2-D Maps Of The O2(a1Δg) Emission During The Mars Aphelion Season

Details 2-D Maps Of The O2(a1Δg) Emission During The Mars Aphelion Season 2-D Maps Of The O2(a1Δg) Emission During The Mars Aphelion Season

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.2407s&link_type=abstract

American Astronomical Society, DPS meeting #39, #24.07; Bulletin of the American Astronomical Society, Vol. 39, p.455

Astronomy and Astrophysics

Astronomy

Scientific paper

We have constructed 2-D maps of the O2 (a1Δg) emission (1.27 μm) for five seasonal dates spanning Mars’ aphelion season. This emission can be used as an indicator of ozone above 20 km. The seasonal dates to be presented are Ls = 333o (Jan 13, 2004), Ls = 357o (Jan 16, 2006), Ls = 85o (Mar 1, 1997), Ls = 114o (Mar 23, 1999), and Ls = 156o (Mar 22, 2003). The data were collected using CSHELL at the NASA Infrared Telescope Facility. The slit was positioned in the North-South direction on Mars. Spectral/spatial data were taken at 1.0 arc-sec increments East to West across Mars. For Ls = 333o, no emissions were detected above the noise level (0.2 MRayleighs). Just before the vernal equinox (Ls = 357o), strong emissions (> 12 MR) were detected in both polar regions with the stronger emission in the North. At Ls = 85o emissions were significant across the planet, but by Ls = 114o the emissions in the Northern Hemisphere were much weaker than those in the South. For Ls = 156o, the emissions are concentrated in the Southern polar region. One-dimensional maps in which the slit is place along the central meridian of Mars will also be presented for Ls = 67o (Jan 21, 1997) and Ls = 133o (Mar 21, 2001). The presence of significant O2 (a1Δg) emission (> 2.0 MR) also indicates that the local hygropause is at a low altitude (< 20 km).
We acknowledge a grant from NSF-RUI (AST-0505765) and the administrators and staff of the NASA-IRTF.

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