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A First Look at the Disk Population in the Auriga-California Molecular Cloud

Published online by Cambridge University Press:  06 January 2014

Hannah Broekhoven-Fiene ,
Brenda C. Matthews ,
Paul M. Harvey  and
members of the Spitzer Gould Belt Survey
Hannah Broekhoven-Fiene
Affiliation:
Department of Physics and Astronomy, University of Victoria, PO Box 3055 STN CSC, Victoria, BC, V8W3P6, Canada email: broekhov@uvic.ca
Brenda C. Matthews
Affiliation:
Department of Physics and Astronomy, University of Victoria, PO Box 3055 STN CSC, Victoria, BC, V8W3P6, Canada email: broekhov@uvic.ca National Research Council of Canada, Victoria, BC, V9E 2E7, Canada
Paul M. Harvey
Affiliation:
Astronomy Department, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712-0259, USA
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Abstract

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The Auriga-California Molecular Cloud (AMC) is one of two nearby (within 500 pc) giant molecular clouds, the other being the Orion A Molecular Cloud (OMC). We aim to study the properties of circumstellar disks in the AMC to compare the planet formation potential and processes within the AMC to those for other clouds. A first look with measurements from Spitzer observations suggests that AMC disk properties, such as the distribution of disk luminosities and the evolution of the mid-IR excesses, are not vastly different from those in other regions. Follow-up observations in the submm, mm and cm can be used to measure disk masses and the degree of grain growth from spectral slopes to more completely characterize the disk population.

Keywords

stars: formationplanetary systems: protoplanetary disksISM: clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 151 - 152
Copyright
Copyright © International Astronomical Union 2013 

References

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