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Evolution of ISM Contents of Massive Galaxies from z = 2 to 0.3

Published online by Cambridge University Press:  21 March 2013

Nick Scoville
Nick Scoville*
Affiliation:
California Institute of Technology, Pasadena, CA 91125, USA email: nzs@astro.caltech.edu
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Abstract

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The mass of ISM in high redshift Galaxies is a major determinant of their morphology, star formation activity and how they will evolve to low redshift. Measurement of the CO lines at z > 0.5 are time consuming, even with the sensitivity of ALMA, and the derived ISM masses are subject to uncertainty in the CO-to-H2 conversion factor. Here I describe a much faster technique— measuring the long wavelength Rayleigh-Jeans dust emission using the spectacular continuum sensitivity of ALMA. Using a metallicity-dependent gas-to-dust abundance ratio derived from studies of low-z galaxies, one then obtains the ISM mass. Initial results from our ALMA Cycle-0 observations are presented for a small sample of stellar-mass selected galaxies in COSMOS. This technique will enable measurement of 100's of galaxies at high-z with observations of typically ∼10 min per galaxy.

Keywords

ISM: dust — ISM: molecules — ISM: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 279 - 282
Copyright
Copyright © International Astronomical Union 2013

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