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Robotic exploration potential of Martian caves

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Martian caves are among the best locations to search for evidence of extinct/extant life, may provide access to stable water ice deposits, and offer a protected environment for human habitation. We examined the robotic exploration potential of a subset of these features. Poster URL: https://www.researchgate.net/publication/349679212_Robotic_exploration_potential_of_Martian_caves
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ROBOTIC EXPLORATION POTENTIAL OF MARTIAN CAVES. M. L. Kearney1, J. J. Wynne2, G. E.
Cushing3, N. M. Bardabelias4, and N. G. Barlow1,5. 1Department of Astronomy and Planetary Sciences, Northern
Arizona University, Flagstaff, AZ; chellykearney@gmail.com; 2Department of Biological Sciences, Merriam-Powell
Center for Environmental Research, Northern Arizona University, Flagstaff, AZ; jut.wynne@nau.edu; 3USGS
Astrogeology Science Center, Flagstaff, AZ; gcushing@usgs.gov; 4Lunar and Planetary Laboratory, University of
Arizona, Tucson, AZ; nmb23@lpl.arizona.edu; 5deceased.
Introduction: Martian caves are among the best
locations to search for evidence of extinct or perhaps
extant life, may provide access to stable water ice
deposits, and can offer a protected environment for
human habitation [1]. In recognition of the emerging
importance of caves on Mars, NASEM’s 2019
Astrobiology Strategy recommended emphasis on
research and exploration of subsurface environments
[2]. Additionally, mission architectures [1] and concepts
[3] were recently developed to provide
recommendations for examining Martian caves for
astrobiological and habitability potential (Fig. 1).
To date, 1,036 cave-like features have been
documented on Mars [4]. Williams et al. [5] modeled
cave water-ice stability on Mars and identified the most
favorable regions for ice to accumulate and persist.
These datasets combined were used as a first order down
selection approach to identify high priority caves for
exploration.
Overall, we aimed to identify the highest priority
targets for a future robotic mission to a Martian cave.
Specifically, we: (1) defined caves within regions of
high subterranean ice accumulation; (2) calculated cave
densities per region; and, (3) identified concentrations
of caves on the Martian landscape. Additionally, we
provide two examples where we applied the selection
criteria for targeting high priority caves for robotic
exploration [6].
Methods: This project examined known cave locations
[4] and a subterranean ice accumulation model [5] to
deduce cave entrances within regions of predicted high
ice accumulation. We selected a subset of these caves
based on existing HiRISE imagery, which became our
dataset. We then evaluated these features using a
candidate selection criteria for robotic exploration [6].
These criteria include the potential for subsurface ice,
access to subsurface geology, and robotic accessibility
including terrain navigability and entrance
configuration. Geologic and structural characteristics
were determined using available geologic maps [7,8]
and HiRISE images. Nearest neighbor analysis was
performed to identify cave clusters. All analyses were
conducted using JMARS 5.1.8 and ArcGIS 10.8.1.
Figure 1. Locations of possible Martian cave entrances (red dots) [2] overlaid on the cave ice accumulation model
(where predictions of annual ice mass amounts (in kg/yr) within hypothetical caves) [5] for global Mars. Areas of
interest occur within the [A] Tharsis and [B] Phoenicis Lacus quadrangles. MOLA base map, courtesy NASA.
Robotic exploration potential of Martian caves: M. L. Kearney et al.
Results: We found 97 caves occurring within regions of
high ice accumulation (0.1-0.7 kg/yr) and 847 within
regions of medium accumulation (0.001-0.1 kg/yr; Fig.
1). The highest density (620 caves) was located within
the Phoenicis Lacus quadrangle with a density of 1.4 x
10-4 caves/km2, while the Tharsis quadrangle was the
second most dense with 0.5 x 10-4 caves/km2 (223
caves).
