Volume 385, Number 2, April II 2002
|Page(s)||454 - 463|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 April 2002|
[CII] at 158 μm as a star formation tracer in late-type galaxies
Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, France
2 Università degli Studi di Milano-Bicocca, Dipartimento di Fisica, Piazza dell'Ateneo Nuovo 1, 20126 Milano, Italy e-mail: Giuseppe.Gavazzi@mib.infn.it
3 DEMIRM and URA 336 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France e-mail: James.Lequeux@obspm.fr
4 Ritter Astrophysical Research Center, The University of Toledo, 2801 West Bancroft, Toledo, OH 43606, USA e-mail: email@example.com
Corresponding author: A. Boselli, Alessandro.Boselli@astrsp-mrs.fr
Accepted: 24 January 2002
We present a calibration of the massive star formation rate vs. [CII] luminosity relation based on a sample of nearby, late-type galaxies observed with ISO-LWS and imaged in the Hα+[NII] line. The relation holds for far-IR luminosities . The derived star formation rates have an uncertainty of about a factor of 10. Part of this uncertainty is due to the different mix of contributions to the [CII] emission from the different components of the interstellar medium in individual galaxies, as discussed in an appendix.
Key words: galaxies: general / galaxies: spiral / ISM: general / star: formation / radio lines: galaxies
© ESO, 2002
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