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

By T. Lejeune, Daniel Schaerer. 2000

451 citations recorded by the source corpus.

We have used an updated version of the empirically and semi-empirically calibrated B a S e L library of synthetic stellar spectra of Lejeune et al.([CITE], [CITE]) and Westera et al.([CITE]) to calculate synthetic photometry in the (UBV) J (RI) C JHKLL ′ M , HST-WFPC2, Geneva, and Washington systems for the entire set of non-rotating Geneva stellar evolution models covering masses from 0.4-0.8 to 120-150 $M_{\odot}$and metallicities $Z=0.0004$ (1/50 $Z_{\odot}$) to 0.1 (5 $Z_{\odot}$). The results are provided in a database which includes all individual stellar tracks and the corresponding isochrones covering ages from 10 3 yr to 16-20 Gyr in time steps of $\Delta \log t=$ 0.05 dex. The database also includes a new grid of stellar tracks of very metal-poor stars ($Z=0.0004$) from $0.8{-}150$ $M_{\odot}$ calculated with the Geneva stellar evolution code.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3b3c5535ad1a6a016a601825433347db54a2f1cd

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In Astronomy and Astrophysics

1. P. Hopkins
2. N. Smith
3. C. Conroy
4. L. Hernquist
5. Volker Springel
6. A. Benson
7. A. Helmi
8. E. Quataert

In Instrumentation

1. C. Conroy
2. A. Helmi
3. A. Benson
4. N. Smith
5. C. Baugh
6. Carlos S. Frenk
7. P. Hopkins
8. James S. Bullock

Citations in the corpus

• Isochrone ages for field dwarfs: method and application to the age–metallicity relation (2004, background): “Some of the most widely used are Girardi et al. (2000), Yi et al. (2001) and Lejeune & Schaerer (2001).”
• Pre-main-sequence isochrones - II. Revising star and planet formation time-scales (2013, methodology): “We adopted the Geneva interior models of Lejeune & Schaerer (2001), specifically the basic ‘c’ grid (Schaller et al. 1992).”
• Fitting the integrated spectral energy distributions of galaxies (2010, background): “Over the past few decades, much work has gone into providing homogeneous sets of stellar tracks from different groups, e.g. Padova (Marigo and Girardi 2007; Marigo et al. 2008), Geneva (Lejeune and Schaerer 2001), Yale (Demarque et al. 2004), MPA (Weiss and Schlattl 2008), BaSTI (Pietrinferni et al.”
• The Spitzer Survey of the Small Magellanic Cloud: S3MC Imaging and Photometry in the Mid- and Far-Infrared Wave Bands (2006, background): “…populate this feature; i.e., theoretical isochrones show a metallicity dependence on the location of the blue loop in the CMD (Girardi et al. 2000; Lejeune & Schaerer 2001), and the observations of different metallicity dwarf irregular galaxies confirm that the location of the blueloop stars…”
• Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data: Revisiting the concept of superclusters (2004, methodology): “12) and using the solarmetallicity isochrones of Lejeune & Schaerer (2001) reveals that the stars forming the HyPl group are by far not coeval (de- spite the fact that HyPl stars have a smaller age spread than the Si and He groups discussed below, especially because the HyPl group is lacking young…”
• The effects of photoionization on galaxy formation - II. Satellite galaxies in the Local Group (2001, methodology): “We use the stellar evolutionary tracks of Lejeune & Schaerer (2001) to obtain the number of stars brighter than a certain luminosity, Lc, in a single stellar population of unit mass, as a function of age and metallicity: c© 0000 RAS, MNRAS 000, 000–000 NLc(t, Z) = ∫ Mmax Mmin SLc(M, t, Z) dn dM dM,…”
• The stellar association around Gamma Velorum and its relationship with Vela OB2 (2008, methodology): “…Kroupa (2001) (ψ(M) ∝ M−2.3 for M > 0.5M⊙ and ψ(M) ∝ M−1.3 for 0.08 M/M⊙ 0.5), then we expect to see 9–14 higher mass stars with 1.8 M/M⊙ 4.4, corresponding to 7 VT 10 at the distance/extinction of the association, according to the solar metallicity models of Lejeune & Schaerer (2001).”
• DISCOVERY OF PRECURSOR LUMINOUS BLUE VARIABLE OUTBURSTS IN TWO RECENT OPTICAL TRANSIENTS: THE FITFULLY VARIABLE MISSING LINKS UGC 2773-OT AND SN 2009ip (2009, background): “The early HST detection, if this is the quiescent progenitor star, thus requires a high luminosity of at least log(L/L⊙) ≈ 5.9 (higher for a nonzero bolometric correction), and implies a high initial mass of 50–80 M⊙ (e.g., Lejeune & Schaerer 2001).”
• The Two Young Star Disks in the Central Parsec of the Galaxy: Properties, Dynamics, and Formation (2006, methodology): “Overplotted are Geneva evolutionary tracks taken from the database of Lejeune & Schaerer (2001).”
• A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS (2013, methodology): “The magnitude and color differences of A,B suggest that component B is a late B-type star, and we used △V , the effective temperature of Aa from Huang & Gies (2008), and the main sequence relations from Lejeune & Schaerer (2001) to estimate the K-band magnitude difference.”
• The Evolutionary Status of Be Stars: Results from a Photometric Study of Southern Open Clusters (2005, methodology): “In each color-magnitude diagram, the closest matching theoretical isochrone, assuming solar metallicity, from Lejeune & Schaerer (2001) is plotted as a solid line.”
• A NEW CLASS OF LUMINOUS TRANSIENTS AND A FIRST CENSUS OF THEIR MASSIVE STELLAR PROGENITORS (2008, background): “−2 (appropriate for stars with ZAMS masses above ≈ 9− 10 M⊙; Lejeune & Schaerer 2001), or (4) total number of red supergiants (RSGs) (MV .”
• A Large Stellar Evolution Database for Population Synthesis Studies. I. Scaled Solar Models and Isochrones (2004, methodology): “At 1.8 Gyr we should employ an isochrone about 1 Gyr older in order to match the Lejeune & Schaerer (2001) isochrone.”
• A Study of Cygnus OB2: Pointing the Way toward Finding Our Galaxy’s Super-Star Clusters (2003, methodology): “Using the new spectral type Teff calibration given by Martins et al., I employed the Z ¼ 0:02, high mass loss isochrones of LeJeune & Schaerer (2001) to predict total luminosity as a function of temperature for the dwarf stars.”