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ABSTRACT Theoretical models indicate that water ice is stable in the shallow subsurface (depths of <1–2 m) of Mars at high latitudes1,2,3,4,5,6,7. These models have been mainly supported

by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft8,9,10. The models and measurements are

consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly

variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover11,12,13. Measurements have, however, been limited to the footprint

(several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the

seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft14, it is possible to observe such heterogeneities at subkilometre

scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and

vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to

orbit-driven climate cycles15,16,17. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The

high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales

that may be sampled by the spacecraft. Access through your institution Buy or subscribe This is a preview of subscription content, access via your institution ACCESS OPTIONS Access through

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Read our FAQs * Contact customer support SIMILAR CONTENT BEING VIEWED BY OTHERS MARTIAN WATER LOSS TO SPACE ENHANCED BY REGIONAL DUST STORMS Article 16 August 2021 FORMATION OF LUNAR SURFACE

WATER ASSOCIATED WITH HIGH-ENERGY ELECTRONS IN EARTH’S MAGNETOTAIL Article 14 September 2023 GLACIAL ISOSTATIC ADJUSTMENT REVEALS MARS’S INTERIOR VISCOSITY STRUCTURE Article Open access 26

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_Icarus_ 167, 148–165 (2004) Article  ADS  CAS  Google Scholar  Download references ACKNOWLEDGEMENTS Thanks to P. Christensen, R. Fergason, H. Kieffer, C. Edwards, R. Luk, K. Bender, and J.

Hill for data processing and targeting help and discussions. AUTHOR INFORMATION AUTHORS AND AFFILIATIONS * School of Earth and Space Exploration, Arizona State University, Tempe, Arizona

85287-6305, USA, Joshua L. Bandfield Authors * Joshua L. Bandfield View author publications You can also search for this author inPubMed Google Scholar CORRESPONDING AUTHOR Correspondence to

Joshua L. Bandfield. ETHICS DECLARATIONS COMPETING INTERESTS Reprints and permissions information is available at www.nature.com/reprints. The author declares no competing financial

interests. SUPPLEMENTARY INFORMATION SUPPLEMENTARY INFORMATION 1 This file contains Supplementary Figures S1-S3 with Legends. (PDF 2641 kb) RIGHTS AND PERMISSIONS Reprints and permissions

ABOUT THIS ARTICLE CITE THIS ARTICLE Bandfield, J. High-resolution subsurface water-ice distributions on Mars. _Nature_ 447, 64–67 (2007). https://doi.org/10.1038/nature05781 Download

citation * Received: 02 December 2006 * Accepted: 26 March 2007 * Issue Date: 03 May 2007 * DOI: https://doi.org/10.1038/nature05781 SHARE THIS ARTICLE Anyone you share the following link

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