Testing Correspondence between Areas with Hydrated Minerals, as Observed by CRISM/MRO, and Spots of Enhanced Subsurface Water Content, as Found by DAN along the Traverse of Curiosity

Possible correlation is studied between Water Equivalent Hydrogen (WEH) in the Martian subsurface, as measured by the DAN (Dynamic Albedo of Neutrons) instrument along the Curiosity traverse, and the presence of hydrated minerals on the surface, as seen from the orbit by CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) instrument onboard MRO (Mars Reconnaissance Orbiter). Cross-analysis of the subsurface WEH values from DAN passive measurements with the distribution of hydrated minerals over the surface of Gale crater according to Specialized Browse Product Mosaics is performed for the initial 20 km part of traverse. As a result, we found an increase up to 0.4 wt% of the mean WEH value for the surface areas with the spectral signatures of polyhydrated sulfates. The increase is shown to be higher with the more prominent spectral signature on the surface. Similar WEH increase for the two other types of hydrated minerals, such as monohydrated sulfates and phyllosilicates, was not found for the tested part of the traverse. Polyhydrated sulfates being a part of the sedimentary deposits composing the surface of Gale crater should have considerable thickness that is necessary for the subsurface neutron sensing by DAN measurements.


Introduction
Gale crater was presumably formed during the late Noachian period (about 3.7-3.8 Ga) as a result of a large meteorite impact [1]. Its radius is about 150 km, and its initial depth is thought to be about 5 km. In its evolutional history from formation to the modern time, one may conditionally distinguish two main stages [2,3]. e first stage corresponds to the Noachian period with a possibly warm and humid climate on the planet (or at least with episodic warm conditions), when Mars had a rather dense atmosphere. During this stage, the crater could be occasionally filled up with water and turned into a lake, at the bottom of which weathering of primary rocks in contact with an alkaline water environment produced phyllosilicates [4,5]. e first stage ended by the beginning of Late Hesperian, when the climate of Mars became close to modern, with a thin atmosphere and a dry and cold surface. By the end of the first stage, Gale crater is thought to be filled up with layered sedimentary deposits [6].
In the second stage, the sedimentary deposits filling Gale crater were exposed, probably by wind erosion, creating Mount Sharp-5.5 km tall central mound which is not related to the central peak formed during the impact event [7]. e lowest visible units of Mount Sharp contain a variety of minerals that are indicative of aqueous conditions. Phyllosilicate (including the groups smectite, vermiculite, illite, kaolinite, serpentine, micas, and chlorite, commonly called clay minerals) spectral signatures are observed in some stratigraphic units near the base of Mount Sharp, and sulfate-bearing minerals (such as anhydrite, bassanite, gypsum, and jarosite) are observed in younger, stratigraphically higher sedimentary units [8,9].
is mineralogical transition suggests that the conditions under which the sediments were deposited changed through time. e broad mineral stratigraphy with sulfatebearing units overlying phyllosilicate-bearing units has been recognized in similarly aged deposits globally on Mars [10]. is mineralogical succession may mark the beginning of the transition from Noachian to Hesperian, e.g., from a relatively wet and warm early Mars to a very dry and cold modern Mars [8,11].
us, the sediments on the modern surface of Gale crater represent a natural record of Mars hydrological evolution, where a study of the composition and sequence of sedimentary strata from the crater floor up to the top of its central mound allows the disclosing of the changes of environmental conditions along the chronology of their formation [6]. At present, the ground water in the Martian soil may precipitate from the current thin atmosphere forming multilayers of molecules on the grains of regolith (as adsorbed water) and filling the porosity volume between grains (as free water ice). ough there is no direct evidence of ground ice, indirect evidence for the formation of frost at the surface of Gale crater exists [12]. erefore, both kinds of water might exist currently in the shallow subsurface of Gale crater: water in the form of chemically bound molecules in hydrated minerals and water as adsorbed molecules in the regolith. e presence of water in the subsurface of Gale crater is proved by the DAN active neutron sensing experiment onboard the Curiosity rover [13][14][15]. is paper presents the results of the comparative analysis of subsurface water abundance, as derived from DAN passive measurements data [16], together with data for the surface minerals distribution, as measured by CRISM onboard MRO. is analysis is thought to allow distinguishing which kind of ground water most likely exists in the subsurface along the Curiosity traverse over the bottom of Gale crater.

