Volume 441, Number 1, October I 2005
|Page(s)||171 - 179|
|Section||Interstellar and circumstellar matter|
|Published online||13 September 2005|
Theoretical HDO emission from low-mass protostellar envelopes
CESR CNRS-UPS, BP 4346, 31028 Toulouse Cedex 04, France e-mail: firstname.lastname@example.org
2 Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 09, France
3 Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor MI 48109-1042, USA
Accepted: 28 May 2005
We present theoretical predictions of the rotational line emission of deuterated water in low-mass protostar collapsing envelopes. The model accounts for the density and temperature structure of the envelope, according to the inside-out collapse framework. The deuterated water abundance profile is approximated by a step function, with a low value in the cold outer envelope and a higher value in the inner envelope where the grain mantles evaporate. The two abundances are the two main parameters of the modeling, along with the temperature at which the mantles evaporate. We report line flux predictions for a 30 and 5 source luminosity respectively. We show that ground-based observations are capable of constraining the three parameters of the model in the case of bright low-mass protostars ( ), and that no space-based observations, such as HSO observations, are required in this case. On the contrary, we show that the study of low-luminosity sources (), assuming the same HDO abundance profile, requires too much integration time to be carried out either with available ground-based telescopes or with the HIFI instrument on board HSO. For these sources, only the large interferometer ALMA will allow one to constrain the HDO abundance.
Key words: ISM: abundances / ISM: molecules / stars: formation
© ESO, 2005
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