Synthetic Photometry

Synthetic Photometry Web Server

Stellar Spectra Models
AMES-Cond 2000
 The AMES-Cond Model grid of theoretical spectra. Brown dwarfs/extrasolar planets atmosphere models without irradiation and no dust opacity (no dust settling). Wavelengths have been converted to air wavelengths.
AMES-Dusty 2000
 The AMES-Dusty Model grid of theoretical spectra. Brown dwarfs/extrasolar planets atmosphere models without irradiation but including dust opacity (fully efficient dust settling). Wavelengths have been converted to air wavelengths.
Black Body
 Black Body flux. Teff from 10 to 200000 K
BT-COND
 The BT-COND Model grid of theoretical spectra. Brown dwarfs/extrasolar planets atmosphere models without irradiation and no dust opacity (no dust settling) but updated abundances. Wavelengths have been converted to air wavelengths.
BT-DUSTY
 The BT-DUSTY Model grid of theoretical spectra. Brown dwarfs/extrasolar planets atmosphere models without irradiation but including dust opacity (fully efficient dust settling) and updated abundances. Wavelengths have been converted to air wavelengths.
BT-NextGen (AGSS2009)
 The NextGen Model grid of theoretical spectra; Gas phase only, valid for Teff > 2700 K. Updated opacities. Wavelengths have been converted to air wavelengths.
BT-NextGen (GNS93)
 The NextGen Model grid of theoretical spectra; Gas phase only, valid for Teff > 2700 K. Updated opacities. Wavelengths have been converted to air wavelengths.
BT-Settl
 The BT-Settl Model grid of theoretical spectra; With a cloud model, valid across the entire parameter range. Wavelengths have been converted to air wavelengths.
BT-Settl 2014
 Testing BT-Settl grid for extreme cases. (Allard priv. communication). Wavelengths have been converted to air wavelengths.
BT-Settl-CIFIST
 The BT-Settl Model grid of theoretical spectra. With a cloud model, valid across the entire parameter range and using the Caffau et al. (2011) solar abundances. Wavelengths have been converted to air wavelengths.
Coelho Synthetic stellar library (High Resolution)
 High resolution theoretical stellar spectra covering 250 to 900nm, fully described in Coelho (2014).
Coelho Synthetic stellar library (SEDs)
 Low resolution theoretical fluxes covering 130nm to 100micron, fully described in Coelho (2014).
DRIFT-PHOENIX
 Drift-Phoenix is a computer code that simulates the structure of an atmosphere including the formation of clouds. The code is part of the Phoenix-code family. Drift describes the formation of mineral clouds and allows to predict cloud details, like the size of the cloud particles and their composition
GRAMS, C-rich grid
 GRAMS (Grid of Red supergiant and Asymptotic giant ModelS) is a grid of radiative transfer (RT) models for dust shells around red supergiant (RSG) and asymptotic giant branch (AGB) stars. This is the model grid for Carbon-rich stars
GRAMS, O-rich original grid
 GRAMS (Grid of Red supergiant and Asymptotic giant ModelS) is a grid of radiative transfer (RT) models for dust shells around red supergiant (RSG) and asymptotic giant branch (AGB) stars. This is the model grid for Oxygen-rich stars
Husfeld et al models for non-LTE Helium-rich stars
 Husfeld et al models for non-LTE Helium-rich stars
Koester
 The NextGen Model grid of theoretical spectra. Only for solar metallicity.
Kurucz ODFNEW /NOVER models
 ATLAS9 Kurucz ODFNEW /NOVER models. Newly computed ODFs with better opacities and better abundances have been used.
Morley 2012
 Morley et al. 2012 T/Y dwarf models
Morley 2014
 Morley et al. 2014 Y dwarf and exoplanet models
NextGen
 The NextGen Model grid of theoretical spectra.
NextGen (solar)
 The NextGen Model grid of theoretical spectra. Only for solar metallicity.
Saumon 2012
 Saumon et al. 2012 T dwarf models
SD Grid
 H/He NLTE spectral library introduced at the SDOB6 conference.
TLUSTY BSTAR2006
 TLUSTY BSTAR2006 Grid: Early B-type stars, Teff = 15000K - 30000 K
TLUSTY OSTAR2002
 TLUSTY OSTAR2002 Grid: O-type stars, Teff = 27500K - 55000 K
TLUSTY OSTAR2002+BSTAR2006
 TLUSTY OSTAR2002+BSTAR2006 Grid, The merged files use the BSTAR2006 models for effective temperatures up to 30,000 K and the OSTAR2002 models for higher temperatures.
TMAP
 TMAP. Hydrogen+Helium NLTE Models
TMAP (Grid 1)
 TMAP. Hydrogen+Helium NLTE Models
TMAP - Tubingen
 Tubingen NLTE Model Atmosphere Package
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.
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.
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.
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.
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.
© CAB 2008