A multi-wavelength study of the Sharpless 151 region
J. Brand 1 and
J.G.A. Wouterloot 2, 3
Received 17 March 1998 / Accepted 27 May 1998
Results are presented of an extensive, multi-wavelength study of the area around the evolved HII region Sh 2-151. We discuss the excitation of the HII region, and analyze its interaction with molecular clouds in the vicinity, the clouds themselves, and their embedded objects.
We present KOSMA 3-m 12CO(2-1) and (3-2) observations of a region around Sh 2-151. These observations reveal five clouds, with a total mass of 2.9104 . A small ( ) region to the SW of Sh 2-151 was mapped in several CO and CS transitions with the IRAM 30-m telescope. The latter region contains 1.8 of molecular mass, and hosts an IRAS- and H2O maser source (WB89-234). Tracers of higher (column-) densities, such as C18O and CS, show the existence of two clumps ( ) connected by a ridge of warm ( K) narrow-line ( ) gas. The southern clump contains the IRAS/maser source, exhibits a molecular outflow (M5 , yr), and is therefore probably a region of active star formation. In the northern clump the line profiles have an intermediate width (1-3 ; partly due to the presence of two emission components) and are non-gaussian (shoulders, wings) at several positions. IRAS (HIRES) observations show there is also FIR emission associated with the northern clump.
NIR (J, H, K, H2) observations show the presence of several red star-like objects and diffuse emission in both clumps; some of the diffuse emission is stronger and more extended in K and H2, and may be due to dust emission around embedded objects.
HIRES data reveal that IRAS23004+5642 (WB89-234) nearly coincides with the H2O maser and the outflow, and not with the strong, narrow-line CO-emitting gas detected towards the point source catalog position. The linewidth of this relatively low-density warm gas, the heating source of which is as yet unknown, indicates the absence of dynamical interaction with both Sh 2-151 and the embedded IR sources.
From the HIRES 60µm and 100µm data we derive dust temperatures of 30-40 K, the highest values occurring near the maser, and a dust mass of 30 ; assuming a gas-to-dust ratio of 100, this implies we detect 10% of the dust. Evidence from the available (literature) data leads to the conclusion that the exciting star(s) of Sh 2-151 has (have) not yet been identified. We suspect that one or more early type (B0) stars may be hidden behind the molecular cloud associated with WB89-234. The ionized gas mass of Sh 2-151 is 700 .
Star formation in the Sh 2-151 area may occur in the whole region of strong FIR emission (as seen in the HIRES maps: 0.5 degrees, or 50 pc, in length); north of Sh 2-151, activity is seen near the edge of a large (20 pc diameter) molecular cloud.
Key words: ISM: clouds ISM: molecules radio lines: ISM ISM: individual objects: Sh 2-151
Send offprint requests to: J. Brand, (firstname.lastname@example.org)
© European Southern Observatory (ESO) 1998
Online publication: August 17, 1998