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Issue A&A
Volume 416, Number 2, March III 2004
Page(s) 577 - 594
Section Interstellar and circumstellar matter
DOI 10.1051/0004-6361:20034157



A&A 416, 577-594 (2004)
DOI: 10.1051/0004-6361:20034157

The H $\mathsf$CO abundance in the inner warm regions of low mass protostellar envelopes

S. Maret1, C. Ceccarelli2, E. Caux1, A. G. G. M. Tielens3, J. K. Jørgensen4, E. van Dishoeck4, A. Bacmann5, A. Castets6, B. Lefloch2, L. Loinard7, B. Parise1 and F. L. Schöier4

1  Centre d'Étude Spatiale des Rayonnements, CESR/CNRS-UPS, BP 4346, 31028 Toulouse Cedex 04, France
2  Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 09, France
3  Space Research Organization of the Netherlands, PO Box 800, 9700 AV Groningen, The Netherlands
4  Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands
5  European Southern Observatory, Karl-Schwarzschild Str. 2, 85748 Garching bei München, Germany
6  Observatoire de Bordeaux, BP 89, 33270 Floirac, France
7  Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 72-3 (Xangari), 58089 Morelia, Michoacán, Mexico

(Received 4 August 2003 / Accepted 9 October 2003)

Abstract
We present a survey of the formaldehyde emission in a sample of eight Class 0 protostars obtained with the IRAM and JCMT millimeter telescopes. The range of energies of the observed transitions allows us to probe the physical and chemical conditions across the protostellar envelopes. The data have been analyzed with three different methods with increasing level of sophistication. We first analyze the observed emission in the LTE approximation, and derive rotational temperatures between 11 and 40 K, and column densities between 1 and $20 \times 10^$ cm -2. Second, we use a LVG code and derive higher kinetic temperatures, between 30 and 90 K, consistent with subthermally populated levels and densities from 1 to $6 \times 10^5$ cm -3. The column densities from the LVG modeling are within a factor of 10 with respect to those derived in the LTE approximation. Finally, we analyze the observations based upon detailed models for the envelopes surrounding the protostars, using temperature and density profiles previously derived from continuum observations. We approximate the formaldehyde abundance across the envelope with a jump function, the jump occurring when the dust temperature reaches 100 K, the evaporation temperature of the grain mantles. The observed formaldehyde emission is well reproduced only if there is a jump of more than two orders of magnitude, in four sources. In the remaining four sources the data are consistent with a formaldehyde abundance jump, but the evidence is more marginal ( ${\leq} 2 ~ \sigma$ ). The inferred inner H 2CO abundance varies between $1 \times 10^$ and $6 \times 10^$. The absolute values of the jump in the H 2CO abundance are uncertain by about one order of magnitude, because of the uncertainties in the density, ortho to para ratio, temperature and velocity profiles of the inner region, as well as the evaporation temperature of the ices. We discuss the implications of these jumps for our understanding of the origin and evolution of ices in low mass star forming regions. Finally, we give predictions for the submillimeter H 2CO lines, which are particularly sensitive to the abundance jumps.


Key words: ISM: abundances -- ISM: molecules -- stars: formation -- ISM: general

Offprint request: S. Maret, sebastien.maret@obs.ujf-grenoble.fr

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