitate the
discussion between experts. The workshop brought
together calibration scientists from the three Herschel
instruments, members of the Herschel Science Centre
and the NASA Herschel Science Centre, planetary and
stellar modellers and observers, and calibration scientists
from ground and space observatories that cover similar
wavelength regions, in particular from ALMA, Astro-F,
ISO, JCMT, Planck, SOFIA, Spitzer Space Telescope
and SWAS.
The scientific preparation for the utilisation of these
facilities, expected to become operational just a few
years from now, is already underway using the legacy of
IRAS and ISO and through the presently operating
ground-based (sub)mm telescopes and the recent Spitzer
IR space telescope. Complementary surveys are obtained
Over 45 scientists from Europe, USA and Japan attended
the meeting. The workshop programme was organised in
both plenary and splinter sessions. The four splinter
sessions focused on the topics of Mars and giant planets,
Asteroids and satellites, Stars and secondary calibrators,
and Calibration and cross-calibration strategies.
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symposia and workshops
The talks in the plenary sessions covered subjects
common across the splinters. They included
presentations on the Herschel mission and of the
Herschel instruments’ calibration strategies. Other talks
provided overviews on the use of Solar System objects as
calibrators, of the current knowledge of solid-state
features in the far-IR and of the work in progress to study
and model the far-IR background. The workshop
achieved its objectives and definitely helped in
determining the future path for the calibration
preparatory work.
The viewgraphs of the presentations and a list of actions
identified during the meeting are collected on the
workshop web page (http://www.rssd.esa.int/Herschel/
hcal_wkshop.shtml). The models and observations of
astronomical calibration sources will be consolidated,
documented and made available to the calibration
scientists through a common database.
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4.2
ESA Technology Programmes
The ESA science directorate relies heavily on three
programmes to ensure technology developments are in
place to support future missions. These are:
— the Core Technology Programme, funded directly
from the Science Programme and covering the needs
of embryonic future missions and of more mature
missions either in assessment or under definition.
This programme focuses on high-priority core
technologies needed specifically within science and
covers the complete range of technology readiness
levels (TRLs 1-10).
— the Technology Research Programme (TRP), funded
by the ESA General Budget and accessed by all
customer directorates. In general, it covers
technology in the early stages of development
(essentially TRL levels 1-3).
— the General Support Technology Programme
(GSTP), funded directly by those Member States
RHESSI/SOHO/TRACE Workshop, ‘Coordinated Observations of Flares and CMEs’, Sonoma, California, USA,
8-11 December 2004
The RHESSI/SOHO/TRACE workshop was oriented
towards the synthesis of data from these three missions
and ground-based data. The workshop was attended by
over 140 participants. With the emphasis being on actual
research work, there were no set presentations other than
four introductory talks. To maximise the exchange of
ideas and foster new research arrangements, the
workshop was organised around seven parallel working
groups covering: pre-event physics; magnetic
reconnection & formation of current sheets; interrelationships of flares/CMEs in ‘super’ events; solar
origins of solar energetic particles; ribbons and footpoints; imaging spectroscopy of the thermal plasma;
particle acceleration and transport.
Figure 4.2/1: The various programmes and their
relationship with the Technology Readiness Levels
used within ESA.
Figure 4.2/2: The overall flow of the technology
planning and implementation process. TDA:
Technology Development Activity. TRM: Technology
Reference Mission.
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coordination/support activities
interested in a specific technology item. Generally, it
matures technology for direct application and
therefore covers TRL levels 4-10.
Figure 4.2/1 illustrates the overall approach to these
various programmes and the associated TRL level.
Of course, the individual items entering the various
programmes, whatever the funding approach, are crucial
to the overall success. Fig. 4.2/2 illustrates this complex
process, which attempts to ensure that the correct
technology needs of the Science Programme are
identified and eventually enter the programme at the
right time. SCI-A conduct studies into test-case missions,
known as Technology Reference Missions (TRMs), that
examine technical feasibility, costs and technology
needs. These TRMs assist the programme in providing
inputs to the science community with regard to possible
future projects as well as identifying core technologies,
often at a very low TRL, that may need to be developed
in the longer term.
4.3
Coordination and Other Supporting Activities
EIROforum
The EIROforum is a partnership between seven leading
European intergovernmental research organisations:
CERN, EFDA, EMBL, ESA, ESO, ESRF and ILL. As
world leaders within their respective fields of science,
the member organisations represent the vanguard of
European science, proving that European scientists can
be competitive at the forefront of research. These
organisations have a vital role to play in the future of
European research. A primary goal of EIROforum is to
play an active role in promoting the quality and impact of
European research through effective high-level interorganisational interaction and coordination. This is
possible by exploiting the existing intimate links
between the member organisations and their respective
European research communities.
The Head of RSSD is a member of the ESA EIROforum
delegation. During the reporting period, ESA has
occupied the chairmanship of the group for the last
6 months, with the Director of Science representing the
Director General of ESA. In this period, a decisive push
has been given to the previously existing working groups
on instrumentations, grid technologies, human resources
and, in particular, the preparation of a knowledge database on the management of large infrastructures. From
the policy point of view, an EIROforum vision paper was
prepared during the last year that is now being presented
to the organisations of the European Union and, in
particular, to the Science and Research Commission.
AVO/EURO-VO
Work continues on the development of Virtual
Observatory (VO) tools in cooperation with other
European organisations. After the success of the
Astrovirtel programme, members of the Department in
ST-ECF and ESAC are preparing the next steps in this
much-needed resource for modern astrophysical research
using a variety of observational databases, both groundand space-based.
The last demonstration of the Astrophysical VO (AVO)
project, before the beginning of the implementation of its
fully-fledged form, was performed at ESAC. The use of
archival data (including ISO and XMM) for this type of
research was found to be particularly useful. Cooperation
with ESO, through ST-ECF, as well as other astronomical
centres in Europe, is envisaged in the preparation of a
proposal to the European Commission for funding of
some of the components of AVO. More information is
given in the Divisional sections of this report.
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coordination/support activities
Opticon
The ST-ECF, on behalf of RSSD, participated in the
Opticon network. This is an ‘Integrated Infrastructure
Initiative (I3)’ European Commission-funded programme that comprises networking, a trans-national
access programme and a series of six technology projects
called Joint Research Activities. RSSD contributes to
these activities through the ST-ECF group in Garching
(D); the involvement of other members of the
Department is being encouraged in specific JRAs linked
more closely to space projects.
103
Fellows, funded to work 1 or 2 years in ESA Member
States’ institutions outside their home countries. These
Fellows contribute to research networking in support of
ESA missions. Research Fellows working with the ESA
SOHO team at NASA/GSFC or at the STScI are also
recruited via this scheme.
General Scientific Support
RSSD staff provided scientific advice and support to and
participated in committee and working groups not
directly within the purview of the Scientific Directorate
or of ESA. These included:
Europlanet
This is a new European Commission-funded network of
coordinated activities in planetary sciences. It was set up
to achieve a long-term integration of this discipline in
Europe. Its aims are to increase the science return of
planetary projects, with emphasis on major exploration
missions, to initiate a long-term improvement of the
European planetary work infrastructure, to improve
European scientific competitiveness, to develop and
spread expertise in this area of research, and to develop
public understanding of and support for planetary science
and exploration.
These goals will be achieved by maximising synergies
between different fields contributing to planetary
sciences: space observations, Earth-based observatories,
laboratory studies, numerical simulations and the
development of databases. In addition, the design and
development of an Integrated and Distributed
Information Service providing access to the full set of
data sources produced by the mentioned complementary
fields is a driver of the project.
Astronet
Very recently, members of RSSD have been involved in
the preparation of a proposal to the European
Commission for funding of a network of European
research agencies in astronomy. Though only associated
members rather than full partners, owing to the nature of
ESA as a European organisation, an ambitious work plan
has been designed aimed at structuring and coordinating
European astronomical research. This plan is based on a
number of work packages, including networking, a
strategic review of European astronomy, an
infrastructure roadmap and coordinated actions to
strengthen astronomy and astrophysics in Europe
External Research Fellows
In addition to the internal Research Fellowship
Programme, there are about 20 External Research
— A. Gimenez is a member of the Council of the
European Astronomical Society and President of the
IAU Commision on Binary Stars.
— G. Schwehm continued to provide support to the
Agency’s Space Debris Working Group and as as
coordinator for all planetary protection activities
within the Agency.
— in coordination with ESA’s International Affairs
Department, RSSD staff have continued to provide
support to the organisation and programme
development of the UN/ESA Workshops on Basic
Space Science. This series of workshops has found a
special niche in identifying opportunities to promote
space science in the developing nations, both in
order to provide opportunities for professional
scientists, and as a means of enhancing the role of
science in the educational systems of these nations.
The results of the first ten of these Workshops were
summarised in the book Developing Basic Space
Science World-Wide (W. Wamsteker, R. Albrecht,
H. Haubold, Eds. Kluwer, Dortrecht, 2004). The
11th UN/ESA Workshop, originally scheduled for
November 2003 in Beijing, China, was rescheduled
owing to the SARS epidemic, and held in May 2004,
hosted by the government of P.R. China and the
Chinese Space Agency. The emphasis was on
promoting international and regional collaboration,
and access to data from high-end facilities via the
Virtual Observatory. The concept of a World Space
Observatory, as an effective means of stimulating
space science in developing countries, and
generating better opportunities for participation of
scientists from developing countries in space science
and education, was further pursued. Responsibility
for liaison with the United Nations was transferred to
R. Albrecht (ST-ECF) after the retirement of
W. Wamsteker.
— B.H. Foing is the ESA representative and Executive
Director of the International Lunar Exploration
Working Group (ILEWG), a body charged with
developing and coordinating an international
strategy for the exploration of the Moon. He also
participated in a Cosmic Study of the International
Academy of Astronautics on ‘Next Steps in
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Exploring Deep Space’, led by Dr. W. Huntress
(Carnegie), released in July 2004. The IAA study
outlines compelling scientific and cultural
imperatives that provide the context for a vigorous
programme of robotic science missions and for a
systematic and evolutionary architecture for human
expansion into the Solar System.
— RSSD staff were active in numerous scientific
societies (EAS, EGS, EPS) and some of the
Scientific Unions (COSPAR, IAU, IRSI, IUPAP),
where they contributed to scientific meetings by
organising special sessions and discussions, and, in
some cases, holding elective offices. For example,
H. Svedhem is a member of EGU Council and
President of the Geophysical Instrumentation
Section of the EGU.
— RSSD staff also taught space sciences and related
topics in Member State universities and in several
instances were also appointed as jury members for
Ph.D. theses. The direct contact between ESA staff
and students and staff at the Universities continues to
be mutually rewarding.
science communications
4.4 Science Communications
Supporting the ESA Corporate and Science Communication Services
RSSD Project Scientists and staff supported a number of
science communication activities related to their
projects. These include text and pictures for leaflets,
posters and brochures, and contributions to 80 web
stories in 2003 and 67 stories in 2004 for the ESA public
website (www.esa.int) and ESA space science pages
(www.esa.int/esaSC). Of the more than 90 and 140 ESA
press releases in 2003 and 2004, respectively, 79 and 67
were related to science. In addition, more than 82 press
releases were issued by STScI over the 2 years.
A large effort was made by RSSD staff to support the
development, input updating and maintenance of the
ESA scitech website (sci.esa.int), aimed at the scientific
and educated communities, with specific information on
all missions: status reports, announcements, upcoming
events, latest publications, mission background, science,
spacecraft and science operations, services, image
gallery and videos. The Chief Scientist proposed an
overall structure for the thematic contents of the scitech
site.
RSSD staff (in particular, Project Scientists) supported
ESA Corporate PR services in the production of TV
broadcast material related to ESA science missions, in a
variety of formats: documentaries for the general public;
documentaries for the technical public; Index, A- and Brolls; video Index, chapter structured; Interviews; Video
News Releases; and live action. This material was
distributed by ESA PR at related events or broadcast on
ESA TV to European channels.
Contents of ESA Science Communication Stories for the
Public in 2003-2004
ESA’s PR emphasis is often directed towards launch
campaigns. RSSD Project Scientists supported ESA PR
offices, in coordination with project teams, by preparing
material, text and pictures for stories about these science
missions from complementary viewpoints at selected
milestones: the science background and goals, preparation and key events for the spacecraft, specific instruments and technologies, initial results and more complete
results.
Mars Express was the subject of 51 web stories in 20032004, including the preparation for launch in June 2003,
the arrival at Mars on 25 December, the search for
Beagle-2 and the related enquiry, and the results from the
orbiter. These included the spectacular stereo imagery of
Mars’ geology, volcanoes, water features, impact craters,
the detection of polar water ice by the instruments, the
detection of methane by the Planetary Fourier Spectro-
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science communications
meter, water loss in the atmosphere, evidence for recent
volcanism and glacial activity. RSSD staff supported a
number of press events, covering both mission aspects
and research.
The communications activities on SMART-1 included
promotion of lunar and planetary science, new
technologies, people and new methods for small space
missions, and exploration. The Project Scientist
supported film crews working on interviews and
documentaries on SMART-1 and lunar exploration. He
supported media briefing events in March 2003, as well
as the pre-launch campaign in September 2003. The first
results from the commissioning, cruise, navigation and
lunar capture on 15 November 2004 were featured. The
SMART-1 team collaborated with ILEWG (sci.esa.int/
ilewg) and the Lunar Explorers Society, (lunarexplorer.
org) in public events. PR events were organised at the
ILEWG conferences in Hawaii (2003) and Udaipur,
India (2004) in the presence of Apollo astronauts and the
President of India, respectively.
The Cassini/Huygens arrival at Saturn prompted 10
stories on the critical Saturn orbit insertion, four from
Cassini flybys (Phoebe, Titan, new moons) and the
preparation for the release of Huygens over Christmas
2004, building up the interest for the 14 January 2005
atmospheric entry and landing.
Rosetta also enjoyed high PR activities during 20032004, with 19 web stories emphasising the launch
campaign, the delay to 2004 and the environmental
testing, as well as the science involved, such as the
origins of the Solar System and the delivery from comets
of the ingredients for life.
RSSD staff also contributed to educational and outreach
activities related to astronomical events such as lunar
eclipses, the Mercury transit in May 2003 and the Venus
transit on 8 June 2004.
Observations and discoveries made with SOHO have
continued to make the headlines, with a number of CNN
news stories. Special stories include the giant Halloween
superflare of October-November 2003, and the detection
(mostly by amateurs) of more than 750 comets with
SOHO. The solution of the high-gain antenna problem
was also newsworthy. Articles about SOHO have
appeared in several popular magazines. Several film and
TV crews visited the operations facility, and SOHO was
featured in a number of science TV programmes. SOHO
observations and images play a prominent role in the 40min giant-screen IMAX documentary ‘SOLARMAX’
(www.solarmovie.com).
Astronomy missions had a modest level of PR and ESA
science communication activities, with seven ESA press
releases and 10 web stories in 2003-2004. Themes
included X-ray astronomy, with stories on stellar coronae
105
and cycles, clusters of galaxies, dark energy, accretion
onto rotating black holes and dead-star magnetism. With
Integral, the stories included the hot trail of Geminga,
gamma-ray bursts, hidden black holes, and the new view
of the Milky Way. The ESA website also mirrored or
expanded some of the HST stories and imagery from
STScI. In addition, some HST stories from STScI
exploited the use of spectacular images, such as the light
echo around an erupting star.
Some general astronomical stories were produced on
virtual observatories, the space grid, the search for
exoplanets, star formation, origin of the Universe,
mapping the Milky Way and preparing the background
for the upcoming Herschel, Planck, Gaia and JWST
observatories.
RSSD scientists supported a large number of other
communication activities during 2003-2004, including:
— Le Bourget, Farnborough and other space fairs.
Animations included presentations on space science
and technology for the press and the public, 3-D
visualisations and demonstration models from some
ESA space missions.
— RSSD Project Scientist staff organised or supported
science communication events aimed at the science
community at large during sessions at the EGU in
Nice, IAF in Bremen and Vancouver, COSPAR in
Paris, IAU, the JENAM joint European astronomy
meeting, and national astronomy meetings. They
assisted in the organisation of a number of exhibition
events (co-sponsored by ESA) featuring ESA space
science missions.
— RSSD staff contributed ESA space science
communication activities (highlights from ESA
science missions, lunar and planetary exploration,
astronomy, space science, etc.) at press conferences,
and scientific and public assemblies (COSPAR,
EGS/EGU, IAF, IAU).
— RSSD staff supported collaborative science
communication events with museums, planetariums
and educational institutions all over Europe. A
network of space science communication partners
was further developed, such as the British Festival of
Science, Space Week and the Association of Science
Journalists.
Supporting Education, Teachers and Student Outreach
Initiatives
RSSD participated in outreach activities such as the
‘Physics on Stage’ events for teachers at ESTEC in
November 2003, and Life in the Universe, Moon, Mars,
planetary and astronomy workshops. They provided
lectures and tutoring as part of the ESA student initiative
that allowed the participation of 300 students at IAF
Bremen in October 2003 and IAF Vancouver in October
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2004. They also served as lecturers and as reviewers in
student projects coordinated by the ESA Outreach and
Education Office. They advised the Education Office on
the science background of hands-on projects for students.
Public outreach activities were conducted during
astronomical events such as the Mercury and Venus
transits. They contributed lectures during conferences,
public events, festivals of science, and university and
institute general lectures and open days.
ESA Science and Technology Website (Missions and
News): http://sci.esa.int
ESA corporate portal: www.esa.int, with public science
website: www.esa.int/esaSC
ILEWG site: http://sci.esa.int/ilewg/
HST news site: http://hubblesite.org
science communications
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ANNEX 1
Manpower Deployment
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manpower deployment
ANNEX 1: MANPOWER DEPLOYMENT
Department Office, ESTEC
Head of Department
Gimenez, A.
Chief Scientist
Foing, B.H., SMART-1 Project Scientist, comparative
planetary and astrobiology, solar-stellar physics.
Administrative staff
Bingham, C., Departmental Assistant Administrator
Ihaddadene, S., Divisional Secretary and Admin.
Assistant
Schroeder, B., Divisional Secretary and Admin.
Assistant
Villien, C., Divisional Secretary and Admin. Assistant
Project Controllers (seconded from SCI-M)
D’Aquino, G.
Davis, R.
Fontaine, R.
Astrophysics Missions Division
Clavel, J., Head of Division, Multiwavelength
observational astronomy.
Boeker, T., (from September 2003), JWST Scientist,
Galaxy formation and evolution
De Bruin, J., Gaia Support Scientist
Favata, F., Eddington Study Scientist, COROT Project
Scientist, support to Gaia studies, cool stars and
stellar activity, X-ray astronomy
Fridlund, M., IRSI/Darwin Study Scientist, astrophysics
of star formation
Heras, A., Herschel scientist, IR astronomy
Jakobsen, P., JWST Study Scientist, optical/UV
astronomy with HST and ground-based astronomy
Laureijs, R., Planck Deputy Project Scientist,
interstellar medium, dust properties
Leeks, S., (from April 2003), Herschel Instrument and
Calibration Scientist
Marston, A., (from April 2003), Herschel Instrument
and Calibration Scientist
Parmar, A., Acting Integral Project Scientist, XEUS,
Lobster, Rosita & EUSO Study Scientist, Leader for
the SAX LEGSPC, X-ray astronomy (X-ray binaries
and AGNs)
Perryman, M.A.C., Hipparcos Project Scientist, Gaia
Project Scientist, exploitation of Hipparcos data
Pilbratt, G.L., Herschel Project Scientist, IR and
sub-mm astronomy
Prusti, T., Herschel Scientist, IR astronomy
Tauber, J., Planck Project Scientist, sub-mm astronomy
Vavrek, R., (from April 2004), Herschel Instrument and
Calibration Scientist
ESA Research Fellows
Boirin, L., (to September 2003), X-ray astronomy
Del Burgo, C., (to September 2004), Modelling of sky
as seen by Planck
Diaz Trigo, M., (from May 2004), Data analysis
concentrating on study of stellar coronae and
absorption lines in compact sources
Dupac, X., (to October 2004), Planck-related science on
cosmic background and interstellar dust
Hony, S., (to January 2005), Interstellar medium, circumstellar envelopes, dust
Husain, G., (from October 2003), Stellar activity,
coronae
McBreen, S., (from October 2004), Analysis of Integral
and XMM data on compact accreting sources
Papadopolous, P., (to March 2003), Interstellar medium
Sanz Forcada, J., (from February 2004), Asteroseismology
Stankov, A., (to January 2004), analysis of stellar
seismology
Spanish/Portuguese Trainees
Perez-Ramirez, D., (to January 2004), Reduction of
XMM-Newton data
Silva, B., (to October 2004), Computer model to
simulate number and distribution of planets that
Eddington could find
Solar and Solar-Terrestrial Missions Division
Opgenoorth, H., (from April 2003), Head of Solar and
Solar-Terrestrial Missions Division
Brekke, P., (to November 2004), Support to SOHO
Project Scientist, solar physics, science
communication
Escoubet, C.P., Cluster and Double Star Project
Scientist, magnetospheric physics
Fehringer, M., (to March 2003), Support to Cluster and
Double Star Project Scientist, Microscope Study
Scientist (under the Fundamental Physics Missions
Division)
Fleck, B., SOHO Project Scientist, Solar Orbiter Study
Scientist, solar physics
Haugan, S., SOHO Science Operations Coordinator,
solar physics
Marsden, R.G., Ulysses Project Scientist and Project
Manager, Solar Orbiter Study Scientist, ILWS
support, energetic particle data interpretation
Sanchez, L., SOHO Science Data Ordinator, SOHO
archive
Sanderson, T.R., Cluster Archive Scientist, energetic
particle instrument development and data
interpretation
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manpower deployment
ESA Research Fellows
Khan, H., (from August 2004), Magnetospheric physics
research based on analysis of Cluster data
Pitout, F., (to December 2004), Magnetospheric
research based on analysis of Cluster data
Regnier, S., (from February 2004), Study of structure
and dynamics of solar surface fields (EU Fellow)
ESA External Fellow
McIntosh, S., (to February 2003), Criticality of solar
flares and chromospheric dynamics
Planetary Missions Division
Schwehm, G., Head of Division, Rosetta Project
Scientist
Chicarro, A., Mars Express Project Scientist, planetary
geology
Grard, R.J.L., (to November 2003), BepiColombo
Project Scientist, modelling and instrument
development
Koschny, D., Support to Rosetta Project Scientist,
science operations planning, meteor research,
planetary cameras
Laakso, H., (from April 2003), Support to Cluster,
magnetospheric plasma research
Lebreton, J.-P., Huygens Mission Manager, Solar
System technology support, plasma physics
instrument development
Martin, P., Mars Express Operations Scientist
Ocampo, A., (to February 2004), Support to Mars
Express and BepiColombo
Schulz, R.M., Bepi Colombo Project Scientist (from
2003), cometary studies
Svedhem, L.H., Venus Express Project Scientist,
development of planetary instrumentation, cosmic
dust studies
Witasse, O., Huygens, planetary atmospheres
Wirth, K., (from August 2003), Planetary
Scientist/Applied Physicist
Research Fellows
Boudin, N., (to February 2004), Astrochemistry
Campbell, M., (to December 2003), Observations and
monitoring of meteors
Cord, A., (from October 2004), Analysis of imaging
Mars Express data
Davidsson, B., (from May 2003), Comet nuclei
thermophysical modelling and observations
Makinen, J., (to December 2003), Cometary science
(data analysis and modelling)
Michael, G., (to April 2004), Comparative planetology.
