# Alteration history of aluminum-rich rocks at Jezero crater, Mars

Adrian P Broz, Briony H N Horgan, Candice Bedford, Clément Royer, Henry Manelski, Stephanie Connell, Roger C Wiens, Emily C Cardarelli, Juan Manuel Madariaga, Lucia Mandon, et al.

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Adrian P Broz, Briony H N Horgan, Candice Bedford, Clément Royer, Henry Manelski, et al. Alteration history of aluminum-rich rocks at Jezero crater, Mars. Communications Earth & Environment, 2025, 6, pp.935. 10.1038/s43247-025-02856-3. hal-05404170

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# Alteration history of aluminum-rich rocks at Jezero crater, Mars

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A. P. Broz Ⓓ1,2✉, B. H. N. Horgan Ⓓ1, C. Bedford Ⓓ1, C. Royer Ⓓ3, H. Manelski¹, S. Connell¹,

R. C. Wiens Ⓓ1, E. C. Cardarelli Ⓓ4, J. M. Madariaga Ⓓ5, L. Mandon⁶,7, A. Klidaras Ⓓ1, M. Bramble Ⓓ8,

B. Kathir⁹, O. Forni Ⓓ10, John Carter¹¹, E. Dehouck Ⓓ12, C. Quantin-Nataf¹², J. R. Johnson Ⓓ13,

J. I. Nuñez Ⓓ13, E. Hausrath Ⓓ14, U. Wolf Ⓓ15, E. A. Cloutis Ⓓ16, P. Beck Ⓓ6, J. F. Bell Ⓓ17, J. I. Simon Ⓓ18 &

A. Cousin Ⓓ15,19

Aluminum-rich clay minerals are detected across the ancient surface of Mars and record intervals of intense alteration by liquid water. On Earth, these clay minerals can form from hydrothermal alteration or rainfall-driven chemical weathering over thousands to millions of years, but how they formed on Mars remains a mystery. The Perseverance rover discovered light-toned, cobble-sized, aluminum-rich (30-45 wt% Al₂O₃) “float” rocks (rock fragments), with some exhibiting spectral signatures of kaolinite, an aluminum-rich clay mineral. These rocks now enable an investigation into the ancient kaolinite-bearing terrains of Mars. To interpret their formation, we use data from the SuperCam and Mastcam-Z instruments onboard the rover to compare the chemistry and reflectance spectra of the float rocks with deeply weathered paleosols and hydrothermal kaolin deposits from Earth’s geological record. Aluminum and titanium enrichments coupled with depletion of iron and magnesium are unlike hydrothermal deposits and instead comparable to bleached horizons of paleosols that formed under high rainfall during past greenhouse climates on Earth. These rocks therefore likely represent some of the wettest intervals of Mars’ history.

The Mars 2020 Perseverance Rover has discovered several thousand small, light-toned rock fragments, or float rocks, that are spectrally and compositionally distinct from outcrops so far observed on the mission¹ (Fig. 1). This unique class of float rock was first observed on the Jezero Crater floor and later on the top of the Jezero sedimentary fan where pebble- to boulder-size clasts were identified², and so far, a total of ~20 of these light-toned float rocks have been investigated in detail with the SuperCam and Mastcam-Z instruments.

A large variety of light-toned float rocks were identified throughout the rover traverse (Fig. 1) ranging from light-to-dark toned, pebble-to-bouldersized rocks. The anomalous chemistry of the float rocks was first identified by their unique aluminum (Al)-rich compositions as determined by the SuperCam instrument¹. A large population was identified at the toe of the western Jezero sedimentary fan (Fig. 1E–H) and again near the ~1-km-wide “Belva crater” on the top of the fan (Fig. 1J). Around mission sol 912, Perseverance encountered several large lag piles (tens of square meters) containing thousands of pebble to cobble-size light-toned float rocks (Fig. 2A), with many examples exhibiting distinct spectral properties in near-infrared spectral wavelengths, likely indicating major differences in composition (Figs. 2B, C, 3).

A striking discovery was that some of the light-toned rocks have a diagnostic spectral signature of a hydrated kaolin group mineral (e.g., kaolinite, halloysite)¹ and are enriched in Al₂O₃ (~17–35 wt%) (e.g., “Chignik”, Fig. 3) with anomalously low total Fe (< 1 wt% FeOₜ, total iron as FeO) compared to other float rocks². Some of these kaolin-bearing Al-rich rocks also have elevated TiO₂ content (> 1 wt%), indicating Ti within primary and/or secondary mineral phases. Others show spectral evidence of a dehydrated Al-rich phase and spinel-group minerals, as well as Al₂O₃ to ~45 wt% and over 1 wt% Ni, (e.g., targets “Dolgoi Island”, “Finch Lake”, Fig. 1E–J), representing ore-grade enrichment of Ni³ (Figs. S1–S2). Some, but not all of the light-toned float rocks are rich in Al; others, such as target AEGIS 910 A (Sol 910), are composed of >90 wt% SiO₂ and have a VISIR signature consistent with hydrated silica⁴.

Deciphering the origin of these float rocks is challenging because they are fully removed from their geological context. However, based purely on the geochemistry of the rocks, it is clear that these materials once experienced intense aqueous alteration¹, which could include hydrothermal and/or pedogenic alteration prior to lithification and transport into Jezero crater². For example, Al enrichments exceeding ~30 wt% coupled with low total Fe are typical of deep weathering profiles⁵⁻⁸ (Ultisols and Oxisols in US

<figure><img src="image_4.png" /></figure>
<figure><img src="image_5.png" /><figcaption>**Fig. 1** | Location and examples of light-toned float rocks discovered at Jezero crater, Mars. Red arrows in E-J indicate analyses by SuperCam confirming the aluminum-rich (> ~30 wt% Al₂O₃) nature of float rocks. A HiRISE Map of Jezero crater showing locations where light-toned float rocks were observed; B Crater floor example (sol 72, zcam 08033); C Crater floor example (sol 388, zcam 08416); Jezero sedimentary fan examples (D sol 711, zcam 08715; E "Dolgoi Island" sol 657, zcam</figcaption></figure>

03505; F "Egegik" sol 662, zcam 03509; G"Unga Island" sol 676, zcam 03517; H "Ouzinkie" sol 691, zcam 03530). Jezero fan top examples (I "Trayfoot Mountain; sol 704, zcam 08704; J "Finch Lake" sol 774, zcam 03625) All images of float rocks are Mastcam-Z enhanced color images (red=630 nm, green=540 nm; blue=480 nm).
<figure><img src="image_6.png" /><figcaption>**Fig. 2** | Mastcam-Z landscape and multispectral images of light-toned float rocks atop the Jezero crater Margin Unit near the Hans Amundson Memorial workspace (Sol 912) demonstrating the spectral diversity of this material. A Mastcam-Z enhanced color landscape image (R = 630 nm), G = 544 nm), B = 480 nm) showing large pile/lag of pebble to cobble-sized light-toned float rocks (Sol 912,</figcaption></figure>

zcam 08919); B Mastcam-Z multispectral image “Lake Blanche” (Sol 913, zcam 03768); showing near-infrared wavelength decorrelation stretch (R = 1022 nm, G = 910 nm, R1 = 800 nm); C Near-infrared wavelength decorrelation stretch of “Learmonth” (sol 920, zcam 03775). Note location for C is not pictured in A.

soil taxonomy)⁹. Specifically, the leaching of Fe²⁺ from a fluctuating water table and the subsequent loss of total iron (e.g., FeO_T > ~1 wt%) contributes to formation of the light-toned, kaolinite-bearing, several -m-thick “pallid zone” in portions of these deep weathering profiles⁶,¹⁰,¹¹. This can occur under diverse chemical conditions including an oxic and slightly acidic, or anoxic/strongly acidic water table¹². Another possibility is aqueous alteration of a highly felsic protolith which may not require a lateritic type of weathering¹³. Ni enrichments > 1 wt% seen in several (but not all) Al-rich float rocks at Jezero crater (e.g., *Dolgoi Island, Finch Lake*) could also be consistent with deeply weathered soils formed on an ultramafic protolith such as serpentinite or dunite⁹ (Figs. S2–S3).

