Synthetic Photometry
|Stellar Spectra Models|Evolutionary Synthesis Models|Stellar Observational Templates|

The SVO Theory Server provides synthetic photometry for 44 collections of theoretical spectra and observational templates (around 123000 spectra) and the 4363 filters in the SVO Filter Profile Service.

This is the synthetic photometry used by VOSA, for some of these collections, to analyse observed SEDs comparing them to theoretical data.

Using this web page you can search for spectra in each collection in terms of the corresponding grid parameter ranges and for a set of filters. Then you can visualize the photometry compared to the corresponding spectrum, and/or download it in ascii or VOTable format.

All these data are also available using the Virtual Observatory SSA protocol (click here for more info).

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
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.

 

Stellar Observational Templates
Bayo et al, M types from Collinder 69
Complete M spectral type sequence for a sample of confirm young sources (members of Collinder 69, ~5-20 Myr). Be aware that most spectra are not flux calibrated.
High-resolution optical library of late type subdwarfs
A high-resolution (R = 40000), flux calibrated, optical+NIR (6400-8900A) library of late type subdwarfs, from late K to M9.5, obtained with UVES at VLT. The library is described in Rajpurohit et al. (2014)
Keck LRIS spectra of late-M, L and T dwarfs
These spectra were obtained between 1997 and 1999; they are all flux calibrated and generally span the wavelength range 6000-10,000 A. Spectral types are on the Kirkpatrick et al system as defined in Kirkpatrick et al ApJS, 77, 417 (1991 - for M dwarfs) and Kirkpatrick et al ApJ 519, 802 (1999 - L dwarfs). While not all of these stars are primary spectral standards, they are all bright and should provide an adequate reference sequence.
Kesseli et al.
An empirical library of stellar spectra created using spectra from the Sloan Digital Sky Survey’s Baryon Oscillation Spectroscopic Survey (BOSS).
L and T dwarf data archive
L and T dwarf data from Chiu et al. 2006, Golimowski et al. 2004 and Knapp et al. 2004
MILES
~1000 stars spanning a large range in atmospheric parameters. The spectra were obtained at the 2.5m INT telescope and cover the range 3525-7500 Å at 2.5 Å (FWHM) spectral resolution
The NIRSPEC Brown Dwarf Spectroscopic Survey
The Brown Dwarf Spectroscopic Survey (BDSS), established in 1998 by Dr. Ian McLean in collaboration with Dr. J. Davy Kirkpatrick at IPAC, is designed to study near-infrared moderate-to-high resolution spectra for a large sample of low-mass stars and sub-stellar mass objects in the M and newly defined L and T dwarf classes.
The SpeX Prism Spectral Libraries
The SpeX Prism Spectral Libraries

 

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