GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
Wrap-up: Science Tools
EGRET >300 MeV
What we got done at the meeting
What needs to get done
Getting to DC1
Who is doing what?
Seth Digel
HEPL/Stanford Univ.
18 July 2003
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
What got done at the meeting
• Talks
– You heard them, too
• Working sessions-type topics
– Observation simulation
• Simulated data sets, variable (periodic) sources, handling multiple
classes of events; Claudia Cecchi will be coordinator of obs. sim.
science tools with Jim Chiang
– Graphics – AIDA & Plplot
• Round table forum. We’ve talked ourselves out of AIDA (too much
overhead just for plotting) and raw Plplot, may be talking ourselves into
ROOT
– HOOPS – how-to
• How went?
– Data layer – core developer-level discussion: what it can do for you
• Binned event class (data type) implemented; need one or two more for
GOODI to be useful for the DC1 science tools
– D1 & D2 details – like how to communicate with them
• How went? Beowulf at SLAC has been rediscovered with Julie
McEnery’s help
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
What got done (2)
– Source detection
• Variable/moving sources, tradeoffs in response functions, computation
time; N-dim Bayesian blocks, ICA, wavelet, other alternative methods
for source detection?
– Interstellar emission model
– D3
• Parameterization of response functions, interface work
– Data products
• ICD between IOC and SSC; L0.5 data
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
What needs to get done
• [Out of our hands] Derivation of LAT response functions
– Parameterizing them, studying them for likelihood analysis, will be
in our hands
– Biggest concern in terms of the end-to-end goal of DC1
– For DC1 goals (at least as far as science tools go), we could get by
with GLAST25 response functions and our high-level simulators
• D1& D2
– For D1, need to converge on contents. Sensible suggestion:
include the variables that are input to the classification trees
[although then would have to include ‘flattening’ information]
– For development, keeping up on the LAT side is the issue
• Likelihood tool
– Source model definition, commanding, user documentation
– Wilks’ theorem?
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
What needs to get done (2)
• Observation simulation
– obsSim & Light Simulator cross check
– Basically close to where we want to be for DC1; livetime <> real
time; read D2 output
• Map generation
– Can DS9 do what we want? Maybe with exposure calculation utility
• L1 pipeline
– Waiting for OPUS code; in the meantime can work on the scripts
that we’ll feed opus
– We’ll want to provide input regarding the ‘Monte Carlo Truth’ sky
• Core
– Graphics – what tools need it for DC1?
– HOOPS and GOODI – really should be in there; don’t foresee that
this will be a problem
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
Penultimate slide
• What do we need from DC1?
– Technical aspects
– Also to get software in a state where non-developer users can use it
– install it, understand it, run it
• For collaboration meeting in September, need to introduce the
DC1-era science tools
• WBS says that we will have a month of testing our tools in
advance of release (pipeline → D1 & D2→ likelihood analysis
(with exposure calc.)→ (pseudo)science
• ‘Release’ means more than a tag
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
Who is doing what?
•
Core – Science Tools Core
–
–
–
–
•
•
•
•
•
•
D1 database and supporting utilities – DB & related utils
D2 pointing/livetime/mode history – DB & related utils
D3 response functions, form and interface – Davis & ?
O1 orbit and attitude simulation – Obs. sim
O2 & interim simulated data set – Obs. sim
A1 & supporting tools
–
–
–
–
•
Development environment, release manager
HOOPS (OO PIL)
GOODI – data representation, i/o
Plplot/AIDA
Ready
Signs of
progress
Signs of life
Moribund
Functional prototype likelihood analysis – Chiang, Source detection
Source model definition - ?
Exposure calculation? – Chiang, Source detection
Response function visualization - ?
Map generation – counts, exposure, intensity, model - ?
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GLAST LAT Project
Ground Software Workshop, July 15-18, 2003
Components of the Standard Analysis
Environment
Pulsar
ephem. (D4)
Level 0.5
Level 1 (D1)
Pointing/livetime
history (D2)
Alternative source
for testing highlevel analysis
Event
display (UI1)
Pulsar period
search (A4)
Ephemeris
extract (U11)
Arrival time
correction (U10)
Pulsar phase
assign (U12)
Pulsar
profiles (A3)1
Data extract
(U1)
Pt.ing/livetime
extractor (U3)
Alternative for
making additional
cuts on alreadyretrieved event
data
Observation
simulator (O2)
Data subselection (U2)
Pt.ing/livetime
simulator (O1)
Pt.ing/livetime
extractor (U3)
Exposure
calc. (U4)
Source model
def. tool (U7)
Catalog
Access (U9)
Likelihood (A1)
Astron.
catalogs (D6)
Src. ID (A2)
Interstellar em.
model (U5)
Map gen
(U6)
IRFs (D3)
IRF visualization (U8)
GRB LAT DRM
gen. (U14)
1
This tool also performs periodicity tests and
the results can be used to refine ephemerides
2 These tools can also take as input binned data
from other instruments, e.g., GBM; the
corresponding DRMs must also be available.
LAT Point source
catalog (D5)
GRB event
binning (A5)
GRB spectral
analysis (A8)2
GRB rebinning
(A6)2
User Interface aspects of the standard
analysis environment, such as
GRB unbinned
Image/plot display (UI2), Command
spectral analysis (A9) line interface & scripting (UI4), and
GUI & Web access (UI5) are not
GRB spectral-temporal shown explicitly.
modeling (A10)
GRB visualization (U13)
GRB temporal
analysis (A7)2
14 Sept 2002
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