The VLT-FLAMES Tarantula Survey

Evans, Christopher J.; Taylor, W. D.; Hénault-Brunet, V.; Sana, H.; Koter, A. de; Simón‐Díaz, S.; Carraro, G.; Bagnoli, T.; Bastian, N.; Bestenlehner, J. M.; Bonanos, A. Z.; Bressert, E.; Brott, I.; Campbell, M.; Cantiello, Matteo; Clark, J. S.; Costa, E.; Crowther, P. A.; Mink, S. E. de; Doran, E.; Dufton, P. L.; Dunstall, P. R.; Friedrich, Karen; García, M.; Gieles, M.; Gräfener, G.; Herrero, A.; Howarth, Ian D.; Izzard, Robert G.; Langer, N.; Lennon, D. J.; Apellániz, J. Maíz; Маркова, Н.; Najarro, F.; Puls, J.; Ramirez, O. H.; Sabín-Sanjulián, C.; Smartt, S. J.; Stroud, V. E.; Loon, Jacco Th. van; Vink, J. S.; Walborn, N. R.

doi:10.1051/0004-6361/201116782

Cited by 244 publications

(139 citation statements)

References 91 publications

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“…Its central MYSC, R136, has 1000 times the ionizing radiation of Orion (Conti et al 2008) and at least five times as many early O stars as Carina (Evans et al 2011); recent HST observations suggest that it is undergoing a merger with a slightly older cluster (Sabbi et al 2012).…”

Section: Doradus (The Tarantula Nebula)mentioning

confidence: 99%

The Massive Star-Forming Regions Omnibus X-Ray Catalog

Townsley

Broos

Garmire

et al. 2014

ApJS

150

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We present the Massive Star-forming Regions (MSFRs) Omnibus X-ray Catalog (MOXC), a compendium of X-ray point sources from Chandra/ACIS observations of a selection of MSFRs across the Galaxy, plus 30 Doradus in the Large Magellanic Cloud. MOXC consists of 20,623 X-ray point sources from 12 MSFRs with distances ranging from 1.7 kpc to 50 kpc. Additionally, we show the morphology of the unresolved X-ray emission that remains after the cataloged X-ray point sources are excised from the ACIS data, in the context of Spitzer and WISE observations that trace the bubbles, ionization fronts, and photon-dominated regions that characterize MSFRs. In previous work, we have found that this unresolved X-ray emission is dominated by hot plasma from massive star wind shocks. This diffuse X-ray emission is found in every MOXC MSFR, clearly demonstrating that massive star feedback (and the several-million-degree plasmas that it generates) is an integral component of MSFR physics.

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Section: Doradus (The Tarantula Nebula)mentioning

confidence: 99%

The Massive Star-Forming Regions Omnibus X-Ray Catalog

Townsley

Broos

Garmire

et al. 2014

ApJS

150

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“…Spectra were obtained in the Medusa-fibre mode of FLAMES using the LR02 setting of the Giraffe spectrograph (3960-4564 Å, R = 7000, e.g. Evans et al 2011). Five pairs of 1800-s exposures were obtained.…”

Section: O P T I C a L S P E C T Ro S C O P Ymentioning

confidence: 99%

“…Additionally, heliocentric correction and subtraction of a median sky spectrum were performed (for details, see e.g. Evans et al 2011). The spectra from all the exposures were then normalized and merged.…”

Section: O P T I C a L S P E C T Ro S C O P Ymentioning

confidence: 99%

Discovery of a Be/X-ray pulsar binary and associated supernova remnant in the Wing of the Small Magellanic Cloud

Hénault-Brunet

Oskinova

Guerrero

et al. 2012

Monthly Notices of the Royal Astronomical Society: Letters

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We report on a new Be/X‐ray pulsar binary located in the Wing of the Small Magellanic Cloud (SMC). The strong pulsed X‐ray source was discovered with the Chandra and XMM–Newton X‐ray observatories. The X‐ray pulse period of 1062 s is consistently determined from both Chandra and XMM–Newton observations, revealing one of the slowest rotating X‐ray pulsars known in the SMC. The optical counterpart of the X‐ray source is the emission‐line star 2dFS 3831. Its B0‐0.5(III)e+ spectral type is determined from VLT‐FLAMES and 2dF optical spectroscopy, establishing the system as a Be/X‐ray binary (Be‐XRB). The hard X‐ray spectrum is well fitted by a power law with additional thermal and blackbody components, the latter reminiscent of persistent Be‐XRBs. This system is the first evidence of a recent supernova in the low‐density surroundings of NGC 602. We detect a shell nebula around 2dFS 3831 in Hα and [O iii] images and conclude that it is most likely a supernova remnant. If it is linked to the supernova explosion that created this new X‐ray pulsar, its kinematic age of (2–4) × 104 yr provides a constraint on the age of the pulsar.

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“…have added to the classification of WN stars. Indeed, the widespread availability of high-quality spectroscopic data sets for O and WN stars -such as the Very Large Telescope Fibre Large Array Multi-Element Spectrograph (VLT-FLAMES) Tarantula Survey (Evans et al 2011) -allows us to reassess the hybrid Of/WN classification.…”

mentioning

confidence: 99%

Spectral classification of O2-3.5 If*/WN5-7 stars

Crowther¹,

Walborn²

2011

Monthly Notices of the Royal Astronomical Society

111

160

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An updated classification scheme for transition O2–3.5 If*/WN5–7 stars is presented, following recent revisions to the spectral classifications for O and WN stars. We propose that O2–3.5 If*, O2–3.5 If*/WN5–7 and WN5–7 stars may be discriminated using the morphology of Hβ to trace increasing wind density as follows: purely in absorption for O2–3.5 If* stars in addition to the usual diagnostics from Walborn et al.; P Cygni for O2–3.5 If*/WN5–7 stars; purely in emission for WN stars in addition to the usual diagnostics from Smith et al. We also discuss approximate criteria to discriminate between these subtypes from near‐infrared spectroscopy. The physical and wind properties of such stars are qualitatively discussed together with their evolutionary significance. We suggest that the majority of O2–3.5 If*/WN5–7 stars are young, very massive hydrogen‐burning stars, genuinely intermediate between O2–3.5 If* and WN5–7 subtypes, although a minority are apparently core helium‐burning stars evolving blueward towards the classical WN sequence. Finally, we reassess classifications for stars exhibiting lower ionization spectral features plus Hβ emission.

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The VLT-FLAMES Tarantula Survey

Cited by 244 publications

References 91 publications

The Massive Star-Forming Regions Omnibus X-Ray Catalog

The Massive Star-Forming Regions Omnibus X-Ray Catalog

Discovery of a Be/X-ray pulsar binary and associated supernova remnant in the Wing of the Small Magellanic Cloud

Spectral classification of O2-3.5 If*/WN5-7 stars

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