1998A&A...338..223H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST07:31:19

1998A&A...338..223H - Astronomy and Astrophysics, volume 338, 223-242 (1998/10-1)

Millimetre study of star formation in southern globules.

HENNING T. and LAUNHARDT R.

Abstract (from CDS):

The paper presents the results of a dedicated millimetre continuum and molecular line (CO and CS) search for cold and dense (protostellar) cores and molecular outflows in 35 southern Bok globules (Dec.≤-30°). Only globules which are associated with cold IRAS point sources (FIR colour temperatures below 35K) were selected for this study. We could demonstrate that globules are often loosely associated with molecular cloud complexes from which they probably formed. Based on such associations, we determined reliable distances for most of the globules of our sample. It turned out that half of the selected globules are located in the local spiral arm at distances between 170 and 400pc. The most prominent features in the spatial distribution of these globules are the Lindblad ring and the Vela-Gum complex. A group of 14 globules is located at larger distances (0.7-4kpc) in the Carina arm. The objects in the far Carina arm (d>2kpc) are clearly different from ``classical'' Bok globules being more massive and more luminous. Out of the 35 globules observed, all globules were detected in the 12CO(2-1) line (detection rate 100%, 3σdetection limit Tmb=0.3K), 24 globules were detected in the CS(2-1) line (69%, detection limit 0.2K), and 18 globules were detected in the 1.3mm continuum emission (51%, detection limit 40mJy/beam). In 12 globules (34%), CO line wings indicating the presence of molecular outflows have been found, of which 8 outflows were previously unkown. The colours of the embedded IRAS point sources, the strength of the millimetre dust continuum emission, the CS line temperatures as well as the presence of molecular outflows are all well correlated with each other. Based on these results and on the IRAS colour-colour diagram, we can clearly distinguish two groups of sources: Objects with active protostellar cores (``Class0'' and ``I'') and globules with less dense and less centrally peaked cores (pre-protostellar cores and globules which may not form stars at all). The objects with active protostellar cores are characterized by centrally condensed cores (typical beam-averaged density of ≃106cm–3) and molecular outflows. The mass spectrum dN/dM of the circum-protostellar envelopes can be fitted with a single slope of -1.8 between 0.15 and 2M and a mean mass of 0.6M. Two objects in our sample clearly resemble the properties of ``Class0'' protostars while the majority of the star-forming cores probably already passed the main accretion phase. Five of the colder and less-condensed objects are proposed to be pre-protostellar cores.

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: formation - ISM: clouds - dust, extinction - ISM: jets and outflows - radio continuum: ISM

