Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

Crowther, P. A.

doi:10.3390/galaxies7040088

Cited by 44 publications

(32 citation statements)

References 109 publications

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“…2). 30 Doradus hosts a very massive cluster R136 of about 10 5 M only a few Myr old (Zinnecker and Yorke 2007) with its light dominated by very massive stars (Crowther 2019). Other, less massive clusters have been found within distances of tens of pc.…”

Section: Observational Constraintsmentioning

confidence: 99%

Star Clusters Near and Far

et al. 2020

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Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e. detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.

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Section: Observational Constraintsmentioning

confidence: 99%

Star Clusters Near and Far

et al. 2020

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“…The 30 Doradus nebula in the Large Magellanic Cloud has often been called the "Rosetta Stone" of giant extragalactic H II regions [11]. Owing to its proximity, its contents of individual stars has been studied extensively (e.g., [12]) and compared to its global properties (e.g., [13]).…”

Section: Massive Stars In Nearby Star Clusters In the Era Of Hubblementioning

confidence: 99%

“…SSC-N is at an early age; therefore, almost all stars are still on the main sequence (in the definition of stellar evolution). The inability of the models to account for the strength of the W-R feature has been found in R136 as well [11]. A plausible explanation is the lack of mixing processes in the evolution models and the subsequent failure to produce chemically enriched stars early-on.…”

Section: Zw 40-a Case Studymentioning

confidence: 99%

Massive Star Formation in the Ultraviolet Observed with the Hubble Space Telescope

Leitherer

2020

Galaxies

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Spectroscopic observations of a massive star formation in the ultraviolet and their interpretation are reviewed. After a brief historical retrospective, two well-studied resolved star clusters and the surrounding H II regions are introduced: NGC 2070 in the Large Magellanic Cloud and NGC 604 in M33. These regions serve as a training set for studies of more distant clusters, which can no longer be resolved into individual stars. Observations of recently formed star clusters and extended regions in star-forming galaxies in the nearby universe beyond the Local Group are presented. Their interpretation relies on spectral synthesis models. The successes and failures of such models are discussed, and future directions are highlighted. I present a case study of the extraordinary star cluster and giant H II region in the blue compact galaxy II Zw 40. The review concludes with a preview of two upcoming Hubble Space Telescope programs: ULLYSES, a survey of massive stars in nearby galaxies, and CLASSY, a study of massive star clusters in star-forming galaxies.

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“…The MCs are a unique laboratory for studying stellar populations, star formation, chemical evolution, among others, as their close distances allow for studies of individual stars within them. One of the hot topics regarding the MCs is the massive star population (initial masses 8 M ), since they are related to many extreme events in the Universe, for example, supernovae (SN), gravitational waves, black holes, and long gammaray bursts (Woosley et al 2002;Smartt 2009;Maeder & Meynet 2012;Massey 2013;Smith 2014;Adams et al 2017;Crowther 2019). In past decades, much progress has been made in research on massive stars from both photometry and spectroscopy (e.g., Humphreys & McElroy 1984;Massey & Olsen 2003;Levesque et al 2006;Evans et al 2011;Yang & Jiang 2011Davies et al 2013;González-Fernández et al 2015;Yang et al 2018;Neugent et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Evolved massive stars at low-metallicity

Yang

Bonanos

Jiang

et al. 2021

A&A

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We present a clean, magnitude-limited (IRAC1 or WISE1 ≤ 15.0 mag) multiwavelength source catalog for the Large Magellanic Cloud (LMC). The catalog was built by crossmatching (1″) and deblending (3″) between the source list of Spitzer Enhanced Imaging Products and Gaia Data Release 2, with strict constraints on the Gaia astrometric solution in order to remove the foreground contamination. It is estimated that about 99.5% of the targets in our catalog are most likely genuine members of the LMC. The catalog contains 197 004 targets in 52 different bands, including two ultraviolet, 21 optical, and 29 infrared bands. Additional information about radial velocities and spectral and photometric classifications were collected from the literature. We compare our sample with the sample from Gaia Collaboration (2018, A&A, 616, A12), indicating that the bright end of our sample is mostly comprised of blue helium-burning stars (BHeBs) and red HeBs with inevitable contamination of main sequence stars at the blue end. After applying modified magnitude and color cuts based on previous studies, we identified and ranked 2974 red supergiant, 508 yellow supergiant, and 4786 blue supergiant candidates in the LMC in six color-magnitude diagrams (CMDs). The comparison between the CMDs from the two catalogs of the LMC and Small Magellanic Cloud (SMC) indicates that the most distinct difference appears at the bright red end of the optical and near-infrared CMDs, where the cool evolved stars (e.g., red supergiant stars (RSGs), asymptotic giant branch stars, and red giant stars) are located, which is likely due to the effect of metallicity and star formation history. A further quantitative comparison of colors of massive star candidates in equal absolute magnitude bins suggests that there is essentially no difference for the BSG candidates, but a large discrepancy for the RSG candidates since LMC targets are redder than the SMC ones, which may be due to the combined effect of metallicity on both spectral type and mass-loss rate as well as the age effect. The effective temperatures (Teff) of massive star populations are also derived from reddening-free color of (J − KS)0. The Teff ranges are 3500 < Teff < 5000 K for an RSG population, 5000 < Teff < 8000 K for a YSG population, and Teff > 8000 K for a BSG population, with larger uncertainties toward the hotter stars.

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Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

Cited by 44 publications

References 109 publications

Star Clusters Near and Far

Star Clusters Near and Far

Massive Star Formation in the Ultraviolet Observed with the Hubble Space Telescope

Evolved massive stars at low-metallicity

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