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Astrophysics Luncheon Seminar

The Formation and Evolution of Dense Gas in Clouds
Presented by Jens Kauffmann
California Institute of Technology

Monday, March 4, 2013
12:00 noon in 169-336

Abstract
In the last few years, we have made great progress with understanding how stars form out of small (<0.1 pc) and dense packages of gas. But we have only a vague understanding how the dense regions in clouds often referred to as clumps and dense cores come about. Understanding the processes leading to the formation of dense gas will be a major goal of star formation research in the next decade. To understand the formation of dense cores and clumps, we must understand the structure of molecular clouds from very large (~10 pc) down to very small (<0.1 pc) spatial scales. I present some first results concerning research in this field. Highlights include an extremely dense Galactic Center cloud: this region concentrates a mass exceeding the one of the Orion A cloud into a radius of only 3 pc but it is essentially devoid of stars. I illustrate the role archival Herschel, Spitzer, and WISE will play for this research in the next few years.


SVCP Astrophysics


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