Modelling the deuterated water emission in the envelope of low-mass protostars. Implications for ground-based and HSO/HIFI observations.

Details Modelling the deuterated water emission in the envelope of low-mass protostars. Implications for ground-based and HSO/HIFI observations. Modelling the deuterated water emission in the envelope of low-mass protostars. Implications for ground-based and HSO/HIFI observations.

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sf2a.conf..409p&link_type=abstract

SF2A-2005: Semaine de l'Astrophysique Francaise, meeting held in Strasbourg, France, June 27 - July 1, 2005, Edited by F. Casoli

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present theoretical predictions of the rotational line emission of deuterated water in low-mass protostar collapsing envelopes, with the aim to determine whether space-based observations are necessary for the study of HDO in these objects. 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. We show that ground-based observations are capable to constrain the three parameters of the model in the case of bright low-mass protostars, and that no space-based observations, like for example HSO observations, are required in this case. On the contrary, the study of low-luminosity sources requires too much integration time to be carried out either with available ground-based telescopes or with the HSO/HIFI. For these sources, only the large interferometer ALMA will allow to constrain the HDO abundance.

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