The Windjana drill sample, a sandstone of the Dillinger member (Kimberley formation, Gale Crater, Mars), was analyzed by CheMin X‐ray diffraction (XRD) in the MSL Curiosity rover. From Rietveld refinements of its XRD pattern, Windjana contains the following: sanidine (21% weight, ~Or95); augite (20%); magnetite (12%); pigeonite; olivine; plagioclase; amorphous and smectitic material (~25%); and percent levels of others including ilmenite, fluorapatite, and bassanite. From mass balance on the Alpha Proton X‐ray Spectrometer (APXS) chemical analysis, the amorphous material is Fe rich with nearly no other cations—like ferrihydrite. The Windjana sample shows little alteration and was likely cemented by its magnetite and ferrihydrite. From ChemCam Laser‐Induced Breakdown Spectrometer (LIBS) chemical analyses, Windjana is representative of the Dillinger and Mount Remarkable members of the Kimberley formation. LIBS data suggest that the Kimberley sediments include at least three chemical components. The most K‐rich targets have 5.6% K2O, ~1.8 times that of Windjana, implying a sediment component with >40% sanidine, e.g., a trachyte. A second component is rich in mafic minerals, with little feldspar (like a shergottite). A third component is richer in plagioclase and in Na2O, and is likely to be basaltic. The K‐rich sediment component is consistent with APXS and ChemCam observations of K‐rich rocks elsewhere in Gale Crater. The source of this sediment component was likely volcanic. The presence of sediment from many igneous sources, in concert with Curiosity's identifications of other igneous materials (e.g., mugearite), implies that the northern rim of Gale Crater exposes a diverse igneous complex, at least as diverse as that found in similar‐age terranes on Earth.

Gale crater, geological context of the rover traverse and samples studiedThe Curiosity rover landing site is located at -4.59° S, 137.44° E). Fig. S1a shows a portion of the THEMIS IR nighttime mosaic of Bradbury Rise. The landing site is marked by a black cross within the landing ellipse. It is located at a distal portion of the alluvial fan stretching below Peace Vallis on the northern rim of Gale crater.Mafic and light-toned igneous float rocks were initially observed by the Curiosity rover close to the Bradbury landing site from sol 1 to 55 in the Hummocky plain unit. After Curiosity left the fluvio-lacustrine deposit of Yellow Knife Bay (sol 55-326), it traversed back across the hummocky unit (Fig. S1b). An increasing number of light-toned rocks dominated by feldspars (porphyritic, felsic coarse-grained, felsic fine-grained) together with three groups of mafic rocks were observed along the traverse from sol 326 to sol 550. The mafic rocks are described in detail in Cousin et al. (2015) 43 and Sautter et al. (2014) 45 . The rocks selected for the present study are summarized in Table S1. Laser-Induced Breakdown Spectrometer (LIBS) spectraChemCam's laser-induced breakdown spectrometer (LIBS) uses a pulsed laser to ablate targets up to ≈ 7 m from the rover. The size of the laser interaction varies with distance, ranging from 350 µm at 1.5 m to 550 µm at 7 m 36 . The light emitted by the ablated plasma spark is collected by the same telescope used to transmit the laser beam, and is analyzed by three spectrometers which record the atomic emission spectrum over the ultraviolet (UV: 240.1-342.2nm), violet (VIO: 382.1-469.3 nm), and visible to near-infrared (VNIR: 474.0-906.5 nm) ranges 21, 22 . The ChemCam LIBS spectra consist of 6144 channels covering the above wavelength range in wavelength with typically several hundred emission peaks covering all of the major elements and many minor and trace elements.A typical ChemCam LIBS observation involves the analysis of multiple locations on the target: common geometries for LIBS observations are square grids (e.g. 3×3, 4×4) and

[1] Gale Crater is filled by sedimentary deposits including a mound of layered deposits, Aeolis Mons. Using orbital data, we mapped the crater infillings and measured their geometry to determine their origin. The sediment of Aeolis Mons is interpreted to be primarily air fall material such as dust, volcanic ash, fine-grained impact products, and possibly snow deposited by settling from the atmosphere, as well as wind-blown sands cemented in the crater center. Unconformity surfaces between the geological units are evidence for depositional hiatuses. Crater floor material deposited around Aeolis Mons and on the crater wall is interpreted to be alluvial and colluvial deposits. Morphologic evidence suggests that a shallow lake existed after the formation of the lowermost part of Aeolis Mons (the Small yardangs unit and the mass-wasting deposits). A suite of several features including patterned ground and possible rock glaciers are suggestive of periglacial processes with a permafrost environment after the first hundreds of thousands of years following its formation, dated to~3.61 Ga, in the Late Noachian/Early Hesperian. Episodic melting of snow in the crater could have caused the formation of sulfates and clays in Aeolis Mons, the formation of rock glaciers and the incision of deep canyons and valleys along its flanks as well as on the crater wall and rim, and the formation of a lake in the deepest portions of Gale.