The description of Pogginati's (1997) models is given at the end of this page. Despite they are not opened at this server, we stored them in this data base. In future, we plan to use them if they will be developed.
We use from this model a wide collection of SED curves from the range of ages between 7x106 and 19x109 years for massive elliptical galaxies.
In 2001, a new improved version PEGASE.2 by Damien Le Borgne and Brigitte Rocca-Volmerange, 2001, ( astro-ph/0202359 ) was appeared. It has a corresponding server, allowing a user to operate with simulated data. We plan to use these new models of standard galaxy types too when estimation of parameters.
The library of synthetic spectra of E-galaxies is formed with the following parameters of star formation rate (SFR): simple stellar population, burst of star formation lasting is 1 billion years, exponential decreasing of SFR (mu-model), solar metallicity. Initial mass function (IMF) with an upper limit of 125 Msun is taken from Miller and Scalo (1979), and as BMP shown in comparison with other IMFs, photometric $z$ estimations are approximately the same for different IMF choice . The model tracks cover the wavelength range from 220 up to 95800 Angstrom, but the default range is specified by redshifts in limits of z from 0 up to 6.
(Homepage of the GISSEL model).
Files can be found here.
The input data are: a photometric catalogue, containing magnitudes and photometric errors, and the corresponding set of filter responses (+ detector if needed). The output data are chosen by the user: best phot, observed SEDs (mean fluxes and errors), best-fit integrated SEDs and spectra, minimum chi2 versus z and possible secondary solutions. The present library of templates has been obtained from the GISSEL98 code (see details in section 4), solar metallicity (new corrected tracks), and Miller and Scalo IMF (toul_62_mi_sc_ssp), plus 4 templates taken from Coleman, Wu and Weedman (1980) and extended in the UV and IR regions with the GISSEL spectra corresponding to the same spectral type. This set of templates can be changed by the user; some specific SEDs should be available in the next version.
This model is based on the calculations including stellar component emission from Barabaro and Olivi (1991), which synthesize SED for galaxies in the spectral range from 1000 up to 10000 Angstrom and includes besides the helium burning phase phases of AGB and post-AGB stellar evolution. The model takes into account chemical evolution in galaxy, therefore, a contribution of different metallicity stellar population to the integral spectrum too. Using model of stellar atmospheres (Kurutz, 1992) Poggianti calculates a spectrum up to 25 000 Angstrom. The Kurutz's model of stars with Teff>5500K is used for the IR range, and observed stellar spectrum library for low effective temperatures (Lancon and Rocca-Volmerange, 1992).
We use SED templates of this model, calculated for elliptical galaxies for various ages of 2.2, 3.4, 4.3, 5.9, 7.4, 8.7, 10.6, 13,2 and 15 x109 years.
Barabaro S., Olivi F.M., 1991, AJ, 101, 922
Bruzual G., Charlot S. 1993, ApJ, 405, 538
Bruzual G., Charlot S. 1996,
Bolzonella M., Miralles J.-M., Pello R. 2000. Astron. Astroph.,
Coleman D.J., Wu C.C., Weedman D.W., 1980, ApJ, 43, 393
Fioc M., Rocca-Volmerange B, 1997, AA, 326, 950
Kurutz R., 1992, in ``The stellar population of Galaxies'',
IAU Symp. No 149, ed. Barbuy B.,Penzini A., Kluwer, Dordrecht,
Lancon A., Rocca-Volmerange B., 1992, AAS, 96, 593.
Miller G.E., Scalo J.M. 1979, ApJS, 41, 513
Poggianti B.M., 1997, AA, 122, 399
Rocca-Volmerange B., Guiderdoni B., 1988, AAS, 75, 93