52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2509.pdf

HIGH-PRECISION TOPOGRAPHIC MAP OF THE MARS 2020 LANDING SITE AS PART OF THE MC-13E SYRTIS MAJOR QUADRANGLE DIGITAL TERRAIN MODEL. A. Neesemann1, S.H.G. Walter1, C. Gross1, R. Jaumann1, K. Gwin- ner2, G.G. Michael1, B.P. Schreiner,1 W. Zuschneid1, D. Neu1, H. Balthasar1, C. Rabethge1, C. Riedel1, E. Kersten2, D. Tirsch2 1Freie Universität Berlin, Institute of Geological Sciences, Planetary Sciences and Remote Sensing. Malteserstr. 74-100, 12249 Berlin, Germany ([email protected]), 2German Aerospace Center (DLR) Berlin, Institute of Planetary Research, Ruther- fordstr.2, 12489 Berlin, Germany

67.5°E 90°E Introduction 30°N 30°N For more than 17 years, the High Resolution Stereo Camera (HRSC) [1] onboard Mars Express (MEx) has acquired image data of the Red Planet on a global scale and at high resolution. 3164

E Although outmatched in spatial resolution by the Context A S S O F Camera (CTX) [2], the High Resolution Imaging Science

I L I Experiment (HiRISE) [3] and more recently by the Colour and Height above Areoid GMM3 Mars (m) N Stereo Surface Imaging System (CaSSIS) [4], providing essenti- al and high quality data necessary for detailed geological and geomorphological studies, the unique capabilities of the HRSC Fig. 3 lie in its virtually simultaneous coverage of large areas by ve panchromatic and four narrow band lters (RGB and IR) at I S I D I S dierent phase angles. Digital Terrain Models (DTMs) P L A N I T I A resulting from high-precision 3D point accuracy and density S Y usually have a grid space of 50 m with at least one 3D point per R T

I

grid cell and are subsequently tied to the Mars Orbiter Laser S

M

Altimeter (MOLA) global reference system [5]. ereby, these A

J

O

datasets not only constitute an ideal base for the production of R 12.5 mpx-1 panchromatic and 50 mpx-1 RGB HRSC ortho- -5063 images but can also be used for the improvement of SPICE1 information and the production of orthoimages and higher- 0° 0° level data products of other cameras. 67.5°E 90°E Fig. 1. Bundle-adjusted HRSC-based DTM of the eastern half of the Data and Methods MC-13 quadrangle Syrtis Major including large parts of the Isidis basin, the Syrtis Major volcanic complex and thr concentric graben system Nili Within the framework of producing multi-orbit bundle-ad- Fossae. Only few, narrow gaps remain as a result of lower data quality justed DTMs [6] and brightness-adjusted panchromatic and (atmospheric contamination, lower resolution) in these areas. colour mosaics [7] for each of the 30 USGS Mars Chart (MC) quadrangles2, the eastern half of the MC-13 Syrtis Major (Fig. [9]. CTX orthoimages are then calibrated to an external 1) was only recently nished. It covers i.a. the Mars 2020 brightness reference [7,10] in order create seamless CTX ortho- Perseverance rover landing site within the 49.8-km-sized Jezero mosaics and pan-sharpened CTX + HRSC RGB color mosaics crater (Fig. 3). Based on the new HRSC topography data and of the landing site for scienti c studies and VR applications. orthoimages, we improved information of the camera pointing and spacecraft position of CTX data covering Jezero crater by Preliminary Investigation, Results, Outlook bundle adjustmend using the USGS ISIS3 application Jigsaw Compared to earlier MOLA-based studies [11] the new data

-1600 20 x vertical exaggeration -1800 In -2000 2 In1 -2200 -2373 m -2400 311 m -2600 In , In : Inlet Valley -2800 1 2 -2684 m Out1 Out1: Outlet Valley -3000

Height above GMM3 Mars Areoid (m) GMM3 Mars Areoid above Height 80 70 60 50 40 30 20 10 0 10 20 30 40 50 60 70 Topographic pro le length, starting from the crater center at 18.40°N/77.71°E (km)

Fig. 2. Topographic pro les of the inlet (In1 and In2) and outlet channels (Out1) and across Jezero crater. e dashed line indicates the water level at the end of water inow and further incision of the outlet channel into the crater. See Fig. 3 for the course of the pro les.

