Modeling gas-phase H2O between 5 μ m and 540 μ m toward massive protostars

Details Modeling gas-phase H2O between 5 μ m and 540 μ m toward massive protostars Modeling gas-phase H2O between 5 μ m and 540 μ m toward massive protostars

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...406..937b&link_type=abstract

Astronomy and Astrophysics, v.406, p.937-955 (2003)

Astronomy and Astrophysics

Astrophysics

37

Ism: Abundances, Ism: Molecules, Infrared: Ism, Ism: Lines And Bands, Molecular Processes

Scientific paper

We present models and observations of gas-phase H2O lines between 5 and 540 mu m toward deeply embedded massive protostars, involving both pure rotational and ro-vibrational transitions. The data have been obtained for 6 sources with both the Short and Long Wavelength Spectrometers (SWS and LWS) on board the Infrared Space Observatory (ISO) and with the Submillimeter Wave Astronomy Satellite (SWAS). For comparison, CO J=7-6 spectra have been observed with the MPIfR/SRON 800 GHz heterodyne spectrometer at the James Clerk Maxwell Telescope (JCMT). A radiative transfer model in combination with different physical/chemical scenarios has been used to model these H2O lines for 4 sources to probe the chemical structure of these massive protostars. The results indicate that pure gas-phase production of H2O cannot explain the observed spectra. Ice evaporation in the warm inner envelope and freeze-out in the cold outer part are important for most of our sources and occur at T ~ 90-110 K. The ISO-SWS data are particularly sensitive to ice evaporation in the inner part whereas the ISO-LWS data are good diagnostics of freeze-out in the outer region. The modeling suggests that the 557 GHz SWAS line includes contributions from both the cold and the warm H2O gas. The SWAS line profiles indicate that for some of the sources a fraction of up to 50% of the total flux may originate in the outflow. Shocks do not seem to contribute significantly to the observed emission in other H2O lines, however, in contrast with the case for Orion. The results show that three of the observed and modeled H2O lines, the 303-212, 212-101, and 110-101 lines, are good candidates to observe with the Herschel Space Observatory in order to further investigate the physical and chemical conditions in massive star-forming regions.
Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands and UK) and with the participation of ISAS and NASA.

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