Mapping of Ozone and Water in the Atmosphere of Mars near the 1997 Aphelion

Identification of a new band system of isotopic CO2 near 3.3 μm: Implications for remote sensing of biomarker gases on Mars

“…The varied surface temperatures and albedos across the Mars surface lead to differences in the apparent thermal/solar ratio, and thus in the apparent equivalent width of the observed Fraunhofer lines. By comparing a residual spectrum to the solar spectrum measured by the ATMOS instrument (Farmer et al, 1994;Farmer and Norton, 1989), we estimated the ratio of the thermal and solar components point-by-point along the slit (Novak et al, 2002). The apparent thermal/solar ratio was typically <20% at these wavelengths.…”

Airglow on Mars: Some model expectations for the OH Meinel bands and the O IR atmospheric band

“…From then, its study has proven useful in the tracing of daytime ozone in the martian atmosphere (Traub et al, 1979;Krasnopolsky, 1997Krasnopolsky, , 2003; Krasnopolsky and Bjoraker, 2000;Novak et al, 2002). During the daytime, O 2 (a 1 ∆ g ) is formed in the lower atmosphere of Mars from ozone photodissociation at wavelengths shorter than the threshold for O 3 + hν → O 2 (a 1 ∆ g ) + O( 1 D) near 3100 Å.…”

Photoemission Phenomena in the Solar System

“…In the dayglows, this intensity can be enhanced even further by reaction (4b) in Table 1, dissociative excitation of O 3 . The fact that in the case of both the Earth (Mlynczak et al 2001) and Mars (Noxon et al 1976) the dayglow intensities are very high is diagnostic of the presence of ozone, and ozone is mapped over the sunlit hemispheres by this emission (Krasnopolsky 2003;Novak et al 2002). For Venus, the 1.27 µ emission from O-atom recombination is extremely variable (Crisp et al 1996).…”