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Evolutionary tracks Isochrones are available for all 0.0001≤Z ≤0.03, and ages from 0 to 17 Gyr, in the range 0.15≤M/M ☉<100. Marigo et al. (2008) (recommended) : Girardi et al. (2000) up to early-AGB + detailed TP-AGB from Marigo & Girardi (2007) (for M ≤7M ☉) + Bertelli et al. (1994) (for M >7M ☉) + additional Z=0.0001 and Z=0.001 tracks. Basic set of Girardi et al. (2002) (superseded by Marigo et al. 2008) : Girardi et al. (2000) + simplified TP-AGB (for M ≤7M ☉) + Bertelli et al. (1994) (for M >7M ☉) + additional Z=0.0001 and Z=0.001 tracks. Use improved interpolation scheme (see FAQ ).
Photometric system Bolometric corrections are computed as in Girardi et al. (2002) . They have been updated and extended with newest ATLAS9 and C-star spectra, but only in the case of Marigo et al. (2008) tracks (see also Girardi et al. (2008) ). If you choose the "Basic set of Girardi et al. (2002) evolutionary tracks" above, you'll be using the 2002 (outdated) library. Available systems:
2MASS + Spitzer (IRAC+MIPS)
2MASS + Spitzer (IRAC+MIPS) + WISE
2MASS JHK s
UBVRIJHK (cf. Maiz-Apellaniz 2006 + Bessell 1990)
UBVRIJHKLMN (cf. Bessell 1990 + Bessell & Brett 1988)
AKARI
BATC
CFHT/Megacam u*g'r'i'z'
DCMC
DENIS
DMC 14 filters
DMC 15 filters
ESO/EIS (WFI UBVRIZ + SOFI JHK )
ESO/WFI
ESO/WFI+SOFI
ESO/WFI2
GALEX FUV+NUV (Vegamag) + Johnson's UBV
HST/ACS HRC
HST/ACS WFC
HST/NICMOS AB
HST/NICMOS ST
HST/NICMOS vega
HST/STIS imaging mode
HST/WFC3 (UVIS1+IR, final throughputs)
HST/WFC3 IR channel (final throughputs)
HST/WFC3 UVIS channel, chip 1 (final throughputs)
HST/WFC3 UVIS channel, chip 2 (final throughputs)
HST/WFPC2 (Vegamag, cf. Holtzman et al. 1995)
Kepler + SDSS griz + DDO51 (in ABmags)
OGLE-II
SDSS ugriz
SDSS ugriz + 2MASS JHK s
SDSS ugriz + UKIDSS ZYJHK
Spitzer IRAC+MIPS
Stroemgren-Crawford
Subaru/Suprime-Cam (ABmags)
Tycho V T B T
UKIDSS ZYJHK
Washington CMT1 T2
Washington CMT1 T2 + DDO51
Circumstellar dust This will only affect stars with significant mass loss, especially the red supergiants, TP-AGB, and upper-RGBs, and only in the case of Marigo et al. (2008) tracks. The following choices refer to the RT calculations, which are applyed using the scaling relations described in the paper. Interstellar extinction If AV >0, extinction coefficients will be applied on a star-to-star basis. See Girardi et al. (2008) for details. Warning: For the moment, interstellar extinction works only for isochrone tables, not for LFs or SSP integrated magnitudes.
Extinction curve: Cardelli et al. (1989) + O'Donnell (1990) with RV =3.1. Total extinction AV = mag.Initial mass function The IMF will be used to compute the stellar occupation along the isochrones, when computing integrated magnitudes, LFs, etc. IMF for single stars:
Salpeter (1955) with cutoff at 0.01 M☉
Chabrier (2001) exponential
Chabrier (2001) lognormal
Kroupa (1998) corrected for binaries
Kroupa (1998) non corrected for binaries
Ages/metallicities Choose your age and metallicity values using the approximation [M/H]=log(Z /Z ☉), with Z ☉=0.019, when necessary: Single isochrone of t = yr, and Z = Sequence of isochrones of constant metallicity, Z = , from log(t /yr) = to at steps of Δ(logt ) = Sequence of isochrones of constant age, t = , from Z = to at steps of ΔZ =
Output Kind of output: Isochrone tables Tag main evolutionary stages. Luminosity functions in the interval from to with bins mag wide SSP integrated magnitudes gzip the output file (Files above 2 Mby will always be gzipped!)
This service is mantained by Léo Girardi at the Osservatorio Astronomico di Padova . Questions, comments and special requests should be directed to leo.girardi@oapd·inaf·it . Last modified: Mon May 18 12:42:19 2009