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Water in low-mass star-forming regions with Herschel: HIFI spectroscopy of NGC1333 | | L.E. Kristensen
; R. Visser
; E.F. van Dishoeck
; U.A. Yıldız
; S.D. Doty
; G.J. Herczeg
; F.-C. Liu
; B. Parise
; J.K. Jørgensen
; T.A. van Kempen
; C. Brinch
; S.F. Wampfler
; S. Bruderer
; A.O. Benz
; M.R. Hogerheijde
; E. Deul
; R. Bachiller
; A. Baudry
; M. Benedettini
; E.A. Bergin
; P. Bjerkeli
; G.A. Blake
; S. Bontemps
; J. Braine
; P. Caselli
; J. Cernicharo
; C. Codella
; F. Daniel
; Th. de Graauw
; A.M. di Giorgio
; C. Dominik
; P. Encrenaz
; M. Fich
; A. Fuente
; T. Giannini
; J.R. Goicoechea
; F. Helmich
; F. Herpin
; T. Jacq
; D. Johnstone
; M.J. Kaufman
; B. Larsson
; D. Lis
; R. Liseau
; M. Marseille
; C. McCoey
; G. Melnick
; D. Neufeld
; B. Nisini
; M. Olberg
; J.C. Pearson
; R. Plume
; C. Risacher
; J. Santiago-Garcia
; P. Saraceno
; R. Shipman
; M. Tafalla
; A.G.G.M. Tielens
; F. van der Tak
; F. Wyrowski
; D. Beintema
; A. de Jonge
; P. Dieleman
; V. Ossenkopf
; P. Roelfsema
; J. Stutzki
; N. Whyborn
; | | Date: |
18 Jul 2010 | | Abstract: | ’Water In Star-forming regions with Herschel’ (WISH) is a key programme
dedicated to studying the role of water and related species during the
star-formation process and constraining the physical and chemical properties of
young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI) on
the Herschel Space Observatory observed three deeply embedded protostars in the
low-mass star-forming region NGC1333 in several H2-16O, H2-18O, and CO
transitions. Line profiles are resolved for five H16O transitions in each
source, revealing them to be surprisingly complex. The line profiles are
decomposed into broad (>20 km/s), medium-broad (~5-10 km/s), and narrow (<5
km/s) components. The H2-18O emission is only detected in broad 1_10-1_01 lines
(>20 km/s), indicating that its physical origin is the same as for the broad
H2-16O component. In one of the sources, IRAS4A, an inverse P Cygni profile is
observed, a clear sign of infall in the envelope. From the line profiles alone,
it is clear that the bulk of emission arises from shocks, both on small (<1000
AU) and large scales along the outflow cavity walls (~10 000 AU). The H2O line
profiles are compared to CO line profiles to constrain the H2O abundance as a
function of velocity within these shocked regions. The H2O/CO abundance ratios
are measured to be in the range of ~0.1-1, corresponding to H2O abundances of
~10-5-10-4 with respect to H2. Approximately 5-10% of the gas is hot enough for
all oxygen to be driven into water in warm post-shock gas, mostly at high
velocities. | | Source: | arXiv, 1007.3031 | | Services: | Forum | Review | PDF | Favorites | |
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