The VLT-FLAMES Tarantula survey

By Christopher H. Evans, W. D. Taylor, V. Hénault-Brunet, H. Sana, A. D. Koter, S. Simón-Díaz, Giovanni Carraro, T. Bagnoli, N. Bastian, J. Bestenlehner and 32 more. Proceedings of the International Astronomical Union, 2009

457 citations recorded by the source corpus.

Abstract The Tarantula Survey is an ESO Large Programme which has obtained multi-epoch spectroscopy of over 1,000 massive stars in the 30 Doradus region of the Large Magellanic Cloud. The assembled consortium will exploit these data to address a range of fundamental questions in both stellar and cluster evolution.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1eced7c68f6c24931b772f41d1ea889908d24b6e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, methodology): “Since these most massive stars dominate the light at early ages, this can alter the observable properties of the integrated light measured from the population (e.g. Haas & Anders 2010; Doran et al. 2013).”
SOUTHERN MASSIVE STARS AT HIGH ANGULAR RESOLUTION: OBSERVATIONAL CAMPAIGN AND COMPANION DETECTION (2014, background): “The two first observations have been discussed by Sana et al. (2013b).”
The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, methodology): “However, the strongest deviation to the results presented by Doran et al. (2013) is obtained in the derived massloss rate, which is more than nine times lower in our analysis.”
Wind modelling of very massive stars up to 300 solar masses (2011, unknown): “This will be a crucial aim of the VLT Flames Tarantula Survey ( Evans et al. 2011, Bestenlehner et al. in prep.).”
Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, background): “We put fbin = 0.5, assuming that 50 per cent of stars are in binaries (see e.g. Sana et al. 2013).”
The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, methodology): “…factor used to take into account the fact that we only simulate binary systems (we assume that 50 per cent of the stars are in binaries fbin = 0.5 Sana et al. 2013); fIMF = 0.285 corrects for the fact that we have simulated only systems which have the primary component more massive than 5M .”
The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, background): “1 Energetically, i.e. with respect to luminosities and winds, WR-stars dominate (e.g. Leitherer, Robert & Drissen 1992; Doran et al. 2013).”
DOUBLE COMPACT OBJECTS. II. COSMOLOGICAL MERGER RATES (2013, result): “We find that the adopted parameters are in accordance with the most recent observations of O-star populations (Sana et al. 2013).”
Merging black hole binaries with the SEVN code (2018, methodology): “To compute Ncor, BHB we assume that only 50 per cent of stars are binaries (Sana et al. 2013), that is fbin = 0.5.”
Re-evaluating old stellar populations (2018, methodology): “1 and earlier versions used a simple distribution of binary periods and mass ratios that was based on behaviour in high mass stellar binaries (Sana et al. 2013), but applied at all masses.”
Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, result): “The latter assumption is consistent with the observational data available so far, which show no statistically significant trends with metallicity or environment (e.g., Moe & Di Stefano 2013; Sana et al. 2013).”
Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, background): “However, Sana et al. (2013) investigated binary properties of a statistically significant number of O-type stars in the Galaxy and in the Large Magellanic Cloud.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “Multiplicity is extremely common among O- and B-type stars; binary mass exchange is believed to occur for & 70% of O-type stars and about a third of those stars will ultimately form a binary merger product (e.g., Chini et al. 2012; Sana et al. 2012, 2013; de Mink et al. 2014).”
The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “5 from Doran et al. (2013).”
The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, background): “There may also be an upper cutoff somewhere between 100 and 150 M (Elmegreen 2000; Weidner & Kroupa 2004; Figer 2005), although this possibility has been challenged by recent observations of stars that appear to exceed the proposed limit (Crowther et al. 2010; Doran et al. 2013).”