Multiple subglacial water bodies below the south pole of Mars unveiled by new MARSIS data


The detection of liquid water by the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) at the base of the south polar layered deposits in Ultimi Scopuli has reinvigorated the debate about the origin and stability of liquid water under present-day Martian conditions. To establish the extent of subglacial water in this region, we acquired new data, achieving extended radar coverage over the study area. Here, we present and discuss the results obtained by a new method of analysis of the complete MARSIS dataset, based on signal processing procedures usually applied to terrestrial polar ice sheets. Our results strengthen the claim of the detection of a liquid water body at Ultimi Scopuli and indicate the presence of other wet areas nearby. We suggest that the waters are hypersaline perchlorate brines, known to form at Martian polar regions and thought to survive for an extended period of time on a geological scale at below-eutectic temperatures.


Mars’s geological record, albeit incomplete, indicates that the climate has undergone dramatic changes throughout its history. The transfer of water between the Martian cryolithospheric and atmospheric global reservoirs is linked to orbital dynamics1. It is generally accepted that quasi-periodic variations of orbital eccentricity2 and planetary obliquity1,3,4,5 profoundly affected the Martian climate6. Proof of the effects of orbital forcing on the climate of Mars is found in the stratigraphy of the north polar layered deposits, where there is good correspondence between the timescales of layer deposition and astronomical cycles5. The relationship between orbital parameters and the actual evolution of the layered deposits at the south pole is however still largely unconstrained7,8. Under present-day climate conditions, Martian polar caps are generally assumed to be cold-based9. However, the late Noachian–early Hesperian circumpolar Dorsa Argentea Formation displays characteristic esker-like morphologies that have been interpreted as evidence of basal melting under thick ice sheets10, possibly caused by a combination of warmer and wetter past climate conditions11 and a significantly higher heat flux (~45–60 mW m–2) than at present (20–22 mW m–2)12. Furthermore, kilometre-scale tectonic deformations in the late Amazonian south polar layered deposits (SPLD)13,14 provide evidence of broad ice movement, suggesting localized basal melting of the Martian southern ice sheet under possible warmer conditions15.

The set of physical conditions conducive to basal melting at the Martian polar and subpolar regions has been explored15,16,17 via the theoretical combination of heat flow parameters that could result in ice melting at the base of the south polar ice cap. Recently, Sori and Bramson18 suggested that a high geothermal gradient (heat flux ≥72 mW m–2) is needed for basal melting of the SPLD, regardless of the salinity level. The same authors thus postulated that magmatic activity must have occurred in the region less than 1 Myr ago for a liquid water body to exist at the base of the SPLD. Evidence for late Amazonian (as young as 2 Myr) magmatic activity has been reported in the Elysium region19,20, suggesting the potential for localized high geothermal gradients on Mars in recent geological times. An anomalously high geothermal gradient is, however, not the only possible cause for temperature increases at the base of extensive ice-sheets. For example, localized basal melting of a thick early Amazonian polythermal ice sheet in Isidis Planitia was modelled by Souček et al.21, who concluded that subglacial wet areas could form under climatic and geologic conditions that are not significantly different from those on present-day Mars.

On Earth, one of the most valuable methods to detect subglacial liquid water is the radio-echo sounding (RES)22 technique, which employs bursts of radio waves to image buried geological structures in a similar fashion to active seismic prospecting. As radio waves propagate with little attenuation in ice, this method is particularly well suited to study the internal structure of the Martian polar layer deposits9 and to detect the bedrock below such deposits23. The possible identification of subsurface liquid water was one of the main goals behind the development of the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS). The sounder was launched in 2003 onboard the Mars Express spacecraft and began to collect data in the summer of 2005. After several years of data acquisition, however, the lack of any clear evidence of basal liquid water below the Martian polar caps seemed to indicate that water, if present, may be located at a greater depth than previously thought24,25. Recently, however, radar detection of subglacial liquid water in Ultimi Scopuli26, at the base of the SPLD, reignited the scientific debate about present-day stability of liquid water at the Martian polar regions. Because the nature of the body of liquid water was not addressed in detail in the previous study, our purpose here is to better constrain and define the characteristics and spatial distribution of the subglacial bright areas associated with basal liquid water and to discuss possible physical and chemical conditions that can explain the formation and persistence of such water at the Martian south polar regions.

We analysed MARSIS observations applying a methodological approach adapted from signal processing procedures commonly used in terrestrial radar sounding studies to discriminate between wet and dry subglacial basal conditions. In Antarctica22 and Greenland27, the combination of qualitative (bedrock morphology in the radar image) and quantitative (signal features) analysis is used to detect subglacial water. East Antarctica was the first area where subglacial lakes were unequivocally found by RES investigations and where specific criteria for lake detection and classification were proposed28 (Methods). Such criteria are suitable for well-defined large subglacial lakes but fail in the detection of more complex water distribution29. In Greenland, given the paucity of subglacial lakes30, the criteria tested in East Antarctica have found very limited application. In this region RES data have been mainly used to constrain the subglacial basal conditions and to define the spatial distribution of the water (ponded/thawed/frozen) at the ice-sheet bed. Recently, however, several previously undetected subglacial lakes have been found by applying some of the criteria originally used in East Antarctica31. Some of these criteria have also been applied to RES data collected in the Canadian Arctic, resulting in the discovery of the first two isolated hypersaline subglacial lakes on Earth32.

The technical characteristics of MARSIS severely limit the application of most of the criteria used in East Antarctica (Methods); conversely, the methodology tested in Greenland to discriminate between ponded water and frozen or dry basal conditions is fully applicable to MARSIS data. Such a methodology is based on signal intensity (which is an indication of the basal reflectivity), signal acuity (which is associated with the smoothness of the bed33) and bed-echo intensity variability (which detects the transition from dry to wet materials at the base of the ice34) (Methods).

