1. The Herschel-SPIRE submillimetre spectrum of Mars
- Author
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José Cernicharo, M. de Val-Borro, L. Decin, J. A. D. L. Blommaert, Ganna Portyankina, M. Renge, R. Moreno, Edwin A. Bergin, M. I. Blecka, Sarah Leeks, B. M. Swinyard, T. Encrenaz, Michael Kueppers, Geoffrey A. Blake, J. Crovisier, Emmanuel Jehin, N. Biver, Matthew Joseph Griffin, E. Lellouch, L. M. Lara, F. Bensch, Dariusz C. Lis, P. J. Encrenaz, G. S. Orton, G. Davis, Daphne Stam, C. Waelkens, Alexander S. Medvedev, Dominique Bockelée-Morvan, H. J. Walker, Christopher Jarchow, Régis Courtin, Bart Vandenbussche, Eva Verdugo, Paul Hartogh, Marek Banaszkiewicz, Rudolf Schieder, Hideo Sagawa, Nicolas Thomas, Thibault Cavalié, Slawomira Szutowicz, Trevor Fulton, M. R. Kidger, Sunil Sidher, T. de Graauw, David A. Naylor, F. Billebaud, Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Center for Mathematics and Physics, University of Aizu, Polska Akademia Nauk = Polish Academy of Sciences (PAN), Space Research Centre of Polish Academy of Sciences (CBK), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), SRON Netherlands Institute for Space Research (SRON), Centre Alexis Vautrin (CAV), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)
- Subjects
010504 meteorology & atmospheric sciences ,[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,Fourier transform spectrometers ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Planet ,0103 physical sciences ,Mixing ratio ,Calibration ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Atmospheric models ,Detector ,Astronomy and Astrophysics ,Mars Exploration Program ,Computational physics ,13. Climate action ,Space and Planetary Science ,Earth and Planetary Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Data reduction - Abstract
We have obtained the first continuous disk averaged spectrum of Mars from 450 to 1550 Ghz using the Herschel-SPIRE Fourier Transform Spectrometer. The spectrum was obtained at a constant resolution of 1.4 GHz across the whole band. The flux from the planet is such that the instrument was operated in "bright source" mode to prevent saturation of the detectors. This was the first successful use of this mode and in this work we describe the method used for observing Mars together with a detailed discussion of the data reduction techniques required to calibrate the spectrum. We discuss the calibration accuracy obtained and describe the first comparison with surface and atmospheric models. In addition to a direct photometric measurement of the planet the spectrum contains the characteristic transitions of 12CO from J 5-4 to J 13-12 as well as numerous H2O transitions. Together these allow the comparison to global atmospheric models allowing the mean mixing ratios of water and 12CO to be investigated. We find that it is possible to match the observed depth of the absorption features in the spectrum with a fixed water mixing ratio of 1 x 10-4 and a 12CO mixing ratio of 9 x 10-4, Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue
- Published
- 2010