Production of pedogenic kaolinite on Mars during the Noachian (~4.1–3.7 Ga)¹⁴,¹⁵ has been inferred from orbital observations of phyllosilicate-bearing outcrops that are mineralogically and topographically consistent with weathering profile(s) formed from precipitation-driven pedogenic leaching¹⁶. One hypothesis for some of these rocks is that they are pieces of these deep weathering profiles that were later altered by different degrees of heating, possibly from impact¹.

Alternatively, these rocks could represent hydrothermal systems rather than a deep weathering profile. On Earth, hydrothermal production of kaolinite tends to occur during extensive subsurface fluid flow through parent rock, typically at temperatures between ~50°–250 °C, with fluids commonly derived from magmatic or geothermal systems¹⁷. Hydrothermal alteration of the Martian surface has also been documented by orbital remote sensing¹⁸, so it is possible that some of the Jezero Al-rich rocks formed as a result of hydrothermal alteration¹.

Although these rocks represent the first clear in-situ detection of kaolin-group minerals by a rover¹,¹⁹, decades of orbital remote sensing have demonstrated the global abundance of Al-rich clays in outcrops across

equatorial to subequatorial latitudes of Mars¹⁵,²⁰ dating from the Noachian to early Hesperian²¹, including locations proximate (tens of kilometers) to Jezero crater²². Al-rich clay minerals have also been identified from orbit within the western Jezero crater rim itself, as well as nearby in incised outcrop exposed within the final meanders of Neretva Vallis²³ (Fig. S4). These fortuitous discoveries of Al-rich float rocks by *Perseverance* now enable initial investigation of kaolinite-bearing terrains of early Mars previously observed only from orbit.

Comparisons with terrestrial analogs (similar materials from Earth) are necessary to explore the possible alteration history of these unique Martian rocks. To begin contextualizing these rocks with analog materials from Earth, we compare the geochemistry and spectral properties of hydrated Al-rich Jezero float rocks to deeply weathered materials from Earth. These include paleosols (ancient, lithified weathering profiles) and ancient hydrothermal kaolin deposits. We hypothesize that some of these float rocks are geochemically and spectrally similar to terrestrial materials that experienced intense and prolonged pedogenic alteration under chemically reducing conditions, followed by burial and lithification. Lastly, to enable future exploration of the source outcrop(s) of this material, we use orbital observations to identify locations in and around Jezero crater from where these rocks could have originated.

## Methods

We used images and data from the SuperCam²⁴⁻²⁶ and Mastcam-Z²⁷ instruments onboard *Perseverance* rover. These included the SuperCam's laser-induced breakdown spectrometer (LIBS) for major element composition of float rocks (Table S1), visible to near-infrared (VISIR) spectrometer (for constraining qualitative mineralogy and bulk hydration state), and Remote Micro-Imager (RMI) for the highest-resolution remote images.
<figure><img src="image_7.png" /><figcaption>**Fig. 3** | Mastcam-Z and SuperCam observations of the "hydrated class"¹ of aluminum (Al)-rich float rocks at Jezero Crater, Mars. These targets are the focus of this study. Left to right: Mastcam-Z multispectral images of targets "Chignik" (Sol 680, zcam 03523), "Elk Mountain (Sol 895, zcam 03750), and "Coral Bay" (Sol 920, zcam 03777). Top row: Mastcam-Z natural color images; Second row: Mastcam-Z</figcaption></figure>

enhanced color images (red = 630 nm, green = 540 nm; blue = 480 nm); Third row: Mastcam-Z near-infrared wavelength decorrelation stretch (red = 1022 nm; green = 910 nm; blue = 800 nm); bottom row: SuperCam Remote Micro-Imager products showing laser-induced breakdown spectroscopy (LIBS) rasters over Al-rich float rock targets.

Diagenetic features including rock coatings were excluded from LIBS and VISIR analyses (Supplementary Information). The typical root mean square error of prediction for SuperCam LIBS analysis (in wt%) are: CaO (1.3), FeO (3.1), Na₂O (0.5), K₂O (0.6), MgO (1.1), SiO₂ (6.1), and TiO₂ (0.3)²⁸. Mastcam-Z multispectral images were also used to examine the spectral diversity and geologic context of these float rocks. We focused on the "hydrated" class of light-toned, Al-rich float rocks from Royer et al.¹, which are characterized by elevated Al₂O₃ (~20–40 wt%), a ~2.21 µm Al-OH band, and the presence of a ~1.9 µm hydration band in the IR spectra¹. We

selected this class since these rocks retain hydration bands and thus may represent targets that have been only minimally altered by later heating related to burial or impact processes¹. SuperCam LIBS data for other Al-rich classes of Jezero float rocks (low-hydration and spinel-bearing) are provided in the Supplementary Information and can also be found in Royer et al., 2024¹. For these comparisons, we included the hydrated Al-rich targets "Chignik" (Sol 680/681); "Rainbow Curve" (Sol 777), "Elk Mountain" (Sol 895) and "Coral Bay" (Sol 924). These targets were remotely observed by both the SuperCam and Mastcam-Z instruments (Fig. 2), but due to their
small size (up to ~10 cm) and engineering constraints, no proximity/contact science was conducted with the PIXL or SHERLOC instruments.

We compared SuperCam LIBS observations of composition with previously published geochemical data from terrestrial kaolinite-bearing paleosols and hydrothermal kaolin deposits (Supplementary Information). These comparisons focused on early Eocene (55 Ma) kaolinitic Ultisol paleosols from Blacks Beach, La Jolla, San Diego, CA that formed on mafic to felsic conglomerate, with estimated mean annual precipitation of 1500 ± 299 mm²⁹ and likely only exposed to low temperatures (< 60–80 °C) during burial diagenesis. We also considered previously published chemical data from drill cores of the Paleoproterozoic (~ 2.2 Ga) Hekpoort paleosol in present-day Botswana and South Africa⁶,³⁰,³¹, selecting samples from the bleached, low-Fe, several-m-thick “pallid zone” of this well-studied Paleoproterozoic paleosol formed on basaltic protolith³⁰. These pedogenic samples were likely subject to comparably more heating (~ 250 °C) during burial diagenesis³¹. For geochemical comparisons with ancient hydrothermal (hypogene) kaolin deposits from Earth, we used three previously published datasets from hypogene kaolin deposits in Iran³², Malaysia³³ and Argentina³⁴ spanning a range of inferred alteration temperatures and protoliths (n = 21 total). The Iran site near Mianeh formed from a parent material of andesite and andesitic tuff during the Oligocene–Miocene at temperatures ranging from 150–240 °C³², whereas the Malaysia sites near Gunung Jerai formed in felsic intrusive rocks (granites and pegmatites) during the Triassic at 94–113 °C³³. The Argentina site near Rio Negro, Patagonia formed in mafic to felsic volcanic rocks and ignimbritic tuffs with some clastic sediments at temperatures up to 350 °C during the Triassic-mid Jurassic and are capped by pedogenic or groundwater silcrete³⁴ All data are included as Supplementary Information.

Comparisons of spectral properties between the early Eocene (55 Ma) San Diego paleosol and LIBS VISIR spectra of the “Chignik” target are presented in the short wave-infrared (IR; 1.3–2.5 µm) wavelengths. Methods for operation and calibration of SuperCam’s IR spectrometer can be found in ref. ²⁴⁻²⁶,³⁵. As of mission sol ~1000, Chignik was the only Al-rich float rock with a strongly kaolin-like IR spectra (see Royer et al.¹ for more information). No IR reflectance data were available for the Paleoproterozoic Hekpoort paleosol, but even in the case of their availability, direct spectral comparisons with the Paleoproterozoic samples are complicated by burial diagenesis that dehydrated and transformed many of the pedogenic clay minerals and other hydrated phases in these samples³⁰,³⁶.

