2013A&A...558A.134D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:58:03

2013A&A...558A.134D - Astronomy and Astrophysics, volume 558A, 134-134 (2013/10-1)

The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus.

DORAN E.I., CROWTHER P.A., DE KOTER A., EVANS C.J., McEVOY C., WALBORN N.R., BASTIAN N., BESTENLEHNER J.M., GRAEFENER G., HERRERO A., KOEHLER K., MAIZ-APELLANIZ J., NAJARRO F., PULS J., SANA H., SCHNEIDER F.R.N., TAYLOR W.D., VAN LOON J.Th. and VINK J.S.

Abstract (from CDS):

The VLT-FLAMES Tarantula Survey has an extensive view of the copious number of massive stars in the 30 Doradus (30 Dor) star forming region of the Large Magellanic Cloud. These stars play a crucial role in our understanding of the stellar feedback in more distant, unresolved star forming regions. The first comprehensive census of hot luminous stars in 30 Dor is compiled within a 10arcmin (150pc) radius of its central cluster, R136. We investigate the stellar content and spectroscopic completeness of the early type stars. Estimates were made for both the integrated ionising luminosity and stellar wind luminosity. These values were used to re-assess the star formation rate (SFR) of the region and determine the ionising photon escape fraction. Stars were selected photometrically and combined with the latest spectral classifications. Spectral types were estimated for stars lacking spectroscopy and corrections were made for binary systems, where possible. Stellar calibrations were applied to obtain their physical parameters and wind properties. Their integrated properties were then compared to global observations from ultraviolet (UV) to far-infrared (FIR) imaging as well as the population synthesis code, Starburst99. Our census identified 1145 candidate hot luminous stars within 150pc of R136 of which >700 were considered to be genuine early type stars and contribute to feedback. We assess the survey to be spectroscopically complete to 85% in the outer regions (>5pc) but only 35% complete in the region of the R136 cluster, giving a total of 500 hot luminous stars in the census which had spectroscopy. Only 31 were found to be Wolf-Rayet (W-R) or Of/WN stars, but their contribution to the integrated ionising luminosity and wind luminosity was ∼40% and ∼50%, respectively. Similarly, stars with Minit>100M (mostly H-rich WN stars) also showed high contributions to the global feedback, ∼25% in both cases. Such massive stars are not accounted for by the current Starburst99 code, which was found to underestimate the integrated ionising luminosity of R136 by a factor ∼2 and the wind luminosity by a factor ∼9. The census inferred a SFR for 30 Dor of 0.073±0.04M/yr. This was generally higher than that obtained from some popular SFR calibrations but still showed good consistency with the far-UV luminosity tracer as well as the combined Hα and mid-infrared tracer, but only after correcting for Hα extinction. The global ionising output was also found to exceed that measured from the associated gas and dust, suggesting that ∼6+55–6% of the ionising photons escape the region. When studying the most luminous star forming regions, it is essential to include their most massive stars if one is to determine a reliable energy budget. Photon leakage becomes more likely after including their large contributions to the ionising output. If 30 Dor is typical of other massive star forming regions, estimates of the SFR will be underpredicted if this escape fraction is not accounted for.

Abstract Copyright:

Journal keyword(s): stars: early-type - stars: Wolf-Rayet - open clusters and associations: individual: 30 Doradus - stars: massive - galaxies: star clusters: general - galaxies: star formation

VizieR on-line data: <Available at CDS (J/A+A/558/A134): tabled1.dat tabled2.dat>