Simbad objects: 68

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Number of rows : 68

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 [DB2002b] G249.44-5.09 DNe 07 45 10 -34 36.2           ~ 5 0
2 IRAS 07435-3430 IR 07 45 26.4 -34 37 59           ~ 3 0
3 CG 30 CGb 08 09 32.8 -36 05 00           ~ 120 0
4 IRAS 08150-5247 IR 08 16 26.4 -52 56 55           ~ 1 0
5 [DB2002b] G268.17-9.72 DNe 08 16 36 -52 54.5           ~ 4 0
6 [DB2002b] G265.65-7.71 MoC 08 18 40 -49 43.9           ~ 10 0
7 IRAS 08171-4933 FIR 08 18 40.0 -49 43 15           ~ 2 0
8 2MASS J08254384-5100326 Y*O 08 25 43.85 -51 00 32.7           ~ 298 1
9 NAME ESO 210- 6A MoC 08 25 44 -51 02.1           ~ 40 1
10 FEST 2-51 Cld 08 26 28 -50 39.9           ~ 4 0
11 IRAS 08250-5030 FIR 08 26 31.7 -50 40 30           ~ 10 0
12 BHR 34 MoC 08 26 34 -50 39.9           ~ 18 0
13 IRAS 08261-5100 MoC 08 27 38.9 -51 10 38           ~ 29 0
14 [DB2002b] G276.21-10.57 MoC 08 44 14 -59 54.0           ~ 10 0
15 IRAS 08433-5945 IR 08 44 21.9 -59 56 10           ~ 7 0
16 IRAS 09449-5052 FIR 09 46 45.2 -51 06 02           ~ 6 0
17 BHR 55 MoC 09 46 51 -51 06.4           ~ 16 0
18 DCld 283.8-03.4 DNe 10 07 14 -60 02.8           ~ 4 0
19 IRAS 10059-5948 GNe 10 07 36.2 -60 03 00           ~ 6 0
20 BHR 58 MoC 10 49 00 -62 23.1           ~ 8 0
21 IRAS 10471-6206 IR 10 49 01.6 -62 22 16           ~ 6 0
22 IRAS 10497-6242 MoC 10 51 40.3 -62 57 03           ~ 6 0
23 IRAS 10501-5630 HII 10 52 15.4 -56 46 28           ~ 9 1
24 IRAS 11277-6057 FIR 11 30 04.0 -61 14 24           ~ 1 0
25 [DB2002b] G292.91+1.32 DNe 11 30 07 -59 57.4           ~ 4 0
26 IRAS 11278-5940 IR 11 30 09.1 -59 57 26           ~ 4 0
27 [DB2002b] G293.31+0.12 MoC 11 30 10 -61 13.4           ~ 7 0
28 IRAS 11306-6311 IR 11 33 00.1277393829 -63 27 21.762218113           ~ 13 0
29 IRAS 11403-6126 IR 11 42 47.7 -61 43 26           ~ 2 0
30 [DB2002b] G294.90+0.05 MoC 11 42 51 -61 44.4           ~ 7 0
31 IRAS 11431-6516 HII 11 45 34.0 -65 32 59           ~ 12 0
32 [DB2002b] G296.22-3.55 DNe 11 45 58 -65 34.0           ~ 7 0
33 IRAS 11436-6017 IR 11 46 01.511 -60 33 59.30           ~ 7 0
34 DCld 295.0+01.3 DNe 11 46 12 -60 33.8           ~ 7 0
35 IRAS 11488-6045 IR 11 51 18.1 -61 02 31           ~ 1 0
36 [DB2002b] G295.73+0.98 DNe 11 51 29 -61 02.9           ~ 4 0
37 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 119 0
38 NAME BHR 71 MM HII 12 01 37.1 -65 08 54           ~ 33 0
39 Sandqvist 160 DNe 13 06.9 -77 01           ~ 41 0
40 PSCz Q13036-7644 Y*O 13 07 36.89 -77 00 09.7           ~ 39 1
41 IRAS 13224-5928 IR 13 25 44.64 -59 43 50.9           ~ 11 0
42 [DB2002b] G307.25+2.86 MoC 13 25 49 -59 42.9           ~ 9 0
43 [DB2002b] G313.33-0.30 DNe 14 20 03 -61 22.5           ~ 4 0
44 IRAS 14183-6050 IR 14 22 03.6 -61 04 22           ~ 6 0
45 IRAS 14188-6054 HII 14 22 32.3 -61 08 19           ~ 6 0
46 IRAS 14189-6115 IR 14 22 42.6 -61 28 49           ~ 4 0
47 IRAS 15075-5307 FIR 15 11 12.7 -53 18 53           ~ 2 0
48 BHR 106 MoC 15 11 14 -53 18.4           ~ 6 0
49 IRAS 15215-6056 IR 15 25 38.1 -61 06 51           ~ 7 0
50 [DB2002b] G320.49-3.62 MoC 15 25 45 -61 07.1           ~ 8 0
51 [DB2002b] G320.11-4.34 MoC 15 26 27 -61 56.0           ~ 6 0
52 IRAS 15223-6146 FIR 15 26 32.6 -61 56 33           ~ 3 0
53 [DB2002b] G319.92-4.77 MoC 15 27 12 -62 23.3           ~ 7 0
54 IRAS 15230-6211 IR 15 27 13.4 -62 22 19           ~ 3 0
55 IRAS 15431-5652 IR 15 47 04.8 -57 02 02           ~ 4 0
56 [DB2002b] G325.12-1.92 DNe 15 47 06 -57 01.8           ~ 4 0
57 DCld 344.5+03.2 DNe 16 49 10 -39 45.1           ~ 3 0
58 IRAS 16458-3939 FIR 16 49 16.2 -39 44 48           ~ 1 0
59 [DB2002b] G337.09-4.90 MoC 16 58 42 -50 35.8           ~ 10 0
60 IRAS 16549-5030 IR 16 58 51.5 -50 35 30           ~ 4 0
61 IRAS 17135-3200 * 17 16 45.8906130848 -32 04 06.180078653           ~ 1 0
62 LDN 1701 DNe 17 16 47 -32 03.9           ~ 6 0
63 IRAS 17151-3202 IR 17 18 23.5 -32 05 32           ~ 8 0
64 BHR 167 MoC 17 18 28 -32 04.6           ~ 6 0
65 IRAS 17181-4405 IR 17 21 46.9 -44 08 42           ~ 10 0
66 BHR 137 MoC 17 21 48 -44 08.8           ~ 7 0
67 BHR 168 MoC 17 55 12 -34 15.7           ~ 5 0
68 IRAS 17518-3414 FIR 17 55 13.1744785757 -34 14 31.560242789           ~ 3 0

    Equat.    Gal    SGal    Ecl

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2020.07.05-07:31:19

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