Issue |
A&A
Volume 389, Number 2, July II 2002
|
|
---|---|---|
Page(s) | 572 - 576 | |
Section | The Sun | |
DOI | https://doi.org/10.1051/0004-6361:20020619 | |
Published online | 27 June 2002 |
VLA observations of water maser emission associated with SVS 13 and other sources in NGC 1333
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
Corresponding author: L. F. Rodríguez, luisfr@astrosmo.unam.mx
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 03 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 H2O maser spots toward this
source, also known as H2O(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 vLSR similar to
that of the ambient cloud
(
km s-1),
for which we detected five
features (with vLSR in the range of 6.5 to 12.2 km s-1)
and a blueshifted velocity group (six features with vLSR 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 H2O
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
© ESO, 2002
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