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Constraining How Star Formation Proceeds: Surveys in the Sub-mm and FIR

Published online by Cambridge University Press:  21 October 2010

Doug Johnstone
Doug Johnstone*
Affiliation:
National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Rd, Victoria, BC, V9E 2E7, Canada email: doug.johstone@nnrc-cnrc.gc.ca Department of Physics & Astronomy, University of Victoria, Victoria, BC, V8P 1A1, Canada
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Abstract

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Coordinated multi-wavelength surveys of molecular clouds are providing strong constraints on the physical conditions within low-mass star-forming regions. In this manner, Perseus and Ophiuchus have been exceptional laboratories for testing the earliest phases of star formation. Highlights of these results are: (1) dense cores form only in high column density regions, (2) dense cores contain only a few percent of the cloud mass, (3) the mass distribution of the dense cores is similar to the IMF, (4) the more massive cores are most likely to contain embedded protostars, and (5) the kinematics of the dense cores and the bulk gas show significant coupling.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 406 - 407
Copyright
Copyright © International Astronomical Union 2010

References

Evans, N. J. II et al. 2003, PASP, 115, 965CrossRefGoogle Scholar
Hatchell, J. & Fuller, G. A. 2009, A&A, 482, 855Google Scholar
Johnstone, D., Di Francesco, J., & Kirk, H. 2004, ApJL, 611, 45CrossRefGoogle Scholar
Jørgensen, J. K., Johnstone, D., Kirk, H., & Myers, P. C. 2007, ApJ, 656, 293CrossRefGoogle Scholar
Jørgensen, J. K., Johnstone, D., Kirk, H., Myers, P. C. et al. 2008, ApJ, 683, 822CrossRefGoogle Scholar
Kirk, H., Johnstone, D., & Di Francesco, J. 2006, ApJ, 646, 1009CrossRefGoogle Scholar
Kirk, H., Johnstone, D., & Tafalla, M. 2007, ApJ, 668, 1042CrossRefGoogle Scholar
Kirk, H., Johnstone, D., & Basu, S. 2009, ApJ, 699, 1433CrossRefGoogle Scholar
Lombardi, M. & Alves, J. 2001, A&A, 377, 1023Google Scholar
Rosolowsky, E. W., Pineda, J. E., Foster, J. B., Borkin, M. A. et al. 2008, ApJS, 175, 509CrossRefGoogle Scholar
Swift, J. & Williams, J. 2008, ApJ, 679, 552CrossRefGoogle Scholar
Ward-Thompson, D., André, P., Crutcher, R. et al. 2007, Protostars and Planets V, 33Google Scholar