H2 column densities and relative HD abundances toward a variety of warm regions in the Galaxy and the LMC/SMC

Details H2 column densities and relative HD abundances toward a variety of warm regions in the Galaxy and the LMC/SMC H2 column densities and relative HD abundances toward a variety of warm regions in the Galaxy and the LMC/SMC

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop...18h&link_type=abstract

Spitzer Proposal ID #18

Mathematics

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Scientific paper

The relative deuterium abundance in the galaxy, and ultimately, the cosmological deuterium abundance, can be determined only if reliable H2 reference column densities can be derived. A promising way to derive H2 column densities is via the mid-IR rotational lines of para-H2 (S(2) 12 micron and S(0) 28 micron) and ortho-H2 (S(1) 17 micron). We use the IRS to observe these lines toward a number of Galactic HII and SNR regions (M17SW, IC443 and NGC1096A) and regions in the LMC and SMC (N44, N81, N83B, N88, N113, N159A, N160A, LIRS36). Corresponding observations of the HD(1-0) line at 112 microns will be performed with SOFIA. One of us (R.Guesten) is PI of the 2.6 THz heterodyne instrument dedicated to observations of this transition aboard SOFIA.

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