The active source in the region of the Herbig star
by
1 Osservatorio Astrofisico di Arcetri,
Largo Enrico Fermi 5, I-50125 Firenze, Italy
2 Dipartimento di Astronomia e
Scienza dello Spazio, Universitá di Firenze, Largo E. Fermi, 5, I-50125 Firenze, Italy
3 Department of Physics, Mathematics &Astronomy, Caltech, Pasadena, CA, 91125, USA
4 Astrophysics Division, Space Science Department, ESTEC, Postbus 299, NL-2200 AG Noordwijk, The Netherlands
Abstract:
We present new near-infrared, millimeter and radio observations of the region
associated with 
, a Herbig Be star located in the direction of the
Cygnus arm. 
is the optically brightest member of a small group of young
emission line stars, including V1318 Cygni and V1686 Cygni.
Near-IR broad-band imaging of V1318 Cygni reveals the presence of two
distinct stellar components oriented north-south, a result recently reported
by Aspin et al. (1994). On a larger scale, the near-IR images also indicate
the presence of many highly embedded sources concentrated in the vicinity
of the bright visible stars. In the central part of the cluster, the
near-IR sources outnumber the optically visible ones by a factor of three.
The distribution of the high density molecular gas traced by the
CS J
emission is highly concentrated around
V1318 and V1686 Cygni, while the total column density of gas traced by the
J
shows a ridge morphology centered on these
sources. The Herbig star 
lies at the edge of both structures.
From the otpically thin 
emission, we derive a total molecular mass
of 
. A molecular outflow has been detected in
CO J
. The high velocity gas is confined to a compact region
of size 
, corresponding to a physical length of 0.1 pc.
The outflow is not well resolved, or collimated, on the observed scales.
We have also detected 
maser emission at 22.2 GHz at a position coincident
with the center of the bipolar outflow. Both the maser and the outflow
are located at the position of the southern source V1318S which we
identify as the source responsible for the activity observed in the
BD+40 region.
Mantained by:
Leonardo Testi
lt@arcetri.astro.it