2018A&A...618A..73S


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.29CET22:16:23

2018A&A...618A..73S - Astronomy and Astrophysics, volume 618A, 73-73 (2018/1-0)

The VLT-FLAMES Tarantula Survey. XXIX. Massive star formation in the local 30 Doradus starburst.

SCHNEIDER F.R.N., RAMIREZ-AGUDELO O.H., TRAMPER F., BESTENLEHNER J.M., CASTRO N., SANA H., EVANS C.J., SABIN-SANJULIAN C., SIMON-DIAZ S., LANGER N., FOSSATI L., GRAFENER G., CROWTHER P.A., DE MINK S.E., DE KOTER A., GIELES M., HERRERO A., IZZARD R.G., KALARI V., KLESSEN R.S., LENNON D.J., MAHY L., MAIZ-APELLANIZ J., MARKOVA N., VAN LOON J.T., VINK J.S. and WALBORN N.R.

Abstract (from CDS):

The 30 Doradus (30 Dor) nebula in the Large Magellanic Cloud (LMC) is the brightest HII region in the Local Group and a prototype starburst similar to those found in high redshift galaxies. It is thus a stepping stone to understand the complex formation processes of stars in starburst regions across the Universe. Here, we have studied the formation history of massive stars in 30 Dor using masses and ages derived for 452 mainly OB stars from the spectroscopic VLT-FLAMES Tarantula Survey (VFTS). We find that stars of all ages and masses are scattered throughout 30 Dor. This is remarkable because it implies that massive stars either moved large distances or formed independently over the whole field of view in relative isolation. We find that both channels contribute to the 30 Dor massive star population. Massive star formation rapidly accelerated about 8Myr ago, first forming stars in the field before giving birth to the stellar populations in NGC 2060 and NGC 2070. The R136 star cluster in NGC 2070 formed last and, since then, about 1Myr ago, star formation seems to be diminished with some continuing in the surroundings of R136. Massive stars within a projected distance of 8 pc of R136 are not coeval but show an age range of up to 6Myr. Our mass distributions are well populated up to 200M. The inferred IMF is shallower than a Salpeter-like IMF and appears to be the same across 30 Dor. By comparing our sample of stars to stellar models in the Hertzsprung-Russell diagram, we find evidence for missing physics in the models above log L/L=6 that is likely connected to enhanced wind mass loss for stars approaching the Eddington limit. Our work highlights the key information about the formation, evolution and final fates of massive stars encapsulated in the stellar content of 30 Dor, and sets a new benchmark for theories of massive star formation in giant molecular clouds.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - stars: massive - stars: luminosity function, mass function - Magellanic Clouds - galaxies: star clusters: individual: 30 Doradus

Simbad objects: 39

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Number of rows : 39

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9564 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5766 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14998 1
4 M 42 HII 05 35 17.3 -05 23 28           ~ 3752 0
5 NAME 30 Dor 016 * 05 37 08.8775810516 -69 07 20.377571697 12.623 13.584 13.546   13.816 O2IIIf* 36 0
6 UCAC2 1803231 * 05 37 39.2305260100 -69 09 51.024963212 15.220 16.099 15.806 16.07 15.118 O9:Vnnne+ 23 0
7 HD 269883 WR* 05 37 40.494 -69 07 57.71 13.454 14.184 14.077 14.03 13.492 WN7h 39 0
8 VFTS 125 * 05 37 42.950 -69 10 35.12   16.87 16.6     F5 9 0
9 VFTS 141 * 05 37 45.740 -69 09 13.33   15.36 15.32     O9.5II-III((n)) 11 0
10 Brey 73 WR* 05 37 46.3440 -69 09 09.360   12.222 12.11     WN6(h) 33 1
11 VFTS 151 SB* 05 37 46.520 -69 09 08.79           O6.5II(f)p 10 0
12 [TLD88] 2A * 05 37 46.6 -69 09 08   14.26 14.13     O4(f)(n)p 4 0
13 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 232 1
14 IRSF J05374670-6909112 ** 05 37 46.710 -69 09 11.27   15.36 15.30     O9III((n)) 8 0
15 NAME TLD1 Cl* 05 37 47.0 -69 09 08           ~ 3 2
16 VFTS 154 SB* 05 37 47.090 -69 09 07.70   14.99 14.94     O8.5V 8 0
17 NGC 2060 SNR 05 37 51.4470067818 -69 10 23.957283532   9.69 9.59     ~ 323 2
18 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 180 0
19 H88 301 Cl* 05 38 16 -69 04.0   11.18 10.89     ~ 66 0
20 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1050 2
21 Brey 75 WR* 05 38 40.53 -69 05 57.2   12.84 12.75   12.34 WN6h 58 0
22 NGC 2070 Cl* 05 38 42 -69 06.0     7.25     ~ 329 1
23 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1751 1
24 Cl* NGC 2070 MH 493 * 05 38 42.407 -69 06 15.01   13.69 13.44   13.07 ~ 6 0
25 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 60 0
26 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 48 0
27 VFTS 1025 * 05 38 42.935 -69 06 04.98           ~ 6 0
28 CPD-69 463 s*y 05 38 51.6167474749 -69 08 07.314653596 11.93 12.45 12.014     F7Ia 80 1
29 UCAC4 105-014417 WR* 05 38 55.5218836143 -69 04 26.810760074   16.66 16.08   14.89 WN5h 49 0
30 HD 269928 WR* 05 38 57.0668705166 -69 06 05.660972436   12.02 11.94 12.00 11.58 WN6/7 121 0
31 [SL63] 639 As* 05 39 39 -69 12.1   12.13 11.53     ~ 22 0
32 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 692 1
33 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1077 1
34 Mrk 42 Sy1 11 53 41.7727871132 +46 12 42.171866526   16.24 15.45     ~ 194 0
35 LBN 028.77+03.43 HII 18 31 26.5 -02 04 22           ~ 189 2
36 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 445 0
37 [MSL2003] W43-MM1 cor 18 47 47.0 -01 54 28           ~ 96 0
38 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 801 0
39 NAME Local Group GrG ~ ~           ~ 7076 0

    Equat.    Gal    SGal    Ecl

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2020.10.29-22:16:23

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