Water in star-forming regions with Herschel (WISH) IV. A survey of low-J H2O line profiles toward high-mass protostars
Artikel i vetenskaplig tidskrift, 2013

Context. Water is a key constituent of star-forming matter, but the origin of its line emission and absorption during high-mass star formation is not well understood. Aims. We study the velocity profiles of low-excitation H2O lines toward 19 high-mass star-forming regions and search for trends with luminosity, mass, and evolutionary stage. Methods. We decompose high-resolution Herschel-HIFI line spectra near 990, 1110 and 1670 GHz into three distinct physical components. Dense cores (protostellar envelopes) are usually seen as narrow absorptions in the H2O 1113 and 1669 GHz ground-state lines, the H2O 987 GHz excited-state line, and the (H2O)-O-18 1102 GHz ground-state line. In a few sources, the envelopes appear in emission in some or all studied lines, indicating higher temperatures or densities. Broader features due to outflows are usually seen in absorption in the H2O 1113 and 1669 GHz lines, in 987 GHz emission, and not seen in (H2O)-O-18, indicating a lower column density and a higher excitation temperature than the envelope component. A few outflows are detected in (H2O)-O-18, indicating higher column densities of shocked gas. In addition, the H2O 1113 and 1669 GHz spectra show narrow absorptions by foreground clouds along the line of sight. The lack of corresponding features in the 987 GHz and (H2O)-O-18 lines indicates a low column density and a low excitation temperature for these clouds, although their derived H2O ortho/para ratios are close to 3. Results. The intensity of the ground state lines of H2O at 1113 and 1669 GHz does not show significant trends with source luminosity, envelope mass, or evolutionary state. In contrast, the flux in the excited-state 987 GHz line appears correlated with luminosity and the (H2O)-O-18 line flux appears correlated with the envelope mass. Furthermore, appearance of the envelope in absorption in the 987 GHz and (H2O)-O-18 lines seems to be a sign of an early evolutionary stage, as probed by the mid-infrared brightness and the L-bol/M-env ratio of the source. Conclusions. The ground state transitions of H2O trace the outer parts of the envelopes, so that the effects of star formation are mostly noticeable in the outflow wings. These lines are heavily affected by absorption, so that line ratios of H2O involving the ground states must be treated with caution, especially if multiple clouds are superposed as in the extragalactic case. The isotopic (H2O)-O-18 line appears to trace the mass of the protostellar envelope, indicating that the average H2O abundance in high-mass protostellar envelopes does not change much with time. The excited state line at 987 GHz increases in flux with luminosity and appears to be a good tracer of the mean weighted dust temperature of the source, which may explain why it is readily seen in distant galaxies.

astrochemistry

stars: formation

ISM: molecules

Författare

F. F. S. van der Tak

Rijksuniversiteit Groningen

Netherlands Institute for Space Research (SRON)

L. Chavarría

Laboratoire d'Astrophysique de Bordeaux

CSIC-INTA - Centro de Astrobiologia (CAB)

F. Herpin

Laboratoire d'Astrophysique de Bordeaux

F. Wyrowski

Max Planck-institutet

C. M. Walmsley

Osservatorio Astrofisico di Arcetri

Dublin Institute for Advanced Studies

E. F. van Dishoeck

Universiteit Leiden

Max Planck-institutet

A. O. Benz

Eidgenössische Technische Hochschule Zürich (ETH)

E. A. Bergin

University of Michigan

P. Caselli

University of Leeds

M. R. Hogerheijde

Universiteit Leiden

D. Johnstone

Joint Astronomy Centre

L. Kristensen

Harvard-Smithsonian Center for Astrophysics

Universiteit Leiden

René Liseau

Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik

B. Nisini

Osservatorio Astronomico di Roma

M. Tafalla

Observatorio Astronomico Nacional

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 554 A83

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.1051/0004-6361/201220976