Ortho-to-para ratio of interstellar heavy water
Artikel i vetenskaplig tidskrift, 2010
Context. Despite the low elemental deuterium abundance in the Galaxy, enhanced molecular D/H ratios have been found in the environments of low-mass star-forming regions, and in particular the Class 0 protostar IRAS 16293-2422. Aims. The CHESS (Chemical HErschel Surveys of Star forming regions) key program aims to study the molecular complexity of the interstellar medium. The high sensitivity and spectral resolution of the Herschel/HIFI instrument provide a unique opportunity to observe the fundamental 1(1,1)-0(0,0) transition of the ortho-D2O molecule, which is inaccessible from the ground, and determine the ortho-to-para D2O ratio. Methods. We detected the fundamental transition of the ortho-D2O molecule at 607.35 GHz towards IRAS 16293-2422. The line is seen in absorption with a line opacity of 0.62 +/- 0.11 (1 sigma). From the previous ground-based observations of the fundamental 1(1,0)-1(0,1) transition of para-D2O seen in absorption at 316.80 GHz, we estimate a line opacity of 0.26 +/- 0.05 (1 sigma). Results. We show that the observed absorption is caused by the cold gas in the envelope of the protostar. Using these new observations, we estimate for the first time the ortho-to-para D2O ratio to be lower than 2.6 at a 3 sigma level of uncertainty, which should be compared with the thermal equilibrium value of 2:1.
submillimeter: ISM
spectroscopy
ISM: abundances
protostar iras 16293-2422
envelope
constraints
astrochemistry
ISM: molecules
molecular processes
line: identification
Författare
C. Vastel
Universite Paul Sabatier Toulouse III
Institut National des Sciences de l'Univers
C. Ceccarelli
Laboratoire d'Astrophysique de Bordeaux
Institut National des Sciences de l'Univers
Université Grenoble Alpes
E. Caux
Universite Paul Sabatier Toulouse III
Institut National des Sciences de l'Univers
A. Coutens
Institut National des Sciences de l'Univers
Universite Paul Sabatier Toulouse III
J. Cernicharo
Centro de Astrobiologia (CAB)
S. Bottinelli
Universite Paul Sabatier Toulouse III
Institut National des Sciences de l'Univers
K. Demyk
Institut National des Sciences de l'Univers
Universite Paul Sabatier Toulouse III
A. Faure
Université Grenoble Alpes
L. Wiesenfeld
Université Grenoble Alpes
Y. Scribano
U.M.R. 5209 C.N.R.S.
A. Bacmann
Université Grenoble Alpes
Institut National des Sciences de l'Univers
Laboratoire d'Astrophysique de Bordeaux
P. Hily-Blant
Université Grenoble Alpes
S. Maret
Université Grenoble Alpes
A. Walters
Institut National des Sciences de l'Univers
Universite Paul Sabatier Toulouse III
E. A. Bergin
University of Michigan
G. A. Blake
California Institute of Technology (Caltech)
A. Castets
Laboratoire d'Astrophysique de Bordeaux
Institut National des Sciences de l'Univers
Université Grenoble Alpes
N. Crimier
Université Grenoble Alpes
Centro de Astrobiologia (CAB)
C. Dominik
Anton Pannekoek Institute for Astronomy
Radboud Universiteit
P. Encrenaz
Ecole Normale Superieure (ENS)
M. Gerin
Ecole Normale Superieure (ENS)
P. Hennebelle
Ecole Normale Superieure (ENS)
C. Kahane
Université Grenoble Alpes
A. Klotz
Institut National des Sciences de l'Univers
Universite Paul Sabatier Toulouse III
G. J. Melnick
Harvard-Smithsonian Center for Astrophysics
L. Pagani
Ecole Normale Superieure (ENS)
B. Parise
Max-Planck-Gesellschaft
P. Schilke
Universität zu Köln
Max-Planck-Gesellschaft
V. Wakelam
Institut National des Sciences de l'Univers
Laboratoire d'Astrophysique de Bordeaux
A. Baudry
Laboratoire d'Astrophysique de Bordeaux
Institut National des Sciences de l'Univers
T. A. Bell
California Institute of Technology (Caltech)
M. Benedettini
Istituto di Fisica dello Spazio Interplanetario, Rome
A. Boogert
California Institute of Technology (Caltech)
S. Cabrit
Ecole Normale Superieure (ENS)
P. Caselli
University of Leeds
C. Codella
Osservatorio Astrofisico di Arcetri
C. Comito
Max-Planck-Gesellschaft
E. Falgarone
Ecole Normale Superieure (ENS)
A. Fuente
Observatorio Astronómico Nacional (OAN)
P. F. Goldsmith
Jet Propulsion Laboratory, California Institute of Technology
F. Helmich
Netherlands Institute for Space Research (SRON)
T. Henning
Max-Planck-Gesellschaft
E. Herbst
Ohio State University
T. Jacq
Institut National des Sciences de l'Univers
Laboratoire d'Astrophysique de Bordeaux
M. Kama
Anton Pannekoek Institute for Astronomy
W. D. Langer
Jet Propulsion Laboratory, California Institute of Technology
B. Lefloch
Université Grenoble Alpes
D. Lis
California Institute of Technology (Caltech)
S. Lord
California Institute of Technology (Caltech)
A. Lorenzani
Osservatorio Astrofisico di Arcetri
D. A. Neufeld
Johns Hopkins University
B. Nisini
Osservatorio Astronomico di Roma
S. Pacheco
Université Grenoble Alpes
J. C. Pearson
Jet Propulsion Laboratory, California Institute of Technology
T. Phillips
California Institute of Technology (Caltech)
M. Salez
Ecole Normale Superieure (ENS)
P. Saraceno
Istituto di Fisica dello Spazio Interplanetario, Rome
K. Schuster
Institut de Radioastronomie Millimétrique (IRAM)
X. Tielens
Universiteit Leiden
F. F. S. van der Tak
Rijksuniversiteit Groningen
Netherlands Institute for Space Research (SRON)
M. H. D. van der Wiel
Netherlands Institute for Space Research (SRON)
Rijksuniversiteit Groningen
S. Viti
University College London (UCL)
F. Wyrowski
Max-Planck-Gesellschaft
H. W. Yorke
Jet Propulsion Laboratory, California Institute of Technology
P. Cais
Institut National des Sciences de l'Univers
Laboratoire d'Astrophysique de Bordeaux
J. M. Krieg
Ecole Normale Superieure (ENS)
Michael Olberg
Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium
L. Ravera
Institut National des Sciences de l'Univers
Universite Paul Sabatier Toulouse III
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 521 1 Article Number: L31 - L31Ämneskategorier (SSIF 2011)
Astronomi, astrofysik och kosmologi
Fundament
Grundläggande vetenskaper
DOI
10.1051/0004-6361/201015101