Infrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds

Keller, Stefan

doi:10.1086/300991

Cited by 22 publications

(22 citation statements)

References 23 publications

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“…The plots show that NGC 458 brightest stars have masses between 4 and 5 M and effective temperatures log(T eff ) between 3.65 and 3.9. The main source of errors here is the uncertainty of the reddening determination and the typical error bars are shown on panel c. Keller (1999) determined for the "blue loop" stars of NGC 458 lower temperatures and much higher luminosities. One possible explanation is that Keller used rather old B, V photometry of Arp (1959) instead of JK photometry.…”

Section: Evolved Starsmentioning

confidence: 98%

The Small Magellanic Cloud star cluster NGC 458. A new UBVI photometric study

Alcaino¹,

Alvarado²,

Borissova³

et al. 2003

A&A

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Abstract. We present a new photometry of the Small Magellanic Cloud star cluster NGC 458 in UBVI filters. We determine the reddening E(B − V) = 0.04 ± 0.02. By comparison with the isochrones by Bertelli et al. (1994) we derive an age of ≈140 Myr. Three candidate blue straggler stars are proposed. The evolved "blue loop" stars of NGC 458 have masses between 4 and 5 M and are hotter than model predictions.

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Section: Evolved Starsmentioning

confidence: 98%

The Small Magellanic Cloud star cluster NGC 458. A new UBVI photometric study

Alcaino¹,

Alvarado²,

Borissova³

et al. 2003

A&A

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“…They estimated the mass M 13 M and the stellar radius R 171 R for the red star; the companion would have M = 1 M . From broadband IR photometry, Keller (1999) showed that the star is a red supergiant with T eff ∼ 4355 K and log(L/L ) = 3.971.…”

Section: A3 Smc5_2807mentioning

confidence: 99%

Be stars and binaries in the field of the SMC open cluster NGC 330 with VLT-FLAMES

Martayan

Floquet

Hubert

et al. 2007

A&A

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Aims. Observations of hot stars belonging to the young cluster SMC-NGC 330 and its surrounding region were obtained with the VLT-GIRAFFE facilities in MEDUSA mode. We investigated the B and Be star properties and proportions in this environment of low metallicity. We also searched for rapid variability in Be stars using photometric databases. Methods. Using spectroscopic measurements, we characterized the emission and properties of Be stars. By cross-correlation with photometric databases such as MACHO and OGLE, we searched for binaries in our sample of hot stars, as well as for short-term variability in Be stars. Results. We report on the global characteristics of the Be star sample (131 objects). We find that the proportion of early Be stars with a large equivalent width of the Hα emission line is higher in the SMC than in the LMC and MW. We find a slight increase in the proportion of Be stars compared to B-type stars with decreasing metallicity. We also discovered spectroscopic and photometric binaries, and for the latter we give their orbital period. We identify 13 Be stars with short-term variability. We determine their period(s) and find that 9 Be stars are multiperiodic.

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“…Both observations and evolutionary models (see, e.g., Keller 1999;Origlia et al 1999;Origlia 2003 and references therein) suggest that RSGs of ages between $6 and 100 Myr and metallicities between 1/10 solar and solar are characterized by low gravities (log g < 1:0), low temperatures ( 4000 K), and relatively high microturbulence velocity ( ! 3 km s À1 ).…”

Section: Ir Spectra and Stellar Abundancesmentioning

confidence: 99%

Stellar and Gaseous Abundances in M82

Origlia

Ranalli

Comastri

et al. 2004

ApJ

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The near-infrared (near-IR) absorption spectra of starburst galaxies show several atomic and molecular lines from red supergiants that can be used to infer reliable stellar abundances. The metals locked in stars give a picture of the galaxy metallicity prior to the last burst of star formation. The enrichment of the new generation of stars born in the last burst can be traced by measuring the hot gas in the X-rays. For the first time, detailed stellar abundances in the nuclear region of the starburst galaxy M82 have been obtained. They are compared with those of the hot gas, as derived from an accurate reanalysis of the XMM-Newton and Chandra nuclear X-ray spectra. The cool stars and the hot gas suggest Fe=H ½ ¼À0:35 AE 0:2 dex and an overall [Si / Fe] and [Mg / Fe] enhancement by $0.4 and 0.5 dex, respectively. This is consistent with a major chemical enrichment by Type II supernova explosions in recursive bursts on short timescales. Oxygen is more puzzling to interpret, since it is enhanced by $0.3 dex in stars and depleted by $0.2 dex in the hot gas. None of the standard enrichment scenarios can fully explain such a behavior compared with that of the other -elements.

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Infrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds

Cited by 22 publications

References 23 publications

The Small Magellanic Cloud star cluster NGC 458. A new UBVI photometric study

The Small Magellanic Cloud star cluster NGC 458. A new UBVI photometric study

Be stars and binaries in the field of the SMC open cluster NGC 330 with VLT-FLAMES

Stellar and Gaseous Abundances in M82

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