DAN Measurements along the Rover Traverse
e DAN instrument is an active neutron detector for sensing the subsurface layer of about 60 cm thickness by pulses of 14 MeV neutrons, produced by the pulsing neutron generator-PNG [15]. Pulses of neutrons produce the postpulse emission or Dynamic Albedo of Neutrons. Two DAN neutron counters record the time profiles of postpulse total neutron emission: CTN at thermal and epithermal energy range and CETN at epithermal energy range.
Since hydrogen in the Martian subsurface is most likely a part of either hydroxyl or water molecules, its content is conventionally measured in terms of Water Equivalent Hydrogen (WEH). On the other hand, the content of the neutron absorbing nuclei in the subsurface is evaluated by a single measurable parameter of the so-called Absorption Equivalent Chlorine-AEC [17]. Chlorine is selected because it is considered the major contributor to neutron absorption in the Martian regolith. e value of AEC takes into account not only the mass fraction of chlorine itself, but also all other absorbers in the subsurface matter, if their mass fractions differ from the values predicted by the so-called "standard composition" model of the Martian soil [18].
DAN started operating on Mars on August 12, 2012, just after the rover landing [19]. e data for the current analysis were obtained since that time until November 2018. at corresponds to 2218 sols and 19 971 m distance along the traverse. According to the rover flight rules, DAN active operations are only allowed at rover stops. us, estimates of WEH and AEC based on active measurements are available for the rover parking spots only [13]. For the first 20 km part of the rover traverse until sol 2218, the mean WEH and AEC values are found to be (2.6 ± 0.7) wt% and (1.0 ± 0.1) wt%, respectively [13].
While PNG operates only during active sessions lasting for 15-30 minutes at stops, DAN counters are working almost continuously, both at rover stops and during drives. When PNG is off, neutron counters continuously measure the local neutron emission. Flux and energy spectra of the surface albedo neutrons produced both by the Multi-Mission Radioisotope ermoelectric Generator and Galactic Cosmic Rays largely depend on the presence of hydrogen, measured as WEH, and neutron absorbers, measured as AEC, in the subsurface matter.
us, DAN continuous passive measurements give an opportunity to determine the WEH value at any particular spot below the rover along the traverse [16].
A special procedure of DAN passive data processing has been developed based on the empirically found relationships between active and passive data, measured simultaneously at the total number of 328 rover stops (see [16], for details).
is empirical relationship, as well as the knowledge on the AEC, is used for obtaining the continuous profile of WEH values. e physical size of an individual spot on the surface for passive neutron sensing is shown to be about 3 meters in diameter [17], so the physical resolution of WEH variations along the traverse could be associated with such scale.
Distances between the rover stops vary from several meters up to hundreds of meters. To estimate AEC between two stops along the traverse, one needs to make an additional assumption for the scale of AEC spatial variations. It was suggested by [16], to use two approaches. e first one assumes a long-range (LR) scaling of AEC variability, when a smooth interpolation of AEC value is thought to be applicable along the path from one stop to another. In this case, the AEC value at each point between two stops could be derived from the interpolated values of active measurements at these stops. e second approach postulates that AEC might vary at a scale of several meters or so, presuming a short-range (SR) scaling of the AEC variability. In this case, the AEC value at each intermediate point of the traverse between two stops is thought to be randomly distributed according to the entire data set of the active measurements. For the part of the rover traverse studied in this paper, the mean AEC value for all active measurements is found to be equal to (1.0 ± 0.1) wt%.
