Cardiff University | Prifysgol Caerdydd ORCA
Online Research @ Cardiff 
WelshClear Cookie - decide language by browser settings

Water in low-mass star-forming regions with Herschel. HIFI spectroscopy of NGC 1333 {Letter]

Kristensen, L. E., Visser, R., van Dishoeck, E. F., Yildiz, U. A., Doty, S. D., Herczeg, G. J., Liu, F. -C., Parise, Berengere, Jorgensen, J. K., van Kempen, T. A., Brinch, C., Wampfler, S. F., Bruderer, S., Benz, A. O., Hogerheijde, M. R., Deul, E., Bachiller, R., Baudry, A., Benedettini, M., Bergin, E. A., Bjerkeli, P., Blake, G. A., Bontemps, S., Braine, J., Caselli, P., Cernicharo, J., Codella, C., Daniel, F., de Graauw, Th., di Giorgio, A. M., Dominik, C., Encrenaz, P., Fich, M., Fuente, A., Giannini, T., Goicoechea, J. R., Helmich, F., Herpin, F., Jacq, T., Johnstone, D., Kaufman, M. J., Larsson, B., Lis, D., Liseau, R., Marseille, M., McCoey, C., Melnick, G., Neufeld, D., Nisini, B., Olberg, M., Pearson, J. C., Plume, R., Risacher, C., Santiago-Garcia, J., Saraceno, P., Shipman, R., Tafalla, M., Tielens, A. G. G. M., van der Tak, F., Wyrowski, F., Beintema, D., de Jonge, A., Dieleman, P., Ossenkopf, V., Roelfsema, P., Stutzki, J. and Whyborn, N. 2010. Water in low-mass star-forming regions with Herschel. HIFI spectroscopy of NGC 1333 {Letter]. Astronomy and Astrophysics 521 , L30. 10.1051/0004-6361/201015100

[thumbnail of Kristensen 2010.pdf]
Preview
PDF - Published Version
Download (259kB) | Preview

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 NGC 1333 in several H216O, H218O, and CO transitions. Line profiles are resolved for five H216O transitions in each source, revealing them to be surprisingly complex. The line profiles are decomposed into broad (>20 km s-1), medium-broad (~5-10 km s-1), and narrow (<5 km s-1) components. The H218O emission is only detected in broad 110–101 lines (>20 km s-1), indicating that its physical origin is the same as for the broad H216O 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.

Item Type: Article
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: astrochemistry ; stars: formation ; ISM: molecules ; ISM: jets and outflows ; ISM: individual objects: NGC 1333
Additional Information: Pdf uploaded in accordance with publisher's policy at http://www.sherpa.ac.uk/romeo/issn/0004-6361/ (accessed 16/04/2014)
Publisher: EDP Sciences
ISSN: 0004-6361
Date of First Compliant Deposit: 30 March 2016
Last Modified: 02 May 2023 18:27
URI: https://orca.cardiff.ac.uk/id/eprint/52789

Citation Data

Cited 68 times in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item Edit Item

Downloads

Downloads per month over past year

View more statistics