POSTER SESSION F: Tp Tm Mt Ma Pl St At Pd Hg

Geologic mapping of the Navua Valles

Wednesday, July 5
3:50 PM - 6:50 PM
Location: Exhibit Hall C

Navua Valles is a valley and channel system on the inner Northeastern rim of Hellas Basin on Mars. We mapped this region and assessed material unit ages based on our crater counting results. In this poster we present the 1:1M scale geologic map, focusing on the process of geological planetary mapping, the sources of uncertanties, and the methods we used to depict the area's geological history in an easily accessible and cartographically accurate, and also aesthetic way.
We mapped an area of 267,000 km2 (445×600 km) between 79.58°E, 28.1°S and 87.1°E, 38.2°S, which overlaps with MC-21 and MC-28 quadrangles. We mapped the region using ESRI’s ArcMap software. We used 161 Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) images as a primary base map (~6 m/px resolution, 99.17% coverage). These were selected using the USGS Planetary Image Locator Tool (PILOT) (Bailen et al. 2013). Raw CTX images were processed using the Astrogeology Cloud Processing tool “Map Projection on the Web” (POW) (Hare et al. 2013), which updates camera pointing information, applies radiometric correction, removes striping, stretches, and projects the images into equirectangular map projection. The Mars Odyssey Thermal Emission Imaging System (THEMIS) night-time IR mosaic (100 m/px resolution) was used to determine the thermal inertia properties of surface materials. Additionally, we used 62 MRO High-Resolution Imaging Science Experiment (HiRISE) images (25–50 cm/pixel resolution) to support the morphological analysis of the surface units.
Since IAU’s policy is that names of planetary surface features are kept at minimum, we refer to unnamed craters with their Robbins Crater Database ID number, which is composed of its MC quad number and an arbitrary ID (Robbins and Hynek 2012). Zeros preceding the local ID were removed from the IDs in this work.
Geological unit symbology was partly taken from Nass et al. (2011). We implemented the Ivanov (2001) production function, the Hartman and Neukum (2001) chronology function and the “Neukum system” of Martian period boundaries that is built into CraterStats II as default (Michael 2013).
Contacts within the visually indistinct plains units were inferred from THEMIS night-time IR data. In an iterative process, we determined crater model ages for these candidate units, and then merged those units that had similar crater size frequency curves and also exhibited similar visual patterns.

Henrik I. Hargitai

Postdoctoral Researcher
NASA Ames Research Center

Henrik I. Hargitai (Ph.D., 2007) is a planetary geomorphologist and media historian. He is a postdoctoral fellow at the NASA Ames Research Center. He taught planetary geomorphology, planetary cartography, typography, and media history as a senior lecturer at Eötvös Loránd University, Budapest, Hungary since 2002. He has a Ph.D. in Earth Sciences and Philosophy (Aesthetics). His study fields include planetary cartography, fluvial geomorphology, and the history and localization of planetary nomenclature. He participated in two Mars Desert Research Station simulations. He is the chair of the ICA Commission on Planetary Cartography.

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