Variations in the Dust-to-Gas Ratio in Nearby Dwarf Galaxies

Details Variations in the Dust-to-Gas Ratio in Nearby Dwarf Galaxies Variations in the Dust-to-Gas Ratio in Nearby Dwarf Galaxies

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21442402s&link_type=abstract

American Astronomical Society, AAS Meeting #214, #424.02; Bulletin of the American Astronomical Society, Vol. 41, p.693

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Scientific paper

We present the first part of a systematic study of the relationship between dust and gas in a large set of nearby dwarf irregular galaxies. These systems are rich in gas but poor in dust and heavy elements, a contrast that sets them apart from the Milky Way and other nearby spiral galaxies. The central role of dust in the creation and shielding of star-forming gas and its close link to the enrichment of the ISM make the dust-to-gas (DGR) ratio a key observable to understand star formation in these systems. We are combining maps of dust emission taken by Spitzer as part of the Local Volume Legacy (LVL) with atomic gas observations by the VLA large programs LITTLE THINGS, VLA-ANGST, and THINGS to measure the DGR as a function of position in a large sample of dwarf galaxies. This will populate the low end of the DGR vs. metallicity relation and allow us to measure the enrichment of the extended HI envelopes that surround many dwarf irregulars. By comparing the DGR in regions of active star formation to the DGR in nearby quiescent, we can also place an upper limit on the amount of H2 that can be present near the star forming peaks, a quantity that is otherwise difficult to constrain.

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