Expected Water line spectrum of the protostar OMC2-FIR4

Details Expected Water line spectrum of the protostar OMC2-FIR4 Expected Water line spectrum of the protostar OMC2-FIR4

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sf2a.conf..238c&link_type=abstract

SF2A-2007: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics held in Grenoble, France, July

Astronomy and Astrophysics

Astrophysics

Scientific paper

We present the expected water line spectrum of the protostar OMC2-FIR4. Dust continuum maps obtained at 350, 450 and 850 μm have been used to constrain the density and dust temperature profiles of the FIR4 envelope. We then compute the gas temperature accordingly by solving the gas thermal balance at each radius. Since previous studies (Jørgensen et al. 2005) have suggested the presence of a strong external illuminating FUV field, we considered this possibility in addition to the standard IS FUV illumination case. Specifically, we computed the water line spectrum for both G0=1 and G0=1000 case and for different water abundances. We show that the two spectra are very different and their observation will therefore allow us to constrain water abundance in the protostar envelope and discriminate between the two possibilities, G0=1 and G0=1000.

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