Tracing unseen gas in the Large Magellanic Cloud

Details Tracing unseen gas in the Large Magellanic Cloud Tracing unseen gas in the Large Magellanic Cloud

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545911r&link_type=abstract

American Astronomical Society, AAS Meeting #215, #459.11; Bulletin of the American Astronomical Society, Vol. 42, p.487

Astronomy and Astrophysics

Astronomy

Scientific paper

The interstellar medium comprises a mixture of molecular, atomic, and ionized gas of various temperatures, with each phase traced by independent data such as mm-wave CO lines, radio 21-cm emission and absorption lines, ultraviolet absorption lines, and optical emission lines. Each phase contains dust, so the total amount of interstellar material can be traced by infrared imaging. We compared the Spitzer images of the LMC to the gas tracers, finding evidence for "excess" infrared emission, relative to that traced by HI and CO, in regions with no ionized gas. We test two obvious hypotheses for the origin of the "excess:" cold H2 not traced by CO and cold HI not traced (linearly) by the 21-cm line. Cold H2 should be detected in UV absorption observations with FUSE or in the 28 micron emission line with Spitzer, while cold HI should be detected in 21-cm line absorption toward bright radio sources with ATCA.

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