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2000ApJ...539L.119A - Astrophys. J., 539, L119-L122 (2000/August-3)

Water abundance and velocity structure in S140, ρ Oph A, and B335.

ASHBY M.L.N., BERGIN E.A., PLUME R., CARPENTER J.M., MELNICK G.J., CHIN G., ERICKSON N.R., GOLDSMITH P.F., HARWIT M., HOWE J.E., KLEINER S.C., KOCH D.G., NEUFELD D.A., PATTEN B.M., SCHIEDER R., SNELL R.L., STAUFFER J.R., TOLLS V., WANG Z., WINNEWISSER G. and ZHANG Y.F.

Abstract (from CDS):

We present Monte Carlo radiative transfer models for B335, S140, and ρ Ophiuchi A that simulate the emission line arising from the 557 GHz 110⟶101 ground-state transition of ortho-H216O. These models reproduce the line profiles with a combination of turbulent and macroscopic motions, and are consistent with gravitational infall in ρ Oph A. We cannot, however, discriminate infall from outflow for S140. Our models are consistent with ortho-H2O abundances relative to H2 of 2x10–8 and 4.5x10–9 in S140 and ρ Oph A, respectively, and an upper limit of 4x10–6 (3 σ) in B335, assuming the ratio ortho-H2/para-H2 = 0.1. We quantify the impact of dust continuum emission on the derived abundances.

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Journal keyword(s): ISM: Abundances - ISM: Clouds - ISM: Molecules - Radio Lines: ISM - Stars: Formation

Simbad objects: 9

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