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Article

Unveiling the Subsurface of Late Amazonian Lava Flows at Echus Chasma, on Mars

by
Federico Mansilla
1,*,
María-Paz Zorzano
1,
Iraklis Giannakis
2 and
Javier Ruiz
3
1
Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, 28850 Madrid, Spain
2
Department of Geology and Geophysics, University of Aberdeen, Meston Building, Kings College, Aberdeen AB24 3EU, UK
3
Departamento de Geodinámica, Estratigrafía y Paleontología, Universidad Complutense de Madrid, 28040 Madrid, Spain
*
Author to whom correspondence should be addressed.
Remote Sens. 2023, 15(5), 1357; https://doi.org/10.3390/rs15051357
Submission received: 27 January 2023 / Revised: 20 February 2023 / Accepted: 24 February 2023 / Published: 28 February 2023
(This article belongs to the Special Issue Radar for Planetary Exploration)
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Abstract

:
The Echus-Kasei region on Mars has been exposed to different episodic volcanic, fluvial, and glacial events in Amazonian time. The goal of the present work is to demonstrate the usefulness of radar instruments to find preserved late Amazonian subsurface structures that may have been encapsulated underneath recent lava flows on Mars. We have analysed 27 radar observations of the SHAllow RADar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO), over the region of Echus Chasma. We discovered the presence of subsurface reflectors in five consecutive SHARAD radargrams at a depth from 35 to 79 m beneath the structure of a lava fan that formed about 59 ± 4 Ma ago. Some vents are preserved above the surface of this lava flow, which stands at a height of 80 m above the surrounding surface. A few kilometres to the north, we find other subsurface reflectors at a depth of about 30 m and a long pit chain formed by the collapse of a lava tube. These kinds of subsurface late Amazonian structures are of interest for astrobiology because they date from the last period when the planet still experienced intense volcanic activity over regions that were previously extensively covered by water.
Keywords:
radar; Mars; lava; Amazonian

1. Introduction

During the most recent history of Mars (namely, the Amazonian epoch), there had been some episodic periods where water, ice, and lava flows may have coexisted or partially overlapped on its surface, rendering the surface of Mars active and potentially habitable [1,2,3]. In particular, previous research of Echus Chasma and the Kasei Valles has shown that this region was affected by at least four episodes of widespread volcanic activity and four periods of episodic fluvio-glacial activity from the Hesperian to the Amazonian Epochs on Mars (from 3.6 Ga to present) [4,5]. The last of the four major volcanic episodes occurred around 90 Ma between the last two episodes of fluvio-glacial activity [4]. This work shows evidence suggesting that glaciers and near-surface ice may have persisted through Amazonian times in local areas over the entire length of the Kasei Valles, and that it was covered by what is now seen as a platy-flow surface material interpreted to be 2100 km runout flood lavas sourced from the Echus Chasma.
More recent research of the Kasei Valles region around 27°N indicates that 1400–3500 km3 of ice were present at the time the lava was emplaced, about 1.3 Ga [3]. Viscous flow features (interpreted as ice-rich deposits buried beneath the sediment mantle [3]) can be located there today, including lobate debris aprons [6]. This region contains geomorphological evidence of lava-ice interactions in the form of depressions surrounding isolated mesas or situated parallel to scarps [7]. These depressions are formed when ice and lava interact, and mark the extent of ice-rich glaciers at the time the lava flow was formed. The dating of these structures suggests that ice survived for up to ∼1 billion years following lava emplacement before its final demise [3]. Its long-term survival was presumably aided by supraglacial debris layers like those on present-day glacier landforms on Mars. These regions represent some of the oldest large glacial ice masses on Mars.
The youngest crater retention ages on the floor of Echus Chasma suggest an age between 54 and 98 Ma [4]. It is noticeable that the most recent activity at Arsia Mons (the southernmost of three volcanoes on Tharsis) peaked at 150 Ma and ceased by 10–90 Ma [8]. This dating was done by studying the fresh lava flows of 29 volcanic vents within the Arsia Mons caldera. Volcanic vents in this study area are located on topographic highs and show lavas emanating from them. Thicknesses of lava flows on Arsia Mons’ flanks have been estimated to be from about 10 to 80 m [9].
Other studies [10,11,12] have discussed the age, structures, and dielectric properties of lava flows on the western flanks of Ascraeus Mons (the northernmost of three Tharsis Montes volcanoes). These studies have described the existence of subsurface reflectors underneath the western flank.
In the present work, we focus on the eastern flank of Ascraeus Mons, in particular the Echus-Kasei system (Figure 1). Our main goal is to demonstrate the usefulness of orbital radar sounders to find reflectors that may inform us on the presence of preserved subsurface layers underneath the most recent lava flows. This would be extremely interesting for astrobiology because the existence of reflectors indicates changes in the subsurface properties, which may be due to changes in porosity or composition [13]. Subsurface encapsulated layers, formed over regions that were previously covered by water, may have been habitable and protected from desiccation and cosmic radiation until now. The second objective of this work is to find caves [14] or lava tubes associated with these lava flows that may be used as settlements for the future human exploration of Mars to avoid the extreme levels of cosmic radiation at surface level [15,16,17].
In the long term, this research has two purposes: (1) to demonstrate the usefulness of combining radar data with other instruments and (2) to establish a methodology that can be extended to analyze the entire surface of Mars.
The material and methods used in this work are presented in Section 2. The specific objectives of this work are covered in Section 3.1, where we describe the discovery of new lava flows in the Echus-Kasei system, collect the radargrams with confirmed reflectors and calculate the thickness of these lava flows; in Section 3.2 we date the lava flow structure using the crater counting method; in Section 3.3 we discuss the potential depth of the subsurface reflectors; and in Section 3.4 we investigate the possible presence further north of other lava-related features, well within the Echus-Kasei system. Finally, Section 4 presents a discussion of the results and analysis presented and Section 5 makes a summary of the findings of this work.