The analysis presented in this work was performed on the data acquired in 134 radar profiles during multiple campaigns over Ultimi Scopuli from 2010 to 2019 (Fig. 1). We focused on a 250 × 300 km2 zone, around and including the bright area previously identified by Orosei et al.26, where we have a large data coverage (90 observations) and many radar profiles that cross each other. Given the MARSIS pulse length of about 200 m in air, the surface of the studied area can be considered smooth with elevation gently decreasing northward (Fig. 1). The basal interface (bottom of the SPLD) is clearly detectable in all radar profiles and it is thus possible to estimate the local thickness of the SPLD under the assumption that the signal velocity does not change in the entire investigated area. Immediately around the bright area the thickness of the SPLD is constant (considering the pulse length and the footprint) but at the regional scale it progressively decreases in the same direction as the surface (Fig. 2), resulting in an essentially flat basal topography (Supplementary Fig. 2). In this work we present and discuss only the data collected at 4 MHz, as it is the largest and most robust dataset (Methods).

Fig. 1: Ultimi Scopuli Mars Orbiter Laser Altimeter topographic map and location of MARSIS profiles collected in the region.

Solid white lines are super-frame data and dashed white lines are flash memory data (Methods). Red lines (observation number I, II, III, IV) highlight the radar profiles used to describe the three diagnostic parameters (Fig. 3) that were applied to discriminate between wet and dry areas. The black star indicates the centre of the bright area detected by Orosei et al.26 at 193° E and 81° S.

Fig. 2: SPLD thickness.

The thickness was computed assuming a velocity value of 163 m μs–1 (permittivity, εice = 3.4) that corresponds to water ice with 10% admixed dust. Grey areas indicate no data available.

In order to describe the meaning of the three chosen diagnostic parameters (intensity, acuity and bed-echo intensity variability) in terms of basal water detection, we selected four representative radar profiles in the investigated region (red lines in Fig. 1): two outside (observations I and II) and two across (observations III and IV) the previously detected bright area. We analysed the trend of these parameters along the observations and compared the spatial behaviour of each parameter between observations (Fig. 3). The surface values of intensity and acuity (black lines in Fig. 3) are broadly similar in both areas with limited variations along each observation, indicating a smooth and flat surface at the MARSIS wavelength. Conversely, the basal values (red lines in Fig. 3) are markedly different. In the background area, along observations I and II, basal intensity and acuity values are constant and much lower than the corresponding surface values, whereas the intensity variability is always above the surface values. These parameters suggest a low reflectivity of the basal material (−10 dB relative to the surface), a relatively rough basal interface (low acuity) and a spatially homogeneous bedrock (relatively constant intensity variability along tracks). Conversely, the observations acquired across the bright area show a marked increase of the along-track basal intensity (about 10 dB), reaching a maximum value (well above the surface values) at the centre of the bright area. Similar trends are observed in the basal acuity values, while intensity variability values change abruptly where the observations approach the bright area. According to Oswald et al.33, the occurrence of high-intensity and high-acuity values in the same location indicates the presence of ponded water, and Jordan et al.34 have shown that intensity variability values exceeding 6 dB mark the transition (edge detector) between dry and wet materials. Moreover, Dowdeswell and Siegert35 emphasized that a change in basal intensity of about 10 dB along track could be evidence of the presence of a lake, whereas smaller variations (for example, on the order of 2 dB) could indicate wet sediments or water intruded in the bedrock around a lake28. The combination of the three criteria makes the interpretation of the basal conditions along the four profiles quite robust and suggests a remarkable difference in the bed material properties between the two areas: observations I and II detected a dry (or frozen) bedrock, whereas observations III and IV crossed at least one large water ponded area.

Fig. 3: Data collected outside and inside the bright area.

From top to bottom observations are: I, II, III, IV. The black lines indicate surface parameters and the red lines basal parameters. In the right column, the dashed blue line indicates the water detection threshold (6 dB) according to Jordan et al.34.

To assess the wet/dry spatial distribution of the basal material below the SPLD, we used all observations collected in the study area (Fig. 1) and generated a basal intensity map and a basal acuity map (Fig. 4). Comparison of the two maps highlights the strong spatial correlation between the two parameters, with only a few exceptions where high values of basal acuity do not correspond to high values of basal intensity and vice versa. Therefore, following Oswald et al.33, we conclude that the basal material in the southern area is uniformly dry whereas the northern area is characterized by the presence of several basal patches of ponded water.

Fig. 4: Spatial distribution of normalized basal reflectivity and acuity.

a,b, Normalized basal reflectivity (a) and normalized basal acuity (b) computed from the radar data collected at 4 MHz. White lines highlight the same red lines (observations) shown in Fig. 1 and used for the analysis of Fig. 3. Both maps clearly show two distinct areas: an upper southern area characterized by a very low and relatively constant signal intensity (from −14 to −6 dB) and acuity (from 0.3 to 0.6), and a lower northern area characterized by several patches of high signal intensity (from −3 to 4 dB) and acuity (from 0.65 to 1).

These results corroborate the initial discovery by Orosei et al.26 of a stable body of liquid water in Ultimi Scopuli using a different and independent technique, highlighting at the same time a more extensive, complex scenario with ubiquitous water patches surrounding the subglacial lake. This is illustrated considering the correlation of the features mapped in Fig. 4 and the plots of the radar parameters of observation III (Fig. 3). The trend of basal intensity and acuity in the plots shows that the area centred at 193° E–81° S (point 0,0 in the maps) is characterized by a large body of water encircled by patchy water pools or wet areas of smaller extent. This interpretation is also supported by the intensity variability values computed on other observations partially crossing the lateral water patches (Supplementary Figs. 4 and 5). The abrupt transitions in bed material properties are still well detectable, however the variability values at the edge of the patches are slightly lower than the 6 dB threshold34, probably due to the fact that the patches are not completely intercepted by the radar footprint and/or that they consist of wet sediments or small volumes of water (Supplementary Fig. 3).

