Cave
Microclimate
Data
Retrieval
and
Volumetric
Mapping,
2009
Atacama
Desert
Expedition,
Chile,
Earth­Mars
Cave
Detection
Project:
Explorers
Club
Flag
Report
(Flag
#
52)
Submitted
27
October
2009
J.
Judson
Wynne1,2,
Timothy
N.
Titus3,
Guillermo
Chong
Diaz4,
Christina
Colpitts5,
W.
Lynn
Hicks6,
Denise
Hill7,
Daniel
W.
Ruby8,
and
Cristian
Tambley9
1SETI
Institute,
Carl
Sagan
Center,
Mountain
View,
CA;
2Colorado
Plateau
Research
Station
(U.S.
Geological
Survey
affiliate),
Northern
Arizona
University,
Flagstaff;
3U.S.
Geological
Survey,
Astrogeology
Science
Center,
Flagstaff,
AZ;
4Departamento
de
Ciencias
Geológicas,
Universidad
Católica
del
Norte,
Antofagasta,
Chile;
5Research
Support
Group,
Inc.,
Torrington,
CT;
6Glynn
Immediate
Care,
Southeast
Georgia
Health
System,
Brunswick,
GA;
7Mutual
Aid
Response
Service,
San
Francisco,
CA;
8Fleischmann
Planetarium
and
Science
Center,
University
of
Nevada‐Reno,
NV;
9Campo
Alto,
Santiago,
Chile.
Corresponding
author:
[email protected]
1.0
Introduction
Caves
on
Earth
are
characterized
by
microclimates
that
often
support
extremophillic
organisms
and
evidence
of
extinct
life
forms.
On
Mars,
because
caves
are
features
that
may
offer
protection
from
harsh
surface
conditions,
these
features
are
important
in
the
search
for
life.
Additionally,
caves
may
serve
as
locations
for
the
establishment
of
habitation
pods
for
astronaut
crews.
Before
Martian
caves
can
be
targeted
for
exploration,
we
must
(1)
develop
an
understanding
of
terrestrial
cave
thermal
behavior
and
(2)
determine
how
thermal
properties
influence
the
thermal
signature
associated
with
the
entrance.
Ultimately,
this
may
enable
us
to
differentiate
caves
from
non‐cave
anomalies,
as
well
large
from
small
subterranean
features.
This
is
a
critical
step
in
the
targeting
process.
Identifying
actual
caves
with
significant
volume
will
be
the
highest
priority
targets
for
NASA.
Researchers
are
actively
developing
techniques
to
understand
how
to
detect
caves
on
Earth
and
Mars,
and
have
identified
compelling
evidence
for
cave‐like
features
on
Mars.
Rinker
(1975)
and
Wynne
et
al.
(2007,
2008a,
2008b,
2009)
have
improved
our
understanding
of
thermal
cave
detection
on
Earth.
Cushing
et
al.
(2007,
2008)
have
analyzed
thermal
and
visible
imagery
to
examine
cave‐like
features
on
Arsia
Mons,
Mars.
On
Mars,
Keszthelyi
et
al.
(2007)
identified
lava
tube
remnants,
Wyrick
et
al.
(2004)
described
the
occurrence
of
pit
crater
chains,
their
geology
and
genesis,
Cushing
et
al.
(2007,
2008)
identified
deep
pit
craters
and
isolated
deep
pits
called
“anomalous
pit
craters,”
and
Cabrol
et
al.
(2009)
identified
at
least
677
features
likely
associated
with
speleogenesis
including
possible
lava
tubes,
deep
cavities
associated
with
pit
chains
morphology,
cracks
associated
with
faulting,
sink
holes,
and
volcanic
vents.
2.0
Background
Terrestrial
Cave
Detection:
Rinker
(1975)
provided
a
baseline
for
detecting
caves
in
the
thermal
infrared,
and
suggested
caves
could
be
detected
by
identifying
the
thermal
signal
associated
with
the
mass
of
air
at
the
entrance
contrasted
against
the
surrounding
ground
surface.
While
air
temperatures
in
cave
entrances
are
expected
to
be
different
from
ambient
temperatures,
Wynne
et
al.
(2008a,
2008b)
suggest
the
basis
for
cave
detection
will
be
the
temperature
contrast
between
the
rock
walls
within
the
cave
entrance
and
external
surface
rock.