To contextualize the in-situ detections and explore possible source outcrops for the Al-rich float rocks, we used orbital VISIR (0.35–2.6 µm) reflectance data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM)³⁷, which acquires spectral images with spatial scales ~18–200 m/pixel, and searched for the diagnostic signatures of kaolin-group clay minerals (Fig. S1), similar to how the SuperCam VISIR spectrometer detects these clay minerals (~ 2.17/2.21 µm bands). To identify putative sources of kaolin-group minerals, we used CRISM High-resolution targeted observations (< 40 m/pixel) of regions in and around Jezero crater, with CRISM mineral detections projected onto Global Context Camera (CTX) basemap images³⁸. These images cover the Jezero crater and Nili Planum region and were processed using the MOCAAS (Mars Orbital Catalog of Aqueous Alteration Signatures) methodology²³, which also includes observations from the Observatoire pour la Minéralogie, l'Eau, les Glaces, et l'Activité (OMEGA) aboard Mars Express. To identify areas of Al clay minerals, large-scale mapping of Al clay distribution was conducted using a global high-resolution map (200 m/pixel) of aqueous minerals from MOCAAS following the methodology of Carter et al.¹⁵. The maps classify minerals into five spectral groups including Fe/Mg phyllosilicate clay minerals, Al clays and hydrated silicates, polyhydrated sulfates, monohydrated sulfates, and carbonates²³. To investigate potential sources within the Neretva Vallis channel, we used CRISM multispectral data products projected onto CTX basemap images with coverage over the westernmost Neretva Vallis Channel (coverage of this region is not available for full-resolution targeted images). These multispectral Al clay maps were also processed with the MOCAAS methodology, though are associated with

larger amounts of uncertainty compared to the high-resolution targeted detections (e.g., 23). These CRISM multispectral data products are included as Supplementary Information (Figs. S4–S5) and a table of all CRISM observations used is included as Table S2.

## Results

### Spectral and geochemical similarities with intensely weathered paleosols from Earth

The early Eocene (55 Ma) San Diego paleosol samples appear spectrally similar to Chignik (Jezero crater) with features diagnostic of kaolin-group minerals³⁹. Similarities in band position and depth for kaolin-diagnostic features (e.g., presence of a ~ 2.17/2.2 µm doublet) were identified (Fig. 4, Figure S1). Unlike comparisons with pure laboratory standards of kaolinite or hallosite²⁰, the paleosols represent a complex natural mixture with contributions from several different mineral phases²⁹. These mixed-phase terrestrial samples are spectrally similar to the float rocks, which are presumably also composed of a complex mixture of secondary minerals and represent a continuum of Al-rich clay minerals produced from alteration. The main differences in the Chignik target are the loss of contrast of the 2.17 µm doublet feature, the shift of the 1.9 µm feature toward longer wavelengths (possibly from an additional phase like sulfate or Fe-hydroxide), and the addition of a 1.6 µm feature that is likely a residual of atmospheric CO₂. Spectral features between 1.9 and 2.1 µm in Chignik are a result of atmospheric corrections to SuperCam IR spectra and thus represent artefacts of processing²⁵. Spectral differences in Chignik versus lab spectra of kaolin minerals could also be due to dehydration, possibly resulting from heating⁴⁰. The excellent spectral match between the Mars and terrestrial samples allows for consideration of paleosols as a candidate for more in-depth comparison of elemental composition.

The major elemental compositions and inferred weathering intensities were compared between Jezero float rocks and analog samples by plotting each on a molar “A-CN-K” (Al₂O₃ -CaO+Na₂O-K₂O) ternary diagram to assess the degree of weathering (Chemical index of alteration, CIA)⁵, as well as an “A-CNK-FM” (Al₂O₃ – CaO+Na₂O + K₂O – FeO₇ + MgO) ternary diagram, a technique commonly used to constrain the weathering intensity of deeply altered mafic materials where reducing conditions during leaching led to loss of Fe⁴¹. To assess the degree of oxidative weathering of mafic materials, we also plotted samples on a “AF-CNK-M” (Al₂O₃ + FeO₇ – CaO + Na₂O + K₂O – MgO) ternary diagram¹¹. The chemical index of alteration (CIA) of the San Diego samples ranges from ~89–98²⁹, while Chignik ranges from ~65–87¹. The San Diego samples plot in a comparable location on the molar A-CNK-FM ternary, indicating a mafic index of alteration for chemically reducing scenarios (MIA₃) of 58–75, comparable to Chignik (MIA₃ of 35–80) and a similar trend towards loss of Fe and Mg. The index of laterization (IOL) of the bleached E- horizon of the San Diego sample was 25, suggesting kaolinization (Fe loss) rather than laterization (Fe gain)⁴¹, and is similar to the light toned regions of Chignik with IOL values ranging from ~14–27¹. These low IOL values in Chignik also support the hypothesis of kaolinization rather than laterization.

The terrestrial hydrothermal kaolin samples (n = 21) generally plotted at the apex of the A-CN-K ternary and had CIA > 95, unlike the lower values observed in the Jezero float rocks (Fig. 5A). In ternary diagrams for mafic index of alteration under oxidizing and reducing scenarios (AF-CNK-FM and A-CNK-FM, respectively) nearly all of the hydrothermal kaolin samples plot near the apex (n = 19), indicating extreme depletion of soluble cations and MIAO / MIA₃ ~ 98.

Perhaps a more striking comparison is with drill core samples from the Paleoproterozoic (~ 2.2 Ga) Hekpoort paleosol³⁰, where points from all four of the hydrated Jezero Al-rich float rocks overlap with those from the ~3-meter-thick kaolinitic, bleached, low Fe (~ 1–8 wt%), high Al (> 30 wt%) “pallid zone” of the weathering profile⁶. These similarities are seen in both ternary diagrams representing A-CN-K and A-CNK-FM for reducing conditions (Fig. 5A, B) and are most apparent with Chignik/Elk Mountain and the Hekpoort paleosol, with several points in the A-CNK-FM (Fig. 5B) plotting atop one another. Less overlap is seen in the MIA(o) ternary (AF-
**Fig. 4** | Infrared spectra comparisons between Al-rich float rock target “Chignik” at Jezero Crater, Mars (points 1-5, color traces, offset by + 0.2), and lithified E-horizon of an early Eocene (55 Ma) kaolinitic paleosol, La Jolla, San Diego, CA, USA (black traces, no offset). A SuperCam RMI showing VISIR raster on Chignik; B Erosional remnant of San Diego paleosol showing truncated E-horizon where VISIR spectra were collected; C Infrared comparisons between Chignik and San Diego paleosol samples. The kaolinite/halloysite diagnostic doublet feature at ~ 2.17 µm/2.2 µm is annotated, and laboratory kaolinite reference spectra are shown in Fig. S1.

<figure><img src="image_8.png" /></figure>

<figure><img src="image_9.png" /></figure>

CNK-M) (Fig. 5C), indicating that the Jezero samples experienced less oxidative weathering compared to analog pedogenic samples. By comparison, the extreme depletion of soluble cations characteristic of terrestrial hydrothermal kaolin deposits from Iran, Malaysia and Argentina across a range of estimated alteration temperatures (Fig. 5A–C) are overall unlike the less deeply weathered, though comparably Al-rich, Jezero float rocks.

## TiO2 content of Al-rich Jezero float rocks

Titania (TiO₂) can serve as a tracer of alteration processes in materials that were subject to chemical alteration. The SuperCam LIBS points from *Chignik, Coral Bay and Elk Mountain* (minus coatings/diagenetic features) (n = 22) have TiO₂ ranging from ~0.3–2 wt% (Fig. 6; Table S1). Other Al-rich float rock targets described in Royer et al.¹ (*Dolgoi Island, Unga Island, Finch Lake, Ouzinke*) are shown for comparison.

*Chignik* (n = 10) contains the highest TiO₂ content of the sample set, with mean and median TiO₂ of 1.2 wt% and 1.4 wt%, respectively (standard deviation of 0.36) (Fig. 6; Table S1). By comparison, *Elk Mountain* (n = 10) and *Coral Bay* (n = 3) have lower median TiO₂ (0.3 and 0.6 wt% TiO₂, respectively). *Unga Island* (n = 10) and *Ouzinke* (n = 10) have median TiO₂ ~ 0.7, whereas *Dolgoi Island* (n = 10) and *Finch Lake* (n = 10) have

median TiO₂ ~ 1 wt%. Several LIBS points on the Al-rich float rocks had TiO₂ values that exceeded the range of SuperCam LIBS TiO₂ calibration used for the determination of major oxide components²* (e.g., ~3 wt. TiO₂ % in a LIBS point on *Chignik*). However, all of the estimated SuperCam LIBS TiO₂ values, including those mentioned above, fell within the ranges of those of the terrestrial samples.