Piot, A., (to February 2004), exploitation of Huygens
test balloon data
Zegers, T., (from May 2003), Geology and hydrology of
Mars with Mars Express
109
Young Gradutate Trainees
Conan, Y., (to April 2004)
Merikallio, S., (from August 2004), Spacecraft
charging
Sarkarati, N., (from May 2004), Experiment modelling
Spanish/Portuguese Trainees
Almeida, M., (from April 2003), SMART-1 AMIE
calibration, science operations support
Perez Ayucar, M., (to June 2004), Telecommunication
Engineer – Huygens
Simoes, F., (to September 2004), Water on Mars
Vazquez Garcia, J.L., (to May 2004),
Telecommunications Engineer – SMART-1
Stagiaires
Andurand, P., (March-September 2003)
Civeit, T., (April-September 2003)
Couturier-Doux, S., (April-October 2004)
Maloreau, S., (March-August 2003)
Nicoll, R., (February-April 2003)
Piberne, R., (April-October 2004)
Roussos, E., (April-July 2004)
Sarmiento Ares, E., (March-August 2004)
Seoane Purrinos, L., (March-August 2004)
Van Kan, M., (March-August 2004)
Vicente, D., (March-August 2003)
Zeyen, B., (April-July 2003)
Fundamental Physics Missions Division
Reinhard, R., Head of Fundamental Physics Division,
LISA Pathfinder Project Scientist
Caccapuoti, L., (from December 2004), ACES Project
Scientist (for D/HME)
Fehringer, M., MICROSCOPE Study Scientist (to
March 2003)
Jafry, Y., (to August 2004), drag-free control expert for
fundamental physics missions
Jennrich, O., LISA Project Scientist
Space Telescope Operations Division
Macchetto, D., Head of Division, AGN, Elliptical
galaxies, gamma-ray bursts
ST-ECF, Garching
ESA scientific staff
Benvenuti, P., (to October 2004), HST Project Scientist,
Head of ECF, extragalactic HII regions, SNRs
Albrecht, R., Deputy Head ECF, Head of Science Data
and Software Group, minor bodies of the Solar
System, computer science
Dolensky, M., (to January 2003), Science archive and
WWW software specialist
Fosbury, R.A.E., Head of HST User Support Group,
galaxies and AGNs
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Micol, A., Science Archive Software Specialist, image
processing techniques and information systems
Rosa, M.R., Head Post-operational Archive Group, HII
regions, star formation, supernovae, evolution of
galaxies
Sforna, D., Science Programmer, Systems Analysis
ESO staff (included here to give the full picture of
ST-ECF team staffing)
Freudling, W., Instrument Scientist, observational
cosmology, peculiar motion of galaxies
Haase, J., Astronomical Data Archive and Pipeline
Software Specialist
Hook, R.N., HST Data Analysis Scientist, scientific
software support, image restoration applications
Kuntschner, H., Instrument Scientist, galaxy formation
and evolution
Pierfederici, F., ASTROVIRTEL Support Scientist
Pirenne, B., HST Archive Scientist, data storage
technology, gravitational lenses
Pirzkal, N., Scientific Analyst/Programmer, pre-mainsequence stars
Sjöberg, B., ST-ECF Admin. Assistant / Secretary
Walsh, J.R., Instrument Scientist, planetary nebulae, HII
regions
manpower deployment
gravitational lensing and cosmology, stellar
dynamics, photometry
Miebach, M., Lead Engineer for Scientific
Instruments
Mobasher, B., STIS Instrument Scientist, Galaxy
surveys, dwarf galaxies, elliptical galaxies
Padovani, P., (to August 2003), Multi-Mission Archive
Scientist, AGN: unified schemes, evolution, X-ray
spectra, blazars
Panagia, N., NGST Science Lead, stars, interstellar
medium, supernovae, galaxies, cosmology
Robberto, M., WFC3 Instrument Scientist, star
formation, massive stars, IR instrumentation
Sirianni, M., ACS Instrument Scientist
Stanghellini, L., (to April 2004), Proposal Scientist,
planetary nebulae and their central stars,
extragalactic distance scale
Villaver, E., (from February 2004), Astronomer
Wiklund, T., NICMOS Instrument Scientist, AGN,
Starburst Galaxies
ESA External Research Fellows
van Bemmel, I., (from March 2003)
Science Operations and Data Systems Division
ESO staff under ESA contract
Alexov, A., Post-Operation Instrument Scientific
Programmer
Bristow, P., Post-Operation Instrument Scientific
Programmer
Christensen, L., HST Outreach Astronomer
Fourniol, N., Archive Operator
Kerber, F., Post-Operation Instrument Scientist, earlytype stars
Kornmesser, M., HST Outreach Technical Editor
Pasquali, A., Instrument Scientist, stellar winds,
nebulae
STScI, Baltimore
Aloisi, A., STIS Instrument Scientist
Arribas, S., NICMOS Instrument Scientist, AGN, highredshift galaxies, cosmology
Boeker, T., (to August 2003), NICMOS Instrument
Scientist, galaxy formation and evolution, in
particular gas dynamics in the central regions
Clampin-Nota, A., Deputy Head, Science Division,
massive stars, late stages of stellar evolution, IMF
studies
De Marchi, G., (to 2003), ACS Instrument Scientist,
initial mass function, globular clusters, dark matter
haloes
Jenkner, H., HST Mission Deputy, Guide Star Catalog
II, microvariability studies using FGS photometry
Kamp, I., (from May 2004), Astronomer
Mais-Appellaniz, J., Spectrographs Instrument Scientist,
HII regions, young clusters
Meylan, G., (to August 2004), Proposal Scientist,
Staff
Kessler, M.F., Head of Division, Infrared
Astronomy
Bennett, K., Gamma-ray astronomy, Planck (Co-I)
Jansen, F., XMM-Newton/Mars Express Mission
Manager, X-ray astronomy
Szumlas, M., Technical coordination, Data Bank
maintenance
Thoerner, G., Divisional system analyst/computer
manager, SAX data analysis and cosmology studies
Toni, A., Senior data technician
Winkler, C., Integral Project Scientist, gamma-ray
astronomy data analysis
Wamsteker, W., (to November 2004), Multidisciplinary scientist, active galaxies, abundances at
high redshifts (located at Vilspa)
Zender, J.J., Data handling/archiving management for
planetary science operations
Research Fellows
Sanz Forcada, J. (from February 2004), Data analysis
on physics of stellar coronae and absorption
Herschel Science Centre, ESTEC
Staff
Riedinger, J., Herschel Science Centre Development
Manager
Mathieu, J-J., Interactive Analsysis (p.t., TOS support)
Ott, S., System Analyst, Interactive Analysis
Coordinator
Prades-Valls, R., Quality Assurance (p.t., TOS
support)
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manpower deployment
Integral Science Operations Centre (ISOC)
Staff
Hansson, L., Integral Science Operations Manager
Barr, P., Operations scientist, mission planning
Much, R., (to August 2004), Operations scientist and
Deputy Project Scientist, Observational astronomy
O’Rourke, L., (from September 2004), Science
Operations Engineer (ESAC)
Orr, A., Operations scientist, JEM-X and OMC expert,
responsible for helpdesk
Sternberg, J., System engineering, ISDC liaison
Integral Science Data Centre (Geneva)
Staff
Texier, D., (to August 2004), Resident Engineer
ISO Data Centre (IDC), (ESAC)
Staff
Garcia-Lario, P., ISO Resident Astronomer, crosscalibration expert, Handbook co-editor, late stages of
stellar evolution
Gry, C., (to October 2004), ISO Resident Astronomer,
LWS expert, LWS Handbook, interstellar medium
Lorente, R., ISO Resident Astronomer, ISOCAM expert
Peschke, S., (to April 2003), ISO Resident Astronomer,
ISOPHOT expert, comets
Salama, A., ISO Project Scientist SWS expert, Titan,
novae and symbiotic stars
Verdugo, E., Resident Astronomer, ISOPHOT expert,
ISO Data Archive products quality
Research Fellows
Garcia-Hernandez, A., (from September 2004), analysis
of stellar ISO archival data
Sanchez Fernandez, C., (to April 2004), ISO and XMMNewton data analysis
Young Gradutate Trainee
Carter, J., (from May 2004), Astronomer
Spanish Trainee
Del Mar Siere Gonzalez, M., (to Novembre 2004), ISO
data reduction and XMM-Newton RGS wavelength
calibration
XMM-Newton SOC (VILSPA)
Staff
Altieri, B., Software and payload support, observational
astronomy
Arpizou, M., Secretarial and administrative support
Ehle, M., XMM-Newton user support, observational
astronomy
Gabriel, C., XMM-Newton instrument support,
supernova remnants, cosmology
Guainazzi, M., XMM-Newton user support,
observational astronomy
Kirsch, M. EPIC Calibration Scientist
Metcalfe, L., XMM-Newton Science Support Manager
Munoz Peiro, J., Instrument Operations Manager
111
Pollock, M. RGS Calibration Scientist
Santos-Lleo, M., XMM-Newton user support,
observational astronomy
Schartel, N., XMM-Newton User Support and Mission
Planning Group Team Leader, observational
astronomy
Research Fellows
Bianchi, S., (from October 2004), XMM-Newton data
analysis of AGN
Gimenez Bailon, E., (from May 2003), Seyfert High
Energy
Piconcelli, E., (from April 2003), Study of AGN
Science Archives Group (VILSPA)
Staff
Arviset, C., System engineering. Archive group leader
Mars Express
Staff
Texier, D., (from August 2004), Mars Express Science
Operations Coordinator
Science Payload and Advanced Concepts Office
Peacock, A., Head of Office, STJ Research Team
Leader
Andersson, S., Electronics engineering for advanced
technologies for semiconductors sensors
Appourchaux, T., Solar Orbiter payload support, solar
research. COROT instrument Research Team
Leader
Adriaens, M., (to June 2002), Mechnical engineer
Arends, H., Mechanical engineer and mechanical
laboratory coordinator
Bavdaz, M., Advanced technologies sensors and optics,
Sensors and Optics Research Team Leader, Head of
Advanced Technology Section (p.i.)
Beaufort, T., Electronics engineer for COROT PDU
Biezen, J.F. van der, Electronics and laboratory
metrology support to advanced technology
programme.
Butler, B.A.C., Instrument development engineer
Dordrecht, A. van., Advanced Sensors electronics
engineer
Erd, C., Sensor research and development, ESA
missions support
Falkner, P., Electronics research and development, Head
of Planetary Exploration Section (p.i.)
Gondoin, Ph., Darwin-Genie instrument manager,
XMM observational research
Heida, J., Instrument support engineer
Jolander, B., Head of Instrument Support Group,
instrument development engineer
Klinge, D., Instrument development engineer
Lumb, D., Advanced sensor research, XEUS and ISS
payload and mission support, XMM observational
research
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Martin, D., SCAM3 instrument manager, Head of
Infrastructure Section (p.i.)
Rando, N., Payload support and development engineer.
Head of Missions Section (p.i.)
Romstedt, J., In-situ planetary instrument development,
Rosetta-MIDAS (AFM) Lead Scientist
Smit, L.C., Instrument development support engineer
Telljohann, U., Instrument electronics engineer
Verveer, J., Laboratory cryogenic systems support
Research Fellows
Molster, F., Rosetta-MIDAS AFM
Stagiares
Kilter, M., (August 2003-January 2004)
Kozak, R., (July-August 2003)
Larfors, K.
Leyder, J.-C., (January-March 2004)
Trainees
Moreira, O., (Portuguese Trainee from April 2002),
Helioseismology
Pitcher, K., (June-August 2001), International Law
RSSD acknowledges the valuable contribution made by
the contractor staff to the work of the Department.
Erratum from previous Report (2001-2002):
Head of Astrophysics Division (to October 2001) and
Acting Head of Department (to May 2001);
Taylor, B.G.
manpower deployment
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ANNEX 2
Publications
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ANNEX 2: PUBLICATIONS
Head of Research and Scientific Support Department
Refereed Journals, 2003
Claret, A., Willems, B., Gimenez, A., Unveiling the
internal constitution of components of close binary
systems, 2003, Recent Research and Development in
Astronomy and Astrophysics, 375.
Clausen, J.V., Storm, J., Larsen, S.S., Gimenez, A.,
Eclipsing binaries in the Magellanic Clouds. uvby
CCD light curves and photometric analyses for HV
982 (LMC), HV 12578 (LMC), HV 1433 (SMC), and
HV 11284 (SMC), 2003, A&A, 402, 509-530.
Domingo, A., Caballero, M.D., Figueras, F., Jordi, C.,
Torra, J., Mas-Hesse, J.M., Giminez, A., Hudcova, V.,
Hudec, R., The Input Catalogue for the OMC camera
onboard INTEGRAL, 2003, A&A, 411, L281-L289.
Gimenez, A., Lund, N., Preface, 2003, Adv. Space Res.,
31/Issue 2, 275.
Mas-Hesse, J.M., Gimenez, A., Culhane, J.L., Jamar, C.,
McBreen, B., Torra, J., Hudec, R., Fabregat, J.,
Meurs, E., Swings, J.P., Alcacera, M.A., Balado, A.,
Beiztegui, R., Belenguer, T., Bradley, L.,
Caballero, M.D., Cabo, P., Defise, J.M., Diaz, E.,
Domingo, A., Figueras, F., Figueroa, I., Hanlon, L.,
Hroch, F., Hudcova, V., Garcia, T., Jordan, B.,
Jordi, C., Kretschmar, P., Laviada, C., March, M.,
Martin, E., Mazy, E., Menendez, M., Mi, J.M., de
Miguel, E., Munoz, T., Nolan, K., Olmedo, R.,
Plesseria, J.Y. Polcar, J., Reina, M., Rnotte, E.,
Rochus, P., Sanchez, A., San Martin, J.C., Smith, A.,
Soldan J., Thomas, P., Timon, V., Walton, D., OMC –
An Optical Monitoring Camera for INTEGRAL.
Instrument and Description, 2003, A&A, 411, L261L268.
Ribas, I., Solano, E., Masana, E., Giminez, A., Effective
temperatures and radii of planet-hosting stars from IR
photometry, 2003, A&A, 411, L501-L504.
Head of Research and Scientific Support Department
Proceedings and other Publications 2003
Favata, F., Gimenez, A., The Eddington Mission
(co-authored by the Eddington Science Team), 2003,
Solar and Solar-like Oscillations – Insights and
Challenges for the Sun and Stars, 25 th Meeting of
IAU, Joint Discussion 12, JD12E, 51F.
Gimenez, A., The Future of Optical Astronomy in ESA’s
Science Programme, 2003, ASP Conf. Proc. Hubble’s
Science Legacy – Future Optical/Ultraviolet Astronomy from Space, 136-2, 22.
Gimenez, A., Concluding Remarks and Future, 2003,
Extragalactic Binaries, 25th meeting of the IAU, Joint
Discussion 13, 18 July 2003. Sydney, Australia,
JD13E, 31G.
Gimenez, A., Eclipsing Binaries and Stellar Astronomy,
publications
2003, New Directions for Close Binary Studies: The
Royal Road to the Stars, 3, 19.
Ribas, I., Jordi, C., Vilardell, F., Guinan, E.F., Hilditch,
R.W., Fitzpatrick, E.L., Valls-Gabaud, D., Gimenez,
A., Properties and Distances of Eclipsing Binaries in
M31, 2003, Extragalactic Binaries, 25th meeting of
the IAU, Joint Discussion 13, JD123E, 35R.
Shaver, P.A., Dilella, L., Gimenez, A., Astronomy,
Cosmology and Fundamental Physics, 2003, Proc.
ESO-CERN-ESA Symposium, ESA.
Silver, E.H., Schnopper, H.W., Jones, C., Forman, W.,
Bandler, S.R., Murray, S.S., Romaine, S.E., Slane,
P.O., Grindlay, J.E., Madden, N.W., Beeman, J.W.,
Haller, E.E., Smith, D.M., Barbera, M., Collura, A.,
Christensen, F.E., Ramsey, B.D., Woosley, S.E.,
Diehl, R., Tucker, G.S., Fabregat, J., Reglero, V.,
Gimenez, A., B-MINE, the balloon-borne microcalorimeter nuclear line explorer, 2003, X-ray and
Gamma-ray telescopes and Instruments for Astronomy, Proc. SPIE, 4851, 905-912.
Head of Research and Scientific Support Department
Refereed Journals, 2004
Ribas, I., Jordi, C., Vilardell, F., Gimenez, A., Guinan,
E.F., A program to determine a direct and accurate
distance to M31 from eclipsing binaries, 2004, New
Astronomy Reviews, 48/9, 755-758.
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publications
Astrophysics Missions Division
Refereed Journals, 2003
Bendo, G.J., Joseph, R.D., Wells, M., Gallais, P., Haas,
M., Heras, A.M., Klaas, U., Laureijs, R.J., Leech, K.,
Lemke, D., Metcalfe, L., Rowan-Robinson, M.,
Schulz, B., Telesco, C., Dust Temperatures in the
Infrared Space Observatory Atlas of Bright Spiral
Galaxies, 2003, AJ, 125, 2361.
Benjamin, R.A., Churchwell, E., Babler, B.L., Bania,
T.M., Clemens, D.P., Cohen, M., Dickey, J.,
Indebetouw, R., Jackson, J.M., Kobulnicky, H.A.,
Lazarian, A., Marston, A.P., Mathis, J.S., Meade,
M.R., Seager, S., Stolovy, S.R., Watson, C., Whitney,
B.A., Wolff, M.J., Wolfire, M.G., GLIMPSE. I. An
SIRTF Legacy Project to Map the Inner Galaxy, 2003,
PASP, 115, 953.
Boirin, L., Parmar, A.N., Discovery of narrow X-ray
absorption features from the low-mass X-ray binary
X 1254-690 with XMM-Newton, 2003, A&A, 407,
1079.
Boirin, L., Parmar, A.N., Barret, D., Paltani, S.,
Discovery of X-ray absorption lines from the lowmass X-ray binaries 4U 1916-053 and X 1254-690
with XMM-Newton, 2003, Nuclear Physics B
Proceedings Supplements, 132, 506.
Bridge, C.M., Cropper, M., Ramsay, G., de Bruijne,
J.H.J., Reynolds, A.P., Perryman, M.A.C., Variability
of the accretion stream in the eclipsing polar EP Dra,
2003, MNRAS, 341, 863.
Carpano, S., Aigrain, S., Favata, F., Detecting planetary
transits in the presence of stellar variability. Optimal
filtering and the use of color information, 2003, A&A,
401, 743.
Corbett, E.A., Kewley, L., Appleton, P.N., Charmandaris,
V., Dopita, M.A., Heisler, C.A., Norris, R.P., Zezas,
A., Marston, A., COLA. II. Radio and Spectroscopic
Diagnostics of Nuclear Activity in Galaxies, 2003,
ApJ, 583, 670.
