Database of Geneva stellar evolution tracks and isochrones for (UBV)$_{\mathsf{J}}$(RI)$_{\mathsf{C}}$ JHKLL'M, HST-WFPC2, Geneva and Washington photometric systems

Lejeune, T.

doi:10.1051/0004-6361:20000214

Cited by 519 publications

(798 citation statements)

References 29 publications

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“…In Figure B1 we plot Lejeune & Schaerer (2001) isochrones along with the positions of the 8 brightest O-stars in Pi 24. We take photometry and spectral types for these O-stars from Massey et al (2001a) except for Pi 24-1, which has since been resolved into two components, Pi 24-1 NE and Pi 24-1 SW (Maíz Apellániz et al 2007), with an optical/near ultraviolet ∆m ∼ 0.1.…”

Section: B01 Pismis 24 and Wr 93mentioning

confidence: 99%

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Rosslowe

Crowther

2015

Monthly Notices of the Royal Astronomical Society

128

143

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We construct revised near-infrared absolute magnitude calibrations for 126 Galactic Wolf-Rayet (WR) stars at known distances, based in part upon recent large scale spectroscopic surveys. Application to 246 WR stars located in the field, permits us to map their Galactic distribution. As anticipated, WR stars generally lie in the thin disk (∼40 pc half width at half maximum) between Galactocentric radii 3.5-10 kpc, in accordance with other star formation tracers. We highlight 12 WR stars located at vertical distances of 300 pc from the midplane. Analysis of the radial variation in WR subtypes exposes a ubiquitously higher N W C /N W N ratio than predicted by stellar evolutionary models accounting for stellar rotation. Models for non-rotating stars or accounting for close binary evolution are more consistent with observations. We consolidate information acquired about the known WR content of the Milky Way to build a simple model of the complete population. We derive observable quantities over a range of wavelengths, allowing us to estimate a total number of 1200 +300 −100 Galactic WR stars, implying an average duration of ∼ 0.25 Myr for the WR phase at the current Milky Way star formation rate. Of relevance to future spectroscopic surveys, we use this model WR population to predict follow-up spectroscopy to K S ≃ 13 mag will be necessary to identify 95% of Galactic WR stars. We anticipate that ESA's Gaia mission will make few additional WR star discoveries via low-resolution spectroscopy, though will significantly refine existing distance determinations. Appendix A provides a complete inventory of 322 Galactic WR stars discovered since the VIIth catalogue (313 including Annex), including a revised nomenclature scheme.

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Section: B01 Pismis 24 and Wr 93mentioning

confidence: 99%

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Rosslowe

Crowther

2015

Monthly Notices of the Royal Astronomical Society

128

143

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“…Another di †erence, which is not clearly seen from the isochrones but has important consequences for the FIG. 16.ÈComparison of solar-metallicity isochrones from the Padua group (Girardi et al 2000) and Geneva group (Lejeune & Schaerer 2001). The Geneva isochrones produce cooler and fainter RSGs for a given age.…”

Section: Uncertaintiesmentioning

confidence: 98%

“…In Figure 16 we compare solar-metallicity isochrones from the two groups for three di †erent ages (8,13,and 40 Myr), showing the Padua isochrones with solid lines and Geneva isochrones with dashed lines. As recommended by Lejeune & Schaerer (2001), we have used their "" extended ÏÏ grids, which incorporate high mass-loss rates for the most massive stars. One shortcoming of the Geneva models is that they do not list colors and magnitudes for Wolf-Rayet stars, because of the lack of accurate atmosphere models for these stars.…”

Section: Uncertaintiesmentioning

confidence: 99%

Hubble Space Telescope Imaging of a Peculiar Stellar Complex in NGC 6946*

Larsen¹,

Efremov²,

Elmegreen³

et al. 2002

ApJ

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The stellar populations in a stellar complex in NGC 6946 are analyzed on images taken with the Wide Field Planetary Camera 2 on board the Hubble Space T elescope. The complex is peculiar because of its very high density of stars and clusters and semicircular shape. Its physical dimensions are about the same as for the local Gould Belt, but the stellar density is 1È2 orders of magnitude higher. In addition to an extremely luminous, D15 Myr old cluster discussed in an earlier paper, accounting for about 17% of the integrated V -band light, we identify 18 stellar clusters within the complex with luminosities similar to the brightest open clusters in the Milky Way. The color-magnitude diagram of individual stars in the complex shows a paucity of red supergiants compared to model predictions in the 10È20 Myr age range for a uniform star formation rate. We thus Ðnd tentative evidence for a gap in the dispersed star formation history, with a concentration of star formation into a young globular cluster during this gap. ConÐrmation of this result must, however, await a better understanding of the late evolution of stars in the corresponding mass range A reddening map based on individual reddenings for 373 early-(Z12 M _ ). type stars is presented, showing signiÐcant variations in the absorption across the complex. These may be responsible for some of the arclike structures previously identiÐed on ground-based images. We Ðnally discuss various formation scenarios for the complex and the star clusters within it.

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“…The comparison has been mainly performed with the Geneva models of Lejeune & Schaerer (2001), with solar metallicity. Other models have been considered (Claret 2004) without any major differences to the derived conclusions.…”

Section: Comparison With Stellar Evolutionary Modelsmentioning

confidence: 99%

“…This is probably the major source of systematic errors. In order to transform the derived temperatures and gravities to surface fluxes, the synthetic spectra are convolved with filter responses and are converted to absolute magnitudes and colors using a series of calibrations (see Lejeune & Schaerer 2001, for a description of the transformations applied). The accuracy of these transformations is usually defined within a few hundredths of magnitude (see Bessell et al 1998, for various determinations of the bolometric corrections for the Sun and the colors of Vega, and Flower 1996, for the dispersion on the bolometric correction for hot stars).…”

Section: The Distance To M 31mentioning

confidence: 99%

The distance to the Andromeda galaxy from eclipsing binaries

Vilardell¹,

Ribas²,

Jordi³

et al. 2010

A&A

112

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The cosmic distance scale largely depends on distance determinations to galaxies of the Local Group. In this sense, the Andromeda galaxy (M 31) is a key rung to better constrain the cosmic distance ladder. A project was started in 1999 to firmly establish a direct and accurate distance to M 31 using eclipsing binaries (EBs). After the determination of the first direct distance to M 31 from EBs, the second direct distance to an EB system is presented: M31V J00443610+4129194. Light and radial velocity curves were obtained and fitted to derive the masses and radii of the components. The acquired spectra were combined and disentangled to determine the temperature of the components. The analysis of the studied EB resulted in a distance determination to M 31 of (m − M) 0 = 24.30 ± 0.11 mag. This result, when combined with the previous distance determination to M 31, results in a distance modulus of (m − M) 0 = 24.36 ± 0.08 mag (744 ± 33 kpc), fully compatible with other distance determinations to M 31. With an error of only 4%, the obtained value firmly establishes the distance to this important galaxy and represents the fulfillment of the main goal of our project.

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Database of Geneva stellar evolution tracks and isochrones for (UBV)$_{\mathsf{J}}$(RI)$_{\mathsf{C}}$ JHKLL'M, HST-WFPC2, Geneva and Washington photometric systems

Cited by 519 publications

References 29 publications

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Hubble Space Telescope Imaging of a Peculiar Stellar Complex in NGC 6946*

The distance to the Andromeda galaxy from eclipsing binaries

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