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a tentative detection of the 183-ghz water vapor line in the martian atmosphere: constraints upon the h2o abundance and vertical distributionThe 183-GHz water vapor line was tentatively detected on Mars in January 1991, with the IRAM 30-m millimeter antenna, under extremely dry atmospheric conditions. The measurement refers to the whole disk. The spectral line, although marginally detected, can be fit with a constant H2O mixing ratio of 1.0 x 10(exp -5), which corresponds to a water abundance of 1 pr-microns; in any case, an upper limit of 3 pr-microns is inferred. This value is comparable to the very small abundances measured by Clancy (1992) 5 weeks before our observation and seems to imply both seasonal and long-term variations in the martian water cycle.
Document ID
Document Type
Reprint (Version printed in journal)
External Source(s)
Encrenaz, TH.
(Observatoire de Paris Meudon, France)
Lellouch, E.
(Observatoire de Paris Meudon, France)
Cernicharo, J.
(Centro Astronomico de Yebes Guadalajara, United States)
Paubert, G.
(IRAM Granada, United States)
Gulkis, S.
(Jet Propulsion Laboratory, Pasadena, CA United States)
Date Acquired
August 16, 2013
Publication Date
January 1, 1995
Publication Information
Publication: Icarus
Volume: 113
Issue: 1
ISSN: 0019-1035
Subject Category
Distribution Limits