2010A&A...520A.102M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.21CET07:36:39

2010A&A...520A.102M - Astronomy and Astrophysics, volume 520, A102-102 (2010/9-2)

LABOCA mapping of the infrared dark cloud MSXDC G304.74+01.32.

MIETTINEN O. and HARJU J.

Abstract (from CDS):

Infrared dark clouds (IRDCs) likely represent very early stages of high-mass star/star cluster formation. The aim is to determine the physical properties and spatial distribution of dense clumps in the IRDC MSXDC G304.74+01.32 (G304.74), and bring these characteristics into relation to theories concerning the origin of IRDCs and their fragmentation into clumps and star-forming cores. G304.74 was mapped in the 870µm dust continuum with the LABOCA bolometer on APEX. The 870 µm map was compared with the 1.2mm continuum map of the cloud by Beltran et al. (2006A&A...447..221B). Archival MSX and IRAS infrared data were used to study the nature and properties of the submillimetre clumps within the cloud. The H2 column densities were estimated using both the 870µm dust emission and the MSX 8µm extinction data. The obtained values were compared with near-infrared extinction which could be estimated along a few lines of sight. We compared the clump masses and their spatial distribution in G304.74 with those in several other recently studied IRDCs. Twelve clumps were identified from the 870µm dust continuum map. Three of them are associated with the MSX and IRAS point sources. Moreover, one of the clumps (SMM 6) is associated with two MSX 8µm point-like sources. Thus, there are 8 clumps within G304.74 which are not associated with mid-infrared (MIR) emission. The H2 column densities derived from the dust continuum and extinction data are similar. The comparison suggests that the dust temperature may be elevated (20-30K) near the southern end of the cloud, whereas the starless clumps in the centre and in the north are cool (Td∼15K). There is a high likelihood that the clump mass distributions in G304.74 and in several other IRDCs represent the samples of the same parent distribution. In most cases the spatial distributions of clumps in IRDCs do not deviate significantly from random distributions. G304.74 contains several massive clumps that are not associated with MIR emission. On statistical grounds it is likely that some of them are or harbour high-mass starless cores (HMSCs). The fact that the clump mass distributions (resembling the high-mass stellar IMF), and in some cases also the random-like spatial distributions, seem to be comparable between different IRDCs, is consistent with the idea that the origin of IRDCs, and their further sub-fragmentation down to scales of clumps is caused by supersonic turbulence in accordance with results from giant molecular clouds.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: clouds - ISM: structure - radio continuum: ISM - submillimeter: ISM

Nomenclature: Fig. 1, Table 1: [MH2010] SMMN (Nos SMM1-SMM9).

