The VLT-FLAMES Tarantula Survey
1 Departamento de Física y AstronomíaUniversidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile
2 Instituto de Investigación Multidisciplinar en Ciencia y Tecnología, Universidad de La Serena, Raúl Bitrán 1305, La Serena, Chile
3 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
5 LMU Munich, Universitätssternwarte, Scheinerstrasse 1, 81679 Munchen, Germany
6 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, United Kingdom
7 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK
8 Centro de Astrobiología (CSIC-INTA), Ctra. de Torrejón a Ajalvir km-4, 28 850 Torrejón de Ardoz, Madrid, Spain
9 University of Vienna, Department of Astronomy, Türkenschanzstr. 17, 1180, Vienna, Austria
10 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA
11 Department of Physics & Astronomy, Hounsfield Road, University of Sheffield, S3 7RH, UK
12 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH, Amsterdam, The Netherlands
13 Instituut voor Sterrenkunde, Universiteit Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
14 Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
15 European Space Astronomy Centre (ESAC), Camino bajo del castillo, s/n Urbanización Villafranca del Castillo, Villanueva de la Cañada, 28 692 Madrid, Spain
16 Centro de Astrobiología, CSIC-INTA, Campus ESAC, Camino bajo del castillo s/n, 28 692 Madrid, Spain
17 Armagh Observatory, College Hill, Armagh, BT61 9DG, Northern Ireland, UK
18 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⋆⋆⋆ Corresponding author: C. Sabín-Sanjulián, e-mail: firstname.lastname@example.org
Received: 29 June 2016
Accepted: 10 February 2017
Context. The VLT-FLAMES Tarantula Survey has observed hundreds of O-type stars in the 30 Doradus region of the Large Magellanic Cloud (LMC).
Aims. We study the properties of a statistically significant sample of O-type dwarfs in the same star-forming region and test the latest atmospheric and evolutionary models of the early main-sequence phase of massive stars.
Methods. We performed quantitative spectroscopic analysis of 105 apparently single O-type dwarfs. To determine stellar and wind parameters, we used the iacob-gbat package, an automatic procedure based on a large grid of atmospheric models that are calculated with the fastwind code. This package was developed for the analysis of optical spectra of O-type stars. In addition to classical techniques, we applied the Bayesian bonnsai tool to estimate evolutionary masses.
Results. We provide a new calibration of effective temperature vs. spectral type for O-type dwarfs in the LMC, based on our homogeneous analysis of the largest sample of such objects to date and including all spectral subtypes. Good agreement with previous results is found, although the sampling at the earliest subtypes could be improved. Rotation rates and helium abundances are studied in an evolutionary context. We find that most of the rapid rotators (v sin i > 300 km s-1) in our sample have masses below ~25 M⊙ and intermediate rotation-corrected gravities (3.9 < log gc < 4.1). Such rapid rotators are scarce at higher gravities (i.e. younger ages) and absent at lower gravities (larger ages). This is not expected from theoretical evolutionary models, and does not appear to be due to a selection bias in our sample. We compare the estimated evolutionary and spectroscopic masses, finding a trend that the former is higher for masses below ~20 M⊙. This can be explained as a consequence of limiting our sample to the O-type stars, and we see no compelling evidence for a systematic mass discrepancy. For most of the stars in the sample we were unable to estimate the wind-strength parameter (hence mass-loss rates) reliably, particularly for objects with lower luminosity (log L/L⊙ ≲ 5.1). Only with ultraviolet spectroscopy will we be able to undertake a detailed investigation of the wind properties of these dwarfs.
Key words: Magellanic Clouds / stars: atmospheres / stars: early-type / stars: fundamental parameters / stars: massive
Based on observations at the European Southern Observatory Very Large Telescope in program 182.D-0222.
Tables A.1 to B.2 are also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A79
© ESO, 2017