Abstract
On a very high dispersion spectrogram of Mars we have searched unsuccessfully for Martian H 2O lines near γ 7200. The plate was taken on a very dry night when the Doppler shift was sufficient to displace any Mars H 2O lines 0.29A˚from their telluric counterparts. From this data we have derived an upper limit for the integrated Martian water vapor abundance of approximately 3.5 × 10 −3 gm/cm 2 (35 μ). The practical limits for detection of Martian water vapor by Earth-bound, ballon, and space probe techniques indicate that spectroscopic observations from the Earth can be refined to a point where they are at least as sensitive as present infrared space experiments.
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