Cropper, M., Barlow, M., Perryman, M.A.C., Horne, K.,
Bingham, R., Page, M., Guttridge, P., Smith, A.,
Peacock, A., Walker, D., Charles, P., A concept for an
STJ-based echelle spectrograph, 2003, MNRAS, 344,
33.
Del Burgo, C., Laureijs, R.J., Abraham, P., Kiss, C., The
far-infrared signature of dust in high latitude regions,
2003, MNRAS, 346, 403.
Dupac, X., Bernard, J.P., Boudet, N., Giard, M., Lamarre,
J.M., Miny, C., Pajot, F., Ristorcelli, I., Serra, G.,
Stepnik, B., Torre, J.P., Inverse temperature
dependence of the dust submillimeter spectral index,
2003, A&A, 404, L11-L15.
Dupac, X., Del-Burgo, C., Bernard, J.P., Giard, M.,
Lamarre, J.M., Laureijs, R.J., Pajot, F., Ristorcelli, I.,
Serra, G., Tauber, J., Torre, J.P., The complete
submillimetre spectrum of NGC 891, 2003, MNRAS,
344/1, 105.
Favata, F., Giardino, G., Micela, G., Sciortino, S., An
XMM-Newton-based X-ray survey of pre-main
115
sequence stellar emission in the L1551 star-forming
complex, 2003, A&A, 403, 187.
Favata, F., Micela, G., Coronal X-ray Astronomy, 2003,
Space Sci. Rev., 108, 577.
Franco, G., Fosalba, P., Tauber, J.A., Systematic Effects
in the Measurement of Polarization by the Planck
Telescope, 2003, A&AS, 405, 349.
Fridlund, M., Gondoin, P., GENIE – The Darwin demonstrator, 2003, Astrophysics & Space Science, 286, 93.
Hony, S., Tielens, A.G.G.M., Waters, L.B.F.M., Koter, A.
de, The circumstellar envelope of the C-rich postAGB star HD 56126, 2003, A&A, 402, 211.
Jakobsen, P., Jansen, R.A., Wagner, S., Reimers, D.,
Caught in the act- a helium-reionizing quasar near the
line of sight to Q0302-003, 2003, A&A, 397, 891.
Katz, D., Favata, F., Aigrain, S., Micela, G., The
photospheric abuyndance of active binaries. I.
Detailed analysis of HD 113816 (IS VIR) and HD
119285 (V851 Cen), 2003, A&A, 397, 747.
Laine, S., van der Marel, R.P., Rossa, J., Boeker, T.,
Mihos, J.C., Hibbard, J.E., Zabludoff, A.I., Hubble
Space Telescope/WFPC2 Investigation of the Nuclear
Morphology in the Toomre Sequence of Merging
Galaxies, 2003, AJ, 126, 2717.
Lehtinen, K., Mattila, K., Lemke, D., Juvela, M., Prusti, T.,
Laureijs, R., Far infrared observations of pre-protostellar sources in Lynds 183, 2003, A&A, 398, 571.
Liseau, R., Brandeker, A., Fridlund, M., Olofsson, G.,
Takeuchi, T., Artymowicz, P., The 1.2 mm image of
the beta Pictoris disk, 2003, A&A, 402, 183.
Morel, T., Micela, G., Favata, F., Katz, D., Pillitteri, I.,
The photospheric abundances of active binaries, 2003,
A&A, 414, 459.
Parmar, A.N., Kuulkers, E., Oosterbroek, T., Barr, P.,
Much, R., Orr, A., Williams, O.R., Winkler, C.,
INTEGRAL observations of the black hole candidate
H1743-322 in outburst, 2003, A&A, 411, L421.
Pillitteri, I., Micela, G., Sciortino, S., Favata, F., The
X-ray Luminosity Distributions of the high-metallicity
open cluster Blanco 1, 2003, A&A, 399, 919.
Prisinzano, L., Micela, G., Sciortino, S., Favata, F.,
Luminosity and mass function of the galactic open
cluster NGC 2422, 2003, A&A, 404, 927.
Roxburgh, I.W., Favata, F., The Eddington Mission,
2003, Ap&SS, 284, 17.
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Bourrachot, A., Camus, P., Couchot, F., Bernardis, P.
de, Delabrouille, J., Desert, F.X., Dore, O., Douspis,
M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P.,
Ganga, K., Gannaway, F., Gautier, B., Giard, M.,
Giraud-Heraud, Y., Gispert, R., Guglielmi, L.,
Hamilton, J.C., Hanany, S., Henrot-Versille, S.,
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C., Marrone, D.P., Masi, S., Mayet, F., Murphy, A.,
Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat,
M., Ponthieu, N., Prunet, S., Puget, J.L., Renault, C.,
Rosset, C., Santos, D., Starobinsky, A., Strukov, I.,
Sudiwala, R.V., Teyssier, R., Tristram, M., Tucker, C.,
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Conference on Multi-wavelength Cosmology, 301,
305.
Parmar, A.N., Arnaud, M., Barcons, X., Bleeker, J.,
Hasinger, G., Inoue, H., Palumbo, G., Turner, M.,
Science with XEUS – the X-ray Evolving Universe
Spectroscopy Mission, 2004, Proceedings SPIE – UV
and Gamma-Ray Space Telescope Systems, 5488, 388.
Peeters, E., Allamandola, L.J., Hudgins, D.M., Hony, S.,
Tielens, A.G.G.M., The Unidentified InfraRed Bands
after ISO, 2004, Astrophysics of Dust, Estes Park,
Colorado, May 26-30, 2003, 309, 141.
Perryman, M.A.C., Detection and Characterization of
Extra-Solar Planets, 2004, The Search for Other
Worlds, 713, 283.
Perryman, M.A.C., Hipparcos and Gaia – the Development of Space Astrometry in Europe, 2004, IAC
Winter School 2003, (Accepted for Publication).
Perryman, M.A.C., Our Galaxy in Three-Dimensions –
the Jeremiah Horrocks Memorial Lecture, 2004,
Transit of Venus – New Views of the Solar System and
Galaxy, IAU Coll 196, (Accepted for Publication).
Sanz-Forcada, J., Dupree, A.K., Active Stars and He I
10830 A, the EUV Connection, 2004, High Resolution
Infrared Spectroscopy in Astronomy, (Accepted for
Publication).
Sanz-Forcada, J., Favata, F., Micela, G., The not-soMAD coronal abundances of active stars, 2004,
Chemical Abundances and Mixing in Stars in the
Milky Way and its Satellites, (Accepted for
Publication).
Sanz-Forcada, J., Favata, F., Micela, G., The not-soMAD coronal abundances of active stars, 2004, 13th
Cambridge Workshop on Cool Stars, (Accepted for
Publication).
Sciortino, S., Micela, G., Favata, F., Giardino, G.,
Flaccomio, E., Damiani, F., X-ray Observations of
Star Formation Regions – EPIC results in L1551 and
Upper Sco-Cen, 2004, Mem. S. A. It., 75, 428.
Sidoli, L., Parmar, A.N., Oosterbroek, T., XMM-Newton
results on the ultracompact low-mass X-ray binary 4U
1850-087 in the globular cluster NGC 6712, 2004,
The 5th INTEGRAL Workshop – The INTEGRAL
Universe, ESA SP-552, 389.
Sidoli, L., Parmar, A.N., Oosterbroek, T., The First
Broad-Band Persistent X-ray Spectrum of the Dipping
Low Mass X-ray Binary EXO 0748-676, 2004, The
5th INTEGRAL Workshop – The INTEGRAL
Universe, ESA SP-552, 385.
Tauber, J., Prospects for Polarimetry of the Interstellar
Medium with the Planck Satellite, 2004, The
Magnetized Interstellar Medium, 191.
Tielens, A.G.G.M., Peeters, E., Bakes, E.L.O., Spoon,
H.W.W., Hony, S., PAHs and Star Formation, 2004,
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ASP Conf. Ser. 323: Star Formation in the Interstellar
Medium Workshop, in Honor of David Hollenbach,
Chris McKee and Frank Shu.
Walter, R., Courvoisier, T.J.-L., Foschini, L., Lebrun, F.,
Lund, N., Parmar, A., Rodiguez, J., Tomsock, J.A.,
Ubertini, P., IGR J16318-4848 & CO – A new
population of hidden high mass X-ray binaries in the
Norma arm of the Galaxy, 2004, Proc. 5th INTEGRAL
Workshop, ESA SP-552, 417.
publications
Planetary Missions Division
Refereed Journals, 2003
Arpigny, C., Jehin, E., Manfroid, J., Hutsemekers, D.,
Schulz, R., Stuewe, J.A., Zucconi, J.-M., Ilyin, I.,
Anomalous nitrogen isotope ratio in comets – possible
connection with interplanetary dust particles and
organic molecules, 2003, Science, 301, 1522-1524.
Clausen, K.C., Hassan, H., Verdant, M., Couzin, P.,
Huttin, G., Brisson, M., Sollazzo, C., Lebreton, J.-P.,
The Huygens Probe System Design, 2003, Space Sci.
Rev., Special Cassini/Huygens issue, 35.
Heather, D.J., Dunkin, S.K., Geology and Stratigraphy of
King Crater, Lunar Farside, 2003, Icarus, 163, 307-329.
Heather, D.J., Dunkin, S.K., Wilson, L., Volcanism on
the Marius Hills plateau – Observational analyses
using Clementine multispectral data, 2003, J.
Geophys. Res., 108/E3, 3-1.
Kolokolova, L., Lara, L.M., Schulz, R., Stuewe, J.A.,
Tozzi, G.P., Color of an ensemble of particles with a
wide power-law size distribution – application to
observations of Comet Hale-Bopp at 3 AU, 2003,
J. Quantitative Spectroscopy and Radiative Transfer,
79-80, 861-871.
Lebreton, J.-P., Matson, D.L., The Huygens Probe –
Science, Payload and Mission, 2003, Space Sci. Rev.,
Special Cassini/Huygens, 41.
Michael, G.G., Coordinate registration by automated
crater recognition, 2003, Planet. Space Sci., 51/9-10,
563.
Molina-Cuberos, G., Witasse, O., Lebreton, J.-P.,
Rodrigo, R., Lopez-Moreno, J.J., Meteoric ion in the
atmosphere of Mars, 2003, Planet. Space Sci., 51/3,
239-249.
Schulz, R., Maximize the Outcome of a Comet Mission,
but how?, 2003, Adv. Space Res., (Accepted for
Publication).
Schulz, R., Stuewe, J.A., Boehnhardt, H., Gaessler, W.,
Tozzi, G.P., Characterization of STARDUST target
comet 81P/Wild 2 from 1996 to 1998, 2003, A&A,
298, 345-352.
Trautner, R., Grard, R., Hamelin, M., Detection of
Subsurface Ice and Water Deposits on Mars with a
Mutual Impedance Probe, 2003, J. Geophys. Res.,
108/E10, 8047.
Witasse, O., Dutuit, O., Correction to “Prediction of a
CO22+ layer in the atmosphere of Mars”, 2003,
Geophys. Res. Lett., 30, 12.
Planetary Missions Division
Proceedings and other Publications, 2003
Aleon, J., Arpigny, C., Robert, F., Jehin, E., Manfroid, J.,
Hutsemekers, D., Zucconi, J.-M., Schulz, R., Stuewe,
J.A., Sangely, L., Chaussidon, M., Marty, B., Engrand,
C., Cometary organic macromolecules in interplanetary dust particles?, 2003, Lunar and Planetary
Science, XXXIV, 1308.
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Arpigny, C., Cochran, A.L., Jehin, E., Manfroid, J.,
Hutsemekers, D., Zucconi, J.-M., Endl, M., Cochran,
W.D., Schulz, R., Anomalous 14N/15N ratio in
comets 122P/1995 S1 (de Vico) and 153P/2002 C1
(Ikeya-Zhang), 2003, Bull. Am. Astron. Soc., 35/4,
986.
Collon, M., Buis, E.J., Beijersbergen, M., Kraft, S., Erd,
C., den Hartog, R., Owens, A., Falkner, P., Schulz, R.,
Peacock, A., Design and performance of the payload
instrumentation of the BepiColombo Mercury
Planetary Orbiter, 2003, Proceedings of the Fifth IAA
International Conference on Low-Cost Planetary
Missions, ESA SP-542, 501.
Falkner, P., Schulz, R., The BepiColombo Mission to
Mercury, 2003, Bull. Am. Astron. Soc., 35/4, 1001.
Fulchignoni, M., Ferri, F., Angrilli, F., Bar-Nun, A.,
Barucci, M.A., Bianchini, G., Borucki, W., Coradini,
M., Coustenis, A., Falkner, P., Flamini, E., Grard, R.,
Hamelin, M., Harri, A.M., Leppelmeier, G.W., LopezMoreno, J.J., McDonnell, J.A.M., McKay, C.P.,
Neubauer, F.H., Pedersen, A., Picardi, G., Pirronello,
V., Rodrigo, R., Schwingenschuh, K., Seiff, A.,
Svedhem, H., Vanzani, V., Zarnecki, J., The
Characterisation of Titan’s Atmospheric Physical
Properties by the Huygens Atmospheric Structure
Instrument (HASI), 2003, The Cassini-Huygens
Mission, 395-431.
Kraft, S., Collon, M., Montella, J., Buis, E.J.,
Beijersbergen, M., Erd, C., Falkner, P., Schulz, R.,
Peacock, A., On the concepts of a highly integrated
payload suite for use in future planetary missions, the
example of the BepiColombo Mercury Planetary
Orbiter, 2003, Proc. Fifth IAA International
Conference on Low-Cost Planetary Missions, ESA
SP-542, 219.
Schulz, R., Kern, Koma und Schweife, 2003, Sterne &
Weltraum Special: Kometen und Asteroiden, 2/03, 2832.
Schulz, R., Wirtanen – A short period comet, 2003,
CNES Magazine, 18, 34.
Schulz, R., Rosetta goes to comet Wirtanen, 2003, The
Observatory, 123/1174, 115-118.
Schulz, R., Falkner, P., Peacock, A., Erd, C., Rando, N.,
Kraft, S., The BepiColombo Mission, 2003,
Highlights in Astronomy, 13.
Schulz, R., Stuewe, J.A., Boehnhardt, H., Postperihelion
monitoring of Comet 67P/Churyumov-Gerasimenko,
the new Rosetta target, 2003, Bull. Am. Astron. Soc.,
35/4, 970.
Thomas, N., Schulz, R., Falkner, P., The BepiColombo
Lander – MSE, 2003, Highlights in Astronomy, 13.
Trautner, R., Chicarro, A.C., Martin, P.D., Coordinated
Science Operations of Mars Express Orbiter and
Lander, 2003, Lunar and Planetary Science, XXXIV,
1634.
Trautner, R., Simoes, F., Grard, R., Hamelin, M., A new
instrument for measuring the low frequency electrical
properties of planetary subsurface materials, 2003,
ESA SP-543, 193.
121
Planetary Missions Division
Refereed Journals, 2004
Bolton, S.J., Hansen, C.J., Matson, D.L., Spilker, L.J.,
Lebreton, J.-P., Cassini/Huygens flyby of the Jovian
system, 2004, J. Geophys. Res., 109, 1-5.
Campbell-Brown, M.D., Koschny, D., Model of the
ablation of faint meteors, 2004, A&A, 418, 751-758.
Culot, F., Lathuillere, C., Lilensten, J., Witasse, O., The
OI 630.0 and 557.7 nm dayglow measured by WINDII
and modeled by TRANSCAR, 2004, Ann. Geophysicae, 22, 1947-1960.
Hansen, C.J., Bolton, S.J., Matson, D.L., Spilker, L.J.,
Lebreton, J.-P., The Cassini-Huygens Flyby of Jupiter,
2004, Icarus, 172, 1-8.
Jehin, E., Manfroid, J., Cochran, A.L., Arpigny, C.,
Zucconi, J.M., Hutsemekers, D., Cochran, W.D., Endl,
M., Schulz, R., Anomalous 14N/15N ratio in comets
122P/de Vico) and 153P/Ikeya-Zhang, 2004, ApJ,
613, L161-L164.
Kazeminjad, B., Perez-Ayúcar, M., Lebreton, J.-P.,
Sanchez-Nogales, M., Belló-Mora, M., Strange, N.,
Roth, D., Popken, L., Clausen, K., Couzin, P., Simulation and analysis of the revised Huygens probe entry
and descent trajectory and radio link modelling., 2004,
Planet. Space Sci., 52, 799-814.
Lara, L.M., Tozzi, G.P., Boehnhardt, H., DiMartino, M.,
Schulz, R., Gas and dust in comet C/2000 WM1
during its closest approach to Earth. Optical imaging
and long-slit spectroscopy, 2004, A&A, 422, 717-729.
Lilensten, J., Simon, C., Witasse, O., Dutuit, O., Thissen,
R., Alcaraz, C., A fast computation on the diurnal
secondary ion production in the ionosphere of Titan,
2004, Icarus, (Accepted for Publication).
Lilensten, J., Witasse, O., Simon, C., Soldi-Lose, H.,
Dutuit, O., Thissen, R., Alcaraz, C., Prediction of a
N2++ layer in the upper atmosphere of Titan, 2004,
Geophys. Res. Lett., (Accepted for Publication).
Michael, G.G., Beagle-2 position determination from the
returned camera panoramas using MOLA data, 2004,
Planet. Space Sci., 52, 271.
Morel, L., Witasse, O., Warnant, R., Cerisier, J.-C.,
Blelly, P.-L., Lilensten, J., Diagnostic of the dayside
ionosphere of Mars using the Total Electron Content
Measurement by the Neige/Netlander experiment – an
assessment study, 2004, Planet. Space Sci., 52/7, 603611.
Schulz, R., Stuewe, J.A., Boehnhardt, H., Rosetta target
comet 67P/Churyumov-Gerasimenko. Postperihelion
gas and dust prodution rates, 2004, A&A, 422, L19L21.
Tozzi, G.P., Lara, L.M., Kolokolova, L., Boehnhardt, H.,
Licandro, J., Schulz, R., Sublimating components in
the Coma of Comet C/2000 WM1 (LINEAR), 2004,
A&A, 424, 325-330.
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Planetary Missions Division
Proceedings and other Publications, 2004
DiMartino, M., Battistelli, E., Carbognani, A., Cellino,
A., Koschny, D., Resti, A., Tommasi, L., The ‘Smart
Panoramic Optical Sensor Head’ – A new Tool for
Detecting Luminous Transient Phenomena on
Planetary Bodies, 2004, Geophysical Research
Abstracts, 6, 02852.
Diaz del Rio, J., Koschny, D., Meteor Orbit and
Trajectory determination Software (MOTS), 2004,
Proc. Int. Meteor Conf., 19-21 Sep 2003,
Bollmannsruh, Germany, Int. Met. Org., Berlin,
Germany, 23-28.
Frew, D., Koschny, D., Harch, A., Planning the
commissioning of a multi-payload mission, 2004,
Proc. SpaceOps 2004, May 17-21, 2004, Montreal,
Canada.
Hoofs, R., Koschny, D., van der Plas, P., Planning
strategy and supporting tools for the science
operations of ESA’s planetary missions, 2004, Proc.
SpaceOps 2004, May 17-21, 2004, Montreal, Canada,
Canadian Space Agency.
Hoofs, R., Titov, D., Svedhem, H., Koschny, D.,
Ocampo, A., Science Operations Planning for Venus
Express, 2004, Geophysical Research Abstracts, 6,
06373.
Josset, J.-L., Beauvivre, S., Almeida, M., Barrucci, A.,
Cerroni, P., Chevrel, S., diSanctis, C., Ehrenfreud, P.,
Hofmann, B., Josset, M., Koschny, D., Langevin, Y.,
Mancuso, S., Muinonen, M., Pinet, P., Plancke, P.,
Shevch, V., Shkuratov, Y., Sodnik, Z., First results
from the Smart-1 AMIE Multi-Colour Micro-Camera,
2004, Geophysical Research Abstracts, 6, 07866.
Koschny, D., Comparing two potential meteor cameras –
the Mintron and the Watec 120N, 2004, Proc. Int.
Meteor Conf., 19-21 Sep 2003, Bollmannsruh,
Germany, Int. Met. Org., Berlin, Germany, 59, 63.
Koschny, D., Dhiri, V., Frew, D., Hoofs, R., Lumb, R.,
Schwehm, G., Wirth, K., Zender, J., Science
Operations for Planetary Missions in the European
Space Agency, 2004, Proc. SpaceOps 2004, May 1721, 2004, Montreal, Canada, Canadian Space Agency.
Koschny, D., DiMartino, M., Oberst, J., Meteor
observations from space – The Smart Panoramical
Optical Sensor (SPOSH), 2004, Proc. Int. Meteor
Conf., 19-21 Sep 2003, Bollmannsruh, Germany, Int.
Met. Org., Berlin, Germany, 64-69.
Koschny, D., Trautner, R., Zender, J., Knöfel, A., Diaz
del Rio, J., Jehn, R., The ESA Leonid campaign 2002
to Spain, 2004, Proc. Int. Meteor Conf., 19-21 Sep
2003, Bollmannsruh, Germany, Int. Met. Org., Berlin,
Germany,70-77.
Lebreton, J.-P., Dicke Luft, 2004, Astronomie Heute, 1-2.
Lebreton, J.-P., Into Thick Air, 2004, Sky and Telescope,
July, 38-41.