Since
Rinker’s
(1975)
seminal
work,
some
advances
have
been
made
in
terrestrial
cave
detection.
Wynne
et
al.
(2009)
have
shown
it
is
possible
to
differentiate
caves
from
cave‐like
anomalies
by
analyzing
their
thermal
signatures
(Figure
1).
While
these
findings
are
encouraging,
these
results
are
preliminary,
and
a
larger
sample
size
will
be
required
to
demonstrate
the
feasibility
of
this
technique.
2
Importance
of
Martian
Caves:
(A)
Caves
may
be
important
in
the
search
for
evidence
of
extraterrestrial
life
(Mazur
1978;
Boston
et
al.,
1992,
1999;
Grin
et
al.
1998;
Klein
1998;
Boston
2000,
2003;
Léveillé
and
Datta
2009)
because
caves
offer
protection
from
inhospitable
surface
conditions
(Mazur
1978;
Klein
1998;
Cabrol
et
al.
2009).
(B)
A
manned
mission
to
Mars
will
require
access
to
significant
H2O
deposits
for
drinking
water,
oxygen
and
hydrogen
fuel.
If
subterranean
water
deposits
exist,
caves
may
provide
the
best
access
to
these
resources
(Baker
et
al.
2003).
(C)
Future
human
exploration
and
possible
establishment
of
a
permanent
settlement
on
Mars
will
require
construction
of
living
areas
sheltered
from
harsh
surface
conditions.
Caves
with
a
protective
rock
ceiling
would
provide
an
ideal
environment
where
these
shelters
may
be
built
(Boston
et
al.
2003).
Figure
1.
Pisgah
lava
beds,
Mojave
Desert,
CA.
[A]
Color
visible
image
containing
cave
entrance
(red
circle)
and
anomaly
(blue
circle).
[B]
IR
image
acquired
at
0510
hr
overlaid
on
the
visible
image.
Cave
entrance
appears
as
a
warmer
feature.
[C]
Results
of
Principle
Components
Analysis
show
output
can
be
used
to
differentiate
between
the
cave
(red),
non‐cave
anomaly
(blue),
and
high
nd
rd
rd
thermal
inertia
basalt
(green).
Scatter
plot
of
the
2 and
3 principle
components.
[D]
Visible
image
with
3 principle
component
output
overlaid;
colors
match
those
used
in
C.
From
Wynne
et
al.
(2009).
Cave
Detection
on
Mars:
Atmospheric
and
surface
conditions
on
Mars
fluctuate
more
dramatically
as
compared
to
Earth.
On
Mars,
large
diurnal
(Kieffer
et
al.
1976;
Ye
et
al.
1990)
and
seasonal
temperature
variations
(Larsen
et
al.
2002)
have
been
documented.
Additionally,
Martian
air
has
lower
pressure,
density,
and
heat
capacity
than
Earth's
atmosphere.
Thus,
much
larger
amplitudes
of
diurnal
and
seasonal
temperature
shifts
are
expected
on
Mars.
Because
these
shifts
would
occur
widely
and
internal
cave
temperature
is
expected
to
be
relatively
constant,
Martian
cave
detection
is
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
3
feasible
using
imagery
at
the
appropriate
wavelength
and
spatial
resolution
(Wynne
et
al.
2008a).
We
anticipate
this
will
influence
signal
strength
of
Martian
cave
entrances
resulting
in
a
stronger
thermal
signal
than
their
terrestrial
counterparts.
3.0
Goals,
Accomplishments
and
Objectives
Goals:
The
overall
goal
of
this
project
is
to
define
mission
and
instrumentation
requirements
for
detecting
caves
on
Mars
using
thermal
infrared
imagery.
Specifically,
we
will
develop
techniques
to
(1)
understand
the
thermal
behavior
and
optimal
detection
times
of
day
and
year
for
terrestrial
and
Martian
caves.
(2)
This
knowledge
will
help
us
to
differentiate
caves
from
non‐cave
anomalies,
and
potentially
infer
cave
volume
from
the
thermal
signal
of
the
cave
entrance.
Figure
2:
HiRISE
[A,B,C]
and
THEMIS
IR
[D,E]
imagery
of
a
pair
of
pit
craters
north
of
Arsia
Mons,
Mars.
Based
on
interpretations
of
features
in
panels
B
and
C,
both
appear
to
have
an
overhanging
rock
rim.