Fig. 5: Relative dielectric permittivity map computed by inverting the radar data considering all regions where the number of samples is larger than 100.

The map only shows the permittivity values retrieved from radar data having acuity values larger than 0.5 (Methods). This procedure has reduced the dimension of the study area to 90 × 120 km2. Values larger than 15 suggest the presence of liquid water.

As a final step, we applied the approach proposed by Lauro et al.36 to compute the basal water distribution map in terms of permittivity (Fig. 5), in the area where a significant number of samples are available (Supplementary Fig. 6) and where the radar profiles cross each other (Methods). The map shows that the areas with high values of basal permittivity (15–40) correspond to the smooth areas (high acuity values) shown in Fig. 4b, whereas the surroundings exhibit much lower permittivity values (about 6–8). On Earth, a permittivity value of 15 can be considered a threshold, with higher values indicating the presence of liquid water in the basal material26 and lower values indicating that the material is dry or frozen. Based on this consideration, the main body of water (with its average permittivity of ~40) has a dimension of approximately 20 × 30 km, it probably contains the largest volume of water and it is separated from the other small water pools by strips of dry basal material.

The unique combination of physical, geological, climatic and topographic conditions that could favour the formation of liquid water and its long-term survival in a subglacial lake at the base of the SPLD is, at best, a matter of speculation at this point in time. It is, however, possible to interpret relevant observations in the context of known experimental data and terrestrial analog studies to propose plausible processes for the formation and persistence of subglacial liquid water on Mars. Combining evidence from radar datasets and thermal models, subglacial hypersaline aqueous solutions were found to persist on Earth at temperatures much lower than the freezing point of water37. Thus, brines have been proposed as the most plausible form of liquid water on the Martian surface and subsurface under present-day physical conditions38.

The process of absorption of atmospheric water by perchlorates and the subsequent formation of hypersaline solutions (that is, deliquescence) was directly observed at the Phoenix landing site39. Considering that Ca-, Mg-, Na- and K-perchlorates, chlorates and hydrated chlorides40,41,42,43 are globally ubiquitous in the Martian regolith, we posit that deliquescence and the formation of brines could plausibly occur at the south polar latitudes as well. Experimental work has shown that soluble salts with low eutectic temperatures deliquesce at low relative humidity values over a wide range of temperatures, overlapping with those expected on Mars44,45,46, suggesting that brines may readily form in subpolar regions when the temperatures are in the higher range (for example, at noon). Re-crystallization of brines (efflorescence) when temperatures drop, however, is often kinetically inhibited47 because high activation energies are required for the transition from liquid to solid (ordered) states. Freezing experiments conducted under conditions similar to those on Mars have shown that perchlorate and chloride brines may exist for long times after their formation without efflorescing48,49. It is therefore plausible that once formed, brines may exist on Mars in a metastable state for an extended period of time on a geological scale50.

Orosei et al.26 suggested that the subglacial water discovered at Ultimi Scopuli could be hypersaline solutions. Subsequently, Sori and Bramson18 computed the geothermal flux at the base of the SPLD that would melt ice when Na-, Mg- and Ca-perchlorates are present in the icy mixture. They used Pestova et al.’s51 eutectics for Mg- and Ca-perchlorate aqueous solutions, and Chevrier et al.’s52 eutectics for Na-perchlorate solutions, determining that an anomalously high geothermal flux of 72 mW m–2 is required for the icy mixture to achieve the temperature of the lowest eutectic (Ca-perchlorate, 199 K). Recent experiments have shown, however, that Mg- and Ca-perchlorate–H2O solutions remain liquid in a super-cooled state at temperatures as low as 150 K (ref. 53). Mean temperatures at the Ultimi Scopuli location have been estimated to be approximately 160 K at the surface26, increasing with depth by a few to a few tens of K per km, depending on the unknown geothermal flux and thermal properties of the SPLD. These temperatures are very close to the lower boundary of super-cooled solutions, where kinetic processes are particularly important. We argue therefore that thermophysical modelling based on equilibrium conditions may not be wholly realistic in this context and propose instead that metastable conditions are likely to produce a remarkable effect, both in terms of the formation of brines and in terms of their longevity on Mars.

Recently, Arnold et al.54 used the subsurface echo time delay data presented in Orosei et al.26 to estimate the SPLD basal topography around the area of the previously detected lake26. The authors used the resulting SPLD bed elevations to calculate the subglacial hydraulic potential surface, finding that the high-reflectivity area did not correspond to any model-predicted lake location and concluding that the bright reflector should be a hydraulically isolated patch of liquid rather than a subglacial lake. This conclusion is based on a well-established methodology55,56, but we note that it depends critically on the accuracy of the basal topography, as stated also in Arnold et al.54. Orosei et al.26 cautioned that the large size of the MARSIS footprint and the diffuse nature of basal echoes outside the bright reflectors prevent a detailed and accurate reconstruction of the basal topography: simple averaging of echo time delays in overlapping footprints, which was used to estimate subglacial topography in both Orosei et al.26 and Arnold et al.54, cannot improve either horizontal or vertical resolution. By taking the vertical resolution of MARSIS (55 m in ice) as the nominal uncertainty on basal topography, it is found that the corresponding uncertainty in the hydraulic potential is about 1 MPa (Supplementary Fig. 2), which is larger than the variation of the hydraulic potential across the area surrounding the bright reflector, affecting the reliability of the local minima in the hydraulic potential.

Our methodological approach, applied to the expanded MARSIS dataset, reinforces Orosei et al.’s26 interpretation of the existence of a subglacial water body at Ultimi Scopuli and provides new evidence of the presence of other discrete wet areas nearby. It is thus reasonable to surmise that patches of ponded liquid water may be ubiquitous at the base of the SPLD, although it might prove impossible for MARSIS to detect them because surface morphologies at Ultimi Scopuli are uniquely suited to quantitative space-borne radar data analysis and such conditions may not be present elsewhere. It is our view that, in the absence of heat flow data or geological evidence pointing to geothermal anomalies, models advocating recent magmatic activity to explain melting at the base of the SPLD rely on largely speculative assumptions that disregard other key evidence acquired from planetary observations to date. We propose instead that known physical and chemical properties of hypersaline aqueous solutions provide a viable interpretive framework based on current observations and measurements of properties of the Martian surface and subsurface. We thus favour the hypothesis that SPLD basal liquid water exists because of a high concentration of dissolved salts, an interpretation consistent with our analysis of MARSIS data.

