EDP Sciences
Free Access
Volume 389, Number 2, July II 2002
Page(s) 572 - 576
Section Diffuse matter in space
DOI https://doi.org/10.1051/0004-6361:20020619
Published online 27 June 2002

A&A 389, 572-576 (2002)
DOI: 10.1051/0004-6361:20020619

VLA observations of water maser emission associated with SVS 13 and other sources in NGC 1333

L. F. Rodríguez1, G. Anglada2, 3, J. M. Torrelles4, J. E. Mendoza-Torres5, A. D. Haschick6 and P. T. P. Ho3

1  Instituto de Astronomía, UNAM, Campus Morelia, Apdo. Postal 3-72, Morelia, Michoacán 58089, México
2  Instituto de Astrofísica de Andalucía, CSIC, Camino Bajo de Huétor 24, 18008 Granada, Spain
    e-mail: guillem@iaa.es
3  Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
    e-mail: ganglada,ho@cfa.harvard.edu
4  Institut d'Estudis Espacials de Catalunya (IEEC/CSIC) and Instituto de Ciencias del Espacio (CSIC), Edifici Nexus, c/ Gran Capità 2-4, 08034 Barcelona, Spain
    e-mail: torrelles@ieec.fcr.es
5  Instituto Nacional de Astrofísica, Optica y Electrónica, Luis Enrique Erro No. 1, Apdo. Postal 51 y 216, 72840 Tonantzintla, Puebla, México
    e-mail: mend@inaoep.mx
6  MIT Haystack Observatory, Westford, MA 01886, USA

(Received 24 October 2001 / Accepted 16 April 2002)

The young stellar object SVS 13 is believed to power the chain formed by the HH 7-11 objects. Recent observations have revealed that in the radio continuum (3.6-cm) the source is a binary with components separated by about 0 $\rlap.{''}$3 in the east-west direction. The members of the binary are named VLA 4A (western component) and VLA 4B (eastern component). In an attempt to ascertain which of the two components of the binary is the most likely candidate to drive the outflow, we obtained accurate positions for the H 2O maser spots toward this source, also known as H 2O(A), derived from Very Large Array observations in its highest angular resolution A configuration. We detected a total of eleven spots over four observational sessions (made in the years 1983, 1985, 1988, and 1989). The spots are segregated in two velocity groups: a velocity group with $v_{\rm LSR}$ similar to that of the ambient cloud ( $v_{\rm LSR} \simeq 8$ km s -1), for which we detected five features (with $v_{\rm LSR}$ in the range of 6.5 to 12.2 km s -1) and a blueshifted velocity group (six features with $v_{\rm LSR}$ in the range of -25.4 to -5.6 km s -1). Remarkably, all the spots in the first velocity group are associated with VLA 4A, while all the spots in the blueshifted velocity group are associated with VLA 4B. We discuss the possible implications of this observation. We also present accurate positions of the H 2O maser HH 7(B) and of the masers associated with IRAS4B (VLA 28) and IRAS7 (VLA 27, the exciting source of HH 6).

Key words: ISM: Herbig-Haro objects -- ISM: jets and outflows -- masers -- stars: pre-main sequence

Offprint request: L. F. Rodríguez, luisfr@astrosmo.unam.mx

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© ESO 2002

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