2011A&A...526A..59D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:37:11

2011A&A...526A..59D - Astronomy and Astrophysics, volume 526A, 59-59 (2011/2-1)

A study of three southern high-mass star-forming regions.

DEDES C., LEURINI S., WYROWSKI F., SCHILKE P., MENTEN K.M., THORWIRTH S. and OTT J.

Abstract (from CDS):

Based on color-selected IRAS point sources, we have started to conduct a survey of 47 high-mass star-forming regions in the southern hemisphere in 870µm dust continuum and molecular line emission in several frequency ranges between 290 GHz and 806 GHz. This paper describes the pilot study of the three sources IRAS 12326-6245, IRAS 16060-5146, and IRAS 16065-5158. To characterize the physical and chemical properties of southern massive star-forming regions, three high-luminosity southern hemisphere hot cores are observed in continuum and molecular line emission. Based on the results obtained in the three sources, which served as templates for the survey, the most promising (and feasible) frequency setups for the remaining 44 sources were decided upon. The sources were observed with the Atacama Pathfinder EXperiment (APEX) in five frequency setups aimed at groups of lines from the following molecules: CH3OH, H2CO, and CH3CN. Using the LTE approximation, temperatures, source sizes, and column densities were determined through modeling of synthetic spectra with the XCLASS program. Dust continuum observations were done with the Large APEX BOlometer CAmera (LABOCA) at 870µm and the 3mm continuum was imaged with the Australia Telescope Compact Array (ATCA). Based on the detection of high-excitation CH3CN lines and lines from complex organic species, the three sources are classified as line rich, hot core type sources. For all three, the modeling indicates that the line emission emerges from a combination of an extended, cooler envelope, and a hot compact component. All three sources show an overabundance of oxygen-bearing species compared to nitrogen-bearing species. While the chemistry in the three sources indicates that they are already in an evolved stage, the non-detection of infrared heating sources at the dust continuum peak of IRAS 16065-5158 points to this source still being deeply embedded. Because this work served as a pilot study, the approach to observe the remaining 44 massive star-forming regions was chosen based on its results. The three sources are massive, luminous hot cores. While IRAS 16065-5158 seems to be a very young deeply embedded object, IRAS 12326-6245 and IRAS 16060-5146 seem more evolved and have already developed UCHII regions.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: lines and bands - submillimeter: general

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 941 2
2 W 3(H2O) Mas 02 27 04.6 +61 52 25           ~ 123 0
3 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
4 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2198 0
5 QSO B1145-676 QSO 11 47 33.4004260218 -67 53 41.777073042   19.66   16.6   ~ 45 1
6 IRAS 12326-6245 mul 12 35 34.1 -63 02 28           ~ 28 0
7 GAL 301.12-00.20 HII 12 35 35.9 -63 02 29           ~ 28 0
8 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2702 2
9 IRAS 13134-6242 mul 13 16 42.9 -62 58 45           ~ 28 0
10 [WBH98] 13134-6242 HII 13 16 46.3 -62 58 35           ~ 23 0
11 GAL 327.30-00.60 HII 15 53 05.0 -54 35 24           ~ 122 0
12 IRAS 16060-5146 HII 16 09 52.776 -51 54 52.20           ~ 22 0
13 IRAS 16065-5158 HII 16 10 23.112 -52 06 06.48           ~ 24 1
14 3FGL J1617.4-5846 AGN 16 17 17.8913859288 -58 48 07.860059063   18.23       ~ 89 1
15 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1035 1
16 NAME NGC 6334-I Cl* 17 20 53.35 -35 47 01.5           ~ 269 0
17 IRAS 17233-3606 HII 17 26 42.8 -36 09 17           ~ 67 0
18 GAL 009.62+00.19 HII 18 06 13.9 -20 31 44           ~ 186 0
19 [GRM93] G09.61+0.20 E HII 18 06 14.7 -20 31 32           ~ 41 0
20 [GRM93] G09.61+0.20 F Rad 18 06 14.89 -20 31 38.9           ~ 26 1
21 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 460 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:37:11

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