CMD 3.0 input form

A web interface dealing with stellar isochrones and their derivatives

NEW! (19july17) Tycho2 system replaced by Gaia+Tycho2+2MASS.
NEW! (17july17) DECAM system revised to include instrumental and atmosphere response.
(05may17) List of filters cleaned.
(18apr17) Several bugs corrected, so the probability of creating empty files is much reduced.

Help FAQ History

Evolutionary tracks

TP-AGB tracks from COLIBRI are now available.

Note: PARSEC isochrones (Bressan et al. (2012)) are computed for a scaled-solar composition and following the Y=0.2485+1.78Z relation. The solar metal content is Z☉=0.0152. They include the pre-main sequence phase. Tables of evolutionary tracks are also available.
PARSEC v1.2S + COLIBRI PR16: as in Marigo et al. (2017). PARSEC and COLIBRI tracks are the same as in the option below (see Marigo et al. (2013) and Rosenfield et al. (2016)), but the isochrones will reflect the improved code and format described in Marigo et al. (2017). You can also specify the resolution of thermal pulse cycles, ninTPC=
PARSEC version 1.2S: available for 0.0001≤Z≤0.06 (-2.2≤[M/H]≤+0.5); for 0.0001≤Z≤0.02 the mass range is 0.1≤M/M☉<350; for 0.03≤Z≤0.04 0.1≤M/M☉<150, and for Z=0.06 0.1≤M/M☉<20 (cf. Tang et al. (2014) for 0.001≤Z≤0.004, and Chen et al. (2015) for other Z). With revised and calibrated surface boundary conditions in low-mass dwarfs (Chen et al. (2014)), and a slightly improved resolution.
PARSEC version 1.1: available for 0.0001≤Z≤0.06 (-2.2≤[M/H]≤+0.5), in the range 0.1≤M/M☉<12. With revised diffusion+overshooting in low-mass stars, and improvements in interpolation scheme.
PARSEC version 1.0: available for 0.0005≤Z≤0.07 (-1.5≤[M/H]≤+0.6), in the range 0.1≤M/M☉<12.

Mass-loss on RGB using the Reimers formula with ηReimers=

Warning: mass loss works fine as long as ηReimers<0.5. Check the results for higher values.

Previous sets: The following 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) with the Girardi et al. (2010) Case A correction for low-mass, low-metallicity AGB tracks
as above but for Case B
Marigo et al. (2008) : 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) : 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.
Photometric system

Choose among the available photometric systems:
They are briefly described here.

Warning: the following options will not work for PARSEC+COLIBRI tracks, which adopt, by default, a mix between ATLAS9 ODFNEW and Aringer et al. (2016) for O-rich stars, and an updated version of Aringer et al. (2009) for C-rich stars (see details in Marigo et al. (2017)).

Sets of bolometric corrections to be applied to "normal stars":
NBC as described on Chen et al. (2014), based on PHOENIX BT-Settl for Teff<4000 K, and on ATLAS9 ODFNEW otherwise or on
OBC as described on Girardi et al. (2008), mostly based on ATLAS9 ODFNEW models (see also Marigo et al. (2008) and Girardi et al. (2002))

For Carbon stars, you can choose bolometric corrections based either on
Loidl et al. (2001) (as in Marigo et al. (2008) and Girardi et al. (2008)) or on
Aringer et al. (2009) (updated to include new spectra from Aringer et al. (2016))

Circumstellar dustThis will only affect stars with significant mass loss. In the case of Bressan et al. (1998) and Groenewegen (2006), the RT calculations are applied using the scaling relations described in Marigo et al. (2008). In the case of Nanni et al. (2016), the dust growth model is fixed for M stars, while one can choose between a few sets of optical data for C stars.
Available dust compositions:
for M stars for C stars

Using scaling relations
as in Marigo et al. (2008):
No dust No dust
Silicates as in Bressan et al. (1998) Graphites as in Bressan et al. (1998)
100% AlOx as in Groenewegen (2006) 100% AMC as in Groenewegen (2006)
60% Silicate + 40% AlOx as in Groenewegen (2006) 85% AMC + 15% SiC as in Groenewegen (2006)
100% Silicate as in Groenewegen (2006)

Warning: The following options will work only for PARSEC+COLIBRI isochrones

Using Nanni et al.'s dust growth models
(these options will change the dust model
for both M and C stars)
For M stars:
Pyroxene, olivine, quartz, periclase, iron,
with fixed optical data sets, as described in
Nanni et al. (2013), Nanni et al. (2014)
For C stars:
For the following choices of optical sets
for amorphous carbon dust
(and including SiC, iron):
Rouleau & Martin (1991) logεS=-13 (see Nanni et al. (2016))
Jaeger et al. (1998) 400K, logεS=-12 (see Nanni et al. (2016))
Rouleau & Martin (1991) logεS=-12 (see Nanni et al. (2016))
Interstellar extinctionIf 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. It also does not work for the latest PARSEC+COLIBRI isochrones.

Extinction curve: Cardelli et al. (1989) + O'Donnell (1994) with RV=3.1.
Total extinction AV = mag.
Initial mass functionThe IMF will be used to compute the stellar occupation along the isochrones, when computing integrated magnitudes, LFs, etc.
IMF for single stars:

Ages/metallicitiesChoose your age and metallicity values using the approximation [M/H]=log(Z/Z☉), with Z☉=0.019 for Marigo et al. (2008) and previous tracks,
and Z☉=0.0152 for PARSEC Bressan et al. (2012) and later tracks,

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 =


Warning: For the moment, these choices do not work for the latest PARSEC+COLIBRI isochrones. We are working on that.

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 50 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: Thu Oct 12 13:10:49 2017