Lebreton, J.-P., Matson, D.L., The Huygens Mission to
Titan. An Overview, 2004, Proc., ESA SP-1278, 229242.
publications
Lebreton, J.-P., Sollazzo, C., Blancquaert, T., Witasse,
O., Maize, E., Matson, D.L., Mitchell, R., Spilker, L.,
Flamini, E., Talevi, M., [and the Huygens Mission
Team], High Ambitions for an Outstanding Planetary
Mission. Cassini-Huygens, 2004, ESA Bulletin, 120,
11-21.
Lebreton, J.-P., Matson, D., The Huygens Mission to
Titan. Overview and Status, 2004, Proc. Planetary
Probe Atmospheric Entry and Descent Trajectory
Analysis and Science, ESA SP-544, 21-30.
Matson, D.L., Lebreton, J.-P., Spilker, L.J., The CassiniHuygens mission to the Saturnian system, 2004,
Proc., ESA SP-1278, 242/I-242/XVi.
Rohner, U., Benz, W., Whitby, J.A., Wurz, P., Schulz, R.,
Romstedt, J., Miniaturised Time-of-Flight Mass
Spectrometer, 2004, Proceedings of the 37th ESLAB
Symposium ‘Tools and Technologies for Future
Planetary Exploration’, ESA SP-543, 131.
Schulz, R., BepiColombo. Visit to Mercury, 2004,
ERCA, From indoor air pollution to the search for
Earth-like planets in the cosmos, J. de Physique IV
Proc., EDP Sciences, 6, 249.
Schulz, R., The Mercury Planetary Orbiter of
BepiColombo, 2004, Geophysical Research
Abstracts, 6, 04807.
Schulz, R., Anomalous Nitrogen Isotopic Ratio in
Comets, 2004, ESA Space Science News, 6, 8-9.
Schulz, R., Comet 67P/Churyumov-Gerasimenko, the
new Rosetta Target, 2004, CNES Magazine, February
2004, 18.
Schulz, R., Stuewe, J.A., Boehnhardt, H., Monitoring
comet 67P/Churyumov-Gerasimenko from ESO in
2003, 2004, The New Rosetta Targets. Observation,
simulations and instrument performances, Kluwer
Academic Publishers, Dordrecht, The Netherlands,
15-24.
Simões, F., Trautner, R., Grard, R., Hamelin, M., The
dielectric properties of Martian Soil Simulant JSC
Mars-1 in the frequency range from 20 Hz to 10kHz,
2004, Lunar and Planetary Conference, XXXIV, 205.
Svedhem, H., Lebreton, J.-P., Zarnecki, J., Hathi, B.,
Using Speed of Sound Measurements to Constrain the
Huygens Probe Descent Profile, 2004, Int. Workshop
‘Planetary Probe Atmospheric Entry and Descent
Trajectory Analysis and Science’, Lisbon, Portugal, 69 October 2003, ESA SP-544, 221-228.
Trautner, R., Bello-Mora, M., Hechler, M., Koschny, D.,
A new celestial navigation method for Mars landers,
2004, Lunar and Planetary Science, XXXV, 1106.
Trautner, R., Koschny, D., A new Application for
Planetary Lander Cameras – Lander Position and
Attitude Determination using Night Sky Images,
2004, Geophysical Research Abstracts, 6, 03614.
Trautner, R., Manaud, N., Michael, G., Griffiths, A.,
Beauvivre, S., Koschny, D., Coates, A., Josset, J.,
Determination of the Beagle2 landing site, 2004, ESA
SP-544, 175.
Wirth, K.R., Hoofs, R., Koschny, D., Frew, D., Dhiri, V.,
Rosetta Science Mission Overview, 2004, 35th
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COSPAR Scientific Assembly, Paris, France, 18-25
July 2004.
Wirth, K.R., Zender, J., Arviset, C., PSA ready to deliver
science data from ESA planetary missions, 2004,
EGU 1st General Assembly, Geophysical Research
Abstracts, 6, 01467.
Zender, J., Witasse, O., Koschny, D., Campbell-Brown,
M., Diaz del Rio, J., Trautner, R., Knöfel, A., Meteor
spectroscopy – Introduction to theory, setup, and data
analysis, 2004, Proc. Int. Met. Conf. 2003, 19-21 Sep
2003, Bollmannsruh, Germany, 168.
Zender, J.J., Schwehm, G., Arviset, C., The Planetary
Science Archive, Introduction and Overview, 2004,
Ensuring the long-term Preservation and Adding
Value to the Scientific and Technical Data,
Proceedings, ESA WPP-232, 31-38.
Zender, J.J., Schwehm, G., Wilke, M., The ROSETTA
Video Approach, An Overview and Lessons Learned
so far, 2004, Proc. 55th International Astronautical
Congress, Zarm, Univ. Bremen, Germany (CD).
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Science Operations and Data Systems Division
Refereed Journals, 2003
Barret, D., Olive, J.F., Oosterbroek, T., Simultaneous
BeppoSAX and Rossi X-ray Timing Explorer
observations of 4U 1812-12, 2003, A&A, 400, 643.
Brandt, S. Budtz-Jorgensen, C., Lund, N., Rasmussen,
L.L., Laursen, S., Chenevez, J., Westergaard, N.J.,
Juchnikowski, G., Walter, R., Schmidt, M., Much, R.,
X-ray observation of the Crab Pulsar and Nebula with
JEM-X on INTEGRAL, 2003, A&A, 411, L433.
Brandt, S., Budtz-Jorgensen, C., Lund, N., Chenevez, J.,
Hornstrup, A., Jensen, P.A., Laursen, S., Rasmussen,
I.L., Omo, K., Oxborrow, C.A., Pedersen, S.M.,
Polny, J., Westergaard, N.J., Andersson, H.,
Andersson, T., Vilhu, O., Huovelin, J., Maisala, S.,
Morawski, M., Juchnikowski, G., Costa, E., Feroci,
M., Frontera, F., Pelliciari, C., Loffredo, G., Reglero,
V., Martinez Nunez, S., Larsson, S., Svensson, R.,
Zdziarski, A.A., Castro-Tirado, A., Goria, M.,
Giulianelli, G., Rezazad, M., Cordero, F., Schmidt,
M., Carli, R., Jensen, P.L., Sarri, G., Gomez, C., Orr,
A., Much, R., Kretschmar, P., JEM-X Inflight
Performance, 2003, A&A, 411, L243.
Burgdorf, M., Orton, G.S., Davis, G.R., Sidher, S.D.,
Feuchtgruber, H., Griffin, M.J., Swinyard, B.M.,
Neptune’s Far-Infrared Spectrum from the ISO LongWavelength and Short-Wavelength Spectrometers –
its Bulk Composition and Effective Temperature,
2003, Icarus, 164, 244.
Cornelisse, R., in ‘t Zand, J.J.M., Verbunt, F., Kuulkers,
E., Heise, J., den Hartog, P.R., Cocchi, M., Natalucci,
L., Bazzano, A., Ubertini, P., Six years of BeppoSAX
Wide Field Cameras observations of nine galactic
type-I X-ray bursters, 2003, A&A, 405, 1033.
Courvoisier, T., Walter, R., Beckmann, V., Dean, A.,
Dubath, P., Hudec, R., Kretschmar, P., Mereghetti, S.,
Montmerle, T., Mowlawi, N., Paltani, S., PreiteMartinez, A., Produit, N., Staubert, R., Strong, A.,
Swings, J.-P., Westergaard, N., White, N., Winkler, C.,
Zdziarski, A., The INTEGRAL Science Data Centre,
2003, A&A, 411, L53.
Coustenis, A., Salama, A., Schulz, B., Ott, S., Lellouch,
E., Encrenaz, T., Gautier, D., Feuchtgruber, H., Titan’s
atmosphere from ISO mid-infrared spectroscopy,
2003, Icarus, 161, 383.
Dahlem, M., Ehle, M., Jansen, F., Heckman, T.M.,
Weaver, K.A., Strickland, D.K., The quest for hot gas
in the halo of NGC 1511, 2003, A&A, 403, 547.
Derriere, S., Ott, S., Gastaud, R., Increasing the
reliability of ISOCAM cross-identifications by use of
a probability pattern, 2003, A&A, 405, 1169-1176.
Diehl, R., Knödlseder, J., Lichti, G., Kretschmar, P.,
Schönfelder, V., Strong, A., v. Kienlin, A., Weidenspointner, G., Winkler, C., Wunderer, C., SPI
measurements of Galactic 26Al, 2003, A&A, 411,
L451.
Duggan, P., McBreen, B., Carr, A.J., Winston, E.,
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Kvick, A., Terry, A., Gamma-ray bursts and X-ray
melting of material to form chondrules and planets,
2003, A&A, 409, 9.
Evans, A., Gehrz, R.D., Geballe, T.R., Woodward, C.E.,
Salama, A., Sanchez, R.A., Starrfield, S.G., Krautter,
J., Barlow, M., Lyke, J.E., Hayward, T.L., Eyres,
S.P.S., Greenhouse, M.A., Hjellming, R.M., Wagner,
R.M., Pequignot, D., Infrared Space Observatory and
Ground-Based Infrared Observations of the Classical
Nova V723 Cassiopeiae, 2003, AJ, 126, 1981.
Goetz, D., Mereghetti, S., Hurley, K., Deluit, S., Feroci,
M., Frontera, F., Fruchter, A., Gorosabel, J.,
Hartmann, D., Hjorth, J., Hudec, R., Mirabel, F., Pian,
E., Pizzichini, G., Ubertini, P., Winkler, C.,
Observation of GRB 030131 with the INTEGRAL
satellite, 2003, A&A, 409, 831.
Gomez de Castro, A.I., Verdugo, E., HST/STIS spectrum
of RW Aur A. Evidence for an ionized belt-like
structure and mass ejection in timescales of a few
hours, 2003, ApJ, 597, 443.
Grandi, P., Guainazzi, M., Maraschi, L., Morganti, R.,
Fusco-Femiano, R., Fiocchi, M., Ballo, L., Tavecchio,
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Ott, S., Parthasarathy, M., Perault, M., Price, S.D.,
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J.M., Lebrun, F., Lund, N., Palumbo, G., Paul, J.,
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N.J., Beckmann, V., Kretschmar, P., Mereghetti, S.,
First results from the INTEGRAL Galactic plane
scans, 2003, A&A, 411, L349.
Zand, J.J.M. in ‘t, Hulleman, F., Markwardt, C.B.,
Mindez, M., Kuulkers, E., Cornelisse, R., Heise, J.,
Strohmayer, T.E., Verbunt, F., Bursts, eclipses, dips
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Science Operations and Data Systems Division
Proceedings and other Publications, 2003
Ali, B., Kong, M., Salama, A., The ISO Visualizer – A
new way to look at ISO data, 2003, Exploiting the ISO
Data Archive, Infrared Astronomy in the Internet Age,
ESA SP-511, 17.
Arviset, C., ESA RSSD Scientific Archives, 2003,
ICATPP 8th Conference Proceedings, ISBN 981-238860-5, 305.
Arviset, C., Osuna, P., Salgado, J., ESA ISO and XMMNewton Archives Inter-Operability and VO services,
2003, ADASS XIII Conference Proceedings, 314, 574.
Baluteau, J., Damour, F., Caux, E., Gry, C., Ceccarelli,
C., Diffuse Gas in the Galaxy I – The Galactic Plane,
2003, Exlpoiting the ISO Data Archive. Infrared
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Baluteau, J.P., Damour, F., Caux, E., Gry, C., Caccarelli,
C., Diffuse gas in the Galaxy. The Galactic Plane,
2003, Exploiting the ISO Data Archive. Infrared
Astronomy in the Internet Age, held in Siguenza, Spain
24-27 June, 2002, ESA SP-511, 209.
Barstow, M.A., Wamsteker, W., The WSO. A world-class
observatory for the ultraviolet, in Future EUV/UV and
Visible Space Astrophysics Missions and Instrumentation., 2003, Proceedings of the SPIE, 4854, 364-374.
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ISO mission, ESA SP-481, 215.
Biviano, A., Metcalfe, L., Mc Breen, B., Kneib, J.-P.,
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Burgdorf, M., Feuchtgruber, H., Salama, A., GarciaLario, P., Mueller, T. Lord, S., Matching the
spectrometers on board ISO, 2003, The calibration
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Dubath, P., Revnivtsev, M., Goldoni, P., Kienlin, A. von,
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Garcia-Lario, P., ISO Cross-Calibration – Internal and
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Garcia-Lario, P., Perea Calderon, J.V., The transition
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2003, Exploiting the ISO Data Archive. Infrared
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Haubold, H.J., Wamsteker, W., The International
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Costa, E., Feroci, M., Ubertini, P., Delsanto, M.,
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A., Winkler, C., Schönfelder, V., Kienlin, A., Lichti,
G., Kretschmar, P., Produit, N., Mereghetti, S., Gotz,
D., Mirabel, F., Woods, P., Gogus, E., Kouveliotou,
C., Finger, M., Thompson, C., Duncan, R., Pedersen,
H., Pavlov, G., Klis, M. van der, An INTEGRAL ToO
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outburst of XTE J1550-564, 2003, The Astronomer’s
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Le Petit, F., Boisse, P., Roueff, E., Rollinde, E., Pineau
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Lim, T., Swinyard, B.M., Burgdorf, M., Caux, E., Davis,
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C., Harwood, A.S., Leeks, S.J., Molinari, S., Pezzuto,
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The LWS Calibration Strategy, 2003, The Calibration
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Matt, G., Guainazzi, M., Maiolino, R., Changing Face –
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T., Baliyan, K., Beaulieu, S., Begon, S., Bertou, X.,
Blommaert, J.A.D.L., Borsenberger, J., Burgdorf, M.,
Caillaud, B., Cesarsky, C., Chitre, A., Copet, E., de
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M., Fouque, P., Ganesh, S., Genzel, R., Glass, I.S.,
Gredel, R., Groenewegen, M.A.T., Guglielmo, F.,
Habing, H.J., Hennebelle, P., Jiang, B., Joshi, U.C.,
Kimeswenger, S., Messineo, M., Miville-Deschenes,
M.A., Moneti, A., Morris, M., Ojha, D.K., Ortiz, R.,
Ott, S., Parthasarathy, M., Perault, M., Price, S.D.,
Robin, A.C., Schultheis, M., Schuller, F., Simon, G.,
Soive, A., Testi, L., Teyssier, D., Tiphene, D.,
Unavane, M., van Loon, J.T., Wyse, R., The ISOGAL
Point Source Catalogue – IGPSC, 2003, VizieR Online Data Catalog, II/243.
Osuna, P., Arviset, C., Salgado, J., Adapting ISO and
XMM-Newton Archives to Inter-Operability VO
Standards, 2003, ADASS XIII Conf. Proc., 314, 129.
Ott, S., The ISO Data Reduction Lesson – Pipeline and
Interactive Analysis are Complementary Systems,
2003, The Calibration Legacy of the ISO Mission,
ESA SP-481, 263.
Ott, S., The ISOCAM parallel survey – 30000 new
celestrial sources, 2003, ESA Today, 12, 17.
Ott, S., Gastaud, R., Guest, S., Delaney, M., Sam-Lone,
J., Starck, J.-L., Ali, B., Aussel, H., Claret, A.,
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Ott, S., Siebenmorgen, R., Schartel, N., Vo, T., Status
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Ott, S., Siebenmorgen, R., Schartel, N., Vu, T., The
ISOCAM Parallel Mode Survey, 2003, ADASS XII,
295, 117.
Patel, S.K., Kouveliotou, C., Tennant, A., Wilson, C.,
Woods, P., Finger, M., Wachter, S., King, A.,
Ubertini, P., Klis, M., Courvoiser, T., Winkler, C.,
The Peculiar X-ray Transient IGR J16358-4726,
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Bubbles, and Explosions: a conference to honor John
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Salama, A., Arviset, C., Dowson, J., Hernández, J.,
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in the Internet Age, ESA SP-511, 3.
Verdugo, E., Talavera, A., Gomez de Castro, A.I.,
Henrichs, H., Geers, V., Wiersema, K., Searching for
Magnetic Fields in A-type Supergiants, 2003,
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Verdugo, E., Talavera, A., Gomez de Castro, A.I.,
Henrichs, H.F., Geers, V.C., Wiersema, K., Magnetic
Fields and Winds in A-type Supergiants, 2003,
International Conference on Magnetic Fields in O, B
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Wamsteker, W., Shustov, B., Barstow, M., Brosch, N.,
Cheng, F.-Z., Dennefeld, M., Dopita, M., Gomez de
Castro, A.I., Haubold, H., Kappelmann, N., Pagano,
I., Sahade, J., The HST Legacy at Midlife – What is
needed in the UV and can it be done?, 2003, Hubble
Science Legacy: Future Opt/UV astronomy from
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Wamsteker, W., [for WSO Implementation Committee],
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2003, Active Galactic Nuclei: from Central Engine to
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Science Operations and Data Systems Division
Refereed Journals, 2004
Belanger, G., Goldwurm, A., Goldoni, P., Paul, J.,
Terrier, R., Falanga, M., Ubertini, P., Bazzano, A.,
DelSanto, M., Winkler, C., Parmar, A., Kuulkers, E.,
Ebisawa, K., Roques, J.P., Lund, N., Melia, F.,
Detection of Hard X-Ray Emission from the Galactic
Nuclear Region with INTEGRAL, 2004, ApJ, 601,
L163.
Bianchi, S., Matt, G., Balestra, I., Guainazzi, M., Perola,
G.C., X-ray reprocessing in Seyfert Galaxies –
simultaneous XMM-Newton/BeppoSAX observations, 2004, A&A, 422, 65.
Bird, A.J., Barlow, E.J., Bassani, L., Bazzano, A.,
Bodaghee, A., Capitanio, F., Cocchi, M., DelSanto,
M., Dean, A.J., Hill, A.B., Lebrun, F., Malaguti, G.,
Malizia, A., Much, R., Shaw, S.E., Stephen, J.B.,
Terrier, R., Ubertini, P., Walter, R., The First
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Biviano, A., Metcalfe, L., McBreen, B., Altieri, B., Coia,
D., Kessler, M.F., Kneib, J.P., Leech, K., Okumura,
K., Ott, S., Perez-Martinez, R., Sanchez-Fernandez,
C., Schulz, B., An ISOCAM survey through
gravitationally lensing galaxy clusters – II. The
properties of infrared galaxies in the A2218 field,
2004, A&A, 425, 33.
Braga, J., Rothschild, R., Heise, J., Staubert, R.,
Remillard, R., DAmico, F., Jablonski, F., Heindl, W.,
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K., Favre, P., Gaber, M., Götz, D., Jaffe, T., Jennings,
D., Kretschmar, P., Landriu, D., Lecoeur, I., Lerusse,
L., Lock, T., Meharga, M., Mereghetti, S., Morisset,
N., Mowlavi, N., Paltani, S., Peachey, J., Pottschmidt,
K., O’Neel, B., Produit, N., Rohlfs, R., Sauvageon, A.,
Shaw, S., Türler, M., Diehl, R., Domingo, A.,
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Guest, S., Huygen, R., de Jonge, A., Mathieu, J.-J.,
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Solar and Solar-Terrestrial Missions Division
Refereed Journals, 2003
Solar and Solar-Terrestrial Missions Division
Refereed Journals, 2004
Bewsher, D., Parnell, C.E., Pike, C.D., Harrison, R.A.,
Dynamics of Blinkers, 2003, Sol. Phys., 215, 217-237.
Brynildsen, N., Maltby, P., Brekke, P., Fredvik, T.,
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32/6, 1097-1102.
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Idir, M., Kleider, J.-P., Lemaire, P., Monroy, E.,
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J.-L., Peacock, A., Schühle, U., van Hoof, C., Imageur
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2003, Journal de Physique IV, 108, 227-231.
Marsden, R.G., Fleck, B., The Solar Orbiter Mission,
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McIntosh, S.W., Fleck, B., Judge, P.G., Investigating the
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McIntosh, S.W., Fleck, B., Tarbell, T.D.,
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Solar and Solar-Terrestrial Missions Division
Proceedings and other Publications, 2003
Fleck, B., Marsden, R.G., Solar Orbiter – a mission
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A., Dhez, P., Fleck, B., Haenen, K., Idir, M., Kleider,
J.-P., Lefeuvre, E., Lemaire, P., Monroy, E., Muret, P.,
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2003, Innovative Telescopes and Instrumentation for
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Solar and Solar-Terrestrial Missions Division
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Brekke, P., Fleck, B., Nearly Eight Years of SOHO
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Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T.,
Schweitzer, G., Chaloupy, M., Space Weather Effects
on SOHO and its Role as a Space Weather Watchdog,
2004, Proc. 8th Spacecraft Charging Technology
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Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T.,
Schweitzer, H., Chaloupy, M., Space weather effects
on SOHO and its leading role in the early-wearning
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Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T.,
Schweitzer, H., Simonin, B., Space weather effects on
SOHO and its leading as a space weather watchdog,
2004, Multiscale Coupling of Sun-Earth Processes,
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Fleck, B., Eight Years of SOHO – Some Highlights,
2004, Solar Magnetic Phenomena, Proc.
