CMD 2.7 input form

A web interface dealing with stellar isochrones and their derivatives

NEW! (26jan16) VST/OMEGAM filters revised and set to ABmags.
(23sep15) A few photometric systems added.
(05may15) More NBC tables are being added and checked. A few photometric systems were recently added (like the LSST and JWST-wide filters).
(12jan15) PARSEC stellar evolutionary tracks have been extended to include very massive stars up to metallicities of Z=0.04. See Tang et al. (2014) and Chen et al. (2015) for details. The resolution and spectral properties at the massive part of the isochrones will be further improved over the next weeks.

(31oct14) Tables with PARSEC stellar evolutionary tracks are online!


Help FAQ History


Evolutionary tracksNote: 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.

Note: We are still extending these isochrones. New versions will be released every few weeks.

Warning: for the moment, PARSEC isochrones do not include the TP-AGB. We are working on this.

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

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))

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

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)

Circumstellar dustThis 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) and later tracks. The following choices refer to the RT calculations, which are applied using the scaling relations described in the paper.
Available dust compositions:
for M stars for C stars
No dust No dust
As in Bressan et al. (1998): Silicates Graphites
As in Groenewegen (2006):
100% AlOx 100% AMC
60% Silicate + 40% AlOx 85% AMC + 15% SiC
100% Silicate
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.

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 =

OutputKind 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 Sep 28 13:48:53 2017