Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21422103l&link_type=abstract
American Astronomical Society, AAS Meeting #214, #221.03; Bulletin of the American Astronomical Society, Vol. 41, p.727
Astronomy and Astrophysics
Astronomy
Scientific paper
Optical/uv/near-IR absorption lines against nearby bright stars show the presence of small molecules in the nearby ISM, even when AV < 1 mag; H2, H3+, CH+, C2, C3, CO, CN, CH, OH and NH. Locally 25%-45% of diffuse neutral H is in H2. Radio studies increase the pool to families such as CN, HCN, and HNC; CH, C2H and C3H2; OH, CO and HCO+; CS, SO, HCS+, H2S; and to H2CO and NH3, with relative abundances of polyatomics like those in TMC-1. In general the origins of these molecules are not understood although N(HCO+) and N(HCS+) account for N(CO) and N(CS). In this talk I will summarize the chemical systematics and what it reveals of the internal physical state of the gas. I will present new images of CO and HCO+ in emission, showing for the first time the broad outlines and turbulent internal gas flows in diffuse clouds. CO emission is much more widespread than in existing "all-sky" CO surveys and may be quite bright (up to 13K), leading to unavoidable confusion with emission from "molecular clouds". Actually seeing internal gas flows on the plane of the sky gives a very different perspective on the meaning of individual absorption line profiles.
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