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Fleck, B., Harrison, R.A., Marsden, R.G., WimmerSchweingruber, R., Summary of the Solar Orbiter
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Lundquist, L.L., Fisher, G.H., McTiernan, J.M.,
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Plasma Topography Through Chromospheric Oscillations, 2004, Proc. SOHO-13: Waves, oscillations and
other small-scale transient events in the solar
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Pickett, J.S., Santolik, O., Kahler, S.W., Masson, A.,
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Parrot, M., Decreau, P., Fazakerley, A., CornilleauWehrlin, N., Balogh, A., Andre, M., Multi-point
Cluster Observations of VLF Risers, Fallers, and
Hooks at and near the Plasmapause, 2004, Multiscale
processes in the Earth’s magnetosphere – From
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Munoz, E., Alvarez, J., Kleider, J.-P., Lemaire, P.,
Appourchaux, T., Fleck, B., Peacock, A., Richter, M.,
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2004, SpaceOps 2004 Proceedings, 3, 238.
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Space Telescope Operations Division
Refereed Journals, 2003
Aloisi, A., Savaglio, S., Heckman, T.M., Hoopes, C.G.,
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Annibali, F., Greggio, L., Tosi, M., Aloisi, A., Leitherer,
C., The Star Formation History of NGC 1705 – A
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AJ, 126, 2752.
Arribas, S., Colina, L., INTEGRAL Spectroscopy of
IRAS 17208-0014. Implications for the Evolutionary
Scenarios of Ultraluminous Infrared Galaxies, 2003,
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Battaner, E., Mediavilla, E., Guijarro, A., Arribas, S.,
Florido, E., Axisymmetrical gas inflow in the central
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A&A, 406, 765.
Bik, A., Lamers, H., Bastian, N., Panagia, N., Romaniello, M., Clusters in the Inner Spiral Arms of M51 –
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A&A, 397, 473.
Binette, L., Groves, B., Villar-Martin, M., Fosbury,
R.A.E., Axon, D.J., High-z nebulae – Ionization by
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Boeker, T., Stanek, R., van der Marel, R.P., Searching
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Bond, H.E., Henden, A., Levay, Z., Panagia, N., Sparks,
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Chiaberge, M., Gilli, R., Macchetto, F.D., Sparks, W.R.,
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D., Maciejewski, W., Marconi, A., Merrifield, M.,
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Strolger, L.-G., Riess, A.G., Dahlen, T., Livio, M.,
Panagia, N., Et, A.L., The Hubble Higher-z Supernova
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on SNIa Progenitor Models, 2004, ApJ, 613, 200.
Tuellmann, R., Rosa, M.R., An unusual high-ionization
nebula in NGC 55, 2004, A&A, 416, 243.
Tuellmann, R., Rosa, M.R., Elwert, T., Bomans, D.J.,
Ferguson, A.M.N., Dettmar, R.-J., Star formation in
gaseous galaxy halos. VLT-spectroscopy of extraplanar
H II-regions in NGC 55, 2004, A&A, 412, 69.
Varano, S., Chiaberge, M., Macchetto, F.D., Capetti, A.,
The nuclear radio-optical properties of intermediate
redshift FRII radio galaxies and quasars, 2004, A&A,
428, 401.
Villaver, E., Stanghellini, L., Shaw, R.A., The Low- and
Intermediate-Mass Stellar Population in the Small
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Zyl, L. van, Charles, P.A., Arribas, S., Naylor, T.,
Mediavilla, E., Hellier, C., The X-ray binary
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Space Telescope Operations Division
Proceedings and other Publications, 2004
Albrecht, R., HST Experience in Data Management, 2004,
Astronomische Nachrichten, 325, 590.
Albrecht, R., The Changing Role of the Telescope in
Astronomy, 2004, Developing Space Science World
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1, 363.
Allen, M., Genova, F., Arviset, C., Derriere, S., Didelon,
P., Garrington, S., Mann, R., Micol, A., Ochsenbein, F.,
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Ballester, P., Rosa, M.R., Instrument Modelling in
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Analysis Software and Systems (ADASS) XIII, ASP
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Bond, H.E., Henden, A., Levay, Z.G., Panagia, N.,
Sparks, W.B., Starrfield, S., Wagner, R.M., Corradi,
R.L.M., Munari, U., Hubble Space Telescope
Observations of the Light Echoes around V838
Monocerotis, 2004, Asymmetrical Planetary Nebulae
III: Winds, Structure and the Thunderbird, ASP
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Clampin, M., Sirianni, M., Hartig, G.F., Ford, H.C.,
Illingworth, G.D., Burmester, W., Martel, A.R., Riess,
A., Schrein, R.J., Sullivan, P.C., Inflight performance
of the Advanced Camera for Surveys, 2004, SPIE
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De Marchi, G., Sirianni, M., Gilliland, R., Bohlin, R.,
Pavlovsky, C., Jee, M., Mack, J., Marel, R. van der,
Boffi, F., Detector Quantum Efficiency and Photometric Zero Points of the ACS (Instrument Science
Report ACS 2004-08), 2004, Hubble Space Telescope
Instrument Science Report, ACS-08, 1.
Durand, D., Micol, A., Schade, D., Simard, L., Corbin,
M., Hook, R., Koekemoer, A., Donahue, M., WFPC2
Associations Pipeline, Publishing HST archives
within VO, 2004, Astronomical Data Analysis
Software and Systems (ADASS) XIII, 314, 209.
Fosbury, R.A.E., The Great Observatories Origins Deep
Survey – A VO Test Case?, 2004, Toward an
International Virtual Observatory, Proceedings of the
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Gómez-Álvarez, P., Mediavilla, E., Sánchez, S., Arribas,
S., Wisotzki, L., Wambsganss, J., Lewis, G., Muñoz,
J., Integral field spectroscopy of the gravitational lens
HE1104-1805, 2004, Astronomische Nachrichten,
325, 132.
Hook, R., Durand, D., Simard, L., Schade, D.,
Koekemoer, A., Corbin, M., Micol, A., HST/ACS
Associations, the Next Step after WFPC2, 2004,
Astronomical Data Analysis Software and Systems
(ADASS) XIII, 314, 62.
Kamp, I., Sammar, F., Circumstellar Disks around Young
Solar-Type Stars, 2004, Stars as Suns: Activity,
Evolution and Planets, IAU Symposium 219, 102.
Kerber, F., Rosa, M.R., Nave, G., Reader, J., Sansonetti,
C.J., Bristow, P., Lercher, G., New Insights from the
ST-ECF Lamp Project, 2004, ST-ECF Newsletter, 37,
5.
Maíz-Apellániz, J., Massive Young Clusters in the Local
Group, 2004, The Local Group as an Astrophysical
Laboratory, (Accepted for Publication).
Maíz-Apellániz, J., Massive Young Clusters, 2004, How
does the Galaxy work? A Galactic tertulia with Don
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Maíz-Apellániz, J., Supernova 2004dj in NGC 2403,
2004, IAU Circ., 8385, 1.
Maíz-Apellániz, J., CHORIZOS, a complete photometric
chi-square code, 2004, The three-dimensional
Universe with Gaia, (Accepted for Publication).
Maíz-Apellániz, J., Self-consistent distance determinations for Lutz-Kelker-limited samples, 2004, The
three-dimensional Universe with Gaia, (Accepted for
Publication).
Maíz-Apellániz, J., MULTISPEC, Crowded-Field Slitless Spectroscopy with HST, 2004, Planets to
Cosmology: Essential Science in Hubble’s Final
Years, (Accepted for Publication).
Maíz-Apellániz, J., Bond, H.E., Siegel, M.H., Lipkin, Y.,
Maoz, D., Ofek, E.O., Poznanski, D., SN 2004dj, a
supernova in a nearby young compact cluster, 2004,
JENAM 2004: The many scales of the Universe,
(Accepted for Publication).
Micol, A., Pierfederici, F., Benvenuti, P., Review of the
ASTROVIRTEL Experience at the end of its Three
Approved Cycles, 2004, Astronomical Data Analysis
Software and Systems (ADASS) XIII, 314, 197.
Modigliani, A., Rosa, M.R., Evaluation of Methods to
Locate Emission Lines From Calibration Lamps in 2D
Spectroscopic Data, 2004, Astronomical Data
Analysis Software and Systems (ADASS) XIII, ASP
Conference Proceedings, 314, 808.
Panagia, N., The Hubble Space Telescope – present and
future, 2004, ESA Bulletin, 118, 4.
Panagia, N., A Geometric Determination of the Distance
to SN 1987A and the LMC, 2004, IAU Colloquium
192 – Cosmic Explosions – Springer Proceedings in
Physics, 99, 585.
Perez-Torres, M.A., Marcaide, J.M., Alberdi, A., Ros, E.,
Guirado, J.C., Lara, L., Mantovani, F., Stockdale, C.,
Weiler, K.W., Diamond, P.J., Van Dyk, S.D.,
Lundqvist, P., Panagia, N., Shapiro, I.I., Sramek, R.A.,
High-resolution Radio Imaging of Young Supernovae,
2004, IAU Colloquium 192 – Cosmic Explosions –
Springer Proceedings in Physics, 99, 97.
Pierfederici, F., Dolensky, M., Micol, A., Pirenne, B.,
ASTROVIRTEL, Tools and Operations, 2004, Toward
an International Virtual Observatory, Proceedings of
the ESO/ESA/NASA/NSF Conference held in Garching, Germany, 10-14 June 2002. ESO Astrophysics
Symposia, 129.
Prada Moroni, P.G., Straniero, O., De Marchi, G.,
Paresce, F., White dwarf cosmochronology and M4,
2004, Memorie della Societa’ Astronomica Italiana,
75, 81.
Pérez, E., Maíz-Apellániz, J., Mas-Hesse, J.M., NGC
604, the Scaled OB Association (SOBA) Prototype,
2004, JENAM 2004: The many scales of the Universe,
(Accepted for Publication).
Quinn, P.J., Allen, M., Andrews, K., Boch, T., Bonnarel,
F., Derriere, S., Dolensky, M., Fernique, P., Hill, M.,
Leoni, M.C., Linde, A., Micol, A., Pirenne, B.,
Richards, A.M.S., Schaaff, A., Tissier, G., Walton,
N.A., Wicenec, A., The AVO Prototype, 2004,
publications
Astronomical Data Analysis Software and Systems
(ADASS) XIII, 314, 304.
Robberto, M., Stiavelli, M., Baggett, S.M., Hilbert, B.,
MacKenty, J.W., Kimble, R.A., Hill, R.J., Cottingham, D.A., Delo, G., Johnson, S.D., Landsman, W.,
Malumuth, E.M., Polidan, E.J., Russell, A.M.,
Waczynski, A., Wassell, E., Wen, Y., Haas, A.K.,
Montroy, J.T., Piquette, E.C., Vural, K., Cabelli, C.A.,
Hall, D.N.B., Selection of the infrared detectors for
Wide Field Camera 3 on the Hubble Space Telescope,
2004, Proc. SPIE ‘Focal Plane Arrays for Space
Telescopes’, 5167, 166.
Sirianni, M., Mutchler, M., Clampin, M., Ford, H.C.,
Illingworth, G.D., Hartig, G.F., van Orsow, D.,
Wheeler, T., Performance of the Advanced Camera
For Surveys CCDs after two years in orbit., 2004,
SPIE Proceedings, 5499, 173.
Tuairisg, S.Ó., Butler, R., Golden, A., Shearer, A., Voisin,
B., Micol, A., Automated reduction and analysis of
images from multiple data archives, 2004,
Astronomical Data Analysis Software and Systems
(ADASS) XIII, 314, 444.
Tuellmann, R., Rosa, M.R., Dettmar, R.-J., SOAP and
the Interstellar Froth, 2004, Extra-planar Gas, ASP
conference proceedings, (Accepted for Publication).
Van Dyk, S.D., Weiler, K.W., Sramek, R.A., Panagia, N.,
Stockdale, C., Lacey, C., Montes, M., Rupen, M., A
Decade of Radio and X-ray Observations of SN1993J,
2004, IAU Colloquium 192, Cosmic Explosions,
Springer Proceedings in Physics, 99, 3.
Voisin, B., Micol, A., Tuairisg, S.Ó., Butler, R., Golden,
A., Shearer, A., Using a Reversed Exposure Time
Calculator for Querying Uncalibrated Archives, 2004,
Astronomical Data Analysis Software and Systems
(ADASS) XIII, 314, 125.
Voisin, B., Micol, A., Tuairisg, S.Ó., Butler, R.F.,
Golden, A., Shearer, A., Simulating instruments for
mining uncalibrated archives, 2004, Optimizing
Scientific Return for Astronomy through Information
Technologies, held in Glasgow, 24 June 2004, 5493,
294.
Wiklind, T., Molecules in the Interstellar Medium, 2004,
Origin and Evolution of the Elements, Carnegie
Observatories Centennial Symposium IV, 4, 357.
Fundamental Physics Missions Division
Refereed Journals, 2003
Pollack, S.E., Jennrich, O., Stebbins, R.T., Bender, P.,
Status of LISA phase measurement work in the US,
2003, Class. Quantum Grav., 20, S193-S199.
Heinzel, G., Wand, V., Garcia, A., Jennrich, O., Braxmaier, C., Robertson, D., Middleton, K., Hoyland, D.,
Rudiger, A., Schilling, R., Johann, U., Danzmann, K.,
The LTP interferometer and phasemeter, 2004, Class.
Quantum Grav., 21, S581-S587.
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Chief Scientist
Refereed Journals, 2003
Duke, M.B., Foing, B.H., Preface to Proceedings of
COSPAR 2002 Moon Session, 2003, Adv. Space Res.,
31, 2291.
Dunkin, S.K., Grande, M., Casanova, I., Fernandes, V.,
Heather, D.J., Kellett, B., Muinonen, K., Russell, S.S.,
Browning, R., Waltham, N., Parker, D., Kent, B.,
Perry, C.H., Swinyard, B., Perry, A., Feraday, J.,
Howe, C., Phillips, K., McBride, G., Huovelin, J.,
Muhli, P., Hakala, P.J., Vilhu, O., Thomas, N.,
Hughes, D., Alleyne, H., Grady, M., Lundin, R.,
Barabash, S., Baker, D., Clark, P.E., Murray, C.D.,
Guest, J., DUston, L.C., Maurice, S., Foing, B.,
Christou, A., Owen, C., Charles, P., Laukkanen, J.,
Koskinen, H., Kato, M., Sipila, K., Nenonen, S.,
Holmstrom, M., Bhandari, N., Elphic, R., Lawrence,
D., Scientific rationale for the D-CIXS X-ray
spectrometer on board ESA’s SMART-1 mission to the
Moon, 2003, Planet. Space Sci., 51, 435.
Foing, B.H., Racca, G.D., Marini, A., Heather, D.J.,
Koschny, D., Grande, M., Huovelin, J., Keller, H.U.,
Nathues, A., Josset, J.L., Malkki, A., Schmidt, W.,
Noci, G., Birkl, R., Iess, L., Sodnik, Z., McManamon,
P., SMART-1 mission to the moon – Technology and
science goals, 2003, Adv. Space Res., 31, 2323.
Garcia-Alvarez, D., Foing, B.H., Montes, D., Oliveira, J.,
Doyle, J.G., Messina, S., Lanza, A.F., Rodono, M.,
Abbott, J., Ash, T.D., Baldry, I.K., Bedding, T.R.,
Buckley, D.A., Cami, J., Cao, H., Catala, C., Cheng,
K.P., Domiciano de Souza, A., Donati, J.F., Hubert,
A.-M., Janot-Pacheco, E., Hao, J.X., Kaper, L.,
Kaufer, A., Leister, N.V., Neff, J.E., Neiner, C.,
Orlando, S., OToole, S.J., Schaefer, D., Smartt, S.J.,
Stahl, O., Telting, J., Tubbesing, S., Simultaneous
optical and X-ray observations of flares and rotational
modulation on the RS CVn binary HR 1099 (V711
Tau) from the MUSICOS 1998 campaign, 2003, A&A,
397, 285.
Grande, M., Browning, R., Waltham, N., Parker, D.,
Dunkin, S.K., Kent, B., Kellett, B., Perry, C.H.,
Swinyard, B., Perry, A., Feraday, J., Howe, C.,
McBride, G., Phillips, K., Huovelin, J., Muhli, P.,
Hakala, P.J., Vilhu, O., Laukkanen, J., Thomas, N.,
Hughes, D., Alleyne, H., Grady, M., Lundin, R.,
Barabash, S., Baker, D., Clark, P.E., Murray, C.D.,
Guest, J., Casanova, I., DUston, L.C., Maurice, S.,
Foing, B., Heather, D.J., Fernandes, V., Muinonen, K.,
Russell, S.S., Christou, A., Owen, C., Charles, P.,
Koskinen, H., Kato, M., Sipila, K., Nenonen, S.,
Holmstrom, M., Bhandari, N., Elphic, R., Lawrence,
D., The D-CIXS X-ray mapping spectrometer on
SMART-1, 2003, Planet. Space Sci., 51, 427.
Shkuratov, Yu.G., Kreslavsky, M.A., Stankevich, D.G.,
Kaydash, V.G., Pinet, P., Shevchenko, V.V., Foing,
B.H., Josset, J.-L., The SMART-1 Mission – Photometric Studies of the Moon with the AMIE Camera,
2003, Solar System Reviews, 37, 251.
141
Shkuratov, Yuriy G., Stankevich, Dmitriy G., Kaydash,
Vadim G., Omelchenko, Vitaliy V., Pieters, Carle M.,
Pinet, Patrick C., Chevrel, Serge D., Daydou, Yves H.,
Foing, Bernard H., Sodnik, Zoran, Josset, Jean-Luc,
Taylor, Lawrence A., Shevchenko, Vladislav V.,
Composition of the lunar surface as will be seen from
SMART-1 – A simulation using Clementine data,
2003, J. Geophys. Res., 108, 1.
Volp, J., Foing, B., www.lunarexplorer.org – Educating
the general public, 2003, Adv. Space Res., 31, 2455.
Chief Scientist
Proceedings and other Publications, 2003
Boudin, N., Ruiterkamp, R., Foing, B.H., A survey of the
PAH electronic spectra and their search in the
Interstellar Medium, 2003, Astrophysics of Dust, May
26-30, 2003, 162.
Cox, N., Ehrenfreund, P., Cami, J., Kaper, L., Foing, B.,
Cordiner, M., Sarre, P., Snow, T., Salama, F., Carbon
chemistry and diffuse interstellar bands in the
Magellanic Clouds, 2003, Astrophysics of Dust, 43.
Ehrenfreund, P., Cami, J., Foing, B.H., Kaper, L., Cox,
N., Jimenez-Vincente, J., Salama, F., Sarre, P., Snow,
T., Maier, J.P., Magellanic Diffuse Interstellar Bands
and Carbon Chemistry, 2003, The Astrochemistry of
External Galaxies, 25th meeting of the IAU, Joint
Discussion 21, 21, 2.
Foing, B.H., Neiner, C., 2003, Observing stellar activity
from space, EAS Publications Series 9, 147.
Foing, B.H., ESA Cosmic Vision programme, 2003,
SF2A Proceedings Societe Francaise d’Astronomie et
Astrophysique, 4.
Foing, B.H., Racca, G.D., Marini, A., Grande, M.,
Huovelin, J., Josset, J.L., Keller, H.U., Nathues, A.,
Koschny, D., Malkki, A., ESA SMART-1 Mission to
the Moon, 2003, Recent Progress in Planetary
Exploration, 25th meeting of the IAU, Special Session
1, 35.
Garcia-Alvarez, D., Foing, B.H., Montes, D., Oliveira, J.,
Doyle, J.G., MUSICOS 98 Collaboration 2003,
MUSICOS 1998: Observations of Rotational
Modulation and Flares on the RS CVn Binary
HR1099, The Future of Cool-Star Astrophysics: 12th
Cambridge Workshop on Cool Stars, Stellar Systems,
and the Sun (2001 July 30 - August 3), Eds. A. Brown,
G.M. Harper and T.R. Ayres, (University of
Colorado), 2003, 12, 958-963.
Racca, G., Foing, B.H., A solar-powered visit to the
Moon. The SMART-1 mission, 2003, ESA Bulletin,
113, 14.
TenKate, I.L., Ruiterkamp, R., Botta, O., Lehmann, B.,
Gomez Hernandez, C., Boudin, N., Foing, B.H.,
Ehrenfreund, P., Simulations of Martian Surface and
Subsurface Processes, 2003, 34th Annual Lunar and
Planetary Science Conference, March 17-21, 2003,
League City, Texas, 1313.
Washuettl, A., Strassmeier, K.G., Foing, B., MUSICOS-
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98 Team 2003, MUSICOS Observations of the
Chromospherically Active Binary Star EI Eridani, The
Future of Cool-Star Astrophysics: 12th Cambridge
Workshop on Cool Stars, Stellar Systems, and the Sun
(2001 July 30 - August 3), Eds. A. Brown, G.M.
Harper and T.R. Ayres, (University of Colorado),
2003, 12, 1008-1013.
Chief Scientist
Refereed Journals, 2004
Crespo-Chacón, I., Montes, D., Fernández-Figueroa,
M.J., López-Santiago, J., GarcÍa-Alvarez, D., Foing,
B.H., High Temporal Resolution Spectroscopic
Observations of the Flare Star V1054 Oph, 2004,
Astrophysics and Space Science, 292/1, 697-703.
