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Dense Cloud Cores revealed by ALMA CO observations in the low metallicity dwarf galaxy WLM

Published online by Cambridge University Press:  21 March 2017

M. Rubio
Affiliation:
Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile email: mrubio@das.uchile.cl
B. Elmegreen
Affiliation:
IBM Research Division, T.J. Watson Research Center NY 10598, USA email: bge@us.ibm.com
D. Hunter
Affiliation:
Lowell Observatory Flagstaff, Arizona 86001, USA email: dah@lowell.edu
J. Cortes
Affiliation:
Joint Alma Observatory Alonso de Cordova 3107, Vitacura, Chile email: jcortes@alma.cl
E. Brinks
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire Hatfield AL10 9AB, UK email: e.brinks@herts.ac.uk
P. Cigan
Affiliation:
Cardiff University School of Physics and Astronomy, Cardiff, UK email: pcigan1@gmail.com
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Abstract

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Understanding stellar birth requires observations of the clouds in which they form. These clouds are dense and self-gravitating, and in all existing observations, they are molecular with H2 the dominant species and CO the best available. When the abundances of carbon and oxygen are low compared to hydrogen, and the opacity from dust is also low, as in primeval galaxies and local dwarf irregular galaxies CO forms slowly and is easily destroyed, so it cannot accumulate inside dense clouds. Then we lose our ability to trace the gas in regions of star formation and we lose critical information on the temperatures, densities, and velocities of the material that collapses. I will report on high resolution observations with ALMA of CO clouds in the local group dwarf irregular galaxy WLM, which has a metallicity that is 13% of the solar value and 50% lower than the previous CO detection threshold and the properties derived of very small dense CO clouds mapped..

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

Bolatto, A. D., Wolfire, M., & Leroy, A. K. 2013, ARA&A 51 207268 Google Scholar
Elmegreen, B. G., Rubio, M., Hunter, D. A., Verdugo, C., Brinks, E., & Schruba, A. 2013, Nature 495 487489 Google Scholar
Hunter, D. A., Ficus-Vita, D., Ashley, T. et al. 2012 AJ, 144, 134 CrossRefGoogle Scholar
Rubio, M., Elmegreen, B. G., Hunter, D. A., Brinks, E., Cortes, J., & Cigan, P. 2015, Nature, 525, 218 Google Scholar
Wolfire, M., Hollenbach, D., & McKee, C. F. 2010, ApJ, 716, 1191 CrossRefGoogle Scholar
Taylor, C., Kobulniky, H. A., & Skillman, E. D. 1998, AJ, 116, 2747 CrossRefGoogle Scholar