For comparison, the terrestrial pedogenic samples across mafic to felsic protoliths also have elevated TiO₂ relative to hydrothermal samples (Supplementary Information). The basaltic Hekpoort paleosol (n = 21) has mean and median TiO₂ of 1.48 wt% and 1.52 wt%, respectively. This TiO₂ range is highly comparable to *Chignik* (Fig. 6). The feldspathic San Diego paleosol (n = 7) has mean and median TiO₂ of 0.72 wt% and 0.69 wt%, respectively. By contrast, all of the terrestrial hydrothermal samples (n = 21) from three localities across a range of protoliths had lower mean and median TiO₂ (0.28 wt% and 0.14 wt%, respectively) (Fig. 6).

Elevated Ti in other classes of Al-rich float rocks such as the “spinel class” (*Dolgoi Island, Ouzinke, Finch Lake*) (Fig. 6) could reflect Ti in primary mineral phases (e.g., spinel)¹ rather than formation of secondary Ti phases, so caution is necessary when using Ti content to infer alteration environment for the full set of Jezero Al-rich float rocks.
<figure><img src="image_10.png" /></figure>

**Fig. 5 |** Geochemical comparisons of Jezero aluminum-rich float rocks with deeply weathered, iron-poor paleosols and hydrothermal kaolin deposits from Earth. A A-CN-K ternary diagram with the chemical index of alteration (CIA) projected showing early Eocene (~55 Ma) kaolinitic paleosols from San Diego (55 Ma, *n* = 7) and Paleoproterozoic (~2.2 Ga) “Hekpoort” paleosol from South Africa (*n* = 21), hydrothermal kaolin samples from three localities in Iran, Malaysia, Argentina (*n* = 21 total) and comparisons with Chignik (*n* = 9), Rainbow Curve

(*n* = 5), Elk Mountain (*n* = 10), and Coral Bay (*n* = 3) targets from Jezero Crater, Mars; B A-CNK-FM ternary diagram with the mafic index of alteration (MIA) for chemically reducing scenarios (MIA<sub>(R)</sub>); C AF-CNK-M ternary diagram integrated with the mafic index of alteration for chemically oxidizing scenarios (MIA<sub>(O)</sub>). Inset panels show lithified hand samples of the Eocene San Diego paleosol (Fig. 4A, point #1) and the sericite zone of the Paleoproterozoic Hekpoort paleosol<sup>30</sup>.

## Orbital detections of kaolin-group minerals in and around Jezero crater

To gain an understanding of the possible locations where Al-rich float rocks such as *Chignik* could have once originated, we used CRISM high-resolution targeted images to identify locations with a candidate kaolin-group mineral signature. At Jezero crater, many outcrops with a kaolin-group mineral signature have a light-toned, patchy, fractured appearance<sup>2,23</sup>. Previous identifications of kaolinite/halloysite in the SW crater rim are associated with light-toned, layered megabreccia blocks that span approximately 100 m<sup>22,23</sup>. The CRISM high resolution images show kaolin clay detections on the Jezero crater rim that are approximately 1-2 km from the current rover traverse (as of sol ~1000). A small (~ 75 m²) area of kaolin detections is identified as the closest location to the rover traverse (Fig. 7B). When cor- relating the CRISM detection with HiRISE images, the candidate kaolin areas appear as patchy light-toned outcrop at the base of NW-SE trending ridges (Fig. 7C). Additional larger areas of detections shown in Fig. 7 in the SW Jezero crater rim are associated with comparably rougher terrain inferred from the CTX image basemaps. In contrast to smaller exposures on the western crater rim (Fig. 7B), examination of several candidate kaolin- bearing outcrops exposed in the final meander of the Neretva Vallis channel

due west of Jezero crater shows laterally continuous, light-toned outcrop exposed over ~500 meters (Fig. S5).

## Discussion

Although the Jezero rocks are removed from their outcrop, a major result of these comparisons are the geochemical similarities to deeply weathered Paleoproterozoic paleosols once formed from precipitation- driven weathering of mafic rocks. Geochemical dissimilarities with ancient terrestrial hydrothermal kaolin deposits across a range of parent materials and alteration temperatures indicate that the hydrated class of float rocks may have experienced overall less alteration, or alteration at lower temperatures, compared to these materials on Earth. In the fol- lowing section, we outline distinct lines of evidence supporting or refuting the pedogenic or hydrothermal hypotheses for the alteration history of the float rocks.

## Distinguishing pedogenic versus hydrothermal kaolinite

On Earth, either pedogenic (supergene) or hydrothermal alteration (hypogene) can form altered material containing both kaolinite and low Fe content<sup>7,42</sup> and distinguishing between the two often requires the geological
<figure><img src="image_11.png" /><figcaption>**Fig. 6** | Laser-induced breakdown spectroscopy (LIBS)-derived TiO₂ estimates of the hydrated class of Jezero Al-rich float rocks and comparisons with the spinel class of Al-rich float rock targets from Royer et al.¹. A Boxplot of TiO₂ within Chignik, Elk Mountain, Rainbow Curve and Coral Bay targets (diagenetic features/ coatings not included); B Comparison with other Al-rich targets from Royer et al¹, also shown in Fig. 1 (Dolgoi Island [sol 657], Unga Island [sol 676], Finch Lake [sol</figcaption></figure>

774], and Ouzinke [sol 691]). The orange line represents the median, boxes show quartiles 1-3, the whiskers represent 1.5 times the interquartile range, and lone dots are outliers. Color gradient indicates general value (~1 wt% TiO₂) used to distinguish pedogenic versus hydrothermal alteration regimes in Earth analog kaolin deposits and paleosols⁸,⁴²,⁴⁵.

context provided by outcrop. Pedogenic kaolinite is often formed across laterally extensive stable land surfaces (e.g., hundreds to thousands of meters along strike) or can be eroded and transported to be deposited in horizontal beds at similar scales. By contrast, hypogene kaolinite is often present in more localized networks of veins that represent subsurface fluid flow (typically <100 m wide)⁷,⁴²⁻⁴⁴.

Geochemical comparisons with terrestrial kaolin deposits indicate that pedogenic kaolinite can be distinguished from hydrothermal kaolinite by considering bulk TiO₂ content, primarily in cases where the protolith(s) are well-constrained⁴⁵. In general, pedogenic kaolin deposits from Earth typically have TiO₂ greater than ~1 wt% due to decreased Ti mobility (relative to other elements) under low temperature (~25 °C) pedogenic alteration conditions¹⁷,⁴²,⁴⁵,⁴⁶. Hydrothermal kaolin deposits formed across a range of higher alteration temperatures (~100–350 °C) do not concentrate Ti to the same degree as pedogenic examples, and typically have TiO₂ of approximately 0.5 wt% or less¹⁷,⁴².

However, caution is necessary when using Ti to infer process in cases where the protolith is unknown, because the starting abundance of Ti is a critical constraint³³. Further, Ti mobility is related to pH, such that Ti is more readily leached at pH <4.⁷ For example, TiO₂ is often higher in pedogenic kaolin because titanium is immobile during weathering, leading to residual enrichment, especially when starting from Ti-poor felsic protoliths where Ti increases as other elements are leached. In contrast, hydrothermal kaolin forms in systems where Ti can be mobile; even if the protolith is Ti-rich (e.g., basalt), alteration may remove Ti so the final kaolin has contents below protolith levels³³.

Chignik (n = 10) shows the highest Ti content of the float rocks examined here, with mean and median TiO₂ of 1.2 wt% and 1.4 wt%, respectively (standard deviation of 0.36) (Fig. 6; Table S1) along with overlap in composition with a well-characterized, deeply weathered terrestrial paleosol (Fig. 5). When considering TiO₂ of all LIBS shots across all Al-rich Jezero float rocks analyzed in Royer et al.¹ (n = 118), TiO₂ averages 0.9 wt% with a median value of 0.7 (standard deviation of 0.45) (Table S1). Such overall elevated values for Ti could be consistent with some amount of pedogenic kaolinization¹⁷,⁴², but as indicated earlier, elevated Ti estimates could also in part be due to some of the points exceeding the SuperCam LIBS TiO₂ calibration²⁸, or, alternatively, a mafic protolith (e.g., basalt) initially rich in Ti. Of the sample set, Chignik stands as distinct from the others because it appears to be the least altered by heat (retention of 1.9 µm and 2.16/2.2 µm features, Fig. 4), so geochemical comparisons with terrestrial paleosols and hydrothermal deposits may be more trustworthy than with

other Jezero samples that could have been subject to heating or other unknowns.

