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. 2020 Feb 24;11:1014. doi: 10.1038/s41467-020-14679-1

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© The Author(s) 2020

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons license and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/.

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Fig. 2 — Image shows the landing ellipse (E9, dark blue, 130 km × 27 km), with trajectory correction maneuver 5 (TCM5) course adjusted target (green dot), the last orbit determination solution and ellipse (LaRC green, 77.4 km × 23.2 km), the extrapolated inertial measurement unit (IMU) surface location, the RISE estimate from Sol 1 (4.49751° ± 0.00471°N, 135.6178693° ± 0.000337°E, hidden behind the lander dot, red), and HiRISE-based location from December 6th, 2018. Background image mosaic is from the daytime Thermal Emission Imaging System (THEMIS) infrared global mosaic at 100 m/pixel. The dominant surface is smooth Early Amazonian-Hesperian plains deformed by north-trending wrinkle ridges (suggesting subsurface basalt flows) with large impact craters^2,3. Craters larger than around 40 m but smaller than around 2 km are dark (indicating colder daytime temperatures with higher thermal inertia), rocky ejecta craters¹⁸. These craters excavate strong coherent rock (basalt) from depths of 4–200 m depth, with a fractured regolith on top and weaker sediments beneath^2,3,18.