From
Cushing
et
al.
2008.
Accomplishments
(2008
Expedition):
We
(1)
deployed
temperature
and
barometric
pressure
data
loggers
at
eight
caves,
four
cave‐like
anomalies
and
on
the
surface
adjacent
to
all
study
sites
in
the
Atacama
Desert,
northern
Chile;
(2)
developed
cartographic
techniques
for
deriving
cave
volume;
and,
(3)
mapped
three
caves
and
one
cave‐like
anomaly
using
traditional
cartographic
(refer
to
Dasher
1994)
and
newly
developed
volumetric
mapping
techniques.
Objectives
(2009
Expedition):
Our
objectives
were
to:
(a)
retrieve
data
from
all
deployed
temperature
and
barometric
pressure
data
loggers;
(b)
relaunch
and
redeploy
data
loggers
(which
included
battery
removal
and
replacement,
as
well
as
relaunching
and
redeploying
all
instruments
at
their
original
sampling
station);
(c)
conduct
near
real‐time
analysis
(i.e.,
each
afternoon
and/
or
evening)
to
determine
if
data
logger
placement
was
adequate
for
characterizing
cave
thermal
behavior
and
modeling
temperature
trends;
and
(d)
draft
sketch
maps
and
derive
cave
volume
for
all
caves
and
cave‐like
anomalies.
4.0
Methods
Study
Area:
We
selected
caves
in
the
Atacama
Desert
of
northern
Chile
due
to
the
region's
hyperaridity,
which
makes
this
area
an
ideal
analog
for
the
Mars.
Recent
studies
suggest
the
climate
may
have
been
arid
for
90
Ma
(e.g.,
Hartley
and
Chong
2002;
Hartley
et
al.
2005)
and
specific
regions
have
been
hyper‐
arid
for
10‐15
Ma
(Ericksen
1983;
Berger
and
Cooke
1997;
Houston
and
Hartley
2003).
Rainfall
in
the
Atacama’s
hyper‐arid
core
is
virtually
indistinguishable
from
zero.
However,
the
Atacama
may
have
been
a
much
wetter
place
‐
much
like
Mars
(e.g.,
Chong
1984,
1988;
Navarro‐Gonzalez
et
al.
2003;
Quinn
et
al.
2005).
Vegetation
cover
in
our
study
area
is
low
to
non‐existent.
This
was
important
for
study
area
consideration
because
vegetation
cover
will
confound
our
ability
to
effectively
measure
temperature
differences
between
cave
entrance
and
surface.
Surface
material
near
the
cave
entrances
were
moderate‐to‐loosely
consolidated
alluvium,
comprised
of
silty
loam
and
clays
with
infrequently
interspersed
gravel
to
boulder
sized
sandstone,
shale,
and
volcanic
clasts.
Due
to
the
loosely
consolidated
nature
of
the
surface,
we
expect
the
surface
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
4
thermal
inertia
to
be
low;
resulting
in
rapid
warming
during
the
day
and
rapid
cooling
following
sunset.
Microclimate
Data:
We
collected
temperature
and
barometric
pressure
using
Onset
Computer
Corp.
Hobo‐Pro
v2
U23
temperature
loggers
and
H21
Micro‐stations.
We
collected
hourly
data
for
approximately
10
months
(August
2008
–
June
2009).
Temperature
data
is
required
to
best
model
cave
thermal
behavior
and
to
best
understand
when
caves
are
most
detectable
in
the
thermal
IR.
Barometric
pressure
data
provides
us
with
an
additional
metric
to
better
understand
why
caves
are
detectable
at
certain
times
and
not
others.
For
example,
as
cave
air
temperature
and
surface
temperatures
equilibrate
due
to
barometric
pressure
shifts,
air
movement
may
influence
the
walls
of
the
cave
entrance
and
thus
detectability.
Data
Logger
Deployment:
In
July‐August
2008,
we
deployed
temperature
and
barometric
pressure
sensors
in
eight
caves
and
four
cave‐like
anomalies.
Cave
–
We
deployed
two
to
three
data
loggers
per
entrance
and
at
all
skylights
within
each
cave;
one
data
logger
was
placed
at
cave
midpoints
(i.e,
midway
between
entrance
and
terminus
of
cave),
at
each
bifurcation
point
(i.e.,
where
passage
divides
into
two
or
more
passageways),
and
at
the
terminus
of
the
cave
(e.g.,
the
deepest
part
of
the
cave).