The Si-rich float rocks also observed by Perseverance likely formed via hydrothermal fluids⁴, and thus also might be related to the Al-rich float rocks examined here. For example, the AEGIS 910 A target might represent chemical precipitates from the olivine-dissolving fluids associated with the alteration in Jezero crater and on the Jezero crater rim⁴. It is therefore possible that the Si-rich float rocks are associated with some of the Al-rich float rocks described in this study, though the geologic context of both materials is currently unknown.

## Comparisons with terrestrial laterite

Our analyses suggest that the aluminum-rich Jezero float rocks might represent prolonged pedogenic weathering of rock or sediment (Fig. 5B). This raises the possibility that the float rocks may have experienced weathering akin to terrestrial laterite, which is rock or sediment subject to deep, strongly oxidative pedogenesis⁴⁷,⁴⁸, where similar enrichments in Al and Ti are common⁴⁷,⁴⁹. In cases of an ultramafic protolith, elevated Ni is also common. Detections of elevated Ni likely > 1 wt% in some targets (Coral Bay, Unga Island, and Finch Lake)³ (Fig. S2–S3) but not others (e.g., Chignik) could be consistent with intense pedogenic alteration of an ultramafic protolith under oxidizing conditions, akin to terrestrial Ni laterite⁴⁹. However, the depletions of Mg and Fe observed in the float rocks are overall dissimilar to the Fe/Mg-rich saprolite layer of ultramafic Ni laterites from Earth’s geological record, where Ni is either concentrated in veins or diffused within Fe/Mg clay minerals and oxides⁴⁹. Likewise, the samples from the mafic, Ni-poor Hekpoort paleosol used in our comparisons have low Ni (~0.05 wt%), high Al (~30 wt%) and Ti (1–2 wt%), with low Fe/Mg/Mn (<~2 wt%)³⁰, unlike Ni-rich laterite from Earth⁴⁷,⁴⁹.

It is possible that the “hydrated class” of Jezero float rocks, such as Chignik, are related to the Ni-bearing “spinel class”¹ of Jezero float rocks, but the hydrated class does not show the same potential Ni abundances as the spinel class (> 1 wt%; e.g., Finch Lake; Fig. S3). One possibility is that the float rocks represent a continuum of material derived from a single, or more likely multiple eroded Noachian paleosol profiles of mafic, ultramafic and/ or felsic composition. In this way, elemental trends in Al, Fe, Ti and Mg relate to protolith, climate, position/horizon in weathering profile, diagenetic alteration, or other unknowns. Protoliths including felsic material are possible²¹, but elevated Ni to ore-grade enrichment (> 1 wt%) is unique to deeply weathered ultramafic parent material, perhaps similar to a Ni-Cu sulfide protolith³,⁵⁰,⁵¹.
<figure><img src="image_12.png" /><figcaption>**Fig. 7** | CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) detections of Al smectite/kaolin-group clay minerals in locations within and around Jezero crater using methods described in Carter et al<sup>23</sup>. A CRISM targeted high-resolution detections of kaolin clay minerals across the Jezero crater region; B Zoom of the Jezero sedimentary fan and SW crater rim. The green circle at center highlights a likely kaolin mineral detection in FRS00031442 at a location on the</figcaption></figure>

crater rim of Jezero and shows the location of the Perseverance rover traverse (as of sol ~ 1000); C Kaolin mineral detections in FRS00031442 correlate with patchy light toned features on the surface. Subframe of HiRISE image ESP_037119_1985_CO-LOR; D Example spectra extracted from CRISM FRS00031442 from location on Jezero crater rim shown in B/C) and comparison with laboratory kaolinite<sup>23</sup>.

## Differences between Jezero float rocks and analog samples

There are several major differences between the Jezero float rocks and Earth analog samples, such as trends in total iron and potash (FeO<sub>T</sub> and K<sub>2</sub>O) abundance. The analog hydrothermal kaolin samples are depleted in K<sub>2</sub>O and FeO<sub>T</sub> relative to pedogenic samples, which could be related to protolith composition, burial diagenesis such as potash metasomatism<sup>36</sup>, or other unknowns. As indicated in Fig. 5, the elemental compositions of the analog hydrothermal samples are overall dissimilar to the hydrated class of Al-rich float rocks at Jezero. Another difference is that the Jezero Al-rich float rocks are enriched in CaO and Na<sub>2</sub>O relative to all of the analog samples, which may be related to the above factors, or alternatively, indicate overall less chemical alteration relative to analog samples (e.g., lower chemical index of alteration (Fig. 5A).

The late diagenetic history of the Jezero float rocks also currently remains unclear. For example, the close geochemical similarities with the Paleoproterozoic (2.2 Ga) Hekpoort paleosol are a challenging result to reconcile because those terrestrial samples were likely subject to comparatively more burial diagenesis than currently known Mars examples (e.g., late diagenetic chlorite, sericite and pyrophyllite indicate temperatures > ~250 °C in the "pallid zone"<sup>30,31</sup>). Unlike the more pristine *Chignik* target with its preserved kaolinite-like signature (Fig. 4), hydrated Al clay minerals in the Hekpoort paleosol were transformed to higher temperature phases during deep burial diagenesis<sup>31</sup>. It is hypothesized that these later mineralogical transformations only minimally influenced the original elemental chemical composition of the weathered soil after it was buried and lithified<sup>6,30</sup>. This phenomenon is common in terrestrial examples of well-

lithified, clay-rich paleosols<sup>36</sup>, which are thought to minimize later diagenetic fluid flow via reduced hydraulic conductivity<sup>52</sup>.

Subtle spectral differences are also apparent between *Chignik* and the terrestrial samples. For example, the loss of contrast of the 2.17 µm feature (Fig. 4) could be due to a less crystalline kaolinite or a mixture of kaolinite with Al-smectite<sup>40</sup>. Furthermore, the 2.2 µm Al-OH band can change due to exposure to heat<sup>53</sup>, so the subtle differences in band position and depth could also be associated with heat-induced alteration. Shock metamorphism has also been shown to reduce crystallinity and ordering, and is manifested by the doublet band losing its finer structure and decreasing in width<sup>54</sup>. Impact alteration, as hypothesized for some of these rocks¹, could cause variable degrees of either heating or shock.

## When, where, and how did these rocks originate?

Kaolin-group minerals have been observed from orbit across the Nili Fossae region outside of Jezero crater, located at the northwest quadrant of the Isidis basin, where they are observed in bedrock units in a stratigraphy always overlying Fe/Mg smectites<sup>55</sup>. These materials have been mapped as exhumed Noachian (~4.1–3.7 Ga) basement rocks and are sometimes associated with impact breccias and craters<sup>22</sup>. They may represent remnants of the regionally extensive Noachian compositional “clay stratigraphy” that is characterized by a distinct Al clay horizon with kaolinite-like spectra (approximately 20–50 m thick) that transitions downward into layered Fe/Mg clay horizons with nontronite-like spectra<sup>17,56,57</sup> (up to ~150 m thick). The light-toned, Al-rich upper portions of these regional and globally distributed sequences have previously been interpreted as the products of
<figure><img src="image_13.png" /><figcaption>**Fig. 8 |** Proposed sequence of events for Al-rich float rocks at Jezero Crater. Aqueous alteration (top-down pedogenic weathering) of a volcanic/volcaniclastic protolith led to the formation of a weathering profile characterized by Al clays</figcaption></figure>

overlying Fe/Mg clays; either lithification from impact (top pathway) or lithification from burial enhanced the hardness of the weathered material. Lastly, incision or impact distributed this Al-rich material into Jezero crater.

prolonged precipitation-driven deep weathering of volcanic ash/tuff in
subaerial settings⁵⁸, a process that on Earth leads to kaolinization, the
endmember of prolonged pedogenic weathering.

