Hostname: page-component-78c5997874-mlc7c Total loading time: 0 Render date: 2024-11-16T17:30:14.209Z Has data issue: false hasContentIssue false
  • English
  • Français

Hidden and Visible Star Formation: new insights from Herschel

Published online by Cambridge University Press:  05 December 2011

V. Buat ,
E. Giovannoli  and
S. Heinis
V. Buat
Affiliation:
Laboratoire d'Astrophysique de Marseille, Technopole de Chateau Gombert 13388 Marseille cedex 13, FRANCE
E. Giovannoli
Affiliation:
Laboratoire d'Astrophysique de Marseille, Technopole de Chateau Gombert 13388 Marseille cedex 13, FRANCE
S. Heinis
Affiliation:
Laboratoire d'Astrophysique de Marseille, Technopole de Chateau Gombert 13388 Marseille cedex 13, FRANCE
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Herschel opens a large field of investigations on the hidden star formation in galaxies. Combining UV and far-IR rest-frame data allows us to measure all the star formation in galaxies and to estimate the net dust attenuation. The analysis can be performed from the local universe using far-IR and GALEX surveys to high z (up to z < 2) by combining deep U data with the Herschel observations of the HerMES project.

The calibration of dust attenuation, and then star formation rate, is reinvestigated. We present the results of the first analyses performed with Herschel data obtained in the Lockman and COSMOS fields as part of the HerMES project and discuss the reliability of dust attenuation corrections.

Keywords

galaxies: evolution-galaxies: stellar content-infrared: galaxies-ultraviolet: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 5 - 8
Copyright
Copyright © International Astronomical Union 2011

References

Bethermin, M., Dole, H., Beelen, A., & Aussel, H. 2010, A&A, 512, 78Google Scholar
Boissier, S., et al. 2007, ApJS, 173, 524CrossRefGoogle Scholar
Buat, V., et al. 2005, ApJ, 619, L51CrossRefGoogle Scholar
Buat, V., et al. 2007, ApJS, 173, 404CrossRefGoogle Scholar
Buat, V., Marcillac, D., & Burgarella, D. 2007, A&A, 469, 19Google Scholar
Buat, V., et al. 2010, MNRAS, 409, L1CrossRefGoogle Scholar
Calzetti, C. et al. 2000, ApJ 533, 682CrossRefGoogle Scholar
Chary, R., & Elbaz, D. 2001, ApJ, 556, 562CrossRefGoogle Scholar
Gordon, K. D., Clayton, G. C., Witt, A. N., & Misselt, K. A. 2000, ApJ, 533, 236CrossRefGoogle Scholar
Griffin, M. et al. 2010, A&A 518, L3Google Scholar
Meurer, G. R., Heckman, T. M., & Calzetti, D., 1999, ApJ, 521, 64CrossRefGoogle Scholar
Munoz-Mateos, et al. 2009, ApJ 701, 1965CrossRefGoogle Scholar
Noll, S., et al. 2009, A&A, 507, 1793Google Scholar
Pilbratt, et al. 2010, A&A 518, L1Google Scholar
Overzier, , et al. 2010, arXiv1011.6098Google Scholar
Roseboom, I. et al. 2010, MNRAS, 409, 48CrossRefGoogle Scholar