2. Materials and Methods

We first perform a visual survey of the region of interest in order to find surface features that may be indicative of lava flows. We use four global datasets to achieve this: (1) Mars Orbital Laser Altimeter (MOLA) topography [18], (2) High-Resolution Stereo Camera (HRSC) [19] image mosaics and topography derived, (3) Context Camera (CTX) mosaic developed by the Bruce Murray Laboratory for Planetary Visualization [20], and (4) Thermal Emission Imaging System (THEMIS), an infrared, daytime mosaic [21]. We analyse the data with QGIS [22] and JMARS [23]. QGIS is a geospatial information system developed by the QGIS Development Team. JMARS is a geospatial information system developed by the Mars Space Flight Facility of Arizona State University. We then investigate the radargrams provided by the SHAllow RADar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO).
MOLA is a payload onboard the Mars Global Surveyor (MGS) spacecraft, launched in 1996, and it was in operation, collecting altimetry data, until June 30, 2001. It measured the travel times of a laser ray emitted from the instrument to the surface of Mars, allowing the construction of the Digital Elevation Models (DEMs) of the surface of Mars. The Mars MGS MOLA DEM 463 m v2 has a spatial resolution of 463 m/px.
The High-Resolution Stereo Camera (HRSC) experiment carried on the Mars Express mission, launched on 2 June 2003, is a stereo camera experiment that allows for the creation of photogrammetrically controlled digital elevation models of the surface of Mars with spatial resolutions ranging between 10 and 30 m. In this work, HRSC was only used for the preliminary surveys as there are no Digital Elevation Models (DEMs) available for the region of interest.
CTX is the Context Camera, onboard the Mars Reconnaissance Orbiter (MRO). It was designed to complement the HiRISE (High Resolution Imaging Science Experiment), another camera experiment onboard MRO with stereo capabilities and a very high resolution (up to 30 cm/px) for the localisation of features in a wide field. The mosaic used was developed by the Murray Lab (the Bruce Murray Laboratory for Planetary Visualisation) at the California Institute of Technology and consists of a seam-corrected and seam-mapped mosaic of Mars rendered at 5 m/px. This product has been used to implement the largest-scale surveys.
THEMIS is an instrument that combines two independent multispectral imaging systems, one with 5 bands in the visible range and another with 10 bands for the infrared imaging system. It was carried by the Mars Odyssey mission, launched on 7 April 2001, and it is still operational today. It is useful for mineral identification using visible and infrared information. We used the derived product, Thermal Emission Imaging System (THEMIS), a daytime infrared (IR) 100 m/pixel mosaic (version 12), released in the summer of 2014 by Arizona State University, to identify features at a small scale.
The Shallow Radar experiment aboard the Mars Reconnaissance Orbiter mission is known as SHARAD. This instrument had been designed to look for frozen or liquid water under the first kilometre of the Martian surface. It uses a 10 m antenna that transmits “chirps” of 85 microseconds at frequencies between 15 and 25 megahertz [24]. With this technology, it is capable of detecting features at a vertical resolution of 10 m and a horizontal resolution of between 0.3 and 3 km.
