CPL - Chalmers Publication Library
| Utbildning | Forskning | Styrkeområden | Om Chalmers | In English In English Ej inloggad.

H2O line mapping at high spatial and spectral resolution Herschel observations of the VLA 1623 outflow

Per Bjerkeli (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; René Liseau (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; B. Larsson ; Gustaf Rydbeck (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; B. Nisini ; M. Tafalla ; S. Antoniucci ; M. Benedettini ; Per Bergman (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; S. Cabrit ; T. Giannini ; G. Melnick ; D. Neufeld ; G. Santangelo ; E. F. van Dishoeck
Astronomy and Astrophysics (0004-6361). Vol. 546 (2012), p. Article Number: A29 .
[Artikel, refereegranskad vetenskaplig]

Context. Apart from being an important coolant, water is known to be a tracer of high-velocity molecular gas. Recent models predict relatively high abundances behind interstellar shockwaves. The dynamical and physical conditions of the water emitting gas, however, are not fully understood yet. Using the Herschel Space Observatory, it is now possible to observe water emission from supersonic molecular outflows at high spectral and spatial resolution. Several molecular outflows from young stars are currently being observed as part of the WISH (Water In Star-forming regions with Herschel) key program. Aims. We aim to determine the abundance and distribution of water, its kinematics, and the physical conditions of the gas responsible for the water emission. The observed line profile shapes help us understand the dynamics in molecular outflows. Methods. We mapped the VLA1623 outflow, in the ground-state transitions of o-H2O, with the HIFI and PACS instruments. We also present observations of higher energy transitions of o-H2O and p-H2O obtained with HIFI and PACS towards selected outflow positions. From comparison with non-LTE radiative transfer calculations, we estimate the physical parameters of the water emitting regions. Results. The observed water emission line profiles vary over the mapped area. Spectral features and components, tracing gas in different excitation conditions, allow us to constrain the density and temperature of the gas. The water emission originates in a region where temperatures are comparable to that of the warm H-2 gas (T greater than or similar to 200 K). Thus, the water emission traces a gas component significantly warmer than the gas responsible for the low-J CO emission. The water column densities at the CO peak positions are low, i.e. N(H2O) similar or equal to (0.03-10) x 10(14) cm(-2). Conclusions. The water abundance with respect to H-2 in the extended outflow is estimated at X(H2O) < 1 x 10(-6), significantly lower than what would be expected from most recent shock models. The H2O emission traces a gas component moving at relatively high velocity compared to the low-J CO emitting gas. However, other dynamical quantities such as the momentum rate, energy, and mechanical luminosity are estimated to be the same, independent of the molecular tracer used, CO or H2O.

Nyckelord: ISM: individual objects: VLA1623, ISM: molecules, ISM: abundances, ISM: jets and outflows, stars:, rho-ophiuchi cloud, wave-astronomy-satellite, molecular outflows, water, emission, shock-waves, h-2, co, excitation, protostar, cores

Denna post skapades 2012-12-12. Senast ändrad 2015-06-23.
CPL Pubid: 167528


Läs direkt!

Lokal fulltext (fritt tillgänglig)

Länk till annan sajt (kan kräva inloggning)