2010MNRAS.408..731C


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET11:30:50

2010MNRAS.408..731C - Mon. Not. R. Astron. Soc., 408, 731-751 (2010/October-3)

The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150M stellar mass limit.

CROWTHER P.A., SCHNURR O., HIRSCHI R., YUSOF N., PARKER R.J., GOODWIN S.P. and KASSIM H.A.

Abstract (from CDS):

Spectroscopic analyses of hydrogen-rich WN5-6 stars within the young star clusters NGC3603 and R136 are presented, using archival Hubble Space Telescope and Very Large Telescope spectroscopy, and high spatial resolution near-IR photometry, including Multi-Conjugate Adaptive Optics Demonstrator (MAD) imaging of R136. We derive high stellar temperatures for the WN stars in NGC3603 (T*∼ 42±2kK) and R136 (T*∼ 53±3kK) plus clumping-corrected mass-loss rates of 2-5x10–5M/yr which closely agree with theoretical predictions from Vink et al. These stars make a disproportionate contribution to the global ionizing and mechanical wind power budget of their host clusters. Indeed, R136a1 alone supplies ∼7 per cent of the ionizing flux of the entire 30Doradus region. Comparisons with stellar models calculated for the main-sequence evolution of 85-500M accounting for rotation suggest ages of ∼1.5Myr and initial masses in the range 105-170M for three systems in NGC3603, plus 165-320M for four stars in R136. Our high stellar masses are supported by consistent spectroscopic and dynamical mass determinations for the components of NGC3603A1. We consider the predicted X-ray luminosity of the R136 stars if they were close, colliding wind binaries. R136c is consistent with a colliding wind binary system. However, short period, colliding wind systems are excluded for R136a WN stars if mass ratios are of order unity. Widely separated systems would have been expected to harden owing to early dynamical encounters with other massive stars within such a high-density environment. From simulated star clusters, whose constituents are randomly sampled from the Kroupa initial mass function, both NGC3603 and R136 are consistent with an tentative upper mass limit of ∼300M. The Arches cluster is either too old to be used to diagnose the upper mass limit, exhibits a deficiency of very massive stars, or more likely stellar masses have been underestimated - initial masses for the most luminous stars in the Arches cluster approach 200Maccording to contemporary stellar and photometric results. The potential for stars greatly exceeding 150M within metal-poor galaxies suggests that such pair-instability supernovae could occur within the local universe, as has been claimed for SN2007bi.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): binaries: general - stars: early-type - stars: fundamental parameters - stars: Wolf-Rayet - galaxies: star clusters: individual: R136 - galaxies: star clusters: individual: NGC 3603

Simbad objects: 41

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Number of rows : 41

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9702 1
2 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SNIIn 297 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15206 1
4 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1059 2
5 Cl* NGC 2070 MH 57 * 05 38 40.230 -69 05 59.76   12.97 13.0   12.91 O3If*/WN6-A 34 1
6 Brey 78 WR* 05 38 40.2960 -69 05 59.640           O2.5If*/WN6 36 0
7 Brey 75 WR* 05 38 40.53 -69 05 57.2   12.84 12.75   12.34 WN6h 58 0
8 Cl* NGC 2070 SMB 88 * 05 38 41.88 -69 06 14.4   14.77 14.50   14.82 ~ 17 1
9 Brey 77 WR* 05 38 42.13 -69 05 55.3   11.08 10.96     O2If* 72 0
10 BAT99 106 WR* 05 38 42.291 -69 06 03.45   12.83 12.93     WN5h 53 0
11 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1777 1
12 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 61 0
13 BAT99 109 WR* 05 38 42.45 -69 06 02.2   13.09 13.38     WN5h 38 0
14 BAT99 110 WR* 05 38 42.47 -69 06 02.0   13.73 13.73     O2If* 36 0
15 BAT99 111 WR* 05 38 42.765 -69 06 03.36   13.51 13.66     WN9ha 39 0
16 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 50 0
17 RMC 136a Cl* 05 38 43.3 -69 06 08           ~ 143 2
18 Brey 84 HXB 05 38 44.2507887068 -69 06 06.008788720     13.10   12.70 WN5h:a 52 0
19 V* V712 Car bL* 10 23 58.0120989646 -57 45 48.938103165 15.466 15.473 13.5 12.6   O3If*/WN6+O3If*/WN6 150 1
20 WR 21a WR* 10 25 56.5023591737 -57 48 43.517827393     12.67     O2If*/WN5 82 0
21 Ass Car OB 1 As* 10 38 -59.0           ~ 146 0
22 Cl* NGC 3603 BLW A1 WR* 11 15 07.31 -61 15 38.4   12.32 11.18     WN6h 60 0
23 HD 97950 Cl* 11 15 07.346 -61 15 38.52 9.64 9.83 9.03 9.69   WR 184 2
24 Cl* NGC 3603 MDS B WR* 11 15 07.41 -61 15 38.6   12.34 11.33     WN6h 38 0
25 Cl* NGC 3603 MDS C WR* 11 15 07.59 -61 15 38.0   12.94 11.89     WN6h 40 0
26 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 970 1
27 SN 2007bi SN* 13 19 20.19 +08 55 44.3       18.3   SNIcpec 190 1
28 GAL 000.0+00.0 gam 17 45 39.60213 -29 00 22.0000           ~ 12003 0
29 WR 102ad WR* 17 45 50.22 -28 49 21.9           WN8-9 22 0
30 WR 102ae WR* 17 45 50.28 -28 49 11.4           WN9h 33 0
31 WR 102af WR* 17 45 50.290 -28 49 17.20           WN7-8 15 0
32 WR 102ag WR* 17 45 50.40 -28 49 20.9           WN8-9 19 0
33 WR 102ah WR* 17 45 50.43 -28 49 21.9           WN8-9h 29 0
34 WR 102aj WR* 17 45 50.48 -28 49 19.2           WN8-9h 24 0
35 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 649 0
36 WR 102al WR* 17 45 50.58 -28 49 17.2           WN7-8 21 0
37 WR 102ba WR* 17 45 50.69 -28 49 22.2           WN8-9 15 0
38 [BSP2001] 8 Em* 17 45 50.76 -28 49 16.2           O4-6If 19 0
39 WR 102bb WR* 17 45 50.84 -28 49 26.0           WN8-9 17 0
40 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 457 0
41 NAME Local Group GrG ~ ~           ~ 7184 0

    Equat.    Gal    SGal    Ecl

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2021.03.03-11:30:50

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