After processing DAN passive data until sol 2218, two continuous profiles of the WEH spatial variability were obtained with a distance resolution of 3 meters using LR and/or SR approaches (Figure 1). e WEH value was found to vary from around zero to 6.3 wt% [16]. ese data were used for cross-analysis with CRISM spectral data products; see below.

CRISM Data Products for Cross-Analysis with DAN Data
CRISM instrument onboard the NASA MRO spacecraft performs imaging spectrometry in the visible and near-infrared wavelength range of 362-3920 nanometers. Such chemicals as iron, oxides, carbonates, etc. on the Martian surface have characteristic spectral features in the visible and infrared ranges and are distinguishable by CRISM [20]. For the current cross-analysis with DAN data, we used the publically available Specialized Browse Product Mosaics [21]. e CRISM team specifically created this data product for studying the Curiosity landing site. Hyperspectral images with high spatial resolution of about 20 m, not degraded by the increased noise or by atmosphere opacity, were selected as the source images for creating the products. Mathematical processing was applied to reflectance values at key wavelengths associated with diagnostic or indicative mineral  Advances in Astronomy structure on the surface. e resulting composites of individual parameters reflect the thematic mineralogical diversity of the surface. A high value in the image plane indicates a relatively strong spectral feature for the particular product as compared to the range present regionally around the landing site [21].
In our study, two Specialized Browse Product Mosaic products were of special interest: "HYD" and "ALT." Both were constructed from images in the IR spectral range, as they characterize the spectral features of minerals that are thought to be formed by the interaction of rocks with liquid water. ese two data products represent the surface distribution of such minerals as phyllosilicates (generally Fesmectites) and mono-or polyhydrated Mg-sulfates (mostly kieserite and hexahydrite, respectively). e "HYD" data product shows indicators of hydrated minerals with a focus on the hydrated sulfates, while the "ALT" data product focuses on Fe/Mg phyllosilicates on the surface.
It should be taken into account that hydrated minerals, which are believed to be present in the shallow subsurface, might not be revealed by detection of their spectral indicators on the surface as they might be covered by dust or by a thin upper layer of some different mineralogical composition. While DAN senses the subsurface down to 1 m depth, CRISM images the uppermost layer of the Martian surface. However, the deposits of hydrated minerals that spread from the top down to the subsurface should be detectable by both instruments, CRISM from the orbit and DAN from the surface. To test the presence of such deposits and to map them along the rover, traverse was the goal of the performed cross-analysis, as presented below.

Cross-Analysis of DAN Passive Data with CRISM Data Products
e total number of 1028 CRISM mapping pixels, located along the traverse of the rover, was selected. For each such pixel with the size of about 20 meters, the mean WEH value was evaluated inside it according to the DAN passive measurements data, processed by the LR and SR approaches (see Section 3, Tables 1 and 2). Uncertainties of the WEH mean values were derived from the uncertainties of WEH values of the contributed distance intervals.
For each of the three types of hydrated minerals, such as phyllosilicates, monohydrated sulfates, and polyhydrated sulfates, the testing groups of corresponding CRISM pixels were selected, which manifest the spectral signatures of these minerals. ree groups with 51, 45, and 101 CRISM pixels were identified for phyllosilicates, monohydrated sulfates, and polyhydrated sulfate, respectively. e reference group of 831 CRISM pixels with no spectral signatures of any of the three types of hydrated minerals was also composed. e method of cross-analysis of DAN and CRISM data is based on the comparison of the distribution of the mean WEH values for the testing group of CRISM pixels attributed to the particular testing mineral with the distribution of the mean WEH values for the reference group of CRISM pixels. As the simplest test, the average values and sample variances of WEH for the testing and the reference groups are compared. In addition, Pearson's chi-squared test is used for more precise testing of the statistical difference between them. Two distributions are thought to be statistically distinct, if the probability for their coincidence (p-level) is sufficiently small, p < 0.001.