Ground-penetrating radar systems have been extensively used to investigate the subsurface of Mars, find water reservoirs, as well as identify possible reflectors that inform on the structure of the uppermost layers of the planet. The two radar systems that have been investigating Mars are MARSIS [25], onboard Mars Express, and SHARAD [24] onboard the Mars Reconnaissance Orbiter. SHARAD has been in operation since November 2006. These instruments transmit low-frequency radio waves that penetrate the subsurface and receive the reflected signal. The difference in the reflected power is due to the different dielectric properties of the materials traversed by the signal. This technique is very useful to remotely investigate the geometry and nature of discontinuities. Cluttergrams are needed to discriminate the echoes from the surface topography from those from true reflectors. Once we have identified potential subsurface reflectors in the radargrams of the region of interest, we make the corresponding cluttergrams of the radargrams for comparison, in order to avoid false positives [26,27]. We first do our own survey, applying the cluttergram method described by Choudahary et al. [27,28]. In order to base the analysis on an open access cluttergram, we use CO SHARPS, the cluttergram-generating code applied to SHARAD data by the instrument team [29]. Both radargrams and cluttergrams are archived in the Planetary Data System node for SHARAD [30,31].
The age of the lava flow is calculated using the crater counting method [32,33,34,35]. To apply it, we digitize the craters within the region of interest, paying attention to their shape. We export the shapefiles with the CSFD tool, which is designed to make crater size-frequency distribution measurements using polygonal-shape files in a format useful for working in Craterstats [36]. This workflow permits the use of any GIS tool to make the crater survey. We work with QGIS because it is open-source software widely used in planetary sciences, and its digitizing tools are very useful and user-friendly. Once we have the crater survey, we make the statistical analysis using Craterstats 2.0 and by applying the chronology system proposed by Hartmann and Daubar, 2017 [37]. The crater counting results are compared with the Martian epochs proposed by Michael in 2013 [35]. With these constraints, we plot the results of the cumulative crater count using a diameter range between 100 and 1000 m and a pseudo-logarithmic scale.
Finally, the depth of reflectors is estimated by converting the time delay  Δ t  (in seconds) to the height  ∆ h  (in meters) using the following equation    ∆ h = c Δ t / √ ε , where  c  is the speed of light and  ε  is the relative permittivity or dielectric constant. The dielectric constant is a property of materials that depends, among other parameters, on their composition, density, and humidity. For dry sedimentary materials, we use the relationship  ε = 1.96   ρ    [38], where  ρ  corresponds to the density. By comparing the existing topography with the estimated depth  ∆ h , the relative permittivity of the material can be estimated in regions where there is a topographic elevation above and the reflector is assumed to be in the underlying plane. This can be used to get first-order information about the density of accumulated materials above the reflector, and to extrapolate for other reflectors for which there is no direct topographic comparison. Permittivity values from the Moon can also be used as a reference to provide an estimate of the density, as the lunar layers are typically dry, and have been compared with measurements of samples brought back to Earth [39]. According to data derived from the FREND workgroup [40], the water content of the shallowest subsurface is apparently low, which allows us to handle this material as dry volcanic rocks.
To end this section, we present graphically (Figure 2) the steps followed in the interpretation of radargrams, using track 3628101 as an example.

