The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds

Massey, Philip; Waterhouse, Elizabeth; DeGioia-Eastwood, K.

doi:10.1086/301345

Cited by 157 publications

(193 citation statements)

References 94 publications

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“…Massey 1998;Massey et al 2000). The selection criteria of our method for the detection of young loose stellar systems in the LMC were based on this coevality concerning their MF slopes and stellar content.…”

Section: Discussionmentioning

confidence: 99%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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Abstract. The method developed by Gouliermis et al. (2000, Paper I), for the detection and classification of stellar systems in the LMC, was used for the identification of stellar associations and open clusters in the central area of the LMC. This method was applied on the stellar catalog produced from a scanned 1.2 m UK Schmidt Telescope Plate in U with a field of view almost 6.• 5 × 6.• 5, centered on the Bar of this galaxy. The survey of the identified systems is presented here followed by the results of the investigation on their spatial distribution and their structural parameters, as were estimated according to our proposed methodology in Paper I. The detected open clusters and stellar associations show to form large filamentary structures, which are often connected with the loci of HI shells. The derived mean size of the stellar associations in this survey was found to agree with the average size found previously by other authors, for stellar associations in different galaxies. This common size of about 80 pc might represent a universal scale for the star formation process, whereas the parameter correlations of the detected loose systems support the distinction between open clusters and stellar associations.

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Section: Discussionmentioning

confidence: 99%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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“…Intrinsic colors were calculated from Q, thanks to its univocal relation with spectral type (hence (B − V) 0 ) that holds for the early-type stars. This relation was parameterized for lowmetallicity stars by Massey et al (2000):…”

Section: Variable Extinction and Extinction Mapmentioning

confidence: 99%

The young stellar population of IC 1613

García¹,

Herrero

Vicente³

et al. 2009

A&A

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Context. Determining the parameters of massive stars is crucial to understand many processes in galaxies and the Universe, since these objects are important sources of ionization, chemical enrichment and momentum. 10m class telescopes enable us to perform detailed quantitative spectroscopic analyses of massive stars in other galaxies, sampling areas of different metallicity. Relating the stars to their environment is crucial to understand the physical processes ruling their formation and evolution. Aims. In preparation for the new instrumentation planned for the Gran Telescopio CANARIAS (GTC), our goal is to build a list of massive star candidates in the metal-poor irregular galaxy IC 1613. The catalogue must have very high astrometric accuracy, suitable for the current generation of multi-object spectrographs. A census of OB associations in this galaxy is also needed, to provide important additional information about the age and environment of the candidate OB stars. Methods. From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friendsof-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context. Results. We have produced a deep catalogue of targets in IC 1613 that covers a large field of view. To achieve high astrometric accuracy, a new astrometric procedure was developed for the INT-WFC data. We also built a catalogue of OB associations in IC 1613 and found that they concentrate in the central regions, especially in the H ii bubbles. The study of extinction confirms that it is patchy, with local values of color-excess above the foreground value.

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“…limit of the mass of a star at the start of the main sequence (MS) in the Galaxy that can become WR stars (Meynet & Maeder 2005;Massey et al 2000). However, it is not clear whether the low ejecta mass is due to heavy mass loss of a single massive star that was on its way, or just entered the WR phase, or whether mass loss was induced by a common envelope phase in a binary system (Young et al 2006).…”

Section: Send Offprint Requests To: B Van Veelenmentioning

confidence: 99%

The hydrodynamics of the supernova remnant Cassiopeia A

Veelen

Langer

Vink

et al. 2009

A&A

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Aims. There are large differences in the proposed progenitor models for the Cas A SNR. One of these differences is the presence or absence of a Wolf-Rayet (WR) phase of the progenitor star. The mass loss history of the progenitor star strongly affects the shape of the Supernova remnant (SNR). In this paper we investigate whether the progenitor star of Cas A had a WR phase or not and how long it may have lasted.Methods. We performed two-dimensional multi-species hydrodynamical simulations of the CSM around the progenitor star for several WR life times, each followed by the interaction of the supernova ejecta with the CSM. We then looked at the influence of the length of the WR phase and compared the results of the simulations with the observations of Cas A. Results. The difference in the structure of the CSM, for models with different WR life times, has a strong impact on the resulting SNR. With an increasing WR life time the reverse shock velocity of the SNR decreases and the range of observed velocities in the shocked material increases. Furthermore, if a WR phase occurs, the remainders of the WR shell will be visible in the resulting SNR. Conclusions. Comparing our results with the observations suggests that the progenitor star of Cas A did not have a WR phase. We also find that the quasi-stationary flocculi (QSF) in Cas A are not consistent with the clumps from a WR shell that have been shocked and accelerated by the interaction with the SN ejecta. We can also conclude that for a SN explosion taking place in a CSM that is shaped by the wind during a short (≤ 15000 yr) WR phase, the clumps from the WR shell will be visible inside the SNR.

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The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds

Cited by 157 publications

References 94 publications

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

The young stellar population of IC 1613

The hydrodynamics of the supernova remnant Cassiopeia A

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