The Al-clay-bearing stratigraphy is most common closest to the Nili
Fossae graben and progresses southwest towards Jezero crater, where the
kaolinite-bearing outcrops transition to patchy detections distributed across
the Noachian basement²²,²³,⁵⁹. The kaolinite-bearing materials are com-
monly tens to hundreds of meters in size in the Nili Planum region, appear
stratigraphically above low-calcium-pyroxene-bearing plateaus, and are
arguably among the youngest features when observed, though the strati-
graphic context is difficult to ascertain²².

One potential source of the Al-rich float rocks examined here include
the light-toned, layered megabreccia blocks (area of ~0.1 km²) nearby in the
crater rim approximately 2 km from the Jezero sedimentary fan that have a
spectral signature of a kaolin-group mineral²²,²³. Other locations identified in
the final meanders of Neretva Vallis are associated with in-place light-toned
outcrop that could also be an additional source (Fig. S5). Other possible
nearby sources include areas upstream from the Neretva Vallis inlet, where
an isolated butte ~16 km west of the Jezero sedimentary fan appears to
contain kaolin-group minerals (Fig. S5). If present, these materials may have
entered the Neretva Vallis channel as lag deposits during erosion of
the butte.

Shallow burial, possibly by Syrtis Major volcanism, or heating from impact processes, may have led to lithification of these presumably soft kaolinized materials to allow their eventual transport into Jezero Crater (Fig. 8). Fluvial, glacial, or impact ejecta transport are plausible mechanisms to explain how they ended up as float rocks in Jezero Crater (Fig. 8).

Future plans for exploration of the crater rim by *Perseverance* includes
targeting and sampling a laterally extensive kaolinite-bearing outcrop⁶⁰, so it
is possible that additional observations of outcrop will further reveal the
alteration history of these enigmatic float rocks.

Implications for early Mars climate and hydrological cycle

Regardless of whether these rocks formed from pedogenesis or hydro-
thermal alteration, from a stoichiometric perspective the presence of kaolin-
group minerals and Al₂O₃ > 30 wt% implies large quantities of liquid water
once participated in intense chemical alteration (e.g., water: rock ratios
[W:R] > 1000:1) to concentrate Al and Ti. Such quantities of water are hard
to envision for a cold and dry Mars today but have been envisaged for the
formation of the “compositional clay stratigraphy”¹⁵ under intermittently
warm intervals during a largely cold Noachian (4.1-3.7 Ga) climate⁶¹.

If the kaolinite is instead due to Noachian impact-driven hydrothermal
systems (either the larger Isidis or smaller Jezero-forming impact)⁶² rather
than top-down pedogenic leaching, similarly abundant liquid water would
have to be available to drive hydrothermal kaolinization. However, in the
hydrothermal scenario, the high W:R settings responsible for kaolin for-
mation may have been much more localized, such as in post-impact
hydrothermal vents or fractures within the fresh ejecta⁶³.

Similarities with paleosols formed during greenhouse climates on
Earth suggest abundant liquid water (mean annual precipitation >
1000 mm), but the nature of fluid chemistry remains unclear (e.g., pH, redox
state). Results from the Al-rich float rocks at Jezero crater confirm there were
conditions able to sustain intense chemical weathering processes over
geological timescales (10³–10⁶ years)⁴¹ on Mars. These rocks and their source
outcrops, especially the *Chignik* target, represent a new line of evidence for
the possibility of precipitation-driven deep weathering of the Martian crust
billions of years ago.

The possibility of weathering-climate feedbacks on early Mars may also
be demonstrated by this material. The presence of both a measurable 1.9 µm
hydration band and a 2.21 µm Al-OH band in *Chignik* (Fig. 4) is in-situ
evidence that some of these ancient rocks retain mineral water and hydroxyl.
This implies some were likely never heated to temperatures needed for
dehydroxylation ( > ~450 °C). Although *Perseverance* is unable to directly
measure the absolute water content of rocks on Mars, terrestrial paleosols and
hydrothermal kaolin deposits rich in kaolinite/halloysite are typically com-
posed of >10 wt% mineral-bound H₂O⁴¹. It is therefore possible that regional-
scale kaolinization of the Martian surface associated with the formation of
these rocks may have consumed large amounts of ancient atmospheric
water⁶⁵. This is water that was once liquid, but is now locked within the
structure of kaolin group minerals and other hydrated alteration phases
formed during chemical weathering of the Martian crust⁶⁶. Unlike Earth,
Mars lacks subduction-driven plate tectonics to recycle the water and
hydroxyl (OH) in hydrated minerals like kaolinite back to the atmosphere via
volcanic eruptions with mantle sources⁶⁷, so the genesis of these minerals
billions of years ago may have contributed to the irreversible drying of the
planet⁶⁸. Their presence on the surface of Mars today, as hydrated/hydro-
xylated Al-rich materials, implies both abundant liquid water during for-
mation and also invokes a pathway for the irreversible sequestration of
exchangeable water from the ancient Martian atmosphere. Kaolinite-forming
conditions at or near the ancient surface may therefore have been associated
with the wettest, and possibly most habitable portions of Mars' history.

Data availability

The supplementary dataset (Supplementary Data) containing elemental
composition and reflectance spectra of all targets examined in this work is
available at https://doi.org/10.5281/zenodo.17109674. All Mars 2020 Per-
severance rover datasets (including those used in this work) are available on
the Planetary Data System (PDS) at the PDS Geosciences Node (https://pds-
geosciences.wustl.edu/missions/mars2020/index.html) and the PDS Car-
tography and Imaging Sciences Node (https://pds-imaging.jpl.nasa.gov/
volumes/mars2020.html). Links to specific instrument dataset bundles are
listed below:

• Mars 2020 Mission bundle: https://doi.org/10.17189/1522642

• SuperCam Instrument bundle: https://doi.org/10.17189/1522646

*   **Mastcam-Z Science Imaging bundle:** https://doi.org/10.17189/q3ts-c749.

Received: 21 May 2025; Accepted: 30 September 2025;
Published online: 01 December 2025

References

1. Royer, C., Bedford, C. C. & Horgan, B. H. N. Intense alteration on early Mars revealed by high-aluminum rocks at Jezero Crater. *Nat. Commun. Earth Environ.* **5**, 671 (2024).

2. Bedford, C. C. et al. Discovery of light-toned float rocks in Jezero crater: A tale of aqueous alteration and high-temperature metamorphism. *Lunar Planet. Sci. Conf.* **2221**, 6–7 (2024).

3. Forni, O. et al. Nickel-Copper deposits on Mars? Discovery of ore-grade abundances and implications for formation and alteration. *Lunar Planet. Sci. Conf.* **1236**, 1–2 (2024).

4. Beck, P. et al. From hydrated silica to quartz: Potential hydrothermal precipitates found in Jezero crater, Mars. *Earth Planet. Sci. Lett.* **656**, 119256 (2025).

5. Brimhall, G. H. & Dietrich, W. E. Constitutive mass balance relations between chemical composition, volume, density, porosity, and strain in metasomatic hydrochemical systems: Results on weathering and pedogenesis. *Geochim. Cosmochim. Acta.* **51**, 567–587 (1987).

6. Beukes, N. J., Dorland, H., Nedachi, M. & Ohmoto, H. Tropical laterites, life on land and the history of atmospheric oxygen in the Paleoproterozoic. *Geology* **30**, 491–494 (2002).

7. Dill, H. G. Kaolin: Soil, rock and ore: from the mineral to the magmatic, sedimentary and metamorphic environments. *Earth Sci. Rev.* **161**, 16–129 (2016).

8. Retallack, G. J. Lateritization and bauxitization events. *Econ. Geol.* **105**, 655–667 (2010).

9. Staff, S. S. Keys to soil taxonomy. *United States Dep. Agric.* **12**, 1–372 (2014).

10. Abbott, P., Minch, J. & Peterson, G. Pre-Eocene paleosol south of Tijuana, Baja Califomia, Mexico. *J. Sediment. Petrol.* **46**, 355–361 (1976).

11. Abbott, P. L. Cenozoic Paleosols of the San Diego Area, California. *Catena* **8**, 223–237 (1981).

12. Drever, J. I. In *The Chemistry of Weathering* (Springer Nature B.V., 1985).

13. Wilson, M. J. Weathering of the primary rock-forming minerals: processes, products and rates. *Clay Miner* **39**, 233–266 (2004).

