EDP Sciences
Free Access
Volume 413, Number 3, January III 2004
Page(s) 993 - 1007
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20031550
Published online 07 January 2004

A&A 413, 993-1007 (2004)
DOI: 10.1051/0004-6361:20031550

The structure of the NGC 1333-IRAS2 protostellar system on 500 AU scales

An infalling envelope, a circumstellar disk, multiple outflows, and chemistry
J. K. Jørgensen1, M. R. Hogerheijde2, E. F. van Dishoeck1, G. A. Blake3 and F. L. Schöier1, 4

1  Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands
2  Steward Observatory, The University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721-0065, USA
3  Division of Geological and Planetary Sciences, California Institute of Technology, MS 150-21, Pasadena, CA 91125, USA
4  Stockholm Observatory, AlbaNova, 106 91 Stockholm, Sweden

(Received 18 June 2003 / Accepted 1 October 2003 )

This paper investigates small-scale (500 AU) structures of dense gas and dust around the low-mass protostellar binary NGC 1333-IRAS2 using millimeter-wavelength aperture-synthesis observations from the Owens Valley and Berkeley-Illinois-Maryland-Association interferometers. The detected $\lambda=3$ mm continuum emission from cold dust is consistent with models of the envelope around IRAS2A , based on previously reported submillimeter-continuum images, down to the 3´´, or 500 AU, resolution of the interferometer data. Our data constrain the contribution of an unresolved point source to 22 mJy. The importance of different parameters, such as the size of an inner cavity and impact of the interstellar radiation field, is tested. Within the accuracy of the parameters describing the envelope model, the point source flux has an uncertainty by up to 25%. We interpret this point source as a cold disk of mass $\ga$ 0.3  $M_\odot$. The same envelope model also reproduces aperture-synthesis line observations of the optically thin isotopic species C 34S and H 13CO +. The more optically thick main isotope lines show a variety of components in the protostellar environment: N 2H + is closely correlated with dust concentrations as seen at submillimeter wavelengths and is particularly strong toward the starless core IRAS2C . We hypothesize that N 2H + is destroyed through reactions with CO that is released from icy grains near the protostellar sources IRAS2A and B. CS, HCO +, and HCN have complex line shapes apparently affected by both outflow and infall. In addition to the east-west jet seen in SiO and CO originating from IRAS2A, a north-south velocity gradient near this source indicates a second, perpendicular outflow. This suggests the presence of a binary companion within $0{\farcs}3$ (65 AU) from IRAS2A as driving source of this outflow. Alternative explanations of the velocity gradient, such as rotation in a circumstellar envelope or a single, wide-angle ( $90^\circ$) outflow are less likely.

Key words: ISM: individual objects: NGC 1333-IRAS2 -- stars: formation -- ISM: molecules -- ISM: jets and outflows

Offprint request: J. K. Jørgensen, joergensen@strw.leidenuniv.nl

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© ESO 2004

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