EDP Sciences
Free Access
Volume 389, Number 1, July I 2002
Page(s) L6 - L10
Section Letters
DOI https://doi.org/10.1051/0004-6361:20020652
Published online 14 June 2002

A&A 389, L6-L10 (2002)
DOI: 10.1051/0004-6361:20020652


The degree of CO depletion in pre-stellar cores

A. Bacmann1, B. Lefloch2, C. Ceccarelli3, 2, A. Castets3, J. Steinacker1 and L. Loinard4

1  Astrophysikalisches Institut und Universitäts Sternwarte (AIU), Schillergäßchen 2-3, 07745 Jena, Germany
    e-mail: stein@astro.uni-jena.de
2  Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
    e-mail: lefloch@obs.ujf-grenoble.fr
3  Observatoire de Bordeaux, 2 rue de l'Observatoire, BP 89, 33270 Floirac, France
    e-mail: ceccarel@observ.u-bordeaux.fr,castets@observ.u-bordeaux.fr
4  Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico
    e-mail: l.loinard@astrosmo.unam.mx

(Received 5 March 2002 / Accepted 24 April 2002 )

We present new results on CO depletion in a sample of nearby pre-stellar cores, based on observations of the millimeter C 17O and C 18O lines and the 1.3 mm dust emission with the IRAM 30 m telescope. In most cases, the distribution of CO is much flatter than that of the dust, whereas other tracers, like $\rm N_2H^{+}$, still probe the latter. In the centre of these objects, we estimate CO to be underabundant by a factor 4-15 depending on the cores. The CO underabundance is more pronounced in the central regions and appears to decrease with increasing distance from the core centre. This underabundance is most likely due to the freezing out of CO onto the dust grains in the cold, dense parts of the cores. We find evidence for an increase of the CO depletion degree with the core density.

Key words: ISM: molecules -- dust, extinction -- stars: formation

Offprint request: A. Bacmann, bacmann@astro.uni-jena.de

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© ESO 2002

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