14. Loizeau, D. et al. Quantifying widespread aqueous surface weathering on Mars: the plateaus south of Coprates Chasma. *Icarus* **302**, 451–469 (2018).

15. Carter, J., Loizeau, D., Mangold, N., Poulet, F. & Bibring, J. Widespread surface weathering on early Mars: a case for a warmer and wetter climate. *Icarus* **248**, 373–382 (2015).

16. Klidaras, A. et al. Global topography of clay deposits signify an epoch of warm and humid climate on early Mars. *Geology* **1516**, 3–4 (2025).

17. Ece, Ö. I., Ercan, H. Ü. Global occurrence, geology and characteristics of hydrothermal-origin kaolin deposits. *Minerals*. **14** https://doi.org/10.3390/min14040353 (2024).

18. Ehlmann, B. L., Mustard, J. F. & Murchie, S. L. Geologic setting of serpentine deposits on Mars. *Geophys. Res. Lett.* **37**, 1–5 (2010).

19. Wang, A. et al. Evidence of phyllosilicates in Wooly Patch, an altered rock encountered at West Spur, Columbia Hills, by the Spirit rover in Gusev crater, Mars. *J. Geophys. Res. Planets*. **111** https://doi.org/10.1029/2005JE002516 (2006).

20. Wray, J. J., Ehlmann, B. L., Squyres, S. W., Mustard, J. F. & Kirk, R. L. Compositional stratigraphy of clay-bearing layered deposits at Mawrth Vallis. *Mars. Geophys. Res. Lett.* **35**, 2–7 (2008).

21. B. Ye, J. R. Michalski, Chemical weathering over hundreds of millions of years of greenhouse conditions on Mars. *Commun. Earth Environ.* **3** https://doi.org/10.1038/s43247-022-00602-7 (2022).

22. Scheller, E. L. & Ehlmann, B. L. Composition, stratigraphy, and geological history of the noachian basement surrounding the isidis impact basin. *J. Geophys. Res. Planets*. **125** https://doi.org/10.1029/2019JE006190. (2020).

23. Carter, J. et al. A Mars orbital catalog of aqueous alteration signatures (MOCAAS). *Icarus* **389**, 115164 (2023).

24. Fouchet, F. et al. The SuperCam infrared spectrometer for the perseverance rover of the Mars2020 mission. *Icarus*. **373** https://doi.org/10.1016/j.icarus.2021.114773 (2022).

25. Wiens, R. C. et al. *The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests* (The Author(s) https://doi.org/10.1007/s11214-020-00777-5) 217 (2021).

26. Maurice, S. et al. *The SuperCam Instrument Suite on the Mars 2020 Rover: Science Objectives and Mast-Unit Description* (The Author(s) 217 https://doi.org/10.1007/s11214-021-00807-w (2021).

27. Bell, J. F. et al. The Mars 2020 Perseverance Rover Mast Camera Zoom (Mastcam-Z) Multispectral, Stereoscopic Imaging Investigation. *Space Sci. Rev.* **217** https://doi.org/10.1007/s11214-020-00755-x (2021).

28. Anderson, R. B. et al. Post-landing major element quantification using SuperCam laser induced breakdown spectroscopy. *Spectrochim. Acta - Part B At. Spectrosc.* **188** https://doi.org/10.1016/j.sab.2021.106347 (2022).

29. Broz, A. P. et al. Eocene (50–55 Ma) greenhouse climate recorded in nonmarine rocks of San Diego, CA, USA. *Sci. Rep.* **14**, 1–19 (2024).

30. Yang, W. & Holland, H. D. The Hekpoort paleosol profile in strata 1 at Gaborone, Botswana: Soil formation during the great oxidation event. *Am. J. Sci.* **303**, 187–220 (2003).

31. Driese, S. G. Pedogenic translocation of Fe in modern and ancient Vertisols and implications for interpretations of the Hekpoort paleosol (2.25 Ga). *J. Geol.* **112**, 543–560 (2004).

32. Abedini, A. & Calagari, A. A. Geochemical characteristics of the Abgarm kaolin deposit, NW Iran. *Neues Jahrb. Geol. Palaontol. Abhandlungen.* **278**, 335–350 (2015).
33. Baioumy, H. et al. Hypogene kaolin deposits from felsic intrusive rocks (Peninsular Malaysia) with special reference to rare earth elements and stable isotopes geochemistry. *Geosci. J.* **25**, 863–876 (2021).

34. Grecco, L. E. & Marfil, S. A. Mineralogy and geochemistry of hydrothermal kaolins from the Adelita mine, Patagonia (Argentina); relation to other mineralization in the area. *Clay Minerals* **47**, 131–146 (2012).

35. Royer, C. et al. Reflectance of Jezero Crater Floor: 1. Data Processing and Calibration of the Infrared Spectrometer (IRS) on SuperCam. *J. Geophys. Res. Planets.* **128** https://doi.org/10.1029/2022JE007481 (2023).

36. Novoselov, A. A., Roberto, C. & Filho, D. S. Potassium metasomatism of Precambrian paleosols. *Precambr. Res.* **262**, 67–83 (2015).

37. Murchie, S. et al. Compact reconnaissance imaging spectrometer for Mars (CRISM) on Mars reconnaissance orbiter (MRO). *J. Geophys. Res.* **112**, 1–57 (2007).

38. Dickson, J. L., Ehlmann, B. L., Kerber, L., Fassett, C. I. The Global Context Camera (CTX) Mosaic of Mars: a product of information-preserving image data processing. *Earth Sp. Sci.* **11** https://doi.org/10.1029/2024EA003555. (2024).

39. Bishop, J. et al. Phyllosilicate diversity and past aqueous activity revealed at Mawrth Vallis, Mars. *Science* **321**, 830–834 (2008).

40. Cloutis, E. A. et al. Spectral reflectance properties of minerals exposed to simulated Mars surface conditions. *Icarus* **195**, 140–168 (2008).

41. Babechuk, M. G., Widdowson, M. & Kamber, B. S. Quantifying chemical weathering intensity and trace element release from two contrasting basalt profiles, Deccan Traps, India. *Chem. Geol.* **363**, 56–75 (2014).

42. Ece, Öl, Ekinci, B., Schroeder, P. A., Crowe, D. & Essenli, F. Origin of the Düvertepe kaolin-alunite deposits in Simav Graben, Turkey: Timing and styles of hydrothermal mineralization. *J. Volcanol. Geotherm. Res.* **255**, 57–78 (2013).

43. Dill, H. G., Kaufhold, S., Ehling, A. & Bowitz, J. Oxidized and reduced kaolin fan deposits: their sedimentological-mineralogical facies and physical-chemical regime (North-Bavarian Kaolin Mining District, Germany). *Ore Geol. Rev.* **72**, 459–484 (2016).

44. Driese, S. G., Medaris, L. G., Kirsimäe, K., Somelar, P. & Stinchcomb, G. E. Oxisolic processes and geochemical constraints on duration of weathering for Neoproterozoic Baltic paleosol. *Precambr. Res.* **310**, 165–178 (2018).

45. Dill, H. G., Bosse, H. R., Henning, K. H., Fricke, A. & Ahrendt, H. Mineralogical and chemical variations in hypogene and supergene kaolin deposits in a mobile fold belt the Central Andes of northwestern Peru. *Miner. Depos.* **32**, 149–163 (1997).

46. Ercan, H. Ü, Ece, I. şik, Schroeder, P. A. & Karacik, Z. Differentiating styles of alteration within kaolin-alunite hydrothermal deposits of çanakkale, NW Turkey. *Clays Clay Miner* **64**, 245–274 (2016).

47. Marsh, E. E., Anderson, E. D., Gray, F. in *Mineral Deposit Models for Resource Assessment* (2013; http://pubs.er.usgs.gov/publication/sir20105070H), p. 49.

48. Marsh, E. E., Anderson, E. Ni-Co laterite deposits — a deposit model. *U.S. Geol. Surv. Open-File Rep.* 2011–1259 (2015).

49. Butt, C. R. M., Cluzel, D. Nickel Laterite Ore Deposits: Weathered Serpentinites, 123–128 (2013).

50. Baumgartner, R. J. et al. Magmatic controls on the genesis of Ni-Cu ±(PGE) sulphide mineralisation on Mars. *Ore Geol. Rev.* **65**, 400–412 (2015).

