An excess of massive stars in the local 30 Doradus starburst

Schneider, F. R. N.; Sana, H.; Evans, C. J.; Bestenlehner, J. M.; Castro, N.; Fossati, L.; Gräfener, G.; Langer, N.; Ramírez-Agudelo, O. H.; Sabín-Sanjulián, C.; Simón‐Díaz, S.; Tramper, F.; Crowther, P. A.; Koter, A. de; Mink, S. E. de; Dufton, P. L.; García, M.; Gieles, M.; Hénault-Brunet, V.; Herrero, A.; Izzard, Robert G.; Kalari, V.; Lennon, D. J.; Apellániz, J. Maíz; Маркова, Н.; Najarro, F.; Podsiadlowski, Ph.; Puls, J.; Taylor, W. D.; Loon, Jacco Th. van; Vink, J. S.; Norman, Colin

doi:10.1126/science.aan0106

Cited by 198 publications

(109 citation statements)

References 107 publications

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“…NGC 3603 seems to have a top-heavy IMF (Pang et al 2013). It is worth noting that Schneider et al (2018) seem to find that the 30 Dor region in the LMC has an IMF with a flatter slope than the canonical Salpeter slope for stars >15 M ⊙ . It is unclear if this is 'top-heavy' or if that is actually the typical slope for high-mass stars as this is the first observation with significant numbers of very high-mass stars to construct a robust IMF at very high-masses.…”

Section: Introductionmentioning

confidence: 96%

Making top-heavy IMFs from canonical IMFs near the Galactic Centre

Park

Goodwin

Kim

2020

Monthly Notices of the Royal Astronomical Society

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We show that dynamical evolution in a strong (Galactic Centre-like) tidal field can create clusters that would appear to have very top-heavy IMFs. The tidal disruption of single star forming events can leave several bound 'clusters' spread along 20 pc of the orbit within 1-2 Myr. These surviving (sub)clusters tend to contain an over-abundance of massive stars, with low-mass stars tending to be spread along the whole 'tidal arm'. Therefore observing a cluster in a strong tidal field with a top-heavy IMF might well not mean the stars formed with a top-heavy IMF.

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Section: Introductionmentioning

confidence: 96%

Making top-heavy IMFs from canonical IMFs near the Galactic Centre

Park

Goodwin

Kim

2020

Monthly Notices of the Royal Astronomical Society

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“…Over 1170 massive stars have been included, revealing a well populated main sequence population up to ∼ 200M , plus classical Wolf-Rayet stars to the left of the main sequence, and evolved blue supergiants up to log(L/L ) ∼ 6, and cool supergiants, up to log(L/L ) ∼5.3 [56]. The addition of all luminous early-type stars from R136 and NGC 2070 fills in the extreme upper main sequence which is somewhat under populated from VFTS alone [40]. The overwhelming majority of the older massive stellar population -i.e.…”

Section: Physical Propertiesmentioning

confidence: 95%

“…As such, the Tarantula Nebula represents our best opportunity to study the highest mass stars known, both individually and collectively. Schneider et al [40] analysed VFTS spectroscopic results to establish an excess of massive stars with respect to a standard Salpeter Initial Mass Function (|MF), indicating 1/3 more stars with ≥ 30M in 30 Doradus compared to expectations from a standard IMF. Finally, although we focus primarily on high mass early-type stars in the Tarantula Nebula, it also hosts red supergiants (RSG).…”

Section: Massive Star Contentmentioning

confidence: 99%

“…7), owing to the use of inadequate wind theory for VMS [93,94]. Consequently, neither Starburst99 nor BPASS accounts for the powerful winds of very massive stars in R136, and the adopted mass function follows a Salpeter slope, rather than the top heavy IMF identified by [40] for the Tarantula region as a whole.…”

Section: Integrated Properties and Comparison With Star-forming Regiomentioning

confidence: 99%

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

Crowther

2019

Galaxies

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A review of the properties of the Tarantula Nebula (30 Doradus) in the Large Magellanic Cloud is presented, primarily from the perspective of its massive star content. The proximity of the Tarantula and its accessibility to X-ray through radio observations permit it to serve as a Rosetta Stone amongst extragalactic supergiant HII regions since one can consider both its integrated characteristics and the individual properties of individual massive stars. Recent surveys of its high mass stellar content, notably the VLT FLAMES Tarantula Survey (VFTS), are reviewed, together with VLT/MUSE observations of the central ionizing region NGC 2070 and HST/STIS spectroscopy of the young dense cluster R136, provide a near complete Hertzsprung-Russell diagram of the region, and cumulative ionizing output. Several high mass binaries are highlighted, some of which have been identified from a recent X-ray survey. Brief comparisons with the stellar content of giant HII regions in the Milky Way (NGC 3372) and Small Magellanic Cloud (NGC 346) are also made, together with Green Pea galaxies and star forming knots in high−z galaxies. Finally, the prospect of studying massive stars in metal poor galaxies is evaluated.

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“…Adopting the traditional conversion from L IR to SFR (e.g. Kennicutt & Evans 2012) -noting that recent evidence for a top-heavy stellar initial mass function in starbursts (Zhang et al 2018b;Schneider et al 2018;Motte et al 2018, cf. Romano et al 2019) would reduce these SFR limits significantly -then corresponds to a maximum 'clump SFR' of 2.6 M ⊙ yr −1 , around 1 per cent of the total for the Cosmic Eyelash, at the low end of the range of SFRs reported for clumps in star-forming galaxies at z ∼ 1-3 (e.g.…”

Section: Lens Modelingmentioning

confidence: 99%

Giant star-forming clumps?

Ivison

Richard

Biggs

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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With the spatial resolution of the Atacama Large Millimetre Array (ALMA), dusty galaxies in the distant Universe typically appear as single, compact blobs of dust emission, with a median half-light radius, ≈ 1 kpc. Occasionally, strong gravitational lensing by foreground galaxies or galaxy clusters has probed spatial scales 1-2 orders of magnitude smaller, often revealing late-stage mergers, sometimes with tantalising hints of sub-structure. One lensed galaxy in particular, the Cosmic Eyelash at z = 2.3, has been cited extensively as an example of where the interstellar medium exhibits obvious, pronounced clumps, on a spatial scale of ≈ 100 pc. Seven orders of magnitude more luminous than giant molecular clouds in the local Universe, these features are presented as circumstantial evidence that the blue clumps observed in many z ∼ 2-3 galaxies are important sites of ongoing star formation, with significant masses of gas and stars. Here, we present data from ALMA which reveal that the dust continuum of the Cosmic Eyelash is in fact smooth and can be reproduced using two Sérsic profiles with effective radii, 1.2 and 4.4 kpc, with no evidence of significant star-forming clumps down to a spatial scale of ≈ 80 pc and a star-formation rate of < 3 M ⊙ yr −1 .

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An excess of massive stars in the local 30 Doradus starburst

Cited by 198 publications

References 107 publications

Making top-heavy IMFs from canonical IMFs near the Galactic Centre

Making top-heavy IMFs from canonical IMFs near the Galactic Centre

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

Giant star-forming clumps?

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