Water abundance and velocity structure in S140, rho Oph A, and B335
Publication Date
2000
Journal or Book Title
ASTROPHYSICAL JOURNAL
Abstract
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 2 × 10-8 and 4.5 × 10-9 in S140 and ρ Oph A, respectively, and an upper limit of 4 × 10-6 (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.
Pages
L119-L122
Volume
539
Issue
2
Recommended Citation
Ashby, MLN; Bergin, EA; Plume, R; Carpenter, JM; Melnick, GJ; Chin, G; Erickson, NR; Goldsmith, PF; Harwit, M; Howe, JE; Kleiner, SC; Koch, DG; Neufeld, DA; Patten, BM; Schieder, R; Snell, RL; Stauffer, JR; Tolls, V; Wang, Z; Winnewisser, G; and Zhang, YF, "Water abundance and velocity structure in S140, rho Oph A, and B335" (2000). ASTROPHYSICAL JOURNAL. 637.
Retrieved from https://scholarworks.umass.edu/astro_faculty_pubs/637
Comments
The published version is located at http://iopscience.iop.org/1538-4357/539/2/L119?fromSearchPage=true