For
caves
with
multiple
passages,
a
data
logger
was
placed
at
the
terminus
of
each
passageway.
Surface
–
We
deployed
at
least
two
temperature
and
barometric
pressure
data
loggers
on
the
surface
within
20
meters
of
each
entrance/
skylight.
For
entrances/
skylights
located
within
canyons,
one
data
logger
was
placed
within
the
canyon
and
a
second
on
the
canyon
rim.
Cave
Mapping
and
Deriving
Volume:
Field
Techniques
(Mapping):
When
available,
we
used
existing
cave
maps
provided
by
Fryer
(2005)
and
Joel
Despain
(NPS).
These
maps
were
accuracy
checked
in
the
field
using
line
plot
and
volumetric
slice
data.
For
caves
and
non‐cave
anomalies
for
which
maps
did
not
exist,
we
used
standard
cave
mapping
techniques
(refer
to
Dasher
1994).
Field
Techniques
(Volume):
For
all
study
sites,
we
used
a
25m
pull
tape,
laser
distance
finders
(distos),
compasses
and
inclinometers.
We
collected
cave
volume
data
every
five
meters
(aka
mapping
stations)
at
eight
points
around
a
protractor
wheel
for
the
total
length
of
each
feature.
Data
Processing:
Line
plot
and
other
measurements
were
entered
into
the
cave
mapping
program
Compass
(Version
5.08.11.6.157).
While
Compass
has
a
cave
volume
calculator,
this
function
generates
a
cave
volume
estimate
using
four
points
around
the
protractor
wheel
(up,
down,
left
and
right
per
each
mapping
station).
Because
we
required
higher
accuracy
volume
estimates,
we
developed
a
Microsoft
Excel
spreadsheet
application
to
calculate
volume
using
eight
data
points
around
the
protractor
wheel
rather
than
four
data
points.
A
full
description
of
these
techniques
and
their
applicability
to
deriving
cave
volume
estimates
are
being
prepared
in
a
paper
to
be
submitted
for
publication
(refer
to
Ruby
et
al.
In
prep.).
5.0
Results
Figure
3.
3‐D
Map
of
Cueva
Chulacao,
Atacama
Desert,
Chile
(drafted
using
Compass).
Using
our
spreadsheet
application,
Chulacao
is
3
approximately
20,005
m (Ruby
et
al.
In
Prep).
Field
operations
were
conducted
from
05
–
20
June
2009.
During
this
period,
we
(1)
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
5
retrieved
data
from
data
loggers
located
at
all
study
sites;
(2)
relaunched
and
redeployed
all
data
loggers
that
were
recovered;
(3)
analyzed
data
and
determined
whether
sensor
placement
was
correct
for
all
study
sites
and
sufficient
to
model
temperature
trends;
we
also
(4)
mapped
and
collected
volumetric
data
at
six
caves
and
two
non‐cave
anomalies
(refer
to
Table
1).
During
field
operations,
one
of
our
data
shuttles
crashed.
This
resulted
in
the
loss
of
10
months
of
data
from
two
caves
and
one
non‐cave
anomaly
in
the
Chulacao
complex.
These
data
could
not
be
recovered.
Names
1Chulacao
1Telocote
2Salon
1Guia
2Luna
y
Media
2Quitor
2Los
Gatos
2Shredder
2Huesos
2Cascada
Pequeña
2Cartape
1Mina
Pequeña
Type
Cave
Cave
Cave
Cave
Cave
Cave
Cave
Cave
Cave‐like
anomaly
Cave‐like
anomaly
Cave‐like
anomaly
Cave‐like
anomaly
Length
(m)
Volume
(m3)
859
20,005
612
5,745
285
3,121
40
400
200
350
106
348
71
275
185
214
25
38
24
17
21
14
4
3
Table
1.
Cave
and
non‐cave
study
sites,
Atacama
Desert,
Chile.
Total
cave
length
was
derived
using
standard
cave
cartographic
techniques
(refer
to
Dasher
1994).
Volume
was
estimated
using
new
volumetric
mapping
techniques
(Ruby
et
al.
In
Prep.).
Data
collected
during
[1]
2008
and
[2]
2009
expeditions.
Additionally,
three
of
our
data
loggers
were
not
recovered.
6.0
Discussion
This
expedition
was
largely
successful.
