An excess of massive stars in the local 30 Doradus starburst

  title={An excess of massive stars in the local 30 Doradus starburst},
  author={Fabian R. N. Schneider and Hugues Sana and C. J. Evans and Joachim M. Bestenlehner and Norberto Castro and Luca Fossati and G{\"o}tz Gr{\"a}fener and Norbert Langer and Oscar Hern{\'a}n Ram{\'i}rez-Agudelo and Carolina Sab{\'i}n-Sanjuli{\'a}n and Sergio Sim{\'o}n-D{\'i}az and Frank Tramper and Paul A. Crowther and Alexander de Koter and Selma E. de Mink and Philip L. Dufton and M. Garcia and Mark Gieles and Vincent H{\'e}nault-Brunet and A. Herrero and Robert G. Izzard and Venu M. Kalari and Daniel J. Lennon and Jes{\'u}s Ma{\'i}z Apell{\'a}niz and N. Markova and Francisco Najarro and Philipp Podsiadlowski and Joachim Puls and William D. Taylor and Jacco Th. van Loon and Jorick S. Vink and Colin Norman},
  pages={69 - 71}
Observing more massive stars The number of stars that form at each mass is known as the initial mass function (IMF). For most masses, the IMF follows a power-law distribution, first determined by Edwin Salpeter in 1955. Schneider et al. used observations of the nearby star-forming region 30 Doradus (also known as the Tarantula Nebula) and combined these with stellar modeling to determine its IMF. They found more stars above 30 solar masses than predicted by the Salpeter distribution. Because… 
Physics and evolution of the most massive stars in 30 Doradus
The identification of stellar-mass black-hole mergers with up to 80 Msun as powerful sources of gravitational wave radiation led to increased interest in the physics of the most massive stars. The
Testing massive star evolution, star formation history, and feedback at low metallicity
Stars that start their lives with spectral types O and early B are the progenitors of core-collapse supernovae, long gamma-ray bursts, neutron stars, and black holes. These massive stars are the
The VLT-FLAMES Tarantula Survey
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
Star Formation in the Ultraviolet
With the launch of JWST and the upcoming installation of extremely large telescopes, the first galaxies in our Universe will finally be revealed. Their light will be dominated by massive stars, which
The Spectroscopic Hertzsprung–Russell Diagram of Hot Massive Stars in the Small Magellanic Cloud
We present a comprehensive stellar atmosphere analysis of 329 O- and B-type stars in the Small Magellanic Cloud (SMC) from the RIOTS4 survey. Using spectroscopically derived effective temperature
The Impact of Binaries on the Stellar Initial Mass Function
(abridged) The stellar initial mass function (IMF) can be conveniently represented as a canonical two-part power law function and is largely invariant for star formation regions evident in the Local
Was the Milky Way a chain galaxy? Using the IGIMF theory to constrain the thin-disc star formation history and mass
The observed present-day stellar mass function (PDMF) of the solar neighborhood is a mixture of stellar populations born in star-forming events that occurred over the life-time of the thin disk of
Stellar populations dominated by massive stars in dusty starburst galaxies across cosmic time
Observations of 13CO and C18O emission for a sample of four dust-enshrouded starbursts at redshifts of approximately two to three reveal that massive stars are more numerous in starburst events than in ordinary star-forming spiral galaxies.
Star formation in the outskirts of DDO 154: a top-light IMF in a nearly dormant disc
We present optical photometry of Hubble Space Telescope (HST) ACS/WFC data of the resolved stellar populations in the outer disc of the dwarf irregular galaxy DDO 154. The photometry reveals that
VLT/X-shooter spectroscopy of massive young stellar objects in the 30 Doradus region of the Large Magellanic Cloud
The process of massive star (M ≥ 8 M⊙) formation is still poorly understood. Observations of massive young stellar objects (MYSOs) are challenging due to their rarity, short formation timescale,


Evidence for a fundamental stellar upper mass limit from clustered star formation
The observed masses of the most massive stars do not surpass about 150 M ○. . This may either be a fundamental upper mass limit which is defined by the physics of massive stars and/or their
The Origin of OB Runaway Stars
This model replicates the key characteristics of OB runaways in the authors' galaxy, and it explains the presence of runaway stars of ≳100 solar masses around young star clusters, such as R136 and Westerlund 2.
Star formation and the origin of stellar masses
SIGNIFICANT progress has been made in recent years in the imaging of star-forming regions and in the theoretical modelling of the process of star formation1, but the physical process that determines
Ages of Young Star Clusters, Massive Blue Stragglers, and the Upper Mass Limit of Stars: Analyzing Age-dependent Stellar Mass Functions
Massive stars rapidly change their masses through strong stellar winds and mass transfer in binary systems. The latter aspect is important for populations of massive stars as more than 70% of all O
Binary Interaction Dominates the Evolution of Massive Stars
More than 70% of all massive stars will exchange mass with a companion, leading to a binary merger in one-third of the cases, greatly exceed previous estimates and imply that binary interaction dominates the evolution of massive stars, with implications for populations ofmassive stars and their supernovae.
Massive stars can be efficiently ejected from their birth star clusters through encounters with other massive stars. We study how the dynamical ejection fraction of O star systems varies with the
The influence of multiple stars on the high-mass stellar initial mass function and age-dating of young massive star clusters
The study of young stellar populations has revealed that most stars are in binary or higher order multiple systems. In this study, the influence on the stellar initial mass function (IMF) of large
Stellar evolution with rotation X: Wolf-Rayet star populations at solar metallicity
We examine the properties of Wolf-Rayet (WR) stars predicted by models of rotating stars taking account of the new mass loss rates for O-type stars and WR stars (Vink et al. 2000. 2001; Nugis &
Rejuvenation of stellar mergers and the origin of magnetic fields in massive stars
Approximately 10% of massive OBA main-sequence (MS) and pre-MS stars harbour strong, large-scale magnetic fields. At the same time there is a dearth of magnetic stars in close binaries. A process
Evolution of Mass Functions of Coeval Stars through Wind Mass Loss and Binary Interactions
Accurate determinations of stellar mass functions and ages of stellar populations are crucial to much of astrophysics. We analyse the evolution of stellar mass functions of coeval main sequence stars