The possibility of extended hypersaline water bodies on Mars is particularly exciting because of the potential for the existence of microbial life, such as extremophiles, anaerobes57 or even aerobes (considering that the solubility of O2 in brines is up to six times the minimum level required for microbial respiration58). The water bodies at the base of the SPLD therefore represent areas of potential astrobiological interest and planetary protection concern, and future missions to Mars should target this region to acquire experimental data in relation to the basal hydrologic system, its chemistry and traces of astrobiological activity.



MARSIS is a nadir-looking pulse-limited radar sounder that can operate in two main observational modalities: subsurface mode and active ionosphere sounding mode. In subsurface mode, MARSIS transmits a 250 µs chirp with a 1 MHz bandwidth. According to the predicted solar zenith angle, the chirp central frequency is selected among 4 different values (1.8, 3, 4 and 5 MHz) to work well above the cut-off plasma frequency of the Martian ionosphere26. After range compression and Hanning windowing, the achievable range resolution in pure ice is about 55 m (assuming a velocity of 170 m µs–1). In this work, we only analysed unprocessed data to avoid the uncertainty due to the incoherent integration performed on-board in normal mode26. Two alternative data acquisition methods were used59: (1) the flash memory technique, which collects discontinuous intervals of unprocessed/raw data along orbits; and (2) the superframe acquisition mode, which continuously collects data but along shorter orbits (Fig. 1).

MARSIS data were collected in different years (2010–2019) and during different Martian seasons, therefore each observation refers to particular conditions of the Martian ionosphere. Because the ionosphere can cause dispersion of the transmitted signal, reducing the echo intensity and producing a broadening of the received signal, we normalized all quantities (that is, surface and basal intensity and acuity) to the median of the relevant surface quantity along each observation. In particular, the use of the median minimizes the effects caused by local surface echo power fluctuations, which are sometimes observed in the data, without altering the along-track variation of the basal reflectivity and acuity.

The 4 MHz dataset was the most complete, and therefore we applied our analysis to this specific dataset to improve the robustness of our statistical analysis. The data collected at the other frequencies are sparser (especially at 3 MHz, which is also more affected by the ionosphere) and thus less statistically significant (Supplementary Fig. 1). Despite this fact, the analysis of such data supports the results obtained at 4 MHz.

Radar signal features for subglacial water detection

Historically, four specific criteria have been proposed to identify and categorize the subglacial lakes in East Antarctica28: (1) standard deviation of the echo strength (values lower than 3 dB indicate that the basal interface is smooth at the scale of the radar footprint); (2) high echo strength relative to the immediate surroundings; (3) absolute echo strength (related to the basal reflection coefficient); and (4) the assumption that a subglacial lake is hydraulically flat28. According to such criteria East Antarctic subglacial lakes have been classified as: ‘definite lakes’, at least partially satisfying all four criteria; ‘dim lakes’, which satisfy the first two quantitative criteria; ‘fuzzy lakes’, which only satisfy the absolute and relative signal intensity requirements; ‘indistinct lakes’, characterized by low standard deviation in echo intensity; and ‘failing lakes’, which only satisfy one of the four criteria28. Recently, however, such criteria have been partially modified and updated to identify more complex subglacial water distribution (for example, active lakes) by using the specularity content, which is related to the variations in the angular distribution of radar bed-echo scattering29,60.

MARSIS is, in principle, similar to the systems used in RES investigations, but several aspects prevent the application of most of the East Antarctica criteria28. Given the operating frequency (1.8–5 MHz), the antenna dimension (40 m) and the altitude of the spacecraft (250–900 km), MARSIS pulse-limited radius footprint is very large (from 6 to 11 km) compared with footprints of the common RES radar allocated on airborne platforms and working at higher frequencies (typically of the order of 100 m). The bright area below the SPLD interpreted as a stable body of liquid water26 was estimated to be approximately 20 km in extent, that is, comparable to the dimension of the MARSIS pulse-limited footprint. For these reasons, it is not possible to compute the standard deviation of the echo strength (first criterion in Carter et al.28). Moreover, as the MARSIS antenna could not be calibrated26 and the signal absorption in the SPLD is not well constrained, the absolute echo strength (second criterion in Carter et al.28) cannot be applied. Finally, the vertical (55 m in ice) and horizontal (7 km) resolution of MARSIS prevents a detailed characterization of the bedrock morphology, topography and hydraulic potential (fourth criterion in Carter et al.28), as the uncertainties associated with the estimation of these parameters are similar in magnitude to the range of measured variations (Supplementary Fig. 2).

Spatial smoothing and acuity

We processed MARSIS data according to the method developed by Oswald and Gogineni27, which applies an along-track average to the radar traces (spatial smoothing) in order to reduce the power variance due to variable roughness27. In our analysis, the along-track waveform averaging window W is set equal to the diameter of the pulse-limited footprint area:

$$W = 2\sqrt {c\frac{p}{2}\left( {H + \frac{z}{n}} \right)} \cong 2\sqrt {c\frac{p}{2}H} ,$$

where p = 1 μs is the transmitted pulse length, H is the spacecraft altitude (this quantity can vary between 250 and 900 km), c is the velocity of light in a vacuum, z is the depth of the reflector and n 1.71 is the water ice refractive index. For example, considering a spacecraft height H = 400 km the resulting window is W 15 km.

