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Available theoretical spectra models
Models: Spectra Isochrones Astroseismology
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Theoretical Models Web Server

Evolutionary Synthesis Models

POPSTAR with Chabrier IMF:
PopStar Evolutionary synthesis models. Using IMF from Chabrier (2003). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Ferrini IMF:
PopStar Evolutionary synthesis models. Using IMF from Ferrini, Penco, Palla (1990). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Kroupa IMF:
PopStar Evolutionary synthesis models. Using IMF from Kroupa (2002). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Salpeter IMF (1):
PopStar Evolutionary synthesis models. Using IMF from Salpeter (1955) with m=(0.85-120)Msun. This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Salpeter IMF (2):
PopStar Evolutionary synthesis models. Using IMF from Salpeter (1955) with m=(0.15-100)Msun. This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))