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Mapping Martian Atmospheric Pressure with Ground-Based Near Infrared Spectroscopy

Published online by Cambridge University Press:  05 March 2013

Sarah A. Chamberlain ,
Jeremy A. Bailey  and
David Crisp
Sarah A. Chamberlain*
Affiliation:
Australian Centre for Astrobiology, Macquarie University, NSW 2109, Australia
Jeremy A. Bailey
Affiliation:
Australian Centre for Astrobiology, Macquarie University, NSW 2109, Australia
David Crisp
Affiliation:
Jet Propulsion Laboratory/Caltech, 4800 Oak Grove Dr, Pasadena, CA 91125, USA
*
CCorresponding author. E-mail: schamber@els.mq.edu.au
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Abstract

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We present images of Mars obtained in the 2.0 μm CO2 band with the United Kingdom Infrared Telescope (UKIRT). The images reveal topographic features of the Martian surface that are usually invisible in direct albedo images at visible or IR wavelengths, but agree remarkably well with the topography of the planet as mapped by the MOLA instrument on Mars Global Surveyor. The CO2 band depth is a measure of the absorbing column of CO2 and hence determined primarily by the surface atmospheric pressure. The surface pressure variations are detected with a sensitivity of 4–5 Pa. We compare our data with radiative transfer models and find that the measured CO2 variation with pressure is consistent with the models. We discuss the possibility that similar observations might be used to observe atmospheric pressure changes due to Martian weather systems.

Keywords

planets and satellites: individual (Mars)techniques: spectroscopicinfrared: solar system
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 23 , Issue 3 , 2006 , pp. 119 - 124
Copyright
Copyright © Astronomical Society of Australia 2006

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