Issue |
A&A
Volume 383, Number 2, FebruaryIV 2002
|
|
---|---|---|
Page(s) | 540 - 547 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20011772 | |
Published online | 15 February 2002 |
The outflow activity of the protostars in S140 IRS*
1
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2
Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland
Corresponding author: T. Preibisch, preib@mpifr-bonn.mpg.de
Received:
24
October
2001
Accepted:
30
November
2001
The S140/L1204 cloud contains a deeply embedded
region of star formation and a powerful molecular outflow.
In this paper, we present images of the S140 region
obtained in the light of the 2.12 μm molecular hydrogen emission line and
adjacent continuum.
Our images reveal several knots of H2 line emission
originating from shocked material close to IRS 1 as well as
further out.
Strong H2 shock emission is found
north-east of IRS1 (at position angle of ~20°–30°),
as well as to the south-west of IRS1 (at position angles around
~190°–220°), clearly demonstrating the presence of
outflow activity in the north-east/south-west direction.
We also find patches of H2 emission
several arcminutes away from IRS1 at a position angles of ∼150° and
, i.e. in directions consistent with the previously known
north-west/south-east molecular outflow.
Our results therefore provide evidence for the existence of two distinct
bipolar outflow systems originating simultaneously from IRS 1.
We also discuss
general aspects of the star formation process in the
S140 region. An inferred high ratio of stellar to gas mass
suggests that the outflows have dispersed most of the cloud mass.
Key words: stars: individual: S140 IRS 1 / stars: individual: S140 IRS 3 / stars: formation / stars: winds, outflows
© ESO, 2002
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