2002A&A...384..225S


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.16CEST00:52:41

2002A&A...384..225S - Astronomy and Astrophysics, volume 384, 225-241 (2002/3-2)

A multiwavelength study of the S106 region. I. Structure and dynamics of the molecular gas.

SCHNEIDER N., SIMON R., KRAMER C., STUTZKI J. and BONTEMPS S.

Abstract (from CDS):

The molecular cloud associated with Sharpless 106 has been studied in a variety of (sub)millimeter CO rotational lines on angular resolution scales from 11'' to 80''. We used the KOSMA 3 m telescope to obtain an extended 12CO J=3-2 map, from which we calculate a total mass of 2000 M and an average density of 1.4x103cm–3 for the molecular cloud. The peak intensity region around the massive young star S106 IR was observed in 13CO J=6-5 and 3-2 with KOSMA and in isotopomeric low-J CO lines with the IRAM 30 m telescope. A clump decomposition made for several lines yields a common clump-mass spectral index of α=1.7, illustrating the self-similarity of the detected structures for length-scales from 0.06 to 0.9 parsec. All 12CO and 13CO line profiles within approximately 2' around S106 IR show blue wing emission and less prominent red wing emission, partly affected by self-absorption in colder foreground material. We attribute this high-velocity emission to the ionized wind of S106 IR driving a shock into the inhomogeneous molecular cloud. We do not find evidence for a smooth or fragmented disk around S106 IR and/or an expanding ring in the observed CO emission distribution. The excitation conditions along a cut through the molecular cloud/HII region are studied with an LTE analysis (and an Escape Probability model at the position of S106 IR), using the observed CO line intensities and ratios. The kinetic gas temperature is typically 40K, the average density of the cloud in the core region is 9x103cm–3, and the local density within the clumps is 9x104cm–3. The 13CO/C18O line and column density ratios away from S106 IR reflect the natural isotopic abundance but towards the optical lobes and the cavity walls, we see enhanced 13CO emission and abundance with respect to C18O. This shows that selective photo-dissociation is only important close to S106 IR and in a thin layer of the cavity walls. In combination with the results from the excitation analysis we conclude that the molecular line emission arises from two different gas phases: (i) rather homogeneous, low- to medium-density, spatially extended clumps and (ii) embedded, small (≪0.2pc), high-density clumps with a low volume filling factor.

Abstract Copyright:

Journal keyword(s): ISM: clouds - ISM: individual objects: S106 - ISM: molecules - ISM: kinematics and dynamics - ISM: jets and outflows - radio lines: ISM

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME SH 2-106 IR Cluster OpC 20 27 23 +37 22.8           ~ 10 1
2 MSX5C G076.3116-00.6582 MIR 20 27 23.3 +37 18 01           ~ 1 0
3 MSX5C G076.3045-00.6721 MIR 20 27 25.4 +37 17 11           ~ 1 0
4 NAME SH 2-106 FIR IR 20 27 25.4 +37 22 48           ~ 48 0
5 NAME SH 2-106 IR Y*O 20 27 26.502 +37 22 42.03           ~ 157 1
6 SH 2-106 HII 20 27 26.8 +37 22 49           ~ 416 2

    Equat.    Gal    SGal    Ecl

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