We
collected
volumetric
data
and
completed
maps
of
all
of
our
study
sites
‐‐
in
total
12
study
sites
(eight
caves
and
four
cave‐like
anomalies)
for
both
the
2008
and
2009
expeditions.
We
were
able
to
retrieve
data
from
only
six
caves
and
three
non‐cave
anomalies.
We
lost
10
months
of
data
from
two
caves
and
one
non‐cave
anomaly.
One
of
our
data
shuttles
crashed
and
the
data
could
not
be
recovered
–
despite
the
efforts
of
the
engineers
at
Onset
Computer
Corp.
Also,
we
were
unable
to
relocate
three
of
our
data
loggers.
We
believe
two
loggers
were
stolen;
these
instruments
were
deployed
in
the
entrances
of
two
caves
frequented
by
tourists.
Despite
our
best
efforts
to
conceal
our
instruments,
they
were
found
and
removed.
The
third
data
logger
was
deployed
in
the
entrance
of
a
remote
cave.
While
we
had
both
copious
notes
and
photographs
on
the
location
of
this
instrument,
we
were
unable
to
relocate
it.
Data
collected
during
the
2009
expedition
will
be
used
to:
(a)
model
temperature
trends
of
the
entrance,
internal
cave,
and
surface
for
all
caves
and
non‐cave
anomalies;
(b)
examine
and
elucidate
temperature
differences
between
caves
and
non‐cave
anomalies;
and
(c)
identify
the
best
and
worst
detection
times
to
conduct
missions
to
collect
aircraft‐borne
thermal
imagery.
While
overflight
times
for
all
study
sites
have
not
been
determined,
we
present
an
example
of
how
this
is
estimated
(refer
to
Figure
4).
For
Shredder
Cave,
two
optimal
overflight
times
exist
–
winter
(June
–
August)
between
0600
and
0800hr
and
summer
(November
–
January)
between
1200
and
1400hr.
The
worst
overflight
time
(i.e.,
the
time
when
there
is
minimal
contrast
between
entrance
and
surface)
are
thermal
cross‐over
periods
and
occur
during
most
of
the
year
(August
–
May)
between
1800
and
2200hr.
We
conducted
preliminary
analysis
on
the
Atacama
data
to
investigate
temperature
trends
of
caves
and
cave‐like
anomalies,
and
examine
differences
between
caves
and
non‐cave
anomalies.
Tentatively,
our
results
largely
concur
with
the
results
presented
by
Wynne
et
al.
(2009).
These
results
will
be
published
in
a
peer‐reviewed
journal.
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
6
Figure
4:
Comparison
of
surface
and
entrance
temperature
data
for
the
upper
entrance
of
Shredder
Cave.
This
is
a
screen
shot
of
a
software
package
developed
during
this
project
and
used
to
analyze
cave
temperature.
The
left
panel
shows
the
surface
(white)
and
entrance
(blue)
temperatures
observed
over
10
months.
The
right
panel
shows
the
time‐of‐day
and
seasonal
comparison
where
warm
colors
(green‐yellow‐red)
show
the
greatest
thermal
contrast
and
the
cool
colors
(purple‐blue)
show
the
least
thermal
contrast.
Once
best
and
worst
overflights
times
for
the
caves
and
cave‐like
anomalies
are
derived
(for
those
sites
that
we
have
data),
we
will
use
these
data
to
schedule
our
overflights.
These
results,
along
with
the
thermal
imagery
analysis
and
interpretation,
will
be
incorporated
into
a
paper
and
will
be
published
in
a
peer‐reviewed
journal.
If
best
and
worst
overflight
times
for
other
caves
and
non‐cave
features
are
similar
to
times
for
Shredder
Cave,
we
may
be
able
to
conduct
both
missions
during
the
same
expedition.
Table
2:
2009
Atacama
Desert
Cave
Expedition
Team
Team
Member
Jut
Wynne,
FN’06
Tim
Titus
Affiliation
SETI‐CSC,
NAU
USGS
Role
Expedition
lead;
Data
retrieval
lead
Deputy
expedition
lead;
Sensor
data
analyst
Dan
Ruby,
MN’09
Fleischmann
Planetarium,
Univ.