In addition, we computed the acuity Ac, which is an indication of interface roughness, from the depth aggregated echo power33 as follows:

$$A_{\mathrm{c}} = \frac{{{\mathrm{max}}\left\{ {x_{\mathrm{r}}^2(t)} \right\}}}{{\mathop {\sum }\nolimits_{t = \tau - T/2}^{\tau + T/2} x_{\mathrm{r}}^2(t)}},$$

where xr(t) is the received pulse generated by a reflector located at a time delay τ (for example, surface or bedrock) and \(T = \sqrt {\frac{H}{{2\nu c}}}\) (v is the operating frequency).

Basal topography and hydraulic potential

We computed the basal topography (B) and the hydraulic potential (ϕH) along the observations reported in Fig. 3 according to the following equations28:

$$B = S - h$$


$$\phi _{\mathrm{H}} = \rho _{\mathrm{w}}g_{\mathrm{M}}(S - h(1 - \rho _{{\mathrm{ice}}}/\rho _{\mathrm{w}})),$$

where S is the surface topography (based on the Mars Orbiter Laser Altimeter data), h is the SPLD thickness computed assuming a permittivity εice = 3.4, ρw = 1,980 kg m–3 is the density of the perchlorate solution17, ρice = 1,100 kg m–3 the average density of the SPLD61 and gM = 3.72 m s–2 is the Martian gravity (Supplementary Fig. 2). The uncertainties Δu associated with these parameters (where u = B or u = ϕH, depending on the used equation) have been computed applying the statistical propagation formula, under the assumption that all uncertainties are independent and uncorrelated:

$${\mathrm{\Delta }}u = \sqrt {\mathop {\sum }\limits_i \left( {\frac{{\partial u}}{{\partial x_i}}{\mathrm{\Delta }}x_i} \right)^2}$$

where xi are the variables (for example S, h, ...) in equations (3) and (4) and Δxi the associated uncertainties. In equation (5), Δh = 61 m, ΔS = 61 m and Δρice = 115 kg m–3. Note that we have neglected the uncertainties related to the density of perchlorate brines and Martian gravity.

Bed-echo intensity variability

We used the intensity variability parameter σI to localize the transition between dry (or frozen) and wet bed conditions34. The parameter σI is given by:

$$\sigma _{\mathrm{I}} = {\mathrm{\Delta }}R\sqrt {f^2\left( {1 - f} \right) + \left( {1 - f} \right)^2f}$$


$${\mathrm{\Delta}} R = 20{\it{{\mathrm{log}}}}_{10}\left( {\left| {\frac{{\sqrt {\varepsilon _{\mathrm{b}}} - \sqrt {\varepsilon _{{\mathrm{ice}}}} }}{{\sqrt {\varepsilon _{\mathrm{b}}} + \sqrt {\varepsilon _{{\mathrm{ice}}}} }}} \right|\left| {\frac{{\sqrt {\varepsilon _{{\mathrm{dry}}}} + \sqrt {\varepsilon _{{\mathrm{ice}}}} }}{{\sqrt {\varepsilon _{{\mathrm{dry}}}} - \sqrt {\varepsilon _{{\mathrm{ice}}}} }}} \right|} \right)$$

With εb the dielectric permittivity of the basal material, εice the permittivity of the SPLD and εdry the permittivity of the dry rock. In addition, f is the fraction of wet area (wet–dry mixing ratio in Jordan et al.34) inside the radar footprint. Supplementary Fig. 3 illustrates the intensity variability as a function of the basal permittivity for three values of the mixing ratio f, assuming a threshold of 15 for the permittivity of wet materials26.

We computed the intensity variability σI (expressed in dB) along each orbit at xi position, as follows:

$$\sigma _{\mathrm{I}}(x_i) = \frac{{10}}{{{\mathrm{ln}}(10)}}\frac{{\sqrt {\frac{1}{N}\mathop {\sum }\nolimits_{x = x_i - W/2}^{x_i + W/2} \left[ {P_{{\mathrm{ag}}}\left( x \right) - \langle P_{{\mathrm{ag}}}\left( {x_i} \right) \rangle } \right]^2} }}{{ \langle P_{{\mathrm{ag}}}\left( {x_i} \right) \rangle }}$$

where Pag(x) is the aggregated power computed according to Jordan et al.34, and \({{ \langle P_{{\mathrm{ag}}}\left( {x_i} \right) \rangle }}\) is the average echo power:

$$\langle P_{{\mathrm{ag}}}\left( {x_i} \right) \rangle = \frac{1}{N}\mathop {\sum }\limits_{x = x_i - W/2}^{x_i + W/2} P_{{\mathrm{ag}}}\left( x \right)$$

The observations collected around the bright area show specific values of the bed-echo intensity variability. In particular, the radar observations (A and D in Supplementary Fig. 5) crossing approximately the centre of the main body of liquid water (Fig. 3 and Supplementary Figs. 4 and 5) exhibit an intensity variability exceeding the fairly conservative threshold of 6 dB (ref. 34) and therefore clearly indicate a transition from dry to wet basal material. On the other hand, the observations passing on the edge of the main body or on the other patches (B, C, E and F in Supplementary Fig. 5), even if still showing an abrupt change in intensity variability, do not exceed 4–5 dB. These results can be explained considering the intersection between the radar footprint and the bed conditions (dry/wet), which is accounted for by the parameter f. Indeed, wet areas smaller than the radar footprint (that is, having a low fraction of wet material illuminated by the radar antenna) cannot generate abrupt intensity variability as high as 6 dB, but can still indicate a transition in the basal conditions from dry to wet (Supplementary Figs. 35).

Permittivity map

The basal permittivity map was generated by applying an inversion probabilistic approach to the intensity values collected along the radar profiles shown in Fig. 1b. The procedure and the parameters used are reported in Lauro et al.36.