One finds that there is no distinction of the distributions of WEH for groups of the CRISM pixels associated with either phyllosilicates or monohydrated sulfates from the reference group (Tables 1 and 2). For both cases of WEH estimation, using either LR or SR approach, the p-level values point out a rather good agreement between WEH distributions for testing and reference groups.
On the other hand, the evident effect of distinction from the reference group is found for the testing group of 101 CRISM pixels with the spectral signature of polyhydrated sulfates (Figure 2(a)). e differences between mean values of WEH are (0.2 ± 0.1) wt% for the LR approach (Table 1) and (0.4 ± 0.1) wt% for the SR approach (Table 2). According to Pearson's chi-squared test, the p-levels for the statistical coincidence between WEH distributions for the testing and reference groups are found to be much less than 0.001 (see Tables 1 and 2). us, the mean WEH value for the testing group of CRISM pixels, associated with the presence of polyhydrated sulfates, is confidently larger than the mean WEH value for the reference group of pixels, which do not have the spectral signature of such type of mineral.
It is reasonable to expect that the stronger spectral signature of the presence of minerals on the surface (seen as larger values in the RGB image plane) might correspond to a higher content of WEH detected by DAN in the subsurface. To check this assumption, the testing group of 101 CRISM pixels linked with polyhydrated sulfates was divided into two subgroups. e subgroup of "high intensity" includes pixels with the brightness >20 in the RGB image plane. Correspondingly, the subgroup of "low intensity" includes pixels with the brightness <20. e value of 20 was chosen as a dividing value for the total group into two statistically equal subgroups. For these two subgroups, the distributions of WEH were built, and their comparison with the reference distribution was performed (Tables 1 and 2). Figure 3 shows the WEH distributions for the testing subgroups of CRISM pixels with "high intensity" polyhydrated sulfates for the cases of LR (a) and SR (b) approaches. e more pronounced shift to larger values is evident for the WEH distributions of "high intensity" subgroup in comparison with the WEH distribution for the reference group (Figure 3). eir mean WEH values become equal to (2.9 ± 0.1) wt% and (3.1 ± 0.1) wt% for the cases of LR and SR approaches, respectively. Besides, the Pearson test proves that WEH distributions for the "high intensity" subgroup of CRISM pixels are confidently distinct from the one for the reference group. e values of the p-level are much less than 0.001 (Tables 1 and 2).
As we stated in Section 2 of this paper, the value of WEH is not measured directly, but is obtained through the modelling of active and passive measurement data and is, therefore, model-dependent. To exclude the probable effects of model dependency, we performed the similar analysis as described above for the initial measured parameter of 4 Advances in Astronomy neutron emission. Instead of the WEH value, we used the ratio of the count rates of total S CTN and epithermal S CETN neutrons emitted by the surface, namely, F DAN � S CTN / C CETN (for more details, see [16]). e results of the performed analysis are described in Table 3. e relationship between the parameters of the F DAN distributions is found to be similar to the same parameters of the WEH distributions (Tables 1 and 2). Only the distribution of F DAN for the testing group of CRISM pixels associated with the presence of polyhydrated sulfates is confidently different from the reference distribution of F DAN for the group of pixels, which do not have the spectral signature of hydrated minerals. So, one    Advances in Astronomy had to conclude that the relationship found between the presence of polyhydrated sulfates and increase of water in the shallow subsurface is not produced by WEH deconvolution procedure, but manifests physical relation between such minerals and neutron emission.

Discussion
us, the conclusion should be drawn that, along the traverse from the landing site to the distance mark of about 20 km, the presence of polyhydrated sulfates on the surface, as observed by CRISM, is consistent with the increase of WEH values within a subsurface layer of about 60 cm thickness, as measured by DAN. On the other hand, no such phenomenon is found for another group of CRISM pixels associated with the spectral signatures of phyllosilicates or monohydrated sulfates. One may speculate that the part of the traverse, which manifests the phenomenon of CRISM-DAN cross-correspondence, is associated with the sedimentary strata containing polyhydrated sulfates probably with significant thickness that leads to enhanced mass fraction of water in comparison with the "usual" subsurface with some standard mass fraction of water. e top surfaces of such matter are observable by CRISM from the Martian orbit and their deeper volumes are detectable by DAN from the Martian surface. One suggests naming such strata as layers of polyhydrated sulfates-rich matter, or PHSR matter.
