CMD 2.3 input form

A web interface dealing with stellar isochrones and their derivatives

New! (05mar12) A few photometric systems/filters were added recently: Pan-STARRS1, Swift/UVOT, Kepler, VISIR.

Help FAQ History

Evolutionary tracksIsochrones 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.
Use improved interpolation scheme (see FAQ).

Photometric systemNew to CMD v2.2: The original bolometric correction tables from Girardi et al. (2002) are now deprecated because based on old ATLAS9 spectra. For backward compatibility, they are still available in CMD v2.1.

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) (Note: The interpolation scheme has been slightly improved w.r.t. to the paper's Fig. 19.)

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, when necessary:

WARNING: with the latest Girardi et al. (2010) TP-AGB tracks, the maximum age for a reliable interpolation in metallicity is 13.5 Gyr, or logt=10.13. Please avoid larger ages for the moment.

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 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: Thu Sep 28 13:49:22 2017