Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..apr.h3005t&link_type=abstract
American Physical Society, April Meeting, 2003, April 5-8, 2003 Philadelphia, Pennsylvania, MEETING ID: APR03, abstract #H3.005
Other
Scientific paper
From studies of the Milky Way, we know that molecular gas is intrinsically tied to the process of forming stars. However, to appreciate fully the role that star formation plays in galaxy evolution, we want to assess the connection between star formation and larger-scale structure in galaxies. This is more straightforward in external galaxies, where we are free of the inherent difficulties of observing from within the structure we are studying. In addition, studies of molecular gas in external galaxies provide a means to examine the variations in galaxy structure and evolution, just as searches for bodies orbiting other stars provide additional perspectives on the formation and motions of planets. Molecular gas not only provides the raw material for star formation, but also responds more significantly than stars do to influences of large-scale dynamical structures such as bars and spiral arms. Thus, spectroscopic measures of molecular emission provide a means to trace large- and small-scale motions in addition to the distribution of gaseous material in galaxies. The challenges facing studies of molecular gas in nearby galaxies include achieving high resolution (while retaining sensitivity to larger-scale information) and assessing the accuracy of various tracers in mapping out the more abundant, but more elusive, molecular hydrogen. In this presentation, I will show recent results mapping out molecular gas in galaxies, chiefly through CO emission and dust extinction, and discuss their connection to star formation and galaxy evolution. In addition, I will outline prospects for future studies of molecular gas and star formation in nearby galaxies.
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