To test this simplest interpretation of the found phenomenon, one might check the possibility that the observed WEH distribution in the area with PHSR matter (Figure 2) could be modeled by a bimodal function with two distinct components: the "less-WEH" component and "more-WEH" component ( Figure 4). e "less-WEH" component could be associated with the "usual" matter. Its shape could be taken from the known distribution of WEH for the reference group of CRISM pixels with no signatures of any of the three types of hydrated minerals (Figure 2). e mean values for WEH of this component are known to be equal to (2.54 ± 0.02) wt% for the LR approach and (2.40 ± 0.02) wt% for the SR approach (see Table 1). e "more-WEH" component could be associated with polyhydrated sulfates. As the simplest option, this "more-WEH" component could be represented by a normal distribution with two free parameters: the mean value and the sample variance.
Using such a bimodal model, one may try to fit the observed WEH distribution in the area of CRISM pixels with a spectral signature of polyhydrated sulfates. In addition to the two free parameters of the "more-WEH" component, one more parameter should be used for fitting: the relative fraction α of this component with respect to the total integral   Advances in Astronomy of the entire observed distribution. Two cases of the observed distributions are tested for WEH derived by either LR or SR approaches of DAN passive data processing. One-tailed Pearson's chi-squared test is applied for finding the best fitting parameters of the bimodal model (Table 4). In both cases, for LR and SR approaches, the Pearson criteria give very good p-level values for consistency between the observed distribution and the modeling function; i.e., it is between 0.001 and 0.15 (Table 4).
e "more-WEH" component has the mean WEH values equal to 3.0 or 3.6 wt % for the cases of LR and SR, respectively (Table 4 and Figure 2).
Taking into account this result, one may speculate that the two components of WEH distribution represent two fractions of PHSR matter. e "less-WEH" component corresponds to the "usual" soil and the "more-WEH" component might be attributed to deposits of polyhydrated sulfates. e bimodal approximation of the observed WEH distribution for the area of PHSR matter allows determining the fraction parameter α for the contribution of "more-WEH" component. is fraction is about 0.37 or 0.12 (as a part of 1) of the entire WEH distributions, based on either LR or SR approaches, respectively. In the case of the proposed identification, such a fraction α corresponds to the part of the subsurface volume, which contains deposits of polyhydrated sulfates with the thickness large enough for neutron sensing. Another fraction (1−α) corresponds to the "usual" soil. Interestingly, the fraction of the "more-WEH" component is approaching the value of 1 for the subgroup of 51 pixels of "high intensity" spectral signature of polyhydrated sulfates (Table 4). It is another piece of evidence for the identification of "more-WEH" component in the areas, the substances of which is the deposition of polyhydrated sulfates. e fraction of "usual" soil in the PHSR matter might exist practically everywhere along the traverse.
is substance does not contain noticeable quantities of any of the three types of hydrated minerals and has an average WEH of about 2.5 wt% (see Tables 1 and 2). e WEH value for this second fraction of PHSR matter corresponds to the number of water molecules in the structure of polyhydrated sulfates. Its value was derived from the DAN data, as about 3 wt% (Table 4). e chemically bound water of hydrated minerals was embedded in their structure long time ago, when these minerals were formed in the aqueous conditions. erefore, the type of PHS-dominated substance is thought to contain the "initial water" of Mars. e mass fraction of polyhydrated sulfates in the subsurface substance may vary along the traverse. At some spots with the most intense spectral signatures of polyhydrated sulfates, the "more-WEH" component, as shown above, may contribute the observed WEH distribution entirely. One may use the DAN passive data for testing the presence of polyhydrated sulfates in the subsurface along the traverse with the spatial resolution about hundreds meters or so.