Foing, B.H., The case for the first Indian Robotic
Mission to the Moon, 2004, Current Science, 87/8,
1061-1065.
Head, J.W., Neukum, G., Jaumann, R., Hiesinger, H.,
Hauber, E., Carr, M., Masson, P., Foing, B.,
Hoffmann, H., Kreslavsky, M., Werner, S., Milkovich,
S., HRSC, C.I., Tropical to Mid-Latitude Glaciation
on Mars – Evidence for Snow and Ice Accumulation
and Flow in Mars Express HRSC Data, 2004, Nature,
(Accepted for Publication).
Kozyrovska, O., Korniichuk, O.S., Voznyuk, T.M.,
Lytvynenko, T.L., Rogutskyy, I.S., Mytrokhyn, O.V.,
Estrella-Lopis, V.R., Borodinova, T.I., Foing, B.H.,
Kordyum, V.A., Microbial community in a precursory
scenario of growing Tagetes patula in a lunar
greenhouse, 2004, Kosmichna nauka i technologiya,
11, 10.
Prinja, R.K., Rivinius, T., Stahl, O., Kaufer, A., Foing,
B.H., Cami, J., Orlando, S., Photospheric and stellar
wind variability in 949 Ori (B0 Ia), 2004, A&A, 418,
727-736.
Unruh, Y.C., Donati, J.F., Oliveira, J.M., Cameron, A.C.,
Catala, C., Henrichs, H.F., Johns-Krull, C.M., Foing,
B., Multisite observations of SU Aurigae, 2004,
MNRAS, 348, 1301-1320.
Chief Scientist
Proceedings and other Publications, 2004
Foing, B.H., 2004., Preface to The Proceedings of
Hawaii International Lunar Exploration Conference
2003, A.A.S./Space Age Publ. (Ed. S.M. Durst et al.),
531.
Foing, B.H., Racca, G.D., Marini, A., Grande, M.,
Huovelin, J., Josset, J.L., Keller, H.U., Nathues, A.,
Heather, D., Koschny, D., Malkki, A., ESA’s
SMART-1 Mission to the Moon – Goals, Status and
First Results, 2004, 35th Lunar and Planetary Science
Conference, March 15-19, 2004, League City, Texas,
LPI, 35, 1413.
Foing, B.H., Racca, G.D., Marini, A., Evrard, E.,
publications
Stagnaro, L., Almeida, M., Koschny, D., Frew, D.,
Zender, J., Heather, J., Grande, M., Huovelin, J.,
Keller, H.U., Nathues, A., Josset, J.L., Malkki, A.,
Schmidt, W., Noci, G., Birkl, R., Iess, L., Sodnik, Z.,
McManamon, P., ESA’s SMART-1 Mission Launched
To The Moon: Technology And Science Goals, Proc.
International Lunar Conference 2003, A.A.S./Space
Age Publ. (Ed. S.M. Durst et al.), 3.
Foing, B.H., Zegers, T.E., van Kan, M., Pischel, R.,
Martin, P., Jaumann, R., Hauber, E., Greeley, R.,
Hoffmann, H., Neukum, G., The HRSC CoInvestigator Team, Gusev Crater and Early Martian
History: Clues from Mars-Express and MGS Study.
Second Conference on Early Mars: Geologic,
Hydrologic, and Climatic Evolution and the
Implications for Life, LPI Publ., 8070.
Greeley, R., Thompson, S., Whelley, P., Neukum, G.,
Squyres, S., Sullivan, R.J., Rafkin, S.C., Michaels, T.,
Golombek, M.P., Arvidson, R., Foing, B.H., Richter,
L., Rongxing, L., Pinet, P., HRSC Science Team,
Athena Science Team, 2004, Wind Patterns at the
Mars Exploration Rover (MER) Sites Inferred from
Mars Express HRSC and MER Images, AGU Fall
Meeting 21, 5.
Racca, G.D., Foing, B.H., Brinkmann, J., de Bijl, J., di
Napoli, L., Estublier, D., Evrard, E., Grnagel, R.,
Lumb, R., Marini, A., Rumler, P., Stagnaro, L., van
Dooren, J., 2004, En Route To The Moon: SMART-1
Final Preparation, Launch And Early Flight. Proc.
International Lunar Conference 2003, A.A.S./Space
Age Publ. (Ed. S.M. Durst et al.), 213.
Zegers, T.E., Conan, Y.G., Foing, B.H., Noachian
Martian highlands; the habitat of ancient life?, 2004,
Proc. Third European Workshop on Exo-Astrobiology,
18-20 November 2003, Madrid, Spain, ESA SP-545,
313.
Zegers, T.E., Conan, Y.G., Foing, B.H., Geology of
Noachian Martian Highlands Surrounding the Gusev
Crater, 2004, 35th Lunar and Planetary Science
Conference, March 15-19, 2004, League City, Texas,
LPI, 1767.
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publications
Science Payload and Advanced Concepts Office
Refereed Journals, 2003
Acker, A., Neiner, C., Quantitative classification of WR
nuclei of planetary nebulae, 2003, A&A, 403, 659.
Bertuccio, G., Casiraghi, R., Maiocchi, D., Owens, A.,
Bavdaz, M., Peacock, A., Andersson, H., Nenonen, S.,
Noise Analysis of Gallium Arsenide Pixel X-Ray
Detectors Coupled to Ultra-Low Noise Electronics,
2003, IEEE Trans. Nucl. Sci., 50, 723.
Brammertz, G., Kozorezov, A.G., Wigmore, J.K.,
Hartog, R. den, Verhoeve, P., Martin, D., Peacock, A.,
Golubov, A.A., Rogalla, H., Energy-dependent kinetic
model of photon absorption by superconducting
tunnel junctions, 2003, J. Appl. Phys, 94, 5854.
Ellery, A., Kolb, C., Lammer, H., Parnell, J., Edwards,
H., Richter, L., Patel, M., Romstedt, J., Dickensheets,
D., Steele, A., Cockell, C., Astrobiological instrumentation for Mars – the only way is down, 2003,
International J. Astrobiology, 1, 365-380.
Gondoin, P., The corona of V390 Aurigae (HD 33798),
2003, A&A, 355, 364.
Gondoin, P., The corona of HD 223460 (HR 9024), 2003,
A&A, 409, 263.
Gondoin, P., Orr, A., Lumb, D., XMM-Newton
observation of the Seyfert 1 galaxy ESO 141-G55,
2003, A&A, 398, 967.
Gondoin, P., Orr, A., Lumb, D., Siddiqui, H., XMMNewton observation of the Seyfert 1 galaxy NGC
3227, 2003, A&A, 397, 883.
Gostilo, V., Owens, A., Bavdaz, M., Lisjutin, I., Peacock,
A., Sipila, H., Zatoloka, S., A comparison of the X-ray
performance of TlBr crystals grown by the
Bridgeman–Stockbarger and travelling molten zone
methods, 2003, Nucl. Instr. & Meth., A509, 47.
Lumb, D.H., Finoguenov, A., Saxton, R., Aschenbach,
B., Gondoin, P., Kirsch, M., Stewart, I., In-orbit
Vignetting Calibrations of XMM-Newton Telescopes,
2003, Experimental Astronomy, 15, 89.
Lumb, D.H., Rando, R., Peacock, A., Favata, F.,
Perryman, M.A.C., Focal plane cameras for ESA
optical astronomy missions, 2003, Nucl. Instr. &
Meth., A513, 112.
Neiner, C., Geers, V.C., Henrichs, H.F., Floquet, M.,
Fremat, Y., Hubert, A.-M., Preuss, O., Wiersema, K.,
Discovery of a magnetic field in the Slowly Pulsating
B star zeta Cassiopeia, 2003, A&A, 406, 1019.
Neiner, C., Henrichs, H.F., Floquet, M., Fremat, Y.,
Preuss, O., Hubert, A.M., Geers, V.C., Tijani, A.H.,
Nichols, J., Jankov, S., Rotation, pulsations and
magnetic field in V2052 Ophiuchi – a new He-strong
star, 2003, A&A, 411, 565.
Neiner, C., Hubert, A.-M., Fremat, Y., Floquet, M.,
Jankov, S., Preuss, O., Henrichs, H.F., Zorec, J.,
Rotation and magnetic field in the Be star omega
Orionis, 2003, A&A, 409, 275.
Neumann, D.M., Lumb, D.H., Pratt, G.W., Briel, U.G.,
The dynamical state of the Coma cluster with XMMNewton, 2003, A&A, 400, 811.
143
Nevalainen, J., Lieu, R., Bonamente, M., Lumb, D., Soft
X-Ray Excess Emission in Clusters of Galaxies
Observed with XMM-Newton, 2003, ApJ, 584, 716.
Owens, A., Bavdaz, M., Brammertz, G., Gostilo, V.,
Graafsma, H., Kozorezov, A., Krumrey, M., Lisjutin,
I., Peacock, A., Puig, A., Sipila, H., Zatokola, S., The
X-ray response of TlBr, 2003, Nucl. Instr. & Meth. A,
A497, 370.
Owens, A., Bavdaz, M., Brammertz, G., Gostilo, V.,
Haack, N., Kozorezov, A., Lisjutin, I., Peacock, A.,
Zatoloka, S., Hard X-ray spectroscopy using a small
format TlBr array, 2003, Nucl. Instr. & Meth. A, A497,
359.
Owens, A., Mosselmans, J., Peacock, A., Near K-edge
linear attenuation coefficients for amorphous and
crystalline GaAs, 2003, J. Radiation Physics and
Chemistry, 66, 1.
Reynolds, A.P., Bruijne, J.H.J. de, Perryman, M.A.C.,
Peacock, A., Bridge, C.M., Temperature determination via STJ optical spectroscopy, 2003, A&A, 400,
1209-1217.
Verhoeve, P., Brammertz, G., Martin, D., Peacock, A.,
Quasiparticle loss rates in Ta-based superconducting
tunnel junctions, 2003, Nucl. Instr. & Meth., 520, 246.
Verhoeve, P., Martin, D., Dordrecht, A. van, Verveer, J.,
Hartog, R. den, Peacock, A., 120-pixel array of superconducting tunnel junctions as spectro-photometer for
optical astronomy, 2003, Nucl. Instr. & Meth., 513,
206.
Science Payload and Advanced Concepts Office
Proceedings and other Publications, 2003
Absil, O., den Hartog, R., Erd, C., Gondoin, P.,
Kaltenegger, L., Fridlund, M., Rando, N., Wilhelm,
R., GENIESIM – The GENIE Simulation Software,
2003, Proc. ‘Towards other Earths’, ESA SP-539,
317.
Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A.,
Jupiter Microsat Explorer Programme, 2003, 5th IAA
Conference on Low-Cost Planetary Missions, ESA
SP-542, 189.
Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A.,
The Jupiter Microsat Explorer Programme, 2003, 37th
ESLAB Symp., 2-4 December 2003, ESA SP-543, 17.
Bavdaz, M., Peacock, A., X-ray Optics – new
technologies at ESA, 2003, SPIE Proceedings –
X-Ray and Gamma-Ray Telescopes and Instruments
for Astronomy, 4851, 421.
Bavdaz, M., Peacock, A., Laan, T. van der, Parmar, A.,
The XEUS – approaches to mission design, 2003,
SPIE Proceedings – X-Ray and Gamma-Ray
Telescopes and Instruments for Astronomy, 4851, 396.
Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A.,
Venus Microsat Explorer Programme, an ESA
Technology Reference Mission, 2003, Proc. 5th IAA
conference on low-cost planetary missions, ESA
SP-542, 73.
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Bertrand, R., Del Bianco, A., Harnisch, B., Jessberger,
E.K., Peuser, P., Romstedt, J., Rost, D., Schneider, K.,
Weber, I., A minituarized laser instrument for
chemical and mineralogical in-situ analysis on
planetary surfaces, 2003, Geophysical Research
Abstracts, 5, EAE03-A-05861.
Erd, C., Owens, A., Brammertz, G., Lumb, D., Bavdaz,
M., Peacock, A., Nenonen, S., Andersson, H.,
Measurements of the quantum efficiency and
depletion depth in gallium-arsenide detectors, 2003,
SPIE Proceedings – X-Ray and Gamma-Ray
Detectors and Applications IV, 4784, 386.
Falkner, P., Erd, C., Highly Integrated Payload Suites and
Related Data Link Requirements, 2003, ISWS –
International SpaceWire Seminar 2003, 1, 25.
Falkner, P., Erd, C., Kraft, S., Peacock, T., Remote
Sensing Instrument Suite for Planetary Exploration,
2003, Geophysical Research Abstracts, 5, 12462.
Falkner, P., Romstedt, J., Verhoeve, P., Peacock, A.,
Instrumentation for in-situ measurements on the
surface of Mercury, 2003, Geophysical Research
Abstracts, 5, 12557.
Fridlund, M., Gondoin, P., The Darwin Mission, 2003,
SPIE Proceedings – Interferometry in Space, 4852,
394.
Gondoin, P., Absil, O., Fridlund, M., Erd, C., Hartog, R.
den, Rando, N., Glindemann, A., Koehler, B.,
Wilhelm, R., Karlsson, A., Labadie, L., Mann, I.,
Peacock, A., Richichi, A., Sodnik, Z., Tarenghi, M.,
Volonte, S., The Darwin Ground-based European
Nulling Interferometry Experiment (GENIE), 2003,
SPIE Proceedings – Interferometry for Optical
Astronomy II, 4838, 700.
Gondoin, P., Absil, O., den Hartog, R., Kaltenegger, L.,
Eiroa, C., Erd, C., Fridlund, M., Karlsson, A.,
Peacock, A., Sodnik, Z., Volonte, S., Wilhelm, R.,
Schoeller, M., Glindemann, A., The Ground-based
European Nulling Interferometry Experiment
(Darwin-GENIE), 2003, Proc. ‘Towards Other
Earths’, ESA SP-539, 121.
Gondoin, P. XMM-Newton observation of the Seyfert 1
galaxy IC4329A, 2003, Active Galactic Nuclei: from
Central Engine to Host Galaxy, ASP Conf. Series 290,
97.
Grard, R., Falkner, P., The Bepi Colombo Mission to
Mercury, 2003, Geophysical Research Abstracts, 5,
10727.
Hartog, R. den, Absil, O., Kaltenegger, L., Gondoin, P.,
Wilhelm, R., Fridlund, M., Could GENIE detect Hot
Jupiters?, 2003, Proc. ‘Towards Other Earths’, ESA
SP-539, 399.
Hartog, R. den, Kozorezov, A., Verhoeve, P., Martin, D.,
Noise in a Quatratran-based detector – a comparison
with Superconducting Tunnel Junctions, 2003, SPIE
Proceedings – X-Ray and Gamma-Ray Telescopes and
Instruments for Astronomy, 4851, 1002.
Hartog, R. den, Owens, A., Kozorezov, A., Bavdaz, M.,
Peacock, A., Gostilo, V., Lisjutin, I., Zatoloka, S.,
Optimization of array design for TlBr imaging
publications
detectors, 2003, SPIE Proceedings – X-Ray and
Gamma-Ray Telescopes and Instruments for
Astronomy, 4851, 922.
Martin, D., Verhoeve, P., Hartog, R. den , Bruijne, J. de,
Reynolds, A., Dordrecht, A. van, Verveer, J., Peacock,
A., 12x10 pixels superconducting tunnel junction
array based spectrophotometer for optical astronomy,
2003, SPIE Proceedings – Instrument Design and
Performance for Optical/Infrared Ground-based
Telescopes, 4841, 805.
Miyaji, T., Griffiths, R.E., Lumb, D., Sarajedini, V.,
Siddiqui, H., XMM-Newton view of the Hubble Deep
Field-North and Groth-Westphal strip regions, 2003,
Astron. Nachtrichten, 324, 24.
Neiner, C., Appourchaux, T., Global fitting of power
spectra of solar-like stars, 2003, 2nd Eddington
Workshop: Stellar structure and habitable planet
finding, ESA SP-538, 373.
Neiner, C., Hubert, A.-M., Floquet, M., Seismology of
Be stars, 2003, 2nd Eddington Workshop: Stellar
structure and habitable planet finding, ESA SP-538,
369.
Owens, A., Peacock, A., Bavdaz, M., Progress in
Compound Semiconductors, 2003, SPIE Proceedings
– X-Ray and Gamma-Ray Telescopes and Instruments
for Astronomy, 4851, 1059.
Rando, N., Murphy, E., Falkner, P., Peacock, A., The
Laser Altimeter for Planetary Exploration (LAPE),
2003, Geophysical Research Abstracts, 5, 12399.
Torkar, K., Riedler, W., Romstedt, J., Jeszensky, H.,
Steller, M., Arends, H., The MIDAS atomic force
microscope for cometary dust – technical highlights
and future perspectives, 2003, Geophysical Research
Abstracts, 5, EAE-A-07246.
Verhoeve, P., Hartog, R. den, Kozorezov, A., Martin, D.,
Dordrecht, A. van, Wigmore, J.K., Peacock, A.,
Integration time dependence of tunnel noise and
energy resolution of superconducting tunnel junctions,
2003, SPIE Proceedings – Instrument Design and
Performance for Optical/Infrared Ground-based
Telescopes, 4841, 141.
Science Payload and Advanced Concepts Office
Refereed Journals, 2004
Brammertz, G., Peacock, A., Verhoeve, P., Martin, D.,
Venn, R., Optical photon detection in Al Superconducting Tunnel Junctions, 2004, Nucl. Instr. &
Meth., A 520, 508.
Gondoin, P., X-ray spectroscopy of the W UMa-type
binary 44 Bootis, 2004, A&A, 426, 1035.
Gondoin, P., The corona of HD 199178 (V 1794 Cygni),
2004, A&A, 413, 1095.
Gondoin, P., X-ray spectroscopy of the W UMa-type
binary VW Cephei, 2004, A&A, 415, 1113.
Gondoin, P., Orr, A., Siddiqui, H., XMM-Newton observations of the dwarf elliptical galaxy NGC 3226,
2004, A&A, 420, 905.
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publications
Kozorezov, A., Wigmore, K., Owens, A., den Hartog, R.,
Peacock, A., The effect of carrier diffusion on the
characteristics of semiconductor imaging arrays,
2004, Nucl. Instr. & Meth., A531, 52.
Lumb, D.H., Bartlett, J.G., Romer, A.K., Blanchard, A.,
Burke, D.J., Collins, C.A., Nichol, R.C., Giard, M.,
Marty, P., Nevalainen, J., Sadat, R., Vauclair, S., The
XMM-NEWTON Omega Project – I. The X-ray
Luminosity-Temperature Relation at z>0.4, 2004,
A&A, 420, 383.
Martin, D.D.E., Peacock, A., Verhoeve, P., FernandezLeon, A., Glass, B., Maehlum, G., 64-channel preamplifier ASICs for superconducting tunnel junction
readout, 2004, Nucl. Instr. & Meth., A 520, 570-573.
Martin, D.D.E., Verhoeve, P., Peacock, A., Dordrecht, A.
van, Verveer, J., Hijmering, R., A 12x10 pixels
superconducting tunnel junction array based spectrophotometer for optical astronomy, 2004, Nucl. Instr. &
Meth., A 520, 512-515.
Owens, A., XANES fingerprinting – a technique for
investigating CCD surface structures and measuring
dead layer thicknesses, 2004, Nucl. Instr. & Meth.,
A526, 391.
Owens, A., Peacock, A., Compound Semiconductor
Radiation Detectors, 2004, Nucl. Instr. & Meth.,
A513, 18.
Rando, N., Lumb, D., Bavdaz, M., Martin, D., Peacock,
A., Space science applications of cryogenic detectors,
2004, Nucl. Instr. & Meth., A-522, 62.
Scelsi, L., Maggio, A., Peres, G., Gondoin, P., X-ray
spectroscopy of the Hertzsprung-gap giant 31 Com,
observed with XMM-Newton, 2004, A&A, 413, 643.
Vaitkus, J., Gostilo, V., Jasinskaite, R., Mekys, A.,
Owens, A., Tamosiunas, S., Zatoloka, S., Zindulis, A.,
Investigation of Degradation of Electrical and
Photoelectrical Properties in TlBr Crystals, 2004,
Nucl. Instr. & Meth., A531, 192.
Science Payload and Advanced Concepts Office
Proceedings and other Publications, 2004
Absil, O., Hartog, R. den, Gondoin, P., Fabry, P.,
D’Arcio, L., Wilhelm, R., Gitton, P., Puech, F.,
Influence of atmospheric turbulence on the
performance and design of GENIE, 2004, Proc. SPIE
Conference 2004 Glasgow, Astronomical Telescopes
& Instrumentation, 5491, 1257.
Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A.,
The Jupiter Minisat Explorer – A Technology
Reference Mission, 2004, Proceedings of 37th ESLAB
Symposium, ESA SP 543, 17.
Bavdaz, M., Lumb, D., Peacock, A., Beijersbergen, M.,
Kraft, S., Development of X-ray optics for the XEUS
Mission, 2004, Proceedings SPIE, 5539, 104.
Bavdaz, M., Lumb, D.H., Peacock, A., XEUS Mission
Reference Design, 2004, Proceedings SPIE, 5488,
530.