To generate the map reported in Fig. 5 we first applied a mesh refinement technique to obtain pixels containing about 100 samples; all pixels having fewer samples were discarded. For each pixel we computed a probability density function of the basal permittivity and assigned the median value of such distribution to the pixel coordinates in the scatter map (Supplementary Fig. 6). Our analysis was focused on the area having the highest pixel density (white dashed box in Supplementary Fig. 6) that was interpolated to generate a contour map (Fig. 5). Nevertheless, the areas with lower pixel densities (outside the white dashed box) are very consistent (spatial continuity) and characterized by low permittivity values (dry rocks) except for a small area in the northeast, where the permittivity values are higher. This latter area was not included in the analysis given the low MARSIS coverage and the lack of crossing orbits.

Note that neither the surface nor basal roughness were accounted for in the inversion procedure. In the area, the surface is very smooth at the MARSIS scale62 whereas the basal roughness is not well constrained. Therefore, the basal permittivity computed with the inversion could be, in principle, underestimated63; to mitigate such an effect the permittivity values associated with acuity values lower than 0.5 (half of the maximum acuity33) were filtered off the map (Fig. 5). Note that the subsurface and surface acuity values for the main body of liquid water are similar (Fig. 3b) and the acuity values computed for the other patches of water are only slightly lower, suggesting that, if present, the underestimation of the permittivity should be small.

Data availability

Data reported in this paper are available through the Zenodo research data repository (

Code availability

The code used to produce the figures and numerical results stated in the text is available from the corresponding author on reasonable request.


  1. 1.

    Laskar, J. et al. Long term evolution and chaotic diffusion of the insolation quantities of Mars. Icarus 170, 343–364 (2004).

    ADS  Google Scholar 

  2. 2.

    Murray, B. C., Ward, W. R. & Yeung, S. C. Periodic insolation variations on Mars. Science 180, 638–640 (1973).

    ADS  Google Scholar 

  3. 3.

    Ward, W. R. Large-scale variations in the obliquity of Mars. Science 181, 260–262 (1973).

    ADS  Google Scholar 

  4. 4.

    Ward, W. R. in Mars (eds Kieffer, H. H. et al.) 298–320 (Univ. Arizona Press, 1992).

  5. 5.

    Laskar, J., Levrard, B. & Mustard, J. F. Orbital forcing of the Martian polar layered deposits. Nature 419, 375–377 (2002).

    ADS  Google Scholar 

  6. 6.

    Byrne, S. The polar deposits of Mars. Annu. Rev. Earth Planet. Sci. 37, 535–560 (2009).

    ADS  Google Scholar 

  7. 7.

    Guallini, L. et al. Regional stratigraphy of the south polar layered deposits (Promethei Lingula, Mars): “discontinuity-bounded” units in images and radargrams. Icarus 308, 76–107 (2018).

    ADS  Google Scholar 

  8. 8.

    Smith, I. B. et al. 6th International Conference on Mars Polar Science and Exploration: conference summary and five top questions. Icarus 308, 2–14 (2018).

    ADS  Google Scholar 

  9. 9.

    Phillips, R. J. et al. Mars north polar deposits: stratigraphy, age, and geodynamical response. Science 320, 1182–1185 (2008).

    ADS  Google Scholar 

  10. 10.

    Head, J. W. & Pratt, S. Extensive Hesperian-aged south polar ice sheet on Mars: evidence for massive melting and retreat, and lateral flow and ponding of meltwater. J. Geophys. Res. 106, 12275–12299 (2001).

    ADS  Google Scholar 

  11. 11.

    Fastook, J. L., Head, J. W., Marchant, D. R., Forget, F. & Madeleine, J.-B. Early Mars climate near the Noachian–Hesperian boundary: independent evidence for cold conditions form basal melting of the south polar ice sheet (Dorsa Argentea Formation) and implications for valley network formation. Icarus 219, 25–40 (2012).

    ADS  Google Scholar 

  12. 12.

    Grott, M. et al. Long-term evolution of the Martian crust-mantle system. Space Sci. Rev. 174, 49–111 (2013).

    ADS  Google Scholar 

  13. 13.

    Grima, C. et al. Large asymmetric polar scarps on Planum Australia, Mars: characterization and evolution. Icarus 212, 96–109 (2011).

    ADS  Google Scholar 

  14. 14.

    Guallini, L., Brozzetti, F. & Marinangeli, L. Large-scale deformational systems in the South Polar Layered Deposits (Promethei Lingula, Mars): “soft-sediment” and deep-seated gravitational slope deformations mechanisms. Icarus 220, 821–843 (2012).

    ADS  Google Scholar 

  15. 15.

    Guallini, L. et al. “Unconformity-bounded” stratigraphic units in the South Polar Layered Deposits (Promethei Lingula, Mars). In STRATI 2013 331–335 (Springer, 2014).

  16. 16.

    Wieczorek, M. A. Constraints on the composition of the Martian south polar cap from gravity and topography. Icarus 196, 506–517 (2008).

    ADS  Google Scholar 

  17. 17.

    Fisher, D. A., Hecht, M. H., Kounaves, S. P. & Catling, D. C. A perchlorate brine lubricated deformable bed facilitating flow on the north polar cap of Mars: possible mechanism for water table recharging. J. Geophys. Res. 115, E00E12 (2010).

    ADS  Google Scholar 

  18. 18.

    Sori, M. M. & Bramson, A. M. Water on Mars, with a grain of salt: local heat anomalies are required for basal melting of ice at the south pole today. Geophys. Res. Lett. 46, 1222–1231 (2019).

    ADS  Google Scholar 

  19. 19.

    Hamilton, C. W., Fagents, S. A. & Wilson, L. Explosive lava-water interactions in Elysium Planitia, Mars: geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups. J. Geophys. Res. 115, E09006 (2010).

    ADS  Google Scholar 

  20. 20.

    Horvath, D. G. & Andrews-Hanna, J. C. The thickness and morphology of a young pyroclastic deposit in Cerberus Palus, Mars: implications for the formation sequence. In 49th Lunar Planet. Sci. Conference Abstract number 2435 (Lunar and Planetary Institute, 2018).