3. Results

3.1. Lava Fan and Potential Reflectors

Through visual inspection of THEMIS-derived images and MOLA-derived hillshade, we have found a lava-flow structure located at −80°E, 5.6°N, in the Echus Chasma region that is very well preserved (Figure 3).
The direction of the flow is consistent with the orientation of the fan. The elevation of the lava fan is higher than 80 m above the plain of Echus Chasma and its surrounding area (a detail of the topography of this structure across one of SHARAD’s tracks is shown in Figure 4). This structure of approximately 3500 km2 shows a lobed shape in the margins and is composed of two main bodies: the proximal one has a more massive aspect and is connected by a narrow arm that grows from west to east, and the distal part whose ending consists of a fan-shaped landform with a southerly trend that is consistent with the underlying topography (see Figure 4). This contrasts with the general inclination of the depression, which points to a massive outflow toward the north [41].
Analysing surface features, we found vents widely distributed over the entire surface of the lava fan, forming smooth surfaces that mark the direction of flow and are consistent with both the slope and the general direction of growth of the main structure (see Figure 5).
We have analysed 27 SHARAD tracks over this area (Table A1), and we have found potential reflectors in five of them (Figure 6 and Figure A2).
These surfaces present high backscattering, returning high-intensity signals that translate into bright reflectors in the radargrams. The brightness contrast in the radargrams is due to the difference in the dielectric properties of the materials crossed by the radar signal (Figure 7).

3.2. Lava Fan Age

We have next performed a crater counting analysis of the lava fans to date the age of their surface (Figure 8). We have not made any differentiation between the layers of the lava fan because there is not enough confidence in small areas to constrain the age through crater dating. The size of 197 craters found in the lava fan region, which covers an extension of about 3518 km2, has been determined. The cumulative crater density for each crater diameter size has been calculated and compared with the age system proposed by Michael (2013) [35]. The lava flow fans are estimated to be only 59 ± 4 Ma old, confirming that this feature is very young. Since all 197 craters seem to follow the same isochrone, we conclude that it is reasonable to interpret that all the lava fans in this structure formed at the same period and have not been modified differently by subsequent processes.

3.3. Depth and Permittivity of Subsurface Layers

We have applied the cluttergram technique to make sure that these reflectors are not artefacts originating from reflections of the surface (Figure 8). Following the method described above, we have found five true reflectors underneath this 59 Ma age structure. For each reflector, we take note of the maximal delay time of the reflector signal. Assuming a dielectric constant, we can retrieve an estimated reflector depth. Figure 2 shows an example of this for Ꜫ = 6, which is a typical value for sedimentary rocks with a dry density of around 2650 kg/m3 [38]. To have a range of possible depths to compare with, we can use the lower and upper bounds of possible permittivities, including those estimated for lava flow-like structures on Mars [11]. The resulting ranges of depths for the five reflector layers are summarised in Table 1.
Most of the reflectors are continuous. Some may be apparently intermittent; in those regions, there is less contrast in permittivity. This may be caused by local changes in material properties or orientation (which may affect the radar reflection) or because they might belong to different lava bodies.
The height of the lava fan is of the order of 80 m, so assuming that the subsurface reflectors are at the level of the current base, this suggests that the material has a permittivity close to 6.2, which is in agreement with the values given for Mars by Carter et al., 2009 [11], where they analyse the permittivities of lava flows on the western flank of Ascraeus Mons, which we consider equivalent; see Table 1, where we summarize the single wave travel time (SWT) (some authors use TWT—twice wave travel time—but the travel time provided by JMARS refers only to one way  ∆ t = ∆ x × 37.5 / 2 ,  where Δx refers to the incremental in pixels on the radargram).

