2009ApJ...703.1308K


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.24CEST05:31:13

2009ApJ...703.1308K - Astrophys. J., 703, 1308-1317 (2009/October-1)

Rotation of the warm molecular gas surrounding ultracompact H II regions.

KLAASSEN P.D., WILSON C.D., KETO E.R. and ZHANG Q.

Abstract (from CDS):

We present molecular line and 1.4 mm continuum observations toward five massive star-forming regions at arcsecond resolution using the Submillimeter Array. We find that the warm molecular gas surrounding each H II region (as traced by SO2 and OCS) appears to be undergoing bulk rotation. From the molecular line emission and thermal component of the continuum emission, we independently derived gas masses for each region which are consistent with each other. From the free-free component of the continuum emission, we estimate the minimum stellar mass required to power the H II region and find that this mass, when added to the derived gas mass, is a significant fraction of the dynamical mass for that region.

Abstract Copyright:

Journal keyword(s): ISM: kinematics and dynamics - molecular data - stars: formation - submillimeter

Simbad objects: 12

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Number of rows : 12

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 W 31c HII 18 10 29.1 -19 56 05           ~ 310 0
2 GRS G012.89 +00.49 HII 18 11 51.3 -17 31 29           ~ 151 0
3 [FCC2002] A1 Y*O 18 36 12.6 -07 12 11           ~ 30 0
4 GAL 028.20-00.04 HII 18 42 58.2 -04 14 05           ~ 52 0
5 NAME W 51 IRS 1 PoC 19 23 41.9 +14 30 36           ~ 101 0
6 W 51e2 Rad 19 23 43.90 +14 30 34.8           ~ 189 0
7 W 51e8 HII 19 23 44.2 +14 30 28           ~ 34 0
8 W 51 SNR 19 23 50 +14 06.0           ~ 1184 1
9 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 405 0
10 LDN 1251 DNe 22 36.1 +75 16           ~ 100 0
11 NGC 7538 OpC 23 13 37 +61 30.0           ~ 838 0
12 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 380 3

    Equat.    Gal    SGal    Ecl

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2021.06.24-05:31:13

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