51. Baumgartner, R. J., Baratoux, D., Gaillard, F. & Fiorentini, M. L. Numerical modelling of erosion and assimilation of sulfur-rich substrate by martian lava flows: Implications for the genesis of massive sulfide mineralization on Mars. *Icarus* **296**, 257–274 (2017).

52. Potter-McIntyre, S. L., Chan, M. A. & McPherson, B. J. Concretion formation in volcaniclastic host rocks: evaluating the role of organics, mineralogy, and geochemistry on early diagenesis. *J. Sediment. Res.* **84**, 875–892 (2014).

53. Cloutis, E. A. et al. Heated kaolinite/halloysite at Barrier Range, Jezero Crater, Mars? In *Lunar and Planetary Science Conference*, Vol. 2806, 2155 (2023).

54. Michalski, J. R. et al. Shock metamorphism of clay minerals on Mars by meteor impact. *Geophys. Res. Lett.* **44**, 6562–6569 (2017).

55. Ehlmann, B. L. et al. Identification of hydrated silicate minerals on Mars using MRO-CRISM: geologic context near Nili Fossae and implications for aqueous alteration. *J. Geophys. Res. Planets.* **114**, 1–33 (2009).

56. Bishop, J. L. et al. Multiple mineral horizons in layered outcrops at Mawrth Vallis, Mars, signify changing geochemical environments on early Mars. *Icarus* **341**, 113634 (2020).

57. Ye, B. & Michalski, J. R. Precipitation-driven pedogenic weathering of volcaniclastics on early Mars. *Geophys. Res. Lett.* **48**, 1–10 (2021).

58. Liu, J. et al. Anoxic chemical weathering under a reducing greenhouse on early Mars. *Nat. Astron.* https://doi.org/10.1038/s41550-021-01303-5 (2021).

59. Bramble, M. S., Mustard, J. F. & Salvatore, M. R. The geological history of Northeast Syrtis Major. *Mars. Icarus.* **293**, 66–93 (2017).

60. Mayhew, L. E. et al. The scientific value of collecting samples from the Jezero Crater rim. *Lunar Planet. Sci. Conf.* **2602**, 8–9 (2024).

61. Bishop, J. L. et al. Surface clay formation during short-term warmer and wetter conditions on a largely cold ancient Mars. *Nat. Astron.* **2**, 206–213 (2018).

62. Mandon, L. et al. Refining the age, emplacement and alteration scenarios of the olivine-rich unit in the Nili Fossae region. *Mars. Icarus.* **336**, 113436 (2020).

63. Schwenzer, S. P. & Kring, D. A. Alteration minerals in impact-generated hydrothermal systems—exploring host rock variability. *Icarus* **226**, 487–496 (2013).

64. Hwang, H. et al. A role for subducted super-hydrated kaolinite in Earth's deep water cycle. *Nat. Geosci.* **10**, 947–953 (2017).

65. Scheller, E. L., Ehlmann, B. L., Hu, R., Adams, D. J. & Yung, Y. L. Long-term drying of Mars by sequestration of ocean-scale volumes of water in the crust. *Science* **372**, 56–62 (2021).

66. Wernicke, L. J. & Jakosky, B. M. Martian hydrated minerals: a significant water sink. *J. Geophys. Res. Planets.* **126**, 1–24 (2021).

67. Rolf, T., Weller, M., Gülcher, A. J. P. Venus mantle dynamics and evolution through time. *Space Sci. Rev.* **218** https://doi.org/10.1007/s11214-022-00937-9 (2022).

68. Mustard, J. F. Sequestration of volatiles in the Martian crust through hydrated minerals: A significant planetary reservoir of water (Elsevier Inc., 2018) https://doi.org/10.1016/B978-0-12-804191-8.00008-8).

## Acknowledgements

The authors are eternally grateful for the Mars 2020 Science and Engineering Teams, and the decades of authors who have studied Earth's kaolinite. Funding sources: NASA contract NNH13ZDA018O for SuperCam (C.R., C.C.B., R.C.W., A.O., S.C.); SuperCam, (1532432) and Mastcam-Z (15-707, 1511125) (JRJ); Mastcam-Z (15-707, 1511125) (BK); Texaco Postdoctoral prize fellowship awarded by the division of Geological and Planetary Sciences of Caltech (L.M.); Spanish Agency for Research AEI/MCIN/FEDER, Grant No. PID2022-1427500B-I00 (J.M.M.), and NASA RSS Participating Scientist grant 80NSSC20K0239 (E.M.H.). A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).

## Author contributions

A.P.B., B.H.N.H., C.B., C.R., H.M., S.C., R.C.W., E.C.C., J.M.M., L.M., A.K., M.B., B.K., O.F., J.C., E.D., C.Q.-N., J.R.J., J.I.N., L.H., U.W., E.A.C., P.B., J.F.B., J.I.S., A.C., A.P.B., B.H.N.H., C.B., C.R., H.M., S.C., R.C.W., E.C.C., J.M.M., L.M., A.K., M.B., O.F., J.C., E.D., J.R.J., J.I.N., L.H., E.A.C., B.H.N.H., J.F.B., R.C.W., A.C., A.P.B., B.H.N.H., C.B., C.R., H.M., S.C., R.C.W., E.C.C., J.M.M., L.M., A.K., M.B., B.K., O.F., J.C., E.D., C.Q.-N., J.R.J., J.I.N., L.H., U.W., E.A.C., P.B., J.F.B., J.I.S., A.C., A.P.B., C.B., C.R., M.B., J.C., A.P.B.,
C.B., C.R., B.H.H., R.C.W., A.P.B., B.H.N.H., C.B., C.R., H.M, S.C., R.C.W., E.C.C., J.M.M., L.M., A. K., M.B., B.K., O.F., J.C., E.D., C.Q.-N., J.R.J., J.I.N., L.H., U.W., E.A.C., P.B., J.F.B., J.I.S., A.C.

**Competing interests**

The authors declare no competing interests. Co-author Candice C. Bedford is an Editorial Board Member for Communications Earth & Environment, but was not involved in the editorial review of, nor the decision to publish this article.

**Additional information**

**Supplementary information** The online version contains supplementary material available at https://doi.org/10.1038/s43247-025-02856-3.

**Correspondence** and requests for materials should be addressed to A. P. Broz.

**Peer review information** *Communications Earth and Environment* thanks John Edgar and Lindsay McHenry for their contribution to the peer review of this work. Primary Handling Editor: Joe Aslin. A peer review file is available.

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<footnote n="1">¹Department of Earth, Atmospheric and Planetary Sciences, Purdue University, West Lafayette, IN, USA. ²Department of Earth Sciences, University of Oregon, Eugene, OR, USA. ³LATMOS (Laboratoire Atmosphères, MilieuxObservations Spatiales), Guyancourt, France. ⁴Department of Earth, Planetary, and Space Sciences, University of California Los Angeles (UCLA), Los Angeles, CA, USA. ⁵University of the Basque Country (UPV/EHU), Leioa, Spain. ⁶Université Grenoble Alpes, Grenoble, France.</footnote>

<footnote n="7">⁷California Institute of Technology (Caltech), Pasadena, CA, USA. ⁸NASA Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA, USA.</footnote>

<footnote n="9">⁹Dartmouth College, Hanover, NH, USA. ¹⁰Université Paul Sabatier, Toulouse, France. ¹¹Institut d'Astrophysique Spatiale, CNRS/Université Paris-Saclay, Orsay, France. ¹²Université Claude Bernard Lyon 1, Lyon, France. ¹³Johns Hopkins University Applied Physics Laboratory (APL), Laurel, MD, USA. ¹⁴University of Nevada, Las Vegas (UNLV), Las Vegas, NV, USA. ¹⁵Los Alamos National Laboratory (LANL), Los Alamos, NM, USA. ¹⁶University of Winnipeg, Winnipeg, MB, Canada.</footnote>

<footnote n="17">¹⁷School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA. ¹⁸Astromaterials Research and Exploration Science Division (ARES), NASA Johnson Space Center, Houston, TX, USA. ¹⁹Institut de Recherche en Astrophysique et Planétologie (IRAP), Toulouse, France. ✉ e-mail: apbroz@purdue.edu</footnote>