Ceccarelli, C.; Caux, E.; Loinard, L.; Castets, A.; Tielens, A. G. G. M.; Molinari, S.; Liseau, R.; Saraceno, P.; Smith, H. and White, G.
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Using the Long Wavelength Specrometer aboard ISO, we have detected far infrared rotational H2O emission lines in five low-mass young stellar objects in a survey of seven such sources. The total H2O fluxes are well correlated with the 1.3 mm continuum fluxes, but - surprisingly - not with the SiO millimeter emission originating in the outflows, suggesting that the water emission arises in the circumstellar envelopes rather than in the outflows. In two of the sources, NGC1333-IRAS4 and IRAS16293-2422, we measured about ten H2O lines, and used their fluxes to put stringent constraints on the physical conditions (temperature, density and column density) of the emitting gas. Simple LVG modelling implies that the emission originates in a very small ( ~ 200 AU), dense (≥ 107) cm-3) and warm ( ~ 100 K) region, with a column density larger than about 1016 cm-2. The detected H2O emission may be well accounted for by thermal emission from a collapsing envelope, and we derive constraints on the accretion rate and central mass of NGC1333-IRAS4. We also discuss an alternative scenario in which the H2O emission arises in an extremely dense shock very close to the central object, perhaps caused by the interaction of the outflow with the inner regions of the circumstellar envelope.
|Item Type:||Journal Article|
|Copyright Holders:||1999 European Southern Observatory (ESO)|
|Keywords:||stellar formation; jets and outflows; infrared; lines and bands; radiative transfer|
|Academic Unit/School:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||23 Feb 2012 16:55|
|Last Modified:||29 Nov 2016 22:01|
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