3.4. Northward Terrains: Subsurface Layers and a Volcanic Pit Chain

A few kilometres towards the north (Figure 9 right), we can also observe a pit chain formed by a collapse along a lava conduit, which was emptied when the volcanic activity stopped (Figure 9 left). These pit caves are well preserved, suggesting that they were formed recently over a relatively fresh structure of lava tubes associated with lava flows from Ascraeus Mons.
The radar track analysis shown in Figure 9 right, just a few kilometres to the north of the lava fan, shows a well-preserved, plain-parallel reflector structure. Assuming the same dielectric constant thresholds suggested above, these reflectors can be estimated to be at depths of between 20 and 12 m; see Figure 10 right. The cluttergram shows no sign of bright layers, confirming that these are true plane-parallel reflectors. The footprint of this track lies within the unit At5, described by Chapman et al., 2010 [4], which according to these authors is characterised by young lava flows dated from 89 Ma on average.

4. Discussion

Subsurface reflectors are expected to be preserved only underneath surfaces that have recently occurred. Pristine volcanic surfaces trapped beneath recent deposits could preserve the original fracture system [43] and original porosity. Both tend to collapse over time due to lithostatic pressure and mineral alteration processes.
The importance of the existence of these reflectors is twofold: (1) on one side, their presence is interesting to confirm the relative youth of this unit because, as Stillman and Grim, 2011 [43] describe, these features are only preserved in the youngest geological units; and (2) the contrast in permittivity between the reflector and the material above could indicate variations in the porosity [13], and that may point to the past or present presence of fluids, water ice, volatiles, etc., which may be a potential habitable environment for life.
We have analysed 27 radar tracks of the SHAllow RADar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO) over the region of Echus Chasma. We have found, underneath a fresh lava flow of about 59 ± 4 Ma years, five subsurface reflectors at depths from 35 to 79 m [13]. Some vents are preserved above this lava flow of >80 m thickness. During this period, Arsia Mons, the southernmost volcano of Tharsis, was active. Our analysis also demonstrates the volcanic activity of Ascraeus Mons, the northernmost volcano, towards the Echus Chasma region.
The existence of preserved, small-scale, surficial vents suggests that this structure has not been covered later by other materials, which would have easily broken or eroded it. Therefore, it is reasonable to think that the lava fan has not been resurfaced and has been exposed directly to the atmosphere from the moment of its formation until now. This suggests that the dating of this structure is the true formation date and not the duration of the exposure after resurfacing.
Overlying lava flows may have helped preserve past ice or liquid water reservoirs from sublimation and evaporation while also serving as a shield from radiation. Only two meters of rock are needed to shield from space radiation [15], but with SHARAD data, we cannot resolve shallow reflectors (of the order of meters) as they would be fused with the surface signal.
The preservation of reflectors in this region is rare. The exception to this, is the existence of those five unique reflectors close to the base of the cliff, within the widest part of the lava fans. The current height of the lava fan is of the order of 80 m above the floor, which suggests that the material must have had a low permittivity value, such as ε = 6.2, so that the depth of the preserved subsurface reflectors is compatible with the measured topography. This permittivity value is the value of lava flows with low density, and porosities are as high as 35% [13].
Our analysis suggest that these fans were formed by high porosity lava flows, which could have been generated by inherent magma degasification or by volatiles provided by an underlaying, water-rich material, at the bottom of Echus Chasma. This degasification process would also be consistent with the formation of vents at the surface of the lava fan to facilitate the release of volatiles from the magma [44].
Finding open lava tubes or pit chains within a planet can be a challenging task, as they are relatively small. To detect a lava tube opened to the sky in the present epoch, it is required that the lava process be recent so that the subsurface structures that were produced by the flow of lava have not been exposed to extensive modification and are well preserved. Additionally, the openings need to be big enough that they have not been covered by dust and can be distinguished from the orbit. Our analysis suggests that using orbital radar to find large scale preserved subsurface reflectors in regions that have been recently formed by lava may increase the chances of finding other well-preserved structures associated with lava flow, such as lava tubes. Indeed, within a few kilometres of these preserved subsurface reflectors, there is a collection of well-preserved plane-parallel reflectors, at an estimated depth of only 12 m (or 20 m at most), together with a pristine open pit chain that extends over several kilometres. Both preserved features are consistent with the hypothesis that this is a relatively young region produced by volcanic activity. It is worth indicating that pits and lava tubes are considered “special regions” on Mars [16] with special planetary protection requirements. Lava tubes are considered of interest for the future of human exploration of Mars, and at the same time they are potentially interesting for the present-day habitability of Mars, as they offer shelter from radiation and thermal contrasts and may have access to subsurface water resources.

