EDP Sciences
Free Access
Volume 385, Number 2, April II 2002
Page(s) 454 - 463
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361:20020156
Published online 15 April 2002

A&A 385, 454-463 (2002)
DOI: 10.1051/0004-6361:20020156

[CII] at 158 $\mu$m as a star formation tracer in late-type galaxies

A. Boselli1, G. Gavazzi2, J. Lequeux3 and D. Pierini4

1  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: pierini@ancona.astro.utoledo.edu

(Received 3 December 2001 / 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 H $\alpha$+[NII] line. The relation holds for far-IR luminosities $10^8 \leq L_{\rm FIR} \le 10^{10.5}~L _\odot$. 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

Offprint request: A. Boselli, Alessandro.Boselli@astrsp-mrs.fr

SIMBAD Objects in preparation

© ESO 2002

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