Number
3;
Mapping
team
lead;
Lead
Nevada,
Reno
cartographer
Guillermo
Chong
UCN
Geologist;
Logistics
Christina
Colpitts
Research
Support
Group
Safety
officer;
Cartography
technician
Lynn
Hicks,
MD,
Glynn
Immediate
Care,
Southeast
Expedition
Doctor;
Sensor
MN’09
Georgia
Health
System
placement;
Cartography
technician
Denise
Hill
MARS
EMT;
Cartography
technician
Cristian
Tambley
Campo
Alto
Logistics
chief
Expected
Results
(upon
project
completion):
Through
our
efforts,
we
will:
(1)
identify
times
when
differences
between
cave
entrances
and
surface
control
stations
are
optimal
and
schedule
thermal
data
collection
overflights
accordingly;
(2)
compare
the
thermal
behavior
of
caves
to
non‐cave
anomalies;
and,
(3)
populate
simulation
models
of
the
thermal
dynamics
of
Martian
caves
and
surface.
Additionally,
this
project
will
result
in
the:
(i)
development
of
a
systematic
approach
for
terrestrial
and
extraterrestrial
cave
detection;
(ii)
establishment
of
a
thermal
signature
library
of
terrestrial
caves
of
various
structure
types;
(iii)
designation
of
optimal
times
for
detection
of
caves
on
a
per
structure
basis
for
Earth
and
Mars;
and
(iv)
identification
of
instrumentation
and
mission
requirements
for
detecting
Martian
caves.
7.0
Acknowledgements
We
extend
our
gratitude
and
thanks
to
Mr.
Edward
Rodréguez
and
Mr.
Tomas
Gerö
Mertens
with
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
7
CONAF‐Antofagasta,
and
Mr.
Roberto
Cruz
Cruz
with
CONAF‐Calama
and
Mr.
Manuel
Cortes
Mora
Asociación
Indígena
Valle
de
la
Luna
for
facilitating
and
issuing
our
research
permits,
and
providing
us
with
continued
support
in
the
field.
We
thank
Mr.
Jose
Luis
Jara,
CONAF‐San
Pedro
for
assistance
with
fieldwork
and
his
continued
support,
Mr.
Don
Felix
Colque,
Mrs.
Dona
Maria
Colque
and
Mr.
Carlos
Colque
with
Colque
Tours‐San
Pedro
for
continued
use
of
our
field
station
(“Rancho
Tonka”),
Mr.
Marc
Tiritilli
and
the
Illinois
cave
search
and
rescue
team
for
their
willingness
to
remain
on
stand‐by
during
this
expedition,
Dr.
Randy
Berthold
and
the
NASA‐ARC
EERRB
Safety
Review
Panel
for
their
direction
leading
to
the
improvement
of
the
expedition
safety
plan,
Mr.
Matt
Arcovio
and
Global
Rescue
for
their
stand‐by
extrication
support,
Mr.
Scott
Ellis
with
ONSET
Computer
Corp.
for
donating
the
data
shuttles
and
for
his
continued
support,
and
Mr.
Joel
DeSpain
and
Mr.
Shane
Fryer
with
the
U.S.
National
Park
Service
for
access
to
and
use
of
Atacama
Desert
cave
maps.
Special
thanks
to
The
Explorers
Club
(Ms.
Constance
Difede
and
The
Flag
and
Honors
Council)
for
recognizing
this
expedition
as
a
Flag
Expedition.
We
also
acknowledge
Drs.
Nathalie
Cabrol
(Project
PI),
Edmond
Grin,
Murzy
Jhabvala,
Jeff
Moersch
and
Peter
Shu
for
their
continuous
efforts
and
contributions
to
the
overall
objectives
of
this
project.
Dr.
Nathalie
Cabrol
and
Mr.
John
Dedecker
(MN’09)
provided
comments
and
suggestions
leading
to
the
improvement
of
this
report.
This
project
is
supported
by
the
NASA
Astrobiology:
Exobiology
and
Evolutionary
Biology
program
under
grant
#
EXOB07‐0040.
8.0
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2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report
9
Appendix
I
(Example
of
Data
Logger
Deployment)
Cueva
Salon,
Atacama
Desert,
Chile.
Boxes
(red)
represent
the
locations
of
where
data
loggers
are
deployed.
Numbers
(blue)
represent
the
number
of
each
data
logger.
Map
modified
from
Fryer
(2005).
2009 Atacama Desert Expedition (05-20 June 2009) – Explorers Club Flag Report