5. Conclusions

For the current and future exploration of Mars, it is interesting to map the subsurface regions of Mars where the environment may be adequate for life at the present time, creating one of the so-called special regions, defined as regions within which terrestrial organisms are likely to replicate [16]. An example of special regions associated with volcanic activity that are of particular interest for human exploration are lava tubes, caves, and pit chains [17]. We have shown that, mapping well-preserved subsurface layers underneath lava structures allows us to investigate the geological processes that took place in the past that could have formed an encapsulated environment that also protects water, ice, or life from surface conditions, that could cause sublimation and, as a result, water loss. We suggest the use of a multi-instrumental and remote sensing approach that combines radar measurements with photointerpretation, geological mapping, and topographic analysis.
Using this approach, we discovered five preserved subsurface layers (Figure A2) at a depth of about 80 m within the Echus Chasma system on Mars, protected beneath a young lava flow of about 59 Ma. Within this same structure, there is a fresh, shallow pit chain that extends over several kilometres and may provide direct access to a special region formed about 59 Ma during the last volcanic activity that affected this region.
We conclude that radar instrumentation is a powerful tool for planetary exploration to detect from orbit potential subsurface regions of interest and plan future surface missions.

Author Contributions

Conceptualisation, F.M. and M.-P.Z.; methodology, F.M., M.-P.Z. and J.R.; validation, F.M., M.-P.Z., J.R. and I.G.; formal analysis, F.M.; investigation, F.M., M.-P.Z., J.R. and I.G.; writing—original draft preparation, F.M., M.-P.Z. and J.R.; writing—review and editing, F.M., M.-P.Z., J.R. and I.G.; supervision, M.-P.Z. and J.R.; project administration, M.-P.Z.; funding acquisition, M.-P.Z. All authors have read and agreed to the published version of the manuscript.

Funding

M.-P.Z. and F.M. were supported by grant PID2019-104205GB-C21 funded by the MCIN/AEI/10.13039/501100011033. The work of F. Mansilla is supported by the grant PRE2020-09170, founded by MCIN/AEI/10.13039/501100011033.

Data Availability Statement

Not applicable.

Acknowledgments

This study was made possible by the JMARS and QGIS teams, who provided free and open-source tools to make planetary research affordable for everyone.

Conflicts of Interest

The authors declare no conflict of interest.

