2017A&A...606A...8D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:19:34

2017A&A...606A...8D - Astronomy and Astrophysics, volume 606A, 8-8 (2017/10-1)

Triggered massive star formation associated with the bubble HII region Sh2-39 (N5).

DURONEA N.U., CAPPA C.E., BRONFMAN L., BORISSOVA J., GROMADZKI M. and KUHN M.A.

Abstract (from CDS):

Aims. We perform a multiwavelength analysis of the bubble HII region Sh2-39 (N5) and its environs with the aim of studying the physical properties of Galactic IR bubbles and exploring their impact in triggering massive star formation.
Methods. To analyze the molecular gas, we used CO(3-2) and HCO+(4-3) line data obtained with the on-the-fly technique from the ASTE telescope. To study the distribution and physical characteristics of the dust, we made use of archival data from ATLASGAL, Herschel, and MSX, while the ionized gas was studied making use of an NVSS image. We used public WISE, Spitzer, and MSX point source catalogs to search for infrared candidate young stellar objects (YSOs) in the region. To investigate the stellar cluster [BDS2003]6 we used IR spectroscopic data obtained with the ARCoIRIS spectrograph, mounted on Blanco 4m Telescope at CTIO, and new available IR Ks band observations from the VVVeXtended ESO Public Survey (VVVX).
Results. The new ASTE observations allowed the molecular gas component in the velocity range from 30km/s to 46km/s, associated with Sh2-39, to be studied in detail. The morphology of the molecular gas suggests that the ionized gas is expanding against its parental cloud. We identified four molecular clumps, which were likely formed by the expansion of the ionization front, and determined some of their physical and dynamical properties. Clumps with HCO+ and 870µm counterparts show evidence of gravitational collapse. We identified several candidate YSOs across the molecular component. Their spatial distribution and the fragmentation time derived for the collected layers of the molecular gas suggest that massive star formation might have been triggered by the expansion of the nebula via the collect and collapse mechanism. The spectroscopical distance obtained for the stellar cluster [BDS2003]6, placed over one of the collapsing clumps in the border of the HII region, reveals that this cluster is physically associated with the nebula and gives more support to the triggered massive star formation scenario. A radio continuum data analysis indicates that the nebula is older and expands at lower velocity than typical IR Galactic bubbles.

Abstract Copyright: © ESO, 2017

Journal keyword(s): molecules data - infrared: ISM - stars: formation - H II regions - stars: massive - stars: massive

VizieR on-line data: <Available at CDS (J/A+A/606/A8): 2m1816ma.dat list.dat fits/*>

Nomenclature: Tables 1-2: [DCB2017] N (Nos 1-4). Table 3: [DCB2017] IRN (Nos IR1-IR3). Table 4: [DCB2017 A (Nos A-B).

Status at CDS:   All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 43

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Number of rows : 43

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 LBN 119.57-00.92 HII 00 21 16 +61 43.5           ~ 36 0
2 SH 2-212 HII 04 40 36.50 +50 27 44.3           ~ 88 2
3 LBN 159.17+03.33 HII 04 58 45.70 +47 59 36.0           ~ 77 2
4 IC 2599 HII 10 37.7 -58 39           ~ 34 2
5 GRS G308.60 +00.60 HII 13 39.9 -61 45           ~ 93 0
6 [CPA2006] S24 bub 16 52 20.1 -44 28 06           ~ 7 0
7 SH 2-3 HII 17 12.4 -38 28           ~ 159 1
8 HD 163336 PM* 17 56 19.0352937873 -15 48 45.099719932   5.967 5.929     A0V 49 0
9 GAL 008.14+00.23 HII 18 03 00.4 -21 48 05           ~ 39 0
10 SSTGLMC G012.4350-01.0616 IR 18 16 40.583 -18 39 53.02           ~ 1 0
11 2MASS J18164094-1839277 IR 18 16 40.944 -18 39 27.75           ~ 1 0
12 WISE J181643.15-183901.2 IR 18 16 43.158 -18 39 01.24           ~ 1 0
13 WISE J181644.14-184135.8 IR 18 16 44.147 -18 41 35.80           ~ 1 0
14 2MASS J18164455-1844020 IR 18 16 44.5519406616 -18 44 02.138175603           ~ 1 0
15 WISE J181644.70-184213.7 IR 18 16 44.702 -18 42 13.71           ~ 1 0
16 WISE J181645.60-183630.9 IR 18 16 45.609 -18 36 30.91           ~ 1 0
17 WISE J181645.76-183857.2 IR 18 16 45.762 -18 38 57.27           ~ 1 0
18 WISE J181647.07-184403.2 IR 18 16 47.073 -18 44 03.27           ~ 1 0
19 SSTGLMC G012.4360-01.0905 IR 18 16 47.132 -18 40 39.39           ~ 1 0
20 SSTGLMC G012.4321-01.0959 IR 18 16 47.887 -18 41 01.02           ~ 1 0
21 WISE J181649.62-184008.4 IR 18 16 49.622 -18 40 08.44           ~ 1 0
22 2MASS J18165054-1842488 IR 18 16 50.5576892779 -18 42 49.579143220           ~ 1 0
23 [BDS2003] 6 Cl* 18 16 51 -18 41.9           ~ 3 0
24 2MASS J18165113-1841488 IR 18 16 51.132 -18 41 48.87           ~ 1 0
25 [UHP2009] VLA G012.4317-01.1112 HII 18 16 51.2 -18 41 28           ~ 2 1
26 MSX6C G012.4314-01.1117 Y*O 18 16 51.3 -18 41 30           ~ 4 1
27 WISE J181651.81-183757.2 IR 18 16 51.811 -18 37 57.27           ~ 1 0
28 WISE J181652.04-184310.1 IR 18 16 52.045 -18 43 10.16           ~ 1 0
29 SH 2-39 HII 18 16 52.5 -18 41 50           ~ 14 0
30 IRAS 18139-1842 Y*O 18 16 53.1 -18 41 40           ~ 14 0
31 IRAS 18139-1839 IR 18 16 53.2 -18 37 57           ~ 5 0
32 WISE J181653.80-183937.4 IR 18 16 53.809 -18 39 36.41           ~ 1 0
33 MSX6C G012.4909-01.0962 IR 18 16 55.0 -18 37 55           ~ 1 0
34 MSX6C G012.4382-01.1252 IR 18 16 55.2 -18 41 32           ~ 1 0
35 MSX6C G012.4452-01.1255 IR 18 16 56.1 -18 41 10           ~ 1 0
36 WISE J181656.50-184358.4 IR 18 16 56.510 -18 43 58.57           ~ 1 0
37 WISE J181657.04-184034.6 IR 18 16 57.048 -18 40 34.64           ~ 1 0
38 2MASS J18165709-1840342 IR 18 16 57.094 -18 40 34.26           ~ 1 0
39 [CPA2006] N5 bub 18 16 59 -18 40.2           ~ 5 0
40 WISE J181703.60-184153.7 IR 18 17 03.605 -18 41 53.73           ~ 1 0
41 WISE J181717.23-183929.2 IR 18 17 17.233 -18 39 29.28           ~ 1 0
42 LBN 063.10+00.46 HII 19 49 11.7 +26 51 36   14.60 13.63     ~ 50 0
43 SH 2-104 HII 20 24 37 +38 31.9           ~ 90 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:19:35

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