Bavdaz, M., Lumb, D.H., Peacock, A., Beijersbergen,
145
M., Kraft, S., Status of X-ray Optics Development for
the XEUS Mission, 2004, Proceedings SPIE, 5488,
829.
Bavdaz, M., Peacock, A., Tomaselli, E., Beijersbergen,
M., Collon, M., Flyckt, E., Fairbend, R., Boutot, J.-P.,
Progress at ESA on High Energy Optics Technologies,
2004, SPIE Proceedings, 5168, 136.
Beijersbergen, M., Kraft, S., Bavdaz, M., Lumb, D.,
Guenther, R., Collon, M., Mieremet, A., Fairbend, R.,
Peacock, A., Development of X-ray pore optics novel
high-resolution silicon millipore optics for XEUS and
ultralow mass glass micropore optics for imaging and
timing, 2004, Proceedings SPIE, 5539, 104.
Beijersbergen, M., Kraft, S., Gunther, R., Mieremet, A.,
Collon, M., Bavdaz, M., Lumb, D.H., Peacock, A.,
Silicon Pore Optics – novel lightweight highresolution X-ray optics developed for XEUS, 2004,
Proceedings SPIE, 5488, 868.
Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A.,
Venus MicroSat Explorer Programme, an ESA
Technology Reference Mission, 2004, Proc.
Workshop on Planetary Probe Atmosphric Entry and
Descent Trajectory Anaylsis and Science, ESA
SP-544, 275.
Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A.,
Venus Entry Probe, an ESA Technology Reference
Mission, 2004, Tool and Technologies for future
planetary exploration, Proc. 37th ESLAB Symposium,
2-4 December 2003, ESA SP-543, 23.
Brammertz, G., Verhoeve, P., Martin, D., Peacock, A.,
Venn, R., Future optical detectors based on Al
superconducting tunnel junctions, 2004, Proceedings
SPIE, 5499, 269.
D’Arcio, L.A., Karlsson, A., Search for Extraterrestrial
Planets – The DARWIN Mission, 2004, Proc. 5th
International Conference on Space Optics – ICSO
2004, ESA SP-554, 213.
D’Arcio, L.A., Karlsson, A., Gondoin, P., Use of OPD
modulation techniques in stellar interferometry, 2004,
SPIE Proceedings New frontiers in stellar
interferometry, 5491, 851.
Falkner, P., ESA’s Technology Reference Studies, 2004,
8th ESA Workshop on Advanced Space Technologies
for Robotics and Automation, ‘ASTRA 2004’, 8, 155.
Falkner, P., Atzei, A., van den Berg, M., Schiele, A.,
Microprobes for in-situ measurements on Planetray
surfaces and Atmospheres, 2004, Geophysical
Research Abstracts, 6, 5458.
Falkner, P., Erd, C., Kraft, S., Highly Integrated Payload
Suites for Planetary Exploration, 2004, Geophysical
Research Abstracts, 6, 6241.
Falkner, P., Rando, N., Murphy, E., Update on Laser
Altimeters for Planetary Exploration, 2004,
Geophysical Research Abstracts, 6, 05450.
Gondoin, P., Absil, O., Hartog, R. den, Wilhelm, R.,
Gitton, P., D’Arcio, L., Fabry, P., Puech, F., Fridlund,
M., Schoeller, M., Glindemann, A., Bakker, E.,
Karlsson, A., Peacock, A., Volonte, S., Paresce, F.,
Richichi, A., Darwin-GENIE: a nulling instrument at
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the VLTI, 2004, Proc. SPIE Conference 2004
Glasgow, Astronomical Telescopes & Instrumentation,
5491, 775.
Hartog, R. den, Absil, O., Gondoin, P., D’Arcio, L.,
Fabry, P., Kaltenegger, L., Wilhelm, R., Gitton, P.,
Puech, F., Fridlund, M., The simulated detection of
low-mass companions with GENIE, 2004, Proc.
SPIE, New Frontiers in Stellar Interferometry, 5491,
160.
Hughes, G.W., Macdonald, M., McInnes, C.R., Atzei, A.,
Falkner, P., Analysis of a Solar Sail Mercury Sample
Return Mission, 2004, Proceedings IAC, Vancouver
2004, CDROM.
Jones, L.R., Maughan, B.J., Ebeling, H., Scharf, C.,
Perlman, E., Lumb, D., Gondoin, P., Mason, K.O.,
Cordova, F., Priedhorsky, W.C., An XMM and
Chandra view of massive clusters of galaxies to z=1,
2004, Clusters of Galaxies: Probes of Cosmological
Structure and Galaxy Evolution, Carnegie Observatories Astrophysics Series, Pasadena, California,
USA, 25.
Kaltenegger, L., Karlsson, A., Requirements on the
stellar rejection for the DARWIN mission, 2004,
Proceedings SPIE, Glasgow, Astronomical Telescopes
& Instrumentation, 5491, 275.
Karlsson, A., Wallner, O., Perdigues Armengol, J., Absil,
O., Three Telescope Nuller, based on multi beam
injection into single mode waveguide, 2004, SPIE –
Astronomical Telescopes, Glasgow 2004, 5491, 831.
Kilter, M., Micropropulsion Assessment for DARWIN,
2004, Micropropulsion Assessment for DARWIN, 5.2,
145.
Kilter, M., Karlsson, A., Micropropulsion Technologies
for the European high-precision Formation Flying
Interferometer DARWIN, 2004, Proc. 4th
International Spacecraft Propulsion Conference, ESA
SP-555, 85.
Lumb, D.H., Instrumentation Package for ESAs (XEUS)
X-ray Early Universe Spectroscopy Mission, 2004,
Proceedings SPIE, 5165, 1.
Lumb, D.H., XEUS Mission – Detector Spacecraft
Instrumentation Package, 2004, Proceedings SPIE,
5488, 539.
Lyngvi, A., Falkner, P., Atzei, A., Renton, D., van den
Berg, M.L., Peacock, A., ESA’s Technology Reference Studies, 2004, Proceedings IAC, Vanouver 2004,
IAC, IAC-04-U.1.06.
Lyngvi, A., Falkner, P., Peacock, A., The Interstellar
Heliopause Probe, 2004, Proceedings of Tools and
Technologies for Future Planetary Exploration, 37th
ESLAB Symposium, ESA SP-543, 11-17.
Lyngvi, A., Falkner, P., Peacock, A., The Interstellar
Heliopause Probe, 2004, Proceedings IAC, Vancover
2004, paper number IAC-04-Q.2.A.06.
Owens, A., Alha, L., Andersson, H., Bavdaz, M.,
Brammertz, G., Helariutta, K., Peacock, A., Ldmsd,
V., Nenonen, S., The effects of proton induced
radiation damage on compound semiconductor X-ray
detectors, 2004, SPIE, 5501, 403.
publications
Owens, A., Andersson, H., Campbell, M., Lumb, D.,
Nenonen, S., Tlustos, L., GaAs arrays for X-ray
spectroscopy, 2004, SPIE, 5501, 241.
Renton, D.C., Falkner, P., Peacock, A., Deimos Sample
Return Technology Reference Mission, 2004, Proc.
‘Tools and Technologies for Future Planetary
Exploration’, 37th ESLAB Symposium, ESA SP-543,
3.
Romstedt, J., Torkar, K., Riedler, W., Jeszenszky, H.,
Arends, H., Butler, B., Biezen, J. van der, Steller, M.,
MIDAS – First Results from Rosetta’s Commissioning Phase, 2004, Geophysical Research Abstracts,
6, EGU04-A-01202.
Stankov, A., Favata, F., Characterization of the field
population in the Pleiades cluster region for
EDDINGTON, 2004, Proc. 2nd Eddington workshop:
Stellar structure and habitable planet finding, ESA
SP-538, 425.
Verhoeve, P., Martin, D., Brammertz, G., Hijmering, R.,
Peacock, A., Photon Counting Cryogenic detectors for
Ground-based and Space Telescopes, 2004, Proc. 5th
International Conference on Space Optics (ICSO
2004), ESA SP-554, 781.
Wallner, O., Perdigues Armengol, J.M., Karlsson, A.,
Multi-Axial Single-Mode Beam Combiner, 2004,
SPIE, Glasgow, 2004, 5491, 798.
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Stagiaire Research Reports and Theses, 2003
Civeit, T. (Observatoire de Meudon, DESS Outils et
Systemes de l’astronomie et de l’espace), Measurement of zonal winds velocity in Titan’s stratosphere
with VLT/UVES observations, RSSD supervisor
O. Witasse.
Coia, D. (Univ. Coll. Dublin), Infrared Observations of
Clusters of Galaxies, Ph.D. Thesis, Faculty of Science,
National University of Ireland, RSSD co-supervisor L.
Metcalfe (with Prof. B. McBreen at U.C.D.).
Cordonnier, R. VILSPA RSSD Network Statistics Tool
Stage Report, RSSD supervisor C. Arviset.
Malloreau, S. (Observatoire de Meudon, DESS Outils et
Systemes de l’astronomie et de l’espace), Huygens
radar data analysis and test campaign preparation,
RSSD supervisor J.-P. Lebreton.
Sierra, M. (Spanish Trainee), Extended Source Analysis
with the RGS aboard XMM-Newton, RSSD
supervisor A. Pollock.
Sierra, M. (Spanish Trainee), The Use of SNRs as
Contamination Monitors for the RGS aboard XMMNewton, RSSD supervisor A. Pollock.
Stagiaire Research Reports and Theses, 2004
Aguardo, D. (U. Complutense Madrid), Refinement of
the EPIC count rate estimation in PHS tools, Practices
at ESAC report, Faculty of Mathematics, RSSD
supervisor M. Kirsch, co-supervisor A.I. Gomez de
Castro at UCM (Universidad Complutense de
Madrid).
Barbarisi, I. VOSpec: a Tool to display and superimpose
spectra from VO compatible Spectra Server, RSSD
supervisor C. Arviset.
Brooks Pollock, E. (University College London),
Simultaneous Analysis of Galaxy Clusters with the
RGS and EPIC Instruments aboard XMM-Newton,
RSSD supervisor A. Pollock.
Carter, J. (YGT), Review of the XMM-Newton SAS
Online Guides and Online Support Structure, RSSD
supervisor A. Pollock.
Carter, J. (YGT), Order Separation and PI Selection
Regions in the Analysis of XMM-Newton RGS data,
RSSD supervisor A. Pollock.
Couturier-Doux, S. (DESS Outils et Systemes de
l’astronomie et de l’espace, Paris-Meudon), Contribution to the operations planning & software tests for the
Camera onboard the SMART-1 Mission, RSSD
supervisor B.H. Foing.
Esquej, M.P. (U. Complutense Madrid), Energy calibration verification of the EPIC cameras with SNR
observations, Practices at ESAC report, Faculty of
Physical Sciences, Astrophysics and Atmosphere
Sciences department, RSSD supervisor M. Kirsch,
co-supervisor J. Zamorano at UCM (Universidad
Complutense de Madrid).
Jimenez-Bailon, E. (U. Autonoma de Madrid), Star
147
Formation in Low Luminosity Active Galactic Nuclei,
2004, Ph.D. Thesis report, published January 2004,
defended March 2004. 1999-2003, RSSD supervisor
M.Santos-Lleo, co-supervisor: M. Mas-Hesse at
LAEFF-INTA, Spain.
Jimenez-Esteban, F.M. An Infrared Study of Galactic
OH/IR Stars, Ph.D. Thesis, June 2004, RSSD
supervisor P. Garcia-Lario, co-supervisor D. Engels at
Hamburg Observatory.
Jiménez Luján, F. (U. Complutense de Madrid), Análisis
de datos de XMM-Newton de galaxias espirales
cercanas: Fuentes de rayos X y emisión extensa de
M83, September 2004 ‘XMM-Newton data analysis
of nearby spiral galaxies: X-ray sources and extended
emission in M83’, Practices at ESAC report, Faculty
of Physical Sciences, Astrophysics and Atmosphere
Sciences department, RSSD supervisor M. Ehle,
co-supervisor J. Zamorano at UCM (Universidad
Complutense de Madrid).
Leyder, J.-C. (Université de Liège), Analysis of
Messenger – The NASA mission to Mercury, May
2004, Master Thesis report, Université de Liège,
Faculty of Applied Sciences, supervisors ESTEC
J. Romstedt, N. Rando, supervisor Univ. Liège,
J.-P. Swings.
Luna, R. Busqueda de Bandas Difusas en Envolturas
Circunestelares, Ph.D. Thesis, November 2004, RSSD
supervisor: P. Garcia-Lario, co-supervisor: M.A.
Satorre at U. Alcoy.
Sarmiento Ares, F. (U. Vigo), System Study of a
Planetary Data Handling and Archiving System, State
of the Art and Outlook, July 2004, RSSD supervisor
J. Zender.
Schoenherr, G. (U. Bonn), Scientific X-ray data analysis
of the Crab supernova remnant, RSSD supervisor
A. Pollock.
Seoane Purrinos, L. (U. Vigo), JMAPPS Client-Server
Interactive Application for browsing the Mars
Surface, RSSD supervisor J. Zender.
Simoes, F. (Portuguese trainee), Subsurface Permittivity
Probe to detect Water/Ice in Planetary Environments,
RSSD supervisors R. Trautner, A. Chicarro, R. Grard.
Stebe, A. ESAC Science Archive Team and Computer
Support Group WebPortal Improvements Stage
Report, RSSD supervisor C. Arviset.
Suarez, O. (U. Vigo), Stellar Evolution in the Post-AGB
Stage, Ph.D. Thesis, May 2004, RSSD supervisor:
P. Garcia-Lario, co-supervisor: M. Manteiga at
U. Vigo.
Vacher, G. VILSPA Science Archive Team and Computer
Support Group WebPortal Design and 1st
Implementation Stage Report, RSSD supervisor
C. Arviset.
van Kan, M. (U. Utrecht), Geologic Evolution of the
Gusev Crater region on Mars – using Mars Express,
MGS and Mars Odyssey, August 2004, Master Thesis
report, Faculty of Earth Sciences Utrecht, RSSD
supervisors T. Zegers, B.H. Foing, co-supervisor
C.G. Langereis at Utrecht U.
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ANNEX 3
Seminars and Colloquia
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150
Seminars held at ESTEC
2003
17 January
An Observational View on the Variability of Disks
around Pre-Main Sequence Stars
C. Eiroa, Astronomy Missions Division
31 January
NASA’s Far-IR/Submillimeter Roadmap Missions:
SAFIR and SPECS
D. Leisawitz, NASA Goddard Space Flight Center
14 February
Cluster Results and Future Multi-Satellite Mission
Concepts
H. Laakso, Solar and Heliospheric Missions Division
28 February
Luminosity Functions of Young Stellar Clusters
T. Prusti, Astronomy Missions Division
seminars and colloquia
26 September
The Young Earth: A Different Planet
T. Zegers, Planetary Missions Division
9 October
ALMA – the Atacama Large Millimetre Array
W. Wild, SRON
24 October
X-ray Emission and Origin of Runaway Stars
E. Meurs, Dunsink Observatory
7 November
What is XMM Telling us About the Unified Scenario
for Active Galactic Nuclei?
M. Guinazzi, VILSPA
5 December
XMM-Newton Observations of Globular Clusters
D. Carrett, CESR
2004
14 March
Remote Sensing of Planetary Minerals and Ices by
NIR Imaging Spectroscopy, Objects and Methods
S. Doute, Laboratoire de Planetologie de Grenoble
28 March
The Transition from AGB Stars to Planetary Nebulae
as seen by ISO
P. Garcia, VILSPA
25 April
Measurig the Gas Content of Galaxies: the Effects of
a Higher H2 Formation Rate
P. Papadopolous, University of Leiden
23 May
Optical and Infrared Interferometry
A. Quirrenbach, University of Leiden
19 June
Measurement of Polarisation of the Cosmic Microwave Background
L. Piccirillo, Cardiff University
4 July
Halo Gas in Spiral Galaxies
F. Fraternali, ASTRON
11 July
Venus: Mysteries of the ‘Forgotten Planet’
D.V. Titov, Max Planck Inst. für Aeronomie
12 September
Magellan Mission to Venus: What Did we Learn about
Venus’ Surface Tectonics and History?