1https://naif.jpl.nasa.gov/naif/index.html .35/0 [8]. 2To gain an insight into the status of produced higher level HRSC data 3Integrated Software for Imagers and Spectrometers (https://isis.astrogeo- products please visit https://maps.planet.fu-berlin.de/#map=3/2074498 logy.usgs.gov/) 52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2509.pdf

77.0°E In2 77.5°E 78.0°E - 500 0 -180

0 19.0°N -180 19.0°N -180 -190 0 0

-220 0 -2400 0 -210 -270 -2600 -220 0 -210 0 - 1000 -1900 0 -2000 0 Out1

-2100 -250 -2000

-190 -260 0 -200 0 0

-240 -200 - 1500 Height above Areoid GMM3 Mars (m) 0 -210 0 0 0 -220 In1 0 LFD -250 18.5°N -2600 18.5°N -230

0 0

-190 -190 0 0 -210 Perseverance LSE -1800 -170 0 -1500 -200 - 2000 -2000 -250 -1400 -160 -2700 0 0 0 0 0 -130 0 0 0 -220 0 0 -200 10 -100 -180 -170 -1 0 -800 0 -120 -700 -200 -220 0

0 -900 0 -230 -190

0 -180 0 -210 0 -260 -170 0 0 - 2500

-240 0 0 -210 -200 18.0°N 18.0°N -200 0 0

-240

0 0 -2100 -250 -250 0-2600 -270 -270 -240 -2900 0 0 0 0 0 0 0 -220 -280 -250 -270 -260 -280 -2900 0 -270 - 3000 0

- 3145 77.0°E 77.5°E 78.0°E km SCALE 1:575,000 (1MM = 0.575 KM) 0 2.5 5 10 15 20 STEREOGRAPHIC PROJECTION (clat: 18.40°N, clon: 77.71°E) Fig. 3. HRSC-based topographic map of the 49.8-km-sized Jezero crater and its surroundings. e solid ellipse indicates the landing site ellipse (LSE) close to the Lacustrine Fan Delta (LFD) in which the Mars 2020 Perseverance rover is supposed to land on February 18, 2021. A high resolution version of this map can be accessed at https://www.geo.fu-berlin.de/en/geol/fachrichtungen/planet/presse/2020_jezero_topo/_content/galerie_li/map-image.jpg?html =1&11214960&ref=111216438.

enable for the rst time for detailed geomorphologic investiga- 50QM1301, 50QM1702 and 50QM2001 (HRSC on Mars tion of the Jezero crater on a broad scale at high lateral precisi- Express), on behalf of the German Federal Ministry for Econo- on. In the rst step we calculated the water level when the mic Aairs and Energy. inow dried up (Fig. 2 and 3) thus stopping further incision of the outow channel into surrounding terrains. Further investi- References gation of volumetric ow and erosion rates are in progress with [1] Jaumann et al. 2015. Planet Space Sci. 112, 53-97. [2] Malin et al. the potential of improving results from previous studies [11]. 2007. J. Geophys. Res. 112(E05). [3] McEwen et al. 2007. J. Geophys. Res. 112(E5). [4] omas et al. 2017. Space Sci. Rev. 212, 1897-1944. [5] Gwinner et al. 2010. Earth Planet Sc. Lett. 294(3-4), 506-519. [6] Acknowledgement Gwinner et al. 2016. Planet Space Sci. 126, 93-138. [7] Michael et al. We thank the HRSC experiment team at DLR Berlin and the 2016. Planet Space Sci. 121, 18-26. [8] Walter et al. 2018. Earth Space Sci. Mars Express operations team at the European Space Opera- 5(7), 308-323. [9] Edmundson et al. 2012. ISPRC Ann. Photogramm. tions Centre (ESOC) for their relentless commitment in Remote Sens. Spatial Inf. Sci. 1-4, 203-208. [10] Robbins et al. 2020. Earth providing high-quality HRSC data products. is work was Space Sci. 7(10). [11] Fassett and Head 2005. Geophys. Res. Lett. 32(14). supported by the German Space Agency (DLR Bonn), grants