Simbad objects: 54

goto Full paper

goto View the reference in ADS

Number of rows : 54

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 NGC 891 H2G 02 22 32.907 +42 20 53.95 11.08 10.81 9.93 7.86   ~ 1546 2
2 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2173 0
3 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2245 0
4 [MH2010] SMM1 MoC 13 06 20.5 -61 30 15           ~ 4 0
5 [MH2010] SMM2 MoC 13 06 26.9 -61 29 39           ~ 4 0
6 [BBC2006] IRAS 13039-6108 Clump 1 cor 13 06 35.8 -61 28 53           ~ 4 0
7 MSXDC G304.74+1.32 DNe 13 06.6 -61 30           ~ 8 0
8 2MASS J13064180-6128529 IR 13 06 41.7979287988 -61 28 52.944234464           ~ 1 0
9 2MASS J13064266-6128213 IR 13 06 42.667 -61 28 21.30           ~ 1 0
10 [BBC2006] IRAS 13039-6108 Clump 3 cor 13 06 44.7 -61 28 35           ~ 4 0
11 [MH2010] SMM5 MoC 13 06 49.9 -61 26 55           ~ 4 0
12 IRAS 13037-6112 HII 13 06 51.0 -61 28 22           ~ 6 0
13 [BBC2006] IRAS 13039-6108 Clump 4 cor 13 06 51.1 -61 27 49           ~ 4 0
14 [BBC2006] IRAS 13039-6108 Clump 8 cor 13 07 02.6 -61 26 18           ~ 4 0
15 IRAS 13039-6108 IR 13 07 06.4 -61 24 29           ~ 9 0
16 [MH2010] SMM8 MoC 13 07 08.9 -61 22 49           ~ 4 0
17 2MASS J13070908-6124303 IR 13 07 09.080 -61 24 30.39           ~ 1 0
18 [BBC2006] IRAS 13039-6108 Clump 6 cor 13 07 12.7 -61 22 49           ~ 6 0
19 IRAS 13042-6105 IR 13 07 20.3 -61 21 45           ~ 4 0
20 Caswell H2O 305.80-00.24 Mas 13 16 42.4 -62 58 32           ~ 5 0
21 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3113 1
22 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11927 0
23 [CCE98b] 011.11-0.12 Cld 18 10.5 -19 23           ~ 86 1
24 [RJS2006] MSXDC G023.60+00.00 MM5 mm 18 34 09.5 -08 18 00           ~ 6 0
25 [RJS2006] MSXDC G023.60+00.00 MM3 mm 18 34 10.0 -08 18 28           ~ 7 0
26 [RJS2006] MSXDC G023.60+00.00 MM1 mm 18 34 11.6 -08 19 06           ~ 13 0
27 MSXDC G023.60+0.00 DNe 18 34 21.0 -08 17 31           ~ 5 0
28 [RJS2006] MSXDC G024.33+00.11 MM7 mm 18 35 09.8 -07 39 48           ~ 5 0
29 MSXDC G024.33+0.11 DNe 18 35 16.30 -07 36 09.3           ~ 7 0
30 [RJS2006] MSXDC G024.33+00.11 MM5 mm 18 35 33.8 -07 36 42           ~ 6 0
31 [RJS2006] MSXDC G024.33+00.11 MM2 mm 18 35 34.5 -07 37 28           ~ 8 0
32 MSXDC G025.04-0.20 DNe 18 37 26.6 -07 09 14           ~ 8 0
33 AGAL G028.324+00.161 cor 18 42 26.8 -04 01 30           ~ 19 0
34 AGAL G028.418+00.141 Y*O 18 42 41.8 -03 57 08           ~ 13 0
35 AGAL G028.244+00.012 smm 18 42 49.7 -04 09 54           ~ 22 0
36 NAME Dragon Nebula DNe 18 42 50.6 -04 03 30           ~ 117 0
37 AGAL G028.291+00.007 cor 18 42 56.3 -04 07 31           ~ 23 0
38 AGAL G028.321-00.009 smm 18 43 03.1 -04 06 24           ~ 21 0
39 [BT2009] C14 mm 18 43 09.9 -04 06 52           ~ 8 0
40 AGAL G028.416-00.007 Y*O 18 43 12.9 -04 01 16           ~ 13 0
41 MSXDC G028.53-0.25 DNe 18 44 17.1 -03 59 37           ~ 17 0
42 MSXDC G031.97+0.07 DNe 18 49 33.7 -00 47 48           ~ 13 0
43 MSXDC G033.69-0.01 DNe 18 52 57.6 +00 42 59           ~ 7 0
44 MSXDC G034.43+0.24 MoC 18 53 18.9 +01 26 39           ~ 65 0
45 [BT2009] H9 mm 18 56 41.2 +02 09 52           ~ 6 0
46 [BT2009] H7 mm 18 56 59.2 +02 04 53           ~ 8 0
47 MSXDC G035.39-0.33 MoC 18 57 09.0 +02 07 46           ~ 91 0
48 2MASS J19213444+1349122 Y*O 19 21 34.45 +13 49 12.2           ~ 2 0
49 [VS2008] S20 Y*O 19 21 40.8 +13 52 36           ~ 2 0
50 NAME W51 IR Dark Cloud cor 19 21 45.3 +13 49 22           ~ 19 0
51 2MASS J19214807+1351249 Y*O 19 21 48.07 +13 51 24.9           ~ 2 0
52 2MASS J19214875+1351034 Y*O 19 21 48.7552599874 +13 51 03.468034692           ~ 2 0
53 2MASS J19214945+1351581 Y*O 19 21 49.4580300548 +13 51 58.153754295           ~ 2 0
54 [VS2008] S10 Y*O 19 21 52.1 +13 52 24           ~ 2 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2010A&A...520A.102M and select 'bookmark this link' or equivalent in the popup menu


2021.01.21-07:36:39

© Université de Strasbourg/CNRS

    • Contact