For performing such test we split the total path of about 20 km into 132 distance intervals of 150 meters long, each including around 50 passive measurements of WEH with a spatial resolution of 3 meters. e distribution of the WEH values for each distance interval is tested by the already known bimodal function with only one variable parameter α, as the fractionation of the already known components of "less-water" and "more-water," α and 1−α, respectively. e best fitting value of α could be considered as the average mass fraction of polyhydrated sulfates in the subsurface. Performing such an analysis for all 132 distance intervals, one obtains the profile of the polyhydrated sulfates mass fraction along the traverse ( Figure 5). e profile shows that the highest value of α equal to 0.21 (the confidence is 15%) is observed at the area around a distance mark of 16,300 m. Indeed, according to the CRISM data, this area is characterized by the increased value of the spectral signature brightness for polyhydrated sulfates ( Figure 6). us, the analysis of the DAN passive data made it possible to identify sites with an increased content of polyhydrated sulfates in the shallow subsurface. One of such sites is found at the distance mark of 16,300 meters of the traverse on the way from Bagnold Dunes to Vera Rubin ridge.

Conclusions
e cross-analysis of the WEH values from the DAN passive measurements onboard Curiosity and Specialized Browse Product Mosaics of CRISM spectrometer onboard the MRO was performed for the part of the rover traverse from the landing site up to the distance mark 19 971 m. It was found that traverse intervals with the spectral signature of polyhydrated sulfates, as detected by CRISM, contain more WEH in the subsurface in comparison with the intervals that do not manifest signatures of any of the three selected types of hydrated minerals, such as phyllosilicates and mono-and polyhydrated sulfates.
is effect points out that polyhydrated sulfates exist at some places along the traverse, as layers with up to 60 cm thickness that are well detectable by DAN with its sensing depth of about 60 cm in the subsurface. e bimodal distribution of WEH was found for such distance intervals along the traverse with the spectral signature of polyhydrated sulfates. e "less-WEH" component of this distribution is consistent with the distribution observed at the dominating majority of distance intervals that do not manifest any spectral signatures of all three tested types of hydrated minerals. e average water content for this type of matter is 2.5 wt%. e "more-WEH" component of this distribution is thought to be associated with the second type of matter, whose composition is likely dominated by polyhydrated sulfates component. e value of WEH for this type is about 3 wt% or larger. e absence of any difference between WEH distributions for the distance intervals without spectral signatures of the three tested types of hydrated minerals and for distance intervals with spectral signatures of phyllosilicates and monohydrated sulfates does not necessarily make a discrepancy between CRISM and DAN observations. Indeed, the uppermost layer of the subsurface with such hydrated minerals may be seen by CRISM, but might be too thin for the detection by DAN. One may suspect that for some reason the top layers with polyhydrated sulfates are thick enough for being detected by DAN, while the top layers of phyllosilicates and monohydrated sulfates are not. e CRISM pixels with the spectral signature of polyhydrated sulfates cover about 10% of the 20 km long rover traverse that was analyzed. e fact of the large thickness of polyhydrated sulfates deposits suggests a long period of time in the past, when such layer had enough time to be accumulated. On the other hand, the areas of CRISM pixels with spectral signatures of phyllosilicates and monohydrated sulfates are most likely associated with rather thin layers on top of the ordinary rocks and soil. DAN is not sensitive to the presence of such thin layers on top of the ordinary matter. One may expect that the presence of such hydrated minerals will also be proved by cross-analysis of CRISM and DAN data, when the rover climbs up Aeolis Mons, where the deposits if phyllosilicates or monohydrated sulfates might be thick enough for the detection of the WEH increase contributed by them.

Data Availability
Data from this work are publicly accessible on the Planetary Data System, https://www.pds.nasa.gov/.
Disclosure is paper was presented at EGU General Assembly 2020 [22].

Conflicts of Interest
e authors declare that they have no conflicts of interest. Advances in Astronomy 9