P. Rosenblatt, Belgium Royal Observatory
9 January
Darwin and Exoplanets: Disks, Exoplanets and
Darwin
M. Fridlund, Astronomy Missions Division
23 January
Early Mission Highlights from the Spitzer Space
Telescope
A. Marsdon, Astronomy Missions Division
6 February
Dust and Gas Content of Quasars and Galaxies in the
Early Universe
P. Cox, Université Paris Sud
19 February
Imaging and Photometry of Mars: Strategy Toward a
Multiscale Understanding of the Optical Properties
P. Pinet, Observatoire Midi-Pyrenées
19 March
Architecture and Concepts for Optical Sensors for
Planetary Exploration and Space-Based Astronomy
H. Michaelis, DLR
2 April
Gas in Elliptical Galaxies and Bulges
S. Peletier, University of Groningen
23 April
The Great Observatories Origins Deep Survey: First
Science Results
B. Mobasher, STScI
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seminars and colloquia
151
7 May
The Origin of Dust at High Redshift
L. Dunne, University of Wales
Colloquia held at ESTEC
4 June
On the Cassini-Huygens Mission
J.-P. Lebreton, Planetary Missions Division
9 May
The Search for the Complete History of the Cosmos
N. Turok, Cambridge University
2 July
LISA – A Mission to Detect and Observe Gravitational Waves
O. Jennrich, Fundamental Physics Missions Division
21 November
Drilling the Chicxulum Dinosaur Killer Crater – How
a Meteorite Impact Changed our World
J. Smit, Vrije Universitaet
9 July
ESO Research Facilities in Chile
C. Alloin, ESO
2004
10 September
The Pioneer Anomaly: the Data, its Meaning and a
Possible Test
M.N. Nieto, Los Alamos
7 October
Latest Results from Spitzer – An Infrared View of
Galaxy Evolution
H. Dole, Université Paris Sud
22 October
Massive Star Nucleosynthesis in Cygnus X
J. Knoedlseder, CESR
5 November
The High Resolution Stereo Camera Experiment on
Mars Express: First Geoscientific Results
R. Jaumann, German Aerospace Centre
12 November
Dynamics and Instability in Jupiter’s Outer Magnetosphere
D. Southwood, Director of Science
19 November
Examples of Studies of the Current Sheet Dynamics
by Cluster
P. Louarn, CESR
3 December
Giant Planets’ Aurora: A Comparative View
J.-C. Gerard, Université Liège
2003
5 March
The Paradoxes of Evolution: Inevitable Humans but in
a Lonely Universe
S. Conway-Morris, Cambridge University
18 June
Archeoastronomy: Stonehenge and Beyond
C. Ruggles, Leicester University
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ANNEX 4
Acronyms
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154
AAS
AAT
ACES
ACS
ADS
AFM
AGB
AGN
AGU
AIV
AKR
ALICE
ALMA
AMIE
AO
APT
APXS
ASCA
ASI
ASIC
ASPOC
ATR
AU
AWG
BeppoSAX
BHE
BLR
CAA
CBRF
CCD
CDS
CDS
CdTe
CELIAS
CEPHAG
CERN
CESR
CETP
CFHT
CIR
CIS
CIVA
CMB
CME
CMOS
CNES
CNR
CNRS
acronyms
American Astronomical Society
Anglo-Australian Telescope
Atomic Clock Ensemble in Space
Advanced Camera for Surveys (HST)
Astrophysics Data System (NASA)
Atomic Force Microscope
Asymptotic Giant Branch
Active Galactic Nuclei
American Geophysical Union
Assembly, Integration & Verification
Auroral Kilometric Radiation
Rosetta Orbiter UV imaging spectrometer
Atacama Large Millimetre Array
Asteroid Moon micro-Imager Experiment
(SMART-1)
Announcement of Opportunity
Astronomers’ Proposal Tool
Alpha-Proton-X-ray Spectrometer (Rosetta)
Advanced Satellite for Cosmology and
Astrophysics (Japan)
Italian Space Agency
Application Specific Integrated Circuit
Active Spacecraft Potential Control (Cluster)
Attenuated Total Reflection
Astronomical Unit
Astronomy Working Group (ESA)
Satellite per Astronomia in raggi X
(Italy/The Netherlands)
banded hiss emission
Broad Line Region
Cluster Active Archive
Cosmic Background Radiation Field
Charge Coupled Device
Coronal Diagnostics Spectrometer (SOHO)
Centre de Données astronomiques de
Strasbourg
cadmium telluride
Charge, Element and Isotope Analysis
System (SOHO)
Centre d’Etude des Phenomenes Aleatoires
et Geophysiques (France)
Centre Européen de Recherches Nucléaires
(France)
Centre d’Etude Spatial des Rayonnements
(France)
Centre d’Etudes des Environments Terrestres
et Planetaires (France)
Canadian-French-Hawaiian Telescope
Corotating Interaction Region; Composite IR
Spectrometer (Cassini)
Cluster Ion Spectrometry
Comet Infrared and Visible Analyser
(Rosetta)
Cosmic Microwave Background
Coronal Mass Ejection
Complementary Metal Oxide Semiconductor
Centre National d’Etudes Spatiales
Consiglio Nazionale della Ricercha (Italy)
Centre National de la Recherche Scientifique
(France)
CNSA
COBE
Co-I
CONSERT
COPUOS
COROT
COS
COSAC
COSIMA
COSPAR
COSPIN
COSTEP
CP
CPM
CR
CS
CSA
CSDS
CsI
CSIRO
CTIO
CTTS
CV
CVF
CXB
D-CIXS
Chinese National Space Administration
Cosmic Background Explorer (NASA)
Co-Investigator
Comet Nucleus Sounding Experiment by
Radiowave Transmission (Rosetta)
Committee for the Peaceful Use of Outer
Space (United Nations)
COnvection, ROtation and planetary Transits
Cosmic Origins Spectrograph (HST)
Comet Sampling and Composition
Experiment (Rosetta)
Cometary Secondary Ion Mass Analyser
(Rosetta)
Committee on Space Research
Cosmic Ray & Solar Charged Particles
Investigation (Ulysses)
Comprehensive Measurements of the SupraThermal and Energetic Particles Populations
(SOHO)
Charge Parity
Chemical Propulsion Module
(BepiColombo)
Carrington Rotation
Control Centre
Canadian Space Agency
Cluster Science Data System
caesium iodide
Commonwealth Scientific & Industrial
Research Organisation (Australia)
Cerro Tololo Inter-American Observatory
Classical T-Tauri Star
Cataclysmic Variable
Circular Variable Filter (ISOCAM)
Cosmic X-ray Background
DSRI
DUO
Demonstration of a Compact Imaging X-ray
Spectrometer (SMART-1)
Directorate of Human Spaceflight,
Microgravity & Exploration (ESA)
Directorate of Scientific Programmes (ESA)
Digital Elevation Model
Observatoire de Paris, Département Spatial
Diffuse Interstellar Band
Descent Imager/Spectral Radiometer
(Huygens)
Deutsches Zentrum für Luft- und Raumfahrt
Data Processing Centre
Data Processing Unit
Disturbance Reduction System (LISA
Pathfinder)
Double Star Data System
Deep Space Network
Digital Signal Processor; Double Star
Programme (China)
Danish Space Research Institute
Dark Universe Observatory (NASA)
EAS
ECF
EC
EDI
EFW
European Astronomical Society
European Coordinating Facility
European Commission
Electron Drift Instrument (Cluster)
Electric Field & Wave experiment (Cluster)
D/HME
D/SCI
DEM
DESPA
DIB
DISR
DLR
DPC
DPU
DRS
DSDS
DSN
DSP
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acronyms
EGS
EGSE
EIRO
EIT
ELAIS
ELF
EM
EP
EPAC
EPDP
EPIC
EPS
EQM
ERNE
ESA
ESAC
ESLAB
ESO
ESOC
ESRIN
ESRO
ESTEC
EUSO
EUV
EW
FEEP
FES
FET
FGM
FGS
FGS-TF
FIRST
155
European Geophysical Society
Electrical Ground Support Equipment
European Intergovernmental Research
Organisation
Extreme UV Imaging Telescope (SOHO)
European Large Array ISO Survey
Extremely Low Frequency
Electrical Model, Engineering Model
Equivalence Principle
energetic particle instrument (Ulysses)
Electric Propulsion Diagnostic Package
(SMART-1)
European Photon Imaging Camera
(XMM-Newton)
European Physical Society
Electrical Qualification Model
Energetic and Relativistic Nuclei and
Electron experiment (SOHO)
European Space Agency
European Space Astronomy Centre (ESA)
European Space Laboratory (former name of
SSD/RSSD)
European Southern Observatory
European Space Operations Centre,
Darmstadt (Germany)
ESA’s Documentation and Information
Centre (Italy)
European Space Research Organisation
European Space Research and Technology
Centre, Noordwijk
(The Netherlands)
Extreme Universe Space Observatory
Extreme Ultra-Violet
equivalent width
FOS
FOV
FP
FPAG
FPGA
FSRQ
FTE
FTS
FUSE
FUV
FWHM
Field Emission Electric Propulsion
Fine Error Sensor
field effect transistor
Flux Gate Magnetometer
Fine Guidance Sensor (HST)
Fine Guidance Sensor-Tunable Filter (JWST)
Far Infrared and Submillimetre Space
Telescope (now Herschel)
Flight Model
Finnish Meteorological Institute
Faint Object Camera (HST)
FOcal Reducer/low dispersion
Spectrograph 2 (ESO VLT)
Faint Object Spectrograph (HST)
Field of View
Fabry-Pérot
Fundamental Physics Advisory Group (ESA)
Field Programmable Gate Array
Flat Spectrum Radio Quasar
Flux Transfer Event
Fourier Transform Spectrometer
Far-UV Spectroscopic Explorer (NASA)
Far-Ultraviolet
Full Width at Half Maximum
GaAs
GC
Gallium Arsenide
Galactic Centre
FM
FMI
FOC
FORS2
GDASS
GENIE
GIADA
GLIMPSE
GMOS
GMT
GOLF
GONG
GOODS
GR
GRB
GSE
GSFC
GSP
GSTP
GTO
HASI
HCS
HCSS
HEB
HEIC
HEMT
HEW
HFI
HGA
HIFI
HIPS
HPOC
HR
HRC
HRSC
HRTS
HSC
HST
IAA
IAC
IAU
IBIS
ICC
IDT
IFE
IFS
ILEWG
ILT
ILWS
IMEWG
IMF
IMPACT
INT
INMS
Gaia Data Access & Analysis Study
Ground-based European Nulling
Interferometer Experiment
Grain Impact Analyser and Dust
Accumulator (Rosetta)
Galactic Legacy IR Mid-Plane Survey
Extraordinaire
Gemini Multi-Object Spectrograph
Greenwich Mean Time
Global Oscillations at Low Frequency
(SOHO)
Global Oscillation Network Group
Great Observatories Origins Deep Survey
General Relativity
Gamma Ray Burst
Ground Support Equipment
Goddard Space Flight Center (NASA)
General Studies Programme (ESA)
General Support & Technology Programme
(ESA)
Geostationary Transfer Orbit
Huygens Atmospheric Structure Instrument
Heliospheric Current Sheet
Herschel Common Science System
Hot Electron Bolometer
Hubble ESA Information Centre
High Electron Mobility Transistor
Half Energy Width
High Frequency Instrument (Planck)
High-Gain Antenna
Heterodyne Instrument for Far-IR (Herschel)
Highly Integrated Payload Suite
Huygens Probe Operations Centre
Hertzsprung-Russell
High-Resolution Channel (HST/ACS)
High Resolution Stereo Camera (Mars
Express)
High-Resolution Telescope & Spectrograph
Herschel Science Centre
Hubble Space Telescope
Instituto de Astrofísica de Andalucía
Instituto de Astrofisica de Canarias
International Astronomical Union
Integral imager
Instrument Control Centre
Instrument Dedicated Team
Instrument Front-End
Integral Field Spectroscopy
International Lunar Exploration Working
Group
Instrument-Level Test
International Living With a Star programme
International Mars Exploration Working
Group
Initial Mass Function; Interplanetary
Magnetic Field
In-situ Measurements of Particles And CME
Transients (STEREO)
Isaac Newton Telescope
Ion & Neutral Mass Spectrometer (Cassini)
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INTA
IOA
IPAC
IR
IRAM
IRAS
IRF-U
ISAS
ISDC
ISGRI
ISM
ISO
ISOC
ISSI
IST
ISWT
ITC
ITT
IUE
IUPAP
IWF
acronyms
Instituto Nacional de Técnica Aerospacial
(Spain)
Institute of Astronomy (Cambridge, UK)
Infrared Processing Analysis Center
Infrared
Institut de Radioastronomie Millimétrique
Infrared Astronomy Satellite
Institute for Space Physics-Uppsala (Sweden)
Institute of Space and Astronautical Science
(Japan), now part of JAXA
Integral Science Data Centre
Integral Soft Gamma Ray Imager
Interstellar Medium
Infrared Space Observatory (ESA)
Integral Science Operations Centre
International Space Science Institute, Bern
(Switzerland)
Instrument Science Team
Integral Science Working Team
International Institute for Geo-Information
Science and Earth Observation (NL)
Invitation to Tender
International Ultraviolet Explorer
International Union of Pure and Applied
Physics
Space Research Institute Graz (A)
JAXA
JCMT
JEM-X
JIVE
JPL
JSOC
JWG
JWST
Japan Aerospace & Exploration Agency
James Clerk Maxwell Telescope
Integral X-ray monitor
Joint Institute for VLBI in Europe
Jet Propulsion Laboratory (NASA)
Joint Science Operation Centre (Cluster)
Joint Working Group
James Webb Space Telescope (formerly
NGST)
KATE
X/Ka-band Telemetry & Telecommand
Experiment (SMART-1)
Kitt Peak National Observatory (USA)
KPNO
LAEFF
LAP
LASCO
LBV
LDAP
LECS
LET
LETG
LFI
LIRG
LISA
LIST
LMC
LMXB
LOI
LP
LPCE
Laboratory for Space Astrophysics and
Fundamental Physics
Langmuir Probe (Rosetta)
Large Angle Spectroscopic Coronagraph
(SOHO)
Luminous Blue Variable
Lightweight Directory Access Protocol
Low Energy Concentrator Spectrometer
(BeppoSAX)
Low Energy Telescope (Ulysses)
Low-Energy Transmission Grating
Low Frequency Instrument (Planck)
Luminous IR Galaxy
Laser Interferometer Space Antenna
LISA International Science Team
Large Magellanic Cloud
Low Mass X-ray Binary
Luminosity Oscillation Imager (SOHO)
LISA Pathfinder
Laboratoire de Physique et Chemie, de
l’Environnement (France)
LPF
LPSP
LPV
LTE
LTP
LWS
MAPPS
MCP
MDI
MDPU
MECS
MER
MHD
Microscope
MIDAS
MIP
MIRI
MIRO
MLH
MLT
MMO
MOC
MOLA
MOS-CCD
MoU
MPAE
MPE
MPI
MPIA
MPIK
MPO
MRR
MSE
MSSL
MUPUS
MUSICOS
MXB
MXU
NAC
NASA
NED
NFI
NGST
NHSC
NICMOS
NIRSpec
LISA Pathfinder
Laboratoire de Physique Stellaire et
Planétaire (France)
Long-Period Variable
Local Thermal Equilibrium
LISA Technology Package
Long Wavelength Spectrometer (ISO)
Mapping & Planning for Payload Science
(Venus Express)
Microchannel Plate
Michelson Doppler Imager (SOHO)
Model Data Processing Unit
Medium-Energy Concentrator Spectrometer
(BeppoSAX)
Mars Exploration Rover (NASA)
Magnetohydrodynamics
MICROSatellite à traînée Compensée pour
l’Observaton du Principe d’Equivalence
(CNES)
Micro-Imaging Dust Analysing System
(Rosetta)
Mutual Impedance Probe (Rosetta)
Mid-IR Instrument (JWST)
Microwave Instrument for the Rosetta
Orbiter (Rosetta)
Mid-Latitude Hiss
Magnetic Local Time
Mercury Magnetospheric Orbiter
(BepiColombo)
Mission Operations Centre
Mars Observer Laser Altimeter
Metal Oxide Semiconductor Charge Coupled
Device
Memorandum of Understanding
Max-Planck-Institut für Aeronomie
Max-Planck-Institut für Extraterrestrische
Physik
Max-Planck Institut (Germany)
Max-Planck-Institut für Astronomie
Max-Planck-Institut für Kernphysik
Mercury Planetary Orbiter (BepiColombo)
Mission Risk Review
Mercury Surface Element (BepiColombo)
Mullard Space Science Laboratory (UK)
Multi-Purpose Sensors for Surface and
Subsurface Science (Rosetta)
Multi-Site Continuous Spectroscopy
Medium X-ray Band
Mask Exchange Unit
Narrow Angle Camera (OSIRIS)
National Aeronautics & Space
Administration (USA)
NASA Extragalactic Database
Narrow Field Instrument (BeppoSAX)
Next Generation Space Telescope (now
James Webb Space Telescope)
NASA Herschel Science Center
Near-Infrared Camera and Multi-Object
Spectrometer (HST)
Near-IR Spectrometer (JWST)
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acronyms
NIS
NLR
NOAO
157
normal incidence spectrometer
Narrow Line Region
National Optical Astronomy Observatories
(US)
Nordic Optical Telescope
National Radio Astronomy Observatory
(USA)
National Space Science Data Center (at
GSFC, USA)
National Synchotron Light Source (USA)
New Technology Telescope
NRAO/VLA Sky Survey
RMOC
ROLIS
ROMAP
Osservatorio Astronomico di Trieste
Observatoire de Haute-Provence
Optical Monitor (XMM-Newton)
Optical Monitor Camera (Integral)
Optical and Spectroscopic Remote Imaging
System (Rosetta)
RTG
SAS
PWG
Photodetector Array Camera and
Spectrometer (Herschel)
Polycyclic Aromatic Hydrocarbon
parsec
Photon Counting Detector
Payload Definition Document
Particle Detector Front End
Phoswich Detector System
Principal Investigator
(ISO)PHOT Interactive Analysis
Planetary Ion Camera (BepiColombo MPO)
Passivated Implanted Planar Silicon
Payload Module
Pre-Main Sequence
Planetary Nebula (plural: PNe)
Payload Operations Service (Mars Express)
Permittivity Probe (SESAME on Rosetta)
parts per million
Public Relations
Project Scientist
Planetary Science Archive
Project Scientist Team; Payload Support Team
Point Spread Function
Planck Science Office
Permitivity, Waves and Altimetry (part of
HASI on Huygens)
Payload Working Group
QED
QM
QPD
QPO
QSO
Quantum Electrodynamics
Qualification Model
Quadrant Photodiode
Quasi Periodic Oscillation
Quasi Stellar Object
R&D
RAID
RAL
RF
RGS
Research and Development
Redundant Array of Inexpensive Disks
Rutherford Appleton Laboratory (UK)
Radio Frequency
Reflection Grating Spectrometer (XMMNewton)
Reuven Ramaty High Energy Solar
Spectroscopic Imager (NASA)
NOT
NRAO
NSSDC
NSLS
NTT
NVSS
OAT
OHP
OM
OMC
OSIRIS
PACS
PAH
pc
PCD
PDD
PDFE
PDS
PI
PIA
PICAM
PIPS
PLM
PMS
PN
POS
PP
ppm
PR
PS
PSA
PST
PSF
PSO
PWA
RHESSI
ROSINA
ROSITA
RPC
RSI
RSOC
RSSD
SAFIR
SAO
SAp/Saclay
SAX
SBC
SCAM
SciSIM
SCOS
SCR
SDT
SED
SEM
SEP
SEPM
SEPP
SEPT
SESAME
SEST
SETI
SFH
SFR
SIMBA
SIMBAD
SIR
SIRTF
SIS
SLP
SM
SMART
SMC
SMEX
SMOG
SN
Rosetta Mission Operations Centre
Rosetta Lander Imaging System
RoLand Magnetometer & Plasma Monitor
(Rosetta)
Rosetta Orbiter Spectrometer for Ion and
Neutral Analysis (Rosetta)
Roentgen Survey with an Imaging Telescope
Array
Rosetta Plasma Consortium
Radio Science Investigation
Rosetta Science Operations Centre
Research and Scientific Support Department
(ESA)
Radioisotope Thermoelectric Generator
Single Aperture Far-IR (NASA)
Smithsonian Astrophysical Observatory
(USA)
Service d’Astrophysique (Commissariat à
l’Energie Atomique; Saclay, France)
Scientific Analysis Software (XMMNewton); Science Analysis Subsystem
(XMM-Newton)
Satellite per Astronomia in raggi X
(Italy/The Netherlands)
Solar-Blind Channel (ACS/HST)
Superconducting Camera
Science Simulator
Spacecraft Operations System
Software Change Request
Science Definition Team
Spectral Energy Distribution
Scanning Electron Microscope
solar energetic particle; solar electric
propulsion; solar electron proton
Solar Electric Propulsion Module
(BepiColombo)
Solar Electric Primary Propulsion
Solar Energetic Particle Telescope
(STEREO)
Surface Electric, Seismic and
Acoustic Monitoring Experiment (Rosetta)
ESO sub-mm telescope
Search for Extra-Terrestrial Intelligence
Star Formation History
Star Formation Rate
SEST Imaging Bolometer Array
Set of Identifications, Measurements and
Bibliography on Astronomical Data
Stream Interacting Region
Space Infrared Telescope Facility (NASA;
now Spitzer)
Superconductor-Insulator-Superconductor
Segmented Langmuir Probe
Servicing Mission (Hubble)
Small Mission for Advanced Research in
Technology (ESA)
Small Magellanic Cloud
Small Explorer (NASA)
Survey of Molecular Oxygen in the Galaxy
(SMART-1)
Supernova
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SNR
SOC
SOHO
SOI
SOS
SOT
SOWG
SPC
SPECS
SPEDE
SPI
SPICAM
SPIRE
SPR
SQUID
SRON
SRR
SRV
SSAC
SSC
SSD
SSP
SSWG
ST
ST-ECF
STAFF
STEREO
STIS
STJ
STOC
STScI
SUMER
SWAN
SWAS
SWS
SWT
SVM
SXB
SXT
SZ
TAC
TNG
ToO
TPF
TRACE
TRIP
acronyms
Supernova Remnant
Science Operations Centre; self-organising
criticality
Solar and Heliospheric Observatory
Saturn Orbit Insertion
Silicon-on-Sapphire
Science Operations Team
Science Operations Working Group
Science Programme Committee (ESA)
Submillimeter Probe of the Evolution of
Cosmic Structure (NASA)
Spacecraft Potential, Electron & Dust
Experiment (SMART-1)
Integral spectrometer
Mars Express UV Spectrometer
Spectral and Photometric Imaging Receiver
(Herschel)
Software Problem Report
Superconducting Quantum Interference
Device
Space Research Organisation Netherlands
System Requirement Review
Semi-Regular Variable
Space Science Advisory Committee (ESA)
Survey Science Consortium (XMM-Newton)
Space Science Department (ESA), now
RSSD
Surface Science Package (Huygens and
Rosetta)
Solar System Working Group (ESA)
Science Team; Space Technology (NASA)
Space Telescope European Coordinating
Facility (Germany)
Spatio-Temporal Analyis of Field
Fluctuations (Cluster)
Solar-Terrestrial Relations Observatory
(NASA)
Space Telescope Imaging Spectrograph
Superconducting Tunnel Junction
Science & Technology Operations
Coordination
Space Telescope Science Institute
Solar UV Measurements of Emitted
Radiation (SOHO)
Solar Wind Anisotropies (SOHO)
Submillimeter Wave Astronomy Satellite
(NASA)
Short Wavelength Spectrometer (ISO)
Science Working Team
Service Module
Soft X-ray Band
Soft X-ray Telescope (Yohkoh)
Sunyaev-Zeldovich Effect
Time Allocation Committee
Telescopio Nazionale Galileo
Target of Opportunity
Terrestrial Planet Finder (NASA)
Transition Region & Coronal Explorer
(NASA)
Technology Readiness and Implementation
Plan
TRL
TRM
TRP
TRS
TSI
Technology Readiness Level
Technology Reference Mission
Technology Research Programme (ESA)
Technology Reference Study
Total Solar Irradiance
UCB
UCLA
ULIRG
URSI
USNO
UT
UV
UVCS
UVES
University of California Berkeley (USA)
University of California Los Angeles (USA)
Ultra-Luminous IR Galaxy
Union Radio Scientifique Internationale
US Naval Observatory
Universal Time
Ultraviolet
Ultra-Violet Coronal Spectrometer (SOHO)
Ultraviolet-Visual Echelle Spectrograph
(ESO VLT)
UV Imaging Spectrometer (Cassini)
UVIS
VILSPA
VIMOS
VIMS
VIRGO
VIRTIS
VLA
VLBI
VLF
VLT
VLTI
VO
VSOC
VTT
WAC
WBD
WEC
WFC
WFPC
WHISPER
WHT
WIYN
WMAP
WWW
XEUS
Villafranca Satellite Tracking Station
VLT Visible Multi-Object Spectrograph
(ESO VLT)
Visual IR Mapping Spectrometer (Cassini)
Variability of Irradiance and Gravity
Oscillations (SOHO)
Visible Infra Red Thermal Imaging
Spectrometer (Rosetta)
Very Large Array
Very Long Baseline Interferometry
Very Low Frequency
Very Large Telescope
Very Large Telescope Interferometer (ESO
VLT)
Virtual Observatory
Venus Express Science Operations Centre
Vacuum Tower Telescope
Wide Angle Camera (OSIRIS on Rosetta)
Wide Band Data (Cluster)
Wave Experiment Consortium (Cluster)
Wide-Field Camera (HST)
Wide-Field Planetary Camera (HST)
Waves of High Frequency and Sounder for
Probing of Density by Relaxation (Cluster)
William Herschel Telescope
Wisconsin Indiana Yale NOAO (US)
Wilkinson Microwave Anisotropy Probe
(NASA)
World Wide Web
XSA
X-ray Evolving Universe Spectroscopy
mission (ESA)
X-ray Multi-Mirror Mission (ESA); now
XMM-Newton
XMM-Newton Science Archive (ESA)
YGT
YSO
Young Graduate Trainee
Young Stellar Object
ZAMS
Zero Age Main Sequence
XMM