2011A&A...535A..29G


Query : 2011A&A...535A..29G

2011A&A...535A..29G - Astronomy and Astrophysics, volume 535A, 29-29 (2011/11-1)

Search for OB stars running away from young star clusters. II. The NGC 6357 star-forming region.

GVARAMADZE V.V., KNIAZEV A.Y., KROUPA P. and OH S.

Abstract (from CDS):

Dynamical few-body encounters in the dense cores of young massive star clusters are responsible for the loss of a significant fraction of their massive stellar content. Some of the escaping (runaway) stars move through the ambient medium supersonically and can be revealed via detection of their bow shocks (visible in the infrared, optical or radio). In this paper, which is the second of a series of papers devoted to the search for OB stars running away from young (≲ several Myr) Galactic clusters and OB associations, we present the results of the search for bow shocks around the star-forming region NGC 6357. Using the archival data of the Midcourse Space Experiment (MSX) satellite and the Spitzer Space Telescope, and the preliminary data release of the Wide-Field Infrared Survey Explorer (WISE), we discovered seven bow shocks, whose geometry is consistent with the possibility that they are generated by stars expelled from the young (∼1-2Myr) star clusters, Pismis 24 and AH03 J1725-34.4, associated with NGC 6357. Two of the seven bow shocks are driven by the already known OB stars, HD 319881 and [N78]34. Follow-up spectroscopy of three other bow-shock-producing stars showed that they are massive (O-type) stars as well, while the 2MASS photometry of the remaining two stars suggests that they could be B0V stars, provided that both are located at the same distance as NGC 6357. Detection of numerous massive stars ejected from the very young clusters is consistent with the theoretical expectation that star clusters can effectively lose massive stars at the very beginning of their dynamical evolution (long before the second mechanism for production of runaway stars, based on a supernova explosion in a massive tight binary system, begins to operate) and lends strong support to the idea that probably all field OB stars have been dynamically ejected from their birth clusters. A by-product of our search for bow shocks around NGC 6357 is the detection of three circular shells typical of luminous blue variable and late WN-type Wolf-Rayet stars.

Abstract Copyright:

Journal keyword(s): stars: kinematics and dynamics - stars: massive - open clusters and associations: general - clusters open and associations: individual: AH03 J1725-34.4 - ISM: individual objects: NGC6357

Nomenclature: Figs 13-15, Table 4: [GKK2011] shell N (Nos 1-3).

Simbad objects: 40

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Number of rows : 40
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 * kap Cas s*b 00 32 59.9911963 +62 55 54.417374 3.50 4.30 4.16 4.02 3.96 B1Ia 452 0
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15534 1
3 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2073 1
4 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1815 1
5 V* GP Vel HXB 09 02 06.8610736194 -40 33 16.896402010 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1398 0
6 GUM 29 HII 10 24 14.6 -57 46 58           ~ 196 0
7 CD-34 6792 PM* 10 32 13.6185042385 -35 37 41.710291605   12.84 11.84     F:wl: 130 0
8 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 454 0
9 NAME Sher 25 star * 11 15 07.6444076894 -61 15 17.608695337   13.63 12.27     B1.5Iab 73 1
10 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 990 1
11 IRAS 17078-3927 * 17 11 16.6862142495 -39 31 31.262920415           ~ 8 0
12 TYC 7370-460-1 * 17 18 15.4062020431 -34 00 06.221222446   13.24 11.79     O6V((f))+O8V 9 0
13 THA 10-15 Em* 17 20 31.7613133919 -33 09 48.915452316   17.80 14.57     M3e 19 1
14 NGC 6334 HII 17 20 51 -36 06.9           ~ 619 0
15 2MASS J17220342-3414241 * 17 22 03.4358569663 -34 14 24.037459788           O5.5 5 0
16 GAL 351.66+00.52 HII 17 22 05.5 -35 39 16           ~ 7 0
17 GEN# +6.20114034 * 17 22 05.6184455944 -35 39 55.458656896   14.86 13.13     O8/B0III/V 7 0
18 [GKK2011] shell 1 IR 17 22 36.7 -33 49 10           ~ 2 0
19 2MASS J17225002-3403223 * 17 22 50.0218664120 -34 03 22.348331160           B0V 4 0
20 IRAS 17207-3404 IR 17 24 04.2 -34 07 12           ~ 7 0
21 CXOU J172405.6-340710 * 17 24 05.6222300226 -34 07 09.509087526           ~ 5 0
22 Cl Pismis 24 OpC 17 24 43.0 -34 12 23   11.00 9.6     ~ 114 0
23 HD 319718 ** 17 24 43.490 -34 11 57.03 12.28 11.94 10.44 10.05   O3.5If* 84 0
24 GAL 353.19+00.91 HII 17 24 48 -34 10.8           ~ 25 0
25 HD 157504 WR* 17 25 08.8534998754 -34 11 12.502902170 12.80 12.10 10.68 10.39 11.546 WC7+O7-9 111 0
26 2MASS J17252916-3425157 Y*O 17 25 29.1668373577 -34 25 15.653961432 13.8 13.36 11.91     O6Vn((f)) 13 0
27 NAME AH03 J1725-34.4 OpC 17 25 32.0 -34 24 20           ~ 13 0
28 [N78] 49 Y*O 17 25 34.232280 -34 23 11.74812 14.34 13.663 11.872 11.357   O5.5IV(f) 13 0
29 GAL 353.1+00.6 HII 17 25 37 -34 22.5           ~ 16 0
30 [GKK2011] shell 2 MIR 17 26 19.107 -35 32 37.74           ~ 1 0
31 NGC 6357 HII 17 26.5 -34 12           ~ 259 0
32 2MASS J17271123-3414349 * 17 27 11.2377753495 -34 14 35.093006672           O7.5 6 0
33 2MASS J17271253-3330399 * 17 27 12.5311361487 -33 30 39.953291630           B0V 3 0
34 HD 319881 * 17 28 21.6707964150 -34 32 30.425692132 11.14 11.21 10.11 10.00   O6Vn 18 0
35 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 968 2
36 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1526 0
37 CD-44 12736 PM* 18 36 25.9487430436 -44 18 36.919462094   10.83 10.22     G0 199 0
38 NAME Sgr Arm PoG 19 00 -30.0           ~ 558 1
39 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1142 1
40 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 837 0

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2021.09.20-18:44:43

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