Gas-phase H2O and CO2 toward massive protostars

Details Gas-phase H2O and CO2 toward massive protostars Gas-phase H2O and CO2 toward massive protostars

2001-05-15

arxiv.org/abs/astro-ph/0105249v1

Astron.Astrophys. 399 (2003) 1063-1072

Astronomy and Astrophysics

Astrophysics

Published in the Proceedings of the `ISO beyond the Peaks' Workshop, eds. A. Salama, M.F. Kessler, K. Leech & B. Schulz. ESA-S

Scientific paper

10.1051/0004-6361:20021868

We present a study of gas-phase H2O and CO2 toward a sample of 14 massive protostars with the Short Wavelength Spectrometer (SWS) on board the Infrared Space Observatory (ISO). Modeling of the H2O spectra using a homogeneous model with a constant excitation temperature T_ex shows that the H2O abundances increase with temperature, up to a few times 10^-5 with respect to H2 for the hottest sources (T_ex ~500 K). This is still a factor of 10 lower than the H2O ice abundances observed toward cold sources in which evaporation is not significant (Keane et al. 2001). Gas-phase CO2 is not abundant in our sources. The abundances are nearly constant for T_ex>~100 K at a value of a few times 10^-7, much lower than the solid-state abundances of ~1--3 times 10^-6 (Gerakines et al. 1999). For both H2O and CO2 the gas/solid ratio increases with temperature, but the increase is much stronger for H2O than for CO2, suggesting a different type of chemistry. In addition to the homogeneous models, a power law model has been developed for one of our sources, based on the physical structure of this region as determined from submillimeter data by van der Tak et al. (1999). The resulting H2O model spectrum gives a good fit to the data.

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