Geological mapping of Mawrth Vallis, Mars, by PLANMAP
Authors: Wright Jack , Balme Matthew , Davis Joel , Fawdon Peter , Rothery David 
Published: October 2020

IntroductionMawrth Vallis is generally considered to be the oldest of Mars&#8217; outflow channels [1]. It incises Noachian (>&#160;3.7&#160;Ga) terrain and is associated with thick (>&#160;150&#160;m), clay-bearing deposits [2]. Clays are important astrobiologically because they are potential catalytic substrates for (pre)biotic chemistry [3] and have a high potential to preserve biosignatures [4]. The presence of clay-bearing deposits was an important factor in the decision to shortlist an area adjacent to Mawrth Vallis as a candidate landing site for the ExoMars &#8220;Rosalind Franklin&#8221; rover [5], whose mission is to search for signs of ancient life on Mars [6]. Ultimately, Mawrth Vallis was not selected as the ExoMars landing site.The origin and geological context of the clay-bearing deposits is not well understood [7]. Furthermore, the geomorphology of Mawrth Vallis, which records its history of deposition/burial and erosion/exhumation, is also less well-studied compared with its mineralogy. Here, we present our ongoing geological mapping of Mawrth Vallis, which we are conducting to investigate the relationship between the channel and the clay-bearing deposits. We are producing a detailed map of the main Mawrth Vallis channel adjacent to the proposed ExoMars landing ellipse. We will also produce an accompanying geomorphic feature map along the whole length of Mawrth Vallis at a smaller scale.We are creating this map as part of the Planmap project [8], which aims to provide standards for European researchers to adhere to in order to aid the dissemination of their maps. Planmap is producing exemplar maps of Mercury [e.g. 9], the Moon [e.g. 10], and Mars [e.g. this work], where various datasets (visual images, elevation models, spectra, crater size-frequency distributions) will be fused to make more fully-intergrated geological maps. The abundance and diversity of data types at Mawrth Vallis, in addition to its scientific interest, make this region particularly suitable for Planmap.DataWe are using a ~6&#160;m/pixel orthorectified CTX [11] mosaic basemap, supplemented by 25&#8211;50&#160;cm/pixel HiRISE images [12], ~4&#160;m/pixel colour CaSSIS images [13], and ~20&#160;m/pixel CTX digital elevation models (DEMs).MethodsWe are mapping using ArcGIS 10.6.1. Mawrth Vallis spans 340&#176;E&#8211;247&#176;E and 18&#176;N&#8211;26&#176;N. We are mapping in a stereographic projection centred on 343&#176;E, 22.4&#176;N. We are digitising the main map on the CTX mosaic at 1:20,000-scale (~full CTX resolution), and intend to publish the map at ~1:100,000-scale. The geomorphic feature map will be published alongside the main map. We will use HiRISE and CaSSIS images to aid unit definition and CTX DEMs to aid stratigraphic interpretation.Results and future workFigure 1 shows the current state of our map.We plan to begin work on the geomorphic feature map soon. Progress on the main map will continue in parallel. We will investigate the stratigraphic position of Mawrth Vallis relative to the large impact craters in the region. We will consider how the stubby depressions that occur with the main channel&#8217;s walls formed.AcknowledgementsThis project has received funding from the European Union&#8217;s Horizon 2020 research and innovation programme under grant agreement No 776276.References[1] Ivanov and Head (2001) J. Geophys. Res., 106, 3275&#8211;3295. [2] Loizeau et al. (2007), J. Geophys. Res. Planets, 112, E8. [3] Hazen and Sverjensky (2010), CSH Perspect. In Biol., 2, a002162. [4] Farmer and Des Marais (1999), J. Geophys. Res. Planets, 104, 26977&#8211;26995. [5] Poulet et al. (2020), Astrobiology, 20, 199&#8211;234. [6] Vago et al. (2017), Astrobiology, 17, 471&#8211;510. [7] [8] Massironi et al. (2018), Geophys. Res. Abs., 20, EGU2018-18106. [9] Wright et al. (2019), J. Maps, 15, 509&#8211;520. [10] P&#246;hler et al. (2020) Europ. Lunar. Sym., Abstract. [11] Malin et al. (2007), J. Geophys. Res. Planets, 112, E5. [12] McEwen et al. (2007), J. Geophys. Res. Planets, 112, E5. [13] Thomas et al. (2017), Space Sci. Rev., 212, 1897&#8211;1944.