2012MNRAS.424.3037G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST06:23:34

2012MNRAS.424.3037G - Mon. Not. R. Astron. Soc., 424, 3037-3049 (2012/August-3)

Field O stars: formed in situ or as runaways?

GVARAMADZE V.V., WEIDNER C., KROUPA P. and PFLAMM-ALTENBURG J.

Abstract (from CDS):

A significant fraction of massive stars in the Milky Way and other galaxies are located far from star clusters and star-forming regions. It is known that some of these stars are runaways, i.e. possess high space velocities (determined through the proper motion and/or radial velocity measurements), and therefore most likely were formed in embedded clusters and then ejected into the field because of dynamical few-body interactions or binary-supernova explosions. However, there exists a group of field O stars whose runaway status is difficult to prove via direct proper motion measurements (e.g. in the Magellanic Clouds) or whose (measured) low space velocities and/or young ages appear to be incompatible with their large separation from known star clusters. The existence of this group led some authors to believe that field O stars can form in situ. Since the question of whether or not O stars can form in isolation is of crucial importance for star formation theory, it is important to thoroughly test candidates of such stars in order to improve the theory. In this paper, we examine the runaway status of the best candidates for isolated formation of massive stars in the Milky Way and the Magellanic Clouds by searching for bow shocks around them, by using the new reduction of the Hipparcos data, and by searching for stellar systems from which they could originate within their lifetimes. We show that most of the known O stars thought to have formed in isolation are instead very likely runaways. We show also that the field must contain a population of O stars whose low space velocities and/or young ages are in apparent contradiction to the large separation of these stars from their parent clusters and/or the ages of these clusters. These stars (the descendants of runaway massive binaries) cannot be traced back to their parent clusters and therefore can be mistakenly considered as having formed in situ. We argue also that some field O stars could be detected in optical wavelengths only because they are runaways, while their cousins residing in the deeply embedded parent clusters might still remain totally obscured. The main conclusion of our study is that there is no significant evidence whatsoever in support of the in situ proposal on the origin of massive stars.

Abstract Copyright: 2012 The Authors Monthly Notices of the Royal Astronomical Society 2012 RAS

Journal keyword(s): stars: early-type - stars: formation - stars: kinematics and dynamics - stars: massive - Magellanic Clouds - galaxies: star formation