Status at CDS:   All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 50

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Number of rows : 50

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 Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
2 Brey 10a WR* 04 57 27.4549113851 -67 39 02.868479987 12.213 13.314 13.496   13.564 O2If*/WN5 52 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
4 LHA 120-N 157 HII 05 35 49 -69 12.6           ~ 46 0
5 HD 38029A WR* 05 36 54.633 -69 11 38.08           WC4 54 1
6 HD 38029 ** 05 36 55.17 -69 11 37.7 14.523 11.71 11.56 11.91 11.680 ~ 58 0
7 HD 38029B s*b 05 36 55.178 -69 11 37.47           B1Ia+ 54 1
8 Brey 69 WR* 05 37 11.4812136852 -69 07 38.184555289 15.959 16.427 16.301   15.936 WN3o 21 0
9 Brey 70a WR* 05 37 35.7057107734 -69 08 40.253264123 17.387 17.957 16.924   16.324 WN4b/WCE 25 0
10 HD 269883 WR* 05 37 40.494 -69 07 57.71 13.454 14.184 14.077 14.03 13.492 WN7h 39 0
11 HD 269888 WR* 05 37 44.6347648981 -69 14 25.676649551 14.413 14.772 14.628 14.81 14.761 WR 40 0
12 Brey 73 WR* 05 37 46.3440 -69 09 09.360   12.222 12.11     WN6(h) 33 1
13 HD 269891 WR* 05 37 49.0345689657 -69 05 08.219994930 11.791 9.447 11.39 11.55   WN6+B1Ia 65 0
14 NGC 2060 SNR 05 37 51.4470067818 -69 10 23.957283532   9.69 9.59     ~ 322 2
15 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 178 0
16 RMC 132 s*b 05 38 14.8988360599 -69 03 48.519323602   12.95 12.90 13.00 12.66 B0.5Ia 20 1
17 H88 301 Cl* 05 38 16 -69 04.0   11.18 10.89     ~ 65 0
18 RMC 135 WR* 05 38 33.62 -69 04 50.4   12.63 13.48     WN7h+OB 55 0
19 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1039 2
20 Brey 81 WR* 05 38 36.4069267803 -69 06 57.535480245   14.02 13.76   12.80 WN8 28 0
21 Brey 79 WR* 05 38 39.1441735472 -69 06 21.299163377     13.5 13.33   WN6 29 0
22 Brey 78 WR* 05 38 40.2960 -69 05 59.640           O2.5If*/WN6 36 0
23 Brey 75 WR* 05 38 40.53 -69 05 57.2   12.84 12.75   12.34 WN6h 58 0
24 RMC 140b WR* 05 38 41.5650 -69 05 15.500   12.61 12.66   12.54 WN6 26 0
25 RMC 140a WR* 05 38 41.600 -69 05 13.39   12.18 12.12   12.40 WN4+WC5 31 0
26 RMC 140 WR* 05 38 41.62 -69 05 14.0   11.213 11.616     WN7+WC4/5pec 76 0
27 NGC 2070 Cl* 05 38 42 -69 06.0     7.25     ~ 328 1
28 BAT99 106 WR* 05 38 42.291 -69 06 03.45   12.83 12.93     WN5h 52 0
29 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
30 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 60 0
31 BAT99 109 WR* 05 38 42.45 -69 06 02.2   13.09 13.38     WN5h 37 0
32 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 48 0
33 BAT99 113 WR* 05 38 43.12 -69 05 46.8   13.56 13.47   13.44 O2If*/WN5 36 0
34 Brey 83 WR* 05 38 44.1120 -69 05 54.960   12.04 11.92     WN 22 0
35 Brey 84 HXB 05 38 44.2507887068 -69 06 06.008788720     13.10   12.70 WN5h:a 52 0
36 HD 269926 WR* 05 38 47.5177886261 -69 00 25.287665455 11.953 12.974 13.116 13.16 12.926 WN4+OB 62 0
37 HD 38282 WR* 05 38 53.3788120199 -69 02 00.896643506   10.98 11.11 11.26   WN5/6h+WN6/7h 150 1
38 UCAC4 105-014417 WR* 05 38 55.5218836143 -69 04 26.810760074   16.66 16.08   14.89 WN5h 49 0
39 HD 269928 WR* 05 38 57.0668705166 -69 06 05.660972436   12.02 11.94 12.00 11.58 WN6/7 119 0
40 Brey 90a WR* 05 39 03.7772881811 -69 03 46.561252441 16.190 15.895 15.834   15.533 WC5 22 0
41 HD 38344 WR* 05 39 11.3191294608 -69 02 01.572235036 12.323 13.04 12.993 13.07 12.574 WN5h 65 0
42 HBH 12 * 09 19.3 +44 47           ~ 5 0
43 Mrk 34 Sy2 10 34 08.606 +60 01 52.33   15.71 14.65     ~ 212 1
44 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 888 2
45 NGC 3353 AGN 10 45 22.390 +55 57 37.36 12.90 13.25 12.79     ~ 319 1
46 Mrk 42 Sy1 11 53 41.7727871132 +46 12 42.171866526   16.24 15.45     ~ 191 0
47 Mrk 1318 H2G 12 19 09.840 +03 51 23.34   14.5       ~ 153 0
48 Mrk 51 GiG 12 24 14.5321232503 +04 13 33.588515642   15.2       ~ 40 0
49 NAME Carina Region reg ~ ~           ~ 152 0
50 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:58:03

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