Appendix A

Table
Table A1. Compendium of analysed radargrams.
Table A1. Compendium of analysed radargrams.
Product_IdOrbit_NumberStart_TimeStop_TimeMin_LatMax_LatMin_LonMax_Lon
S_00410001410011-6-07 23:0311-6-07 23:10−2.920319.8318279.0911281.9278
S_016666011666615-2-10 3:4915-2-10 3:56−1.865620.3096279.4862282.2436
S_018229021822916-6-10 22:0016-6-10 22:07−3.398219.6182278.2445281.1048
S_018367021836727-6-10 16:5627-6-10 17:03−2.890219.8162278.958281.7788
S_01844001184403-7-10 8:353-7-10 8:43−2.982119.7163277.6721280.4944
S_026582022658228-3-12 19:4928-3-12 19:581.57131.3288280.0101283.8356
S_026793012679314-4-12 6:2414-4-12 6:34−1.01731.3151279.3546283.4961
S_027004022700430-4-12 16:5830-4-12 17:08−0.989331.3583279.1326283.2766
S_02742601274262-6-12 14:062-6-12 14:151.561529.6277279.3886282.9802
S_027637022763719-6-12 0:3819-6-12 0:471.532731.3059279.5775283.4053
S_035437013543716-2-14 18:5716-2-14 19:09−19.819619.7662278.6106283.5576
S_03564801356485-3-14 5:375-3-14 5:44−2.979319.7798278.1862281.0312
S_03607001360707-4-14 2:417-4-14 3:02−19.785249.6769273.3545282.8225
S_036281013628123-4-14 13:1423-4-14 13:36−19.778549.6844273.4422282.9112
S_03649201364929-5-14 23:4810-5-14 0:00−19.79919.7861277.974282.9227
S_03684801368486-6-14 17:386-6-14 17:50−19.818619.7668277.7591282.7086
S_036993023699318-6-14 0:5518-6-14 1:02−3.01619.7426278.8105281.6553
S_03762601376266-8-14 8:356-8-14 8:47−19.818719.7657277.7287282.6791
S_037837013783722-8-14 19:0822-8-14 19:21−19.831319.7534277.848282.7982
S_03797501379752-9-14 14:012-9-14 14:125.213739.3474280.1568284.7314
S_03804802380488-9-14 5:408-9-14 5:53−21.787519.7817278.1784283.3845
S_03922201392228-12-14 16:268-12-14 16:46−14.438149.6829273.8819282.598
S_066274016627415-9-20 14:1415-9-20 14:27−12.832629.7481277.1595282.6131
S_066828026682828-10-20 17:5528-10-20 18:040.027429.7475279.9733283.8164
S_06689402668942-11-20 21:172-11-20 21:270.024629.7443278.9569282.8028
S_069388026938816-5-21 2:1016-5-21 2:200.03629.7556279.9379283.7863
S_071874017187425-11-21 18:1025-11-21 18:15−3.950613.7761278.9445281.1334
Remotesensing 15 01357 g0a1 550
Figure A1. Traces of analysed radargrams are enumerated in Table A1. The marked red traces correspond to the positive cases, marked in bold in Table A1.
Figure A1. Traces of analysed radargrams are enumerated in Table A1. The marked red traces correspond to the positive cases, marked in bold in Table A1.
Remotesensing 15 01357 g0a1
Remotesensing 15 01357 g0a2 550
Figure A2. Paired cluttergrams (Left) and radargrams (Right) for each positive case.
Figure A2. Paired cluttergrams (Left) and radargrams (Right) for each positive case.
Remotesensing 15 01357 g0a2