Simbad objects: 54

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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 - 2020
#notes
1 SMC ASS 16 As* 00 48 40 -73 25.8           ~ 7 0
2 [BS95] 43 As* 00 49 15 -73 22.3           ~ 6 0
3 NAME [B91] 6W HII 00 49 15 -72 52.8           ~ 12 0
4 LHA 115-N 33 Em* 00 49 29.32080 -73 26 34.7208   16.28 15.92 15.74 14.70 O6.5-7V 21 0
5 AzV 58 * 00 49 57.8946135338 -72 51 54.785163234   14.11 14.29     B0.5III 13 0
6 AzV 67 Em* 00 50 11.1185380998 -72 32 35.139681707 12.55 13.60 13.73   13.89 O9III 16 0
7 NAME SMC-N 36W As* 00 50 21 -72 52.9           ~ 7 0
8 [H86] 119 Cl* 00 51 37 -72 32.5           ~ 6 0
9 AzV 106 * 00 51 43.3554488791 -72 37 25.337929227   14.14 14.18     B1II 10 0
10 OGLE SMC-SC6 85632 As* 00 51 49.62 -72 32 59.7   16.54 16.38     B0-5(IV) 8 0
11 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
12 NGC 330 Cl* 00 56 20.59 -72 27 12.5 9.37 9.76 9.55   8.89 ~ 366 0
13 [BS95] 83 As* 00 57 06 -72 32.7           ~ 6 0
14 AzV 186 * 00 57 26.9388728646 -72 33 13.560551338 12.66 13.88 13.86   14.15 O8III((f)) 23 0
15 AzV 223 * 00 59 13.4275434874 -72 39 02.635295577 12.36 13.47 13.67   13.95 O9.5II 15 0
16 AzV 226 * 00 59 20.7287691158 -72 17 10.615963093 12.97 14.12 14.19     O7IIIn((f)) 24 0
17 [MLD95] SMC 16 Be? 01 00 43.9410121774 -72 26 05.151951622 13.16 14.18 14.35   14.49 O9.5III 14 0
18 [B91] 18 As* 01 00 55 -72 29.7           ~ 6 0
19 AzV 302 * 01 02 19.0563200592 -72 22 04.467104234 13.07 14.09 14.18   14.40 O9III 13 0
20 DEM S 118 HII 01 02 41.1 -72 24 41           ~ 12 0
21 SK 151 s*b 01 13 00.4001520261 -73 17 04.124180844 12.66 13.62 13.63   13.41 O9.5I 20 0
22 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
23 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
24 HD 32228 WR* 04 56 34.666 -66 28 26.34   10.685 10.830     WC4+O9.5II: 90 0
25 NGC 1761 As* 04 56 39 -66 29.0     9.94     ~ 96 0
26 [L72] LH 10-3061 * 04 56 42.460 -66 25 18.09 12.699 13.595 13.491   13.405 ON2III(f*) 25 0
27 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 234 0
28 NGC 1763 As* 04 56 51.5 -66 24 25     9.40     ~ 154 3
29 Brey 10a WR* 04 57 27.4549113851 -67 39 02.868479987 12.213 13.314 13.496   13.564 O2If*/WN5 52 1
30 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
31 HD 269810 Em* 05 35 13.8987303206 -67 33 27.540351680   12.08 12.22 12.53   O3III(f*) 99 0
32 LH 82 As* 05 35 14 -67 33.8           ~ 24 0
33 SK -69 206 * 05 35 35.9718209948 -69 07 06.552137672   12.99 12.82 12.99   OB 11 0
34 BI 237 * 05 36 14.6329670483 -67 39 19.168530216 12.865 13.790 13.830   13.948 O2V(f*) 32 0
35 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1039 2
36 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
37 UCAC4 105-014417 WR* 05 38 55.5218836143 -69 04 26.810760074   16.66 16.08   14.89 WN5h 49 0
38 HD 269928 WR* 05 38 57.0668705166 -69 06 05.660972436   12.02 11.94 12.00 11.58 WN6/7 119 0
39 HD 48279 ** 06 42 40.54719 +01 42 58.2571 7.26 8.03 7.86     O8V+F2V 138 0
40 HD 57682 * 07 22 02.0544956184 -08 58 45.761168747 5.20 6.24 6.43     O9.2IV 232 0
41 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49   11.59 10.5     ~ 277 0
42 HD 123056 * 14 07 25.6377162147 -60 28 14.148538108 7.54 8.28 8.14 9.00   O9.5IV(n) 54 0
43 HD 124314 ** 14 15 01.60615 -61 42 24.3831   8.96 6.64 6.45 6.31 O6V(n)((f)) 133 1
44 LBN 006.00+24.73 HII 16 35 56.8 -12 43 05           ~ 51 0
45 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1723 2
46 HD 153426 * 17 01 13.0075706903 -38 12 11.888514524 6.79 7.61 7.47 8.49   O8.5III 87 0
47 HD 165319 * 18 05 58.8360539028 -14 11 52.998719141 8.15 8.63 8.04 7.50 7.00 O9.7Ib 68 1
48 RCW 158 HII 18 06.3 -14 12           ~ 6 0
49 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 935 2
50 HD 193793 WR* 20 20 27.9763345925 +43 51 16.289775091 6.90 7.25 6.85 4.58   WC7p+O5 649 1
51 HD 195592 s*b 20 30 34.9690436039 +44 18 54.858025184 7.75 7.95 7.08 6.29 5.60 O9.7Ia 197 1
52 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 790 0
53 BD+43 3654 s*b 20 33 36.0795380204 +43 59 07.362541702   11.24 10.06     O4If 50 0
54 HD 202124 s*b 21 12 28.3896915394 +44 31 54.125407798 7.33 7.94 7.76     O9Iab 89 0

    Equat.    Gal    SGal    Ecl

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2020.07.05-06:23:34

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