The Herschel-SPIRE submillimetre spectrum of Mars

被引：9

作者：

Swinyard, B. M. ^{[1
]}

Hartogh, P. ^{[2
]}

Sidher, S. ^{[1
]}

Fulton, T. ^{[3
]}

Lellouch, E. ^{[5
]}

Jarchow, C. ^{[2
]}

Griffin, M. J. ^{[4
]}

Moreno, R. ^{[5
]}

Sagawa, H. ^{[2
]}

Portyankina, G. ^{[6
]}

Blecka, M. ^{[7
]}

Banaszkiewicz, M. ^{[7
]}

Bockelee-Morvan, D. ^{[5
]}

Crovisier, J. ^{[5
]}

Encrenaz, T. ^{[5
]}

Kueppers, M. ^{[8
]}

Lara, L. ^{[9
]}

Lis, D.

Medvedev, A. ^{[2
]}

Rengel, M. ^{[2
]}

Szutowicz, S. ^{[7
]}

Vandenbussche, B. ^{[11
]}

Bensch, F. ^{[12
]}

Bergin, E. ^{[13
]}

Billebaud, F. ^{[14
]}

Biver, N. ^{[5
]}

Blake, G.

Blommaert, J. ^{[11
]}

de Val-Borro, M. ^{[2
]}

Cernicharo, J. ^{[15
]}

Cavalie, T. ^{[2
]}

Courtin, R. ^{[5
]}

Davis, G. ^{[16
]}

Decin, L. ^{[11
]}

Encrenaz, P. ^{[5
]}

de Graauw, T.

Jehin, E. ^{[17
]}

Kidger, M. ^{[8
]}

Leeks, S. ^{[1
]}

Orton, G. ^{[10
]}

Naylor, D. ^{[18
]}

Schieder, R. ^{[19
]}

Stam, D.

Thomas, N. ^{[6
]}

Verdugo, E. ^{[8
]}

Waelkens, C.

Walker, H. ^{[1
]}

机构：

[1] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England

[2] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany

[3] Bluesky Spect, Lethbridge, AB, Canada

[4] Cardiff Univ, Sch Phys & Astron, Cardiff, S Glam, Wales

[5] Observ Paris, LESIA, Paris, France

[6] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland

[7] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland

[8] European Space Agcy, European Space Astron Ctr, Madrid, Spain

[9] Inst Astrofis Andalucia, E-18080 Granada, Spain

[10] CALTECH, Jet Prop Lab, Pasadena, CA USA

[11] Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium

[12] Univ Bonn, Argelander Inst Astron, D-5300 Bonn, Germany

[13] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[14] Univ Bordeaux, Lab Astrophys Boredeaux, Bordeaux, France

[15] INTA, CAB CSIC, Lab Mol Astrophys, Madrid, Spain

[16] Joint Astron Ctr, Hilo, HI 96720 USA

[17] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium

[18] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada

[19] Univ Cologne, Inst Phys 1, D-5000 Cologne 41, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

instrumentation: spectrographs; space vehicles: instruments; planets and satellites: atmospheres; planets and satellites: individual: Mars; planets and satellites: composition; MARTIAN WATER-VAPOR; VERTICAL-DISTRIBUTION; ATMOSPHERE; EXPRESS; CO; INSTRUMENT; SURFACE; CLIMATE; HELLAS;

D O I：

10.1051/0004-6361/201014717

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 (CO)-C-12 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 (CO)-C-12 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 (CO)-C-12 mixing ratio of 9 x 10(-4).

引用

页数：4

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