  21. 21.

    Souček, O., Bourgeois, O., Pochat, S. & Guidat, T. A 3 Ga old polythermal ice sheet in Isidis Planitia, Mars: dynamics and thermal regime inferred from numerical modeling. Earth Planet. Sci. Lett. 426, 176–190 (2015).

    ADS  Google Scholar 

  22. 22.

    Siegert, M. J. A 60-year international history of Antarctic subglacial lake exploration. J. Geol. Soc. Lond. 461, 7–21 (2018).

    Google Scholar 

  23. 23.

    Picardi, G. et al. Radar soundings of the subsurface of Mars. Science 310, 1925–1928 (2005).

    ADS  Google Scholar 

  24. 24.

    Clifford, S. M. et al. Depth of the Martian cryosphere: revised estimates and implications for the existence and detection of subpermafrost groundwater. J. Geophys. Res. 115, E07001 (2010).

    ADS  Google Scholar 

  25. 25.

    Lasue, J., Clifford, S. M., Conway, S. J., Mangold, N. & Butcher, F. E. in Volatiles in the Martian Crust 185–246 (Elsevier, 2019).

  26. 26.

    Orosei, R. et al. Radar evidence of subglacial liquid water on Mars. Science 361, 490–493 (2018).

    ADS  Google Scholar 

  27. 27.

    Oswald, G. K. A. & Gogineni, S. P. Recovery of subglacial water extent from Greenland radar survey data. J. Glaciol. 54, 94–106 (2008).

    ADS  Google Scholar 

  28. 28.

    Carter, S. P. et al. Radar-based subglacial lake classification in Antarctica. Geochem. Geophys. Geosys. 8, Q03016 (2007).

    ADS  Google Scholar 

  29. 29.

    Young, D. A., Schroeder, D. M., Blankenship, D. D., Kempf, S. D. & Quartini, E. The distribution of basal water between Antarctic subglacial lakes from radar sounding. Phil. Trans. R. Soc. A 374, 20140297 (2016).

    ADS  Google Scholar 

  30. 30.

    Palmer, S. J. et al. Greenland subglacial lakes detected by radar. Geophys. Res. Lett. 40, 6154–6159 (2013).

    ADS  Google Scholar 

  31. 31.

    Bowling, J. S., Livingstone, S. J., Sole, A. J. & Chu, W. Distribution and dynamics of Greenland subglacial lakes. Nat. Commun. 10, 2810 (2019).

    ADS  Google Scholar 

  32. 32.

    Rutishauer, A. et al. Discovery of a hypersaline subglacial lake complex beneath Devon Ice Cap, Canadian Arctic. Sci. Adv. 4, eaar4353 (2018).

    ADS  Google Scholar 

  33. 33.

    Oswald, G. K., Rezvanbehbahani, S. & Stearns, L. A. Radar evidence of ponded subglacial water in Greenland. J. Glaciol. 64, 711–729 (2018).

    ADS  Google Scholar 

  34. 34.

    Jordan, T. M. et al. A constraint upon the basal water distribution and thermal state of the Greenland Ice Sheet from radar bed echoes. Cryosphere 12, 2831–2854 (2018).

    ADS  Google Scholar 

  35. 35.

    Dowdeswell, J. A. & Siegert, M. J. The physiography of modern Antarctic subglacial lakes. Glob. Planet. Change 35, 221–236 (2003).

    ADS  Google Scholar 

  36. 36.

    Lauro, S. E. et al. Liquid water detection under the south polar layered deposits of Mars—a probabilistic inversion approach. Remote Sens. 11, 2445 (2019).

    ADS  Google Scholar 

  37. 37.

    Hubbard, A., Lawson, W., Anderson, B., Hubbard, B. & Blatter, H. Evidence for subglacial ponding across Taylor Glacier, Dry Valleys, Antarctica. Ann. Glaciol. 39, 79–84 (2004).

    ADS  Google Scholar 

  38. 38.

    Brass, G. W. Stability of brines on Mars. Icarus 42, 20–28 (1980).

    ADS  Google Scholar 

  39. 39.

    Rennó, N. O. et al. Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site. J. Geophys. Res. 114, E00E03 (2009).

    Google Scholar 

  40. 40.

    Hecht, M. H. et al. Detection of perchlorate and soluble chemistry of Martian soil at the Phoenix Lander site. Science 325, 64–67 (2009).

    ADS  Google Scholar 

  41. 41.

    Osterloo, M. M., Anderson, F. S., Hamilton, V. E. & Hynek, B. M. Geologic context of proposed chloride‐bearing materials on Mars. J. Geophys. Res. 115, E10012 (2010).

    ADS  Google Scholar 

  42. 42.

    Hanley, J., Chevrier, V. F., Berget, D. J. & Adams, R. D. Chlorate salts and solutions on Mars. Geophys. Res. Lett. 39, L08201 (2012).

    ADS  Google Scholar 

  43. 43.

    Glavin, D. P. et al. Evidence for perchlorates and the origin of chlorinated hydrocarbons detected by SAM at the Rocknest Aeolian deposit in Gale Crater. J. Geophys. Res. 118, 1955–1973 (2013).

    Google Scholar 

  44. 44.

    Zorzano, M.-P., Mateo-Martí, E., Prieto-Ballesteros, O., Osuna, S. & Renno, N. Stability of liquid saline water on present day Mars. Geophys. Res. Lett. 36, L20201 (2009).

    ADS  Google Scholar 

  45. 45.

    Gough, R. V., Chevrier, V. F. & Tolbert, M. A. Formation of aqueous solutions on Mars via deliquescence of chloride–perchlorate binary mixtures. Earth Planet. Sci. Lett. 393, 73–82 (2014).

    ADS  Google Scholar 

  46. 46.

    Gough, R. V., Chevrier, V. F. & Tolbert, M. A. Formation of liquid water at low temperatures via the deliquescence of calcium chloride: implications for Antarctica and Mars. Planet. Space Sci. 131, 79–87 (2016).