HiRISE imagery is available for 28 caves, which
were all within the Tharsis volcanic province. We
summarized structural and geologic characteristics for
these features (Table 1). Angular and jagged outcrops
along pit rims suggestive of examinable stratigraphy
was observed for 58% of the vertical features
potentially permitting robotic examination and
sampling of “deep” subsurface geology. At least 23
features would permit dual-axle rover access to the
entrance; this would be required for subterranean
ingress of a secondary tethered rover. Most (82%) of the
features were located on the lava fans and surrounding
plains of Arsia Mons. Nearest neighbor analysis
revealed that three features had from three to six
additional features within a 25 km distance and up to 10
potential cave entrances within a 50 km radius; clusters
will provide greater flexibly as multiple features could
then be closely scrutinized if aerial drone technologies
are employed.
While 28 features are currently being evaluated for
their exploration potential, we provide preliminary
results for two features as examples. The first feature is
a possible skylight situated on the southern lava fan of
Arsia Mons (Fig. 2A). Angular protrusions suggestive
of viewable stratigraphy are situated along the eastern
rim. Access could be gained via a drone or tethered
rover. We cannot discern whether a lateral entrance is
associated with this feature, which is a key requirement
for robotic exploration.
Our second feature is probably not viable as it is an
isolated feature occurring at an elevation of 20,244 m
within Caldera V [sensu 9], the southernmost caldera of
Olympus Mons. However, this is presently the only
feature suggestive of laterally-trending passage for
which HiRISE imagery is available. Located within the
southeastern wall of the caldera, the feature is likely a
conduit related to the caldera, possibly a vent.
Conclusions: While our work will ultimately involve a
thorough examination of all 28 potential cave entrances,
we have provided examples of how the selection criteria
will be applied. Ultimately, we will examine and
quantify the robotic exploration (as well as human use)
potential for all features using geospatial techniques.
Caves occurring within clusters will be further
examined and recommendations will likely be made for
additional HiRISE imagery acquisition.
Figure 2. [A] Skylight on southern lava fan on Arsia
Mons, diameter ~30 m (HiRISE ESP_042942_1680).
[B] Possible laterally trending feature on Olympus
Mons, length of apparent entrance, north to south, is ~10
m (HiRISE ESP_007669_1980).
References: [1] Titus, T.N. et al. (2020) Planetary
Caves Decadal Survey white paper. [2] NASEM (2019)
doi:10.177226/25252. [3] Phillips-Lander et al. (2020)
MACIE Decadal Survey white paper. [4] Cushing, G.E.
(2017) Mars Global Cave Candidate Catalog (MGC3),
PDS Archive. [5] Williams, K. et al. (2010) Icarus 209:
358368. [6] Wynne, J.J. et al. (2014) NASA JPL
Planetary Cave Workshop white paper. [7] Masursky,
H. et al. (1978) USGS Mars Geologic Map of the
Phoenicis Lacus Quadrangle. [8] Scott, D. & J.
Zimbelman. (1996) USGS Geologic Map of Arsia Mons.
[9] Neukum, G. et al. (2004) Nature 432: 971-979.
Lava Fans and Surrounding Plains of
Arsia Mons
Caldera and Flanks of Shield -
Volcanoes
Cliff
Cave category
APC
Sky
End
Irr
APC
Rim
SRP
Lat
Irr
Number of caves/
Category
12
5
1
2
1
1
1
1
1
Diameter (m)
105-250
4-460
92
5-40
170
60
45
-
12
Elevation (m)
6,296 - 12,330
14,477 - 20,244
4,739
Entrance type
All vertical
3 vertical, 1 lateral
Vertical
Visible
stratigraphy
6
3
-
-
-
1
-
1
-
-
Table 1. Geologic and structural characteristics of the 28 caves with HiRISE imagery. Cave types: atypical pit crater
(APC), crack (Crk), skylight (Sky), irregularly shaped feature (Irr), entrance to rim of caldera (Rim), small rimless pit
(SRP), laterally trending entrance (Lat), and pit in the end of a trough (End) [4].
... Within the caves, temperatures are likely cold (<−25°C or 248 K) and thus could harbor metastable water ice. 74 Cave locations and predicted ice accumulation rates 75 ...
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