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We report new exposures of water ice along the scarps wall located within craters in the northern midlatitude region of Mars using high‐resolution imagery and spectral data of Mars Reconnaissance Orbiter. The exposed water‐ice deposits are shallower and exhibit 1.5 and 2 μm absorption. These scarps are located on the pole‐facing walls and equator‐facing wall origin floor deposits which formed over the latitude dependent mantle. Our observations advance in bracketing the younger ice deposits through the crater size‐frequency distributions of host craters, which formed around ~25 and ~95 Myr and exposed around ~1 Myr. This reveals that ice transportation, accumulation, compaction, and ice‐dust mixing occurred in recent epochs. Our study complements the earlier studies that shallow water ice is spatially widespread and consistent with subsurface water‐ice detection by neutron spectrometer. We interpret the ice remnants likely to preserve in craters pole‐facing wall and equator‐facing wall‐associated floor deposits, which demonstrates widespread water‐ice resources on Mars.

Boulder falls and their tracks are typically observed on Mars and the Moon using high-resolution images (McEwen et al., 2007;Robinson et al., 2010). These falls indicate recent active mass wasting processes on these bodies. Such tracks are ubiquitous on steeply sloping terrain, and where particularly abundant have been used to infer active seismicity (Bickel et al., 2019;Brown & Roberts, 2019;Taylor et al., 2013), giving insight into endogenic processes. Repeat temporal imaging has shown that boulder falls are ongoing on Mars, as first observed by the Mars Global Surveyor-Mars Orbiter Camera images from the southern hemisphere and Valles Marineris (https://www.msss.com/mars_images/moc/2005/09/20/bouldertracks/). Subsequently, several studies have used repeat temporal imaging using HiRISE to identify and study recent boulder falls (Dundas &

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