    ADS  Google Scholar 

  47. 47.

    Gough, R. V., Chevrier, V. F., Baustian, K. J., Wise, M. E. & Tolbert, M. A. Laboratory studies of perchlorate phase transitions: support for metastable aqueous perchlorate solutions on Mars. Earth Planet. Sci. Lett. 312, 371–377 (2011).

    ADS  Google Scholar 

  48. 48.

    Primm, K. M., Gough, R. V., Chevrier, V. F. & Tolbert, M. A. Freezing of perchlorate and chloride brines under Mars-relevant conditions. Geochim. Cosmochim. Acta 212, 211–220 (2017).

    ADS  Google Scholar 

  49. 49.

    Primm, K. M., Stillman, D. E. & Michaels, T. I. Investigating the hysteretic behavior of Mars-relevant chlorides. Icarus 342, 113342 (2020).

    Google Scholar 

  50. 50.

    Toner, J. D. & Catling, D. C. Chlorate brines on Mars: implications for the occurrence of liquid water and deliquescence. Earth Planet. Sci. Lett. 497, 161–168 (2018).

    ADS  Google Scholar 

  51. 51.

    Pestova, O. N., Myund, L. A., Khripun, M. K. & Prigaro, A. V. Polythermal study of the systems M(ClO4)2-H2O (M2+ = Mg2+, Ca2+, Sr2+, Ba2+). Russ. J. Appl. Chem. 78, 409–413 (2005).

    Google Scholar 

  52. 52.

    Chevrier, V. F., Hanley, J. & Altheide, T. S. Stability of perchlorate hydrates and their liquid solutions at the Phoenix landing site, Mars. Geophys. Res. Lett. 36, L10202 (2009).

    ADS  Google Scholar 

  53. 53.

    Toner, J. D., Catling, D. C. & Light, B. The formation of supercooled brines, viscous liquids, and low-temperature perchlorate glasses in aqueous solutions relevant to Mars. Icarus 233, 36–47 (2014).

    ADS  Google Scholar 

  54. 54.

    Arnold, N. S., Conway, S. J., Butcher, F. E. & Balme, M. R. Modeled subglacial water flow routing supports localized intrusive heating as a possible cause of basal melting of Mars' south polar ice cap. J. Geophys. Res. 124, 2101–2116 (2019).

    Google Scholar 

  55. 55.

    Willis, I. C., Pope, E. L., Gwendolyn, J. M., Arnold, N. S. & Long, S. Drainage networks, lakes and water fluxes beneath the Antarctic ice sheet. Ann. Glaciol. 57, 96–108 (2016).

    ADS  Google Scholar 

  56. 56.

    Livingstone, S., Clark, C., Woodward, J. & Kingslake, J. Potential subglacial lake locations and meltwater drainage pathways beneath the Antarctic and Greenland ice sheets. Cryosphere 7, 1721–1740 (2013).

    ADS  Google Scholar 

  57. 57.

    Maus, D. et al. Methanogenic archaea can produce methane in deliquescence-driven Mars analog environments. Sci. Rep. 10, 6 (2020).

    ADS  Google Scholar 

  58. 58.

    Stamenković, V., Ward, L. M., Mischna, M. & Fischer, W. W. O2 solubility in Martian near-surface environments and implications for aerobic life. Nat. Geosci. 11, 905–909 (2018).

    ADS  Google Scholar 

  59. 59.

    Cicchetti, A. et al. Observations of Phobos by the Mars Express radar MARSIS: description of the detection techniques and preliminary results. Adv. Space Res. 60, 2289–2302 (2017).

    ADS  Google Scholar 

  60. 60.

    Schroeder, D. M., Blankenship, D. D. & Young, D. A. Evidence for a water system transition beneath Thwaites Glacier, West Antarctica. Proc. Natl Acad. Sci. USA 110, 12225–12228 (2013).

    ADS  Google Scholar 

  61. 61.

    Li, J. et al. Density variations within the south polar layered deposits of Mars. J. Geophys. Res. 117, E04006 (2012).

    ADS  Google Scholar 

  62. 62.

    Mouginot, J. et al. MARSIS surface reflectivity of the south residual cap of Mars. Icarus 201, 454–459 (2009).

    ADS  Google Scholar 

  63. 63.

    Lauro, S. E. et al. Dielectric constant estimation of the uppermost Basal Unit layer in the Martian Boreales Scopuli region. Icarus 219, 458–467 (2012).

    ADS  Google Scholar 

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This work was supported by the Italian Space Agency (ASI) through contract ASI-INAF 2019–21-HH.0 and, in part, by EU H2020 agreement 776276 Planmap. MARSIS is operating onboard the European Space Agency spacecraft Mars Express. We would like to thank S. E. Beaubien for careful proofreading of the manuscript and improvement of the English.

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S.E.L. and E.P. designed the research, developed the methodology, performed data analysis and wrote the manuscript. G.C., L.G. and A.P.R. developed the geological context and contributed to writing relevant sections of the manuscript. G.C. and E.P. developed and wrote the geochemical discussion. E.M. and B.C. performed data analysis, contributed text and figures, and co-wrote the manuscript. A.C. conducted data pre-processing. F.S. contributed to inverse electromagnetic modelling, to the interpretation of the geophysical data and to writing of the manuscript. M.C. contributed to data acquisition and analysis and discussed ideas. F.D.P. contributed text and figures and discussed ideas. R.N. contributed to data acquisition and analysis. R.O. discussed ideas and co-wrote the manuscript. S.E.L., E.P., G.C., L.G., A.P.R., E.M., B.C., F.S. and R.O. edited and revised the manuscript.

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Correspondence to Elena Pettinelli.

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Lauro, S.E., Pettinelli, E., Caprarelli, G. et al. Multiple subglacial water bodies below the south pole of Mars unveiled by new MARSIS data. Nat Astron (2020).

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