CMD 2.2 input form

A web interface dealing with stellar isochrones and their derivatives

New! (23jan10) Kepler system added.
New! (08oct09) The WFC3 systems were rebuilt with the final WFC3 throughputs from the on-orbit SMOV4 observations (J. Kalirai, private comm.). This replaces the previously available "preliminary WFC3 system". All W and LP filters are considered.

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) (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 (2002) (superseded by Marigo et al.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 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 A_V>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 R_V=3.1.
Total extinction A_V = 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:

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 13:49:28 2017