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Figure 1. MOLA-derived situation map of the area of study, where the three main features of interest are located: Ascraeus Mons as the source area, Echus Chasma, where the dated lava fan is located, and Kasei Valles.
Figure 1. MOLA-derived situation map of the area of study, where the three main features of interest are located: Ascraeus Mons as the source area, Echus Chasma, where the dated lava fan is located, and Kasei Valles.
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Figure 2. Graphical description of the process used to discriminate true or false subsurface reflectors using SHARAD radargrams, here illustrated with the 3628101 radargram. (a) Track of the radargram over the lava body. (b) Our own cluttergram simulation. (c) PDS simulation cluttergram for this radargram. (d) A radargram with the reflector (blue) that reflects the signal with a travel time of 625 ns. This can be converted to an estimated depth of 76.5 m (assuming Ꜫ = 6).
Figure 2. Graphical description of the process used to discriminate true or false subsurface reflectors using SHARAD radargrams, here illustrated with the 3628101 radargram. (a) Track of the radargram over the lava body. (b) Our own cluttergram simulation. (c) PDS simulation cluttergram for this radargram. (d) A radargram with the reflector (blue) that reflects the signal with a travel time of 625 ns. This can be converted to an estimated depth of 76.5 m (assuming Ꜫ = 6).
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Figure 3. Large-scale lava flow directions from the Ascraeus/Pavonis area towards the Echus-Kasei system. MOLA-derived base map.
Figure 3. Large-scale lava flow directions from the Ascraeus/Pavonis area towards the Echus-Kasei system. MOLA-derived base map.
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Figure 4. (a) Map showing the structure of the lava flow composed of two distinguishable bodies in radargram 6689402. The orange line marks the radar trajectory. (b) A cross-sectional radargram showing the thickest layer of the fan in its northern part and the thinnest body that forms the southern lobe, and below, the corresponding cluttergram. White arrows indicate the detected reflectors. (c) A topographic profile over MOLA corresponding to the same path. The black dashed line marks the presumed original surface and the green line shows the maximum depth of the main reflector (approximately 80 m).
Figure 4. (a) Map showing the structure of the lava flow composed of two distinguishable bodies in radargram 6689402. The orange line marks the radar trajectory. (b) A cross-sectional radargram showing the thickest layer of the fan in its northern part and the thinnest body that forms the southern lobe, and below, the corresponding cluttergram. White arrows indicate the detected reflectors. (c) A topographic profile over MOLA corresponding to the same path. The black dashed line marks the presumed original surface and the green line shows the maximum depth of the main reflector (approximately 80 m).
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Figure 5. A closer view of the lava vents observed on the surface of the lava fan. Curvilinear black arrows indicate the direction of the flow.
Figure 5. A closer view of the lava vents observed on the surface of the lava fan. Curvilinear black arrows indicate the direction of the flow.
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Figure 6. Footprint of the five SHARAD tracks that show preserved reflectors. See Table A1 and Figure A1 for coordinates and traces of the twenty-seven SHARAD tracks analysed in this study.
Figure 6. Footprint of the five SHARAD tracks that show preserved reflectors. See Table A1 and Figure A1 for coordinates and traces of the twenty-seven SHARAD tracks analysed in this study.
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Figure 7. Paired cluttergram vs. radargram for the 3783701, which illustrates a positive case of a true reflector.
Figure 7. Paired cluttergram vs. radargram for the 3783701, which illustrates a positive case of a true reflector.
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Figure 8. Crater counting dating of the lava fan using Craterstats [35,37,42]. The isochrone suggests an age of 59 ± 4 Ma.
Figure 8. Crater counting dating of the lava fan using Craterstats [35,37,42]. The isochrone suggests an age of 59 ± 4 Ma.
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Figure 9. (Left) Image of pit chain observed with CTX at 7.88°N, −8.62°E. (Right) Regional context map (derived from the MOLA base map).
Figure 9. (Left) Image of pit chain observed with CTX at 7.88°N, −8.62°E. (Right) Regional context map (derived from the MOLA base map).
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Figure 10. (Left) Cluttergram, where the shallower reflectors do not appear. (Right) Radargram of a north-to-south SHARAD track, 6682802, marked in red in Figure 9, which shows bright subsurface plane parallel reflectors that are not seen in the cluttergram.
Figure 10. (Left) Cluttergram, where the shallower reflectors do not appear. (Right) Radargram of a north-to-south SHARAD track, 6682802, marked in red in Figure 9, which shows bright subsurface plane parallel reflectors that are not seen in the cluttergram.
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Table
Table 1. Maximum depth of the preserved layers at the Echus Chasma eastern fan [11].
Table 1. Maximum depth of the preserved layers at the Echus Chasma eastern fan [11].
Maximum Depths SWT (Single Wave Travel Time) at Echus Chasma Eastern Fan
Longitude (Deg. E)Latitude (Deg. N)Δt (ns)Lower Bound ε Estimated Depth (m)
ε = 6.2
(Carter et al., 2009)		Upper Bound ε Estimated Depth (m)
ε = 17.3
(Carter et al., 2009)
3607001−80.365.79637.507746
3628101−80.225.43656.257947
3649201−80.375.61693.758450
3783701−80.375.63656.257947
6689402−80.345.71600.007243
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Mansilla, F.; Zorzano, M.-P.; Giannakis, I.; Ruiz, J. Unveiling the Subsurface of Late Amazonian Lava Flows at Echus Chasma, on Mars. Remote Sens. 2023, 15, 1357. https://doi.org/10.3390/rs15051357

AMA Style

Mansilla F, Zorzano M-P, Giannakis I, Ruiz J. Unveiling the Subsurface of Late Amazonian Lava Flows at Echus Chasma, on Mars. Remote Sensing. 2023; 15(5):1357. https://doi.org/10.3390/rs15051357

Chicago/Turabian Style

Mansilla, Federico, María-Paz Zorzano, Iraklis Giannakis, and Javier Ruiz. 2023. "Unveiling the Subsurface of Late Amazonian Lava Flows at Echus Chasma, on Mars" Remote Sensing 15, no. 5: 1357. https://doi.org/10.3390/rs15051357

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