The SVO Theory Server provides data for 70 collections of theoretical spectra and observational templates (around 285000 spectra and 668 Gb of data). Using this web page you can search for spectra in each collection in terms of the corresponding grid parameter ranges, visualize the spectra and/or download them in ascii or VOTable format. You will be able to compare spectra from different collections too. Synthetic Photometry is also available for these spectra and all the filters in the SVO Filter Profile Service. This is the synthetic photometry used by VOSA to analyse observed SEDs comparing them to theoretical data. All these collections are also available using the Virtual Observatory SSA protocol (click here for more info). Stellar Spectra Models (Stellar fluxes have been calculated on the surface of the star)| 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.
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| | 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.
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| | ATMO 2020, CEQ | | A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Equilibrium chemistry. Valid temperature range: 200-2000K. Only for solar metallicity.
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| | ATMO 2020, NEQ strong | | A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Non equilibrium chemistry (strong). Valid temperature range: 200-2000K. Only for solar metallicity.
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| | ATMO 2020, NEQ weak | | A set of atmosphere models for cool T-Y brown dwarfs and giant exoplanets. Non equilibrium chemistry (weak). Valid temperature range: 200-2000K. Only for solar metallicity.
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| | 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.
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| | 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.
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| | 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.
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| | 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.
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| | 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.
- Allard et al 2003, IAUS 211, 325
- Allard et al 2007, A&A 474L, 21
- Allard et al 2011, ASPC 448, 91A
- Allard et al 2012, RSPTA 370. 2765A
- Allard et al. 2013, MSAIS 24, 128
- Asplund et al. 2009, A&A 47, 481
- Barber et al 2006, MNRAS 368, 1087
- Star, Brown Dwarf & Planet Simulator
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| | BT-Settl (AGSS2009) | The BT-Settl Model grid of theoretical spectra; With a cloud model, valid across the entire parameter range. Using AGSS2009 abundances. Wavelengths have been converted to air wavelengths.
- Allard et al 2003, IAUS 211, 325
- Allard et al 2007, A&A 474L, 21
- Allard et al 2011, ASPC 448, 91A
- Allard et al 2012, RSPTA 370. 2765A
- Allard et al. 2013, MSAIS 24, 128
- Asplund et al. 2009, A&A 47, 481
- Barber et al 2006, MNRAS 368, 1087
- Star, Brown Dwarf & Planet Simulator
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| | 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.
- Allard et al 2003, IAUS 211, 325
- Allard et al 2007, A&A 474L, 21
- Allard et al 2011, ASPC 448, 91A
- Allard et al 2012, RSPTA 370. 2765A
- Allard et al. 2013, MSAIS 24, 128
- Barber et al 2006, MNRAS 368, 1087
- Caffau et al. 2011, SoPh 268, 255
- Star, Brown Dwarf & Planet Simulator
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| | BT-Settl (GNS93) | The BT-Settl Model grid of theoretical spectra; With a cloud model, valid across the entire parameter range. Using GNS93 abundances. Wavelengths have been converted to air wavelengths.
- Allard et al 2003, IAUS 211, 325
- Allard et al 2007, A&A 474L, 21
- Allard et al 2011, ASPC 448, 91A
- Allard et al 2012, RSPTA 370. 2765A
- Allard et al. 2013, MSAIS 24, 128
- Barber et al 2006, MNRAS 368, 1087
- Grevesse et al. 1993, A&A 271, 587
- Star, Brown Dwarf & Planet Simulator
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| | BT-Settl 2014 | | Testing BT-Settl grid for extreme cases. (Allard priv. communication). Wavelengths have been converted to air wavelengths. |
| | Black Body | | Black Body flux. Teff from 10 to 200000 K |
| | | | 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
- Baron et al. 2003, IAU 210, 19
- Hauschildt & Baron 1999, JCoAM 109, 41
- Helling C., Woitke P., 2006, A&A, 455, 325
- Helling et al. 2008, A&A, 485, 547
- Helling et al. 2008, ApJL, 675, L105
- Witte et al. 2009, A&A, 506, 1367
- Witte et al. 2011, A&A, 529, A44
- Woitke P., Helling C., 2003, A&A, 399, 297
- Woitke P., Helling C., 2004, A&A, 414, 335
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| | 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
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| | 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
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| | Granada HRES Library | | A High-Resolution Stellar Library for Evolutionary Population Synthesis at 0.3 A
resolution from 3000 to 7000 A based in PHOENIX, ATLAS9 and TLUSTY models
and optimized for Evolutionary Population Synthesis codes as described in Martins et al. (2005)
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| | | Koester WD models | | These models are for white dwarfs of spectral type DA with pure hydrogen atmospheres. They use LTE (local thermodynamic equilibrium), hydrostatic equilibrium and plane-parallel, one-dimensional structure. Basic methods and data are described in Koester (2010, Mem.S.A.It. Vol. 81, 921). Since then many improvements were implemented, most notably the hydrogen Stark profiles by Tremblay & Bergeron (2009, ApJ 696,1755), and Tremblay (2015, priv. comm). Original models have been transformed to air wavelengths and rescaled to 4π*Eddington flux in erg/cm2/s/A
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| | Kurucz ODFNEW /NOVER (2003) | | ATLAS9 Kurucz ODFNEW /NOVER models. Newly computed ODFs with better opacities and better abundances have been used.
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| | Kurucz ODFNEW /NOVER models | | ATLAS9 Kurucz ODFNEW /NOVER models. Newly computed ODFs with better opacities and better abundances have been used.
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| | | | Levenhagen 2017 | | A grid of LTE and non-LTE synthetic spectra of hot DA white dwarfs. It covers Teff from 17,000 K to 100,000 K and log(g) from 7.0 to 9.5. The stellar models are built for pure hydrogen and the spectra cover a wavelength range from 90 nm to 2.5 micron.
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| | | Morley 2014 | | Morley et al. 2014 Y dwarf and exoplanet models
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| | NextGen | The NextGen Model grid of theoretical spectra.
- Allard et al 1997, ARA&A 35, 137
- Baraffe et al 1997, A&A 327, 1054
- Baraffe et al 1998, A&A 337, 403B
- Grevesse et al. 1993, A&A 271, 587
- Hauschildt et al 1999, ApJ 512, 377
- Schryber, Miller & Tennyson 1995
- Star, Brown Dwarf & Planet Simulator
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| | NextGen (solar) | The NextGen Model grid of theoretical spectra. Only for solar metallicity.
- Allard et al 1997, ARA&A 35, 137
- Baraffe et al 1997, A&A 327, 1054
- Baraffe et al 1998, A&A 337, 403B
- Grevesse et al. 1993, A&A 271, 587
- Hauschildt et al 1999, ApJ 512, 377
- Schryber, Miller & Tennyson 1995
- Star, Brown Dwarf & Planet Simulator
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| | Pacheco et al 2021 | | A Grid of Synthetic Spectra for Subdwarfs: NLTE line-blanketed atmosphere models
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| | | TLUSTY BSTAR2006 | TLUSTY BSTAR2006 Grid: Early B-type stars, Teff = 15000K - 30000 K
- Hubeny, I., Lanz, T. 1995, ApJ, 439, 875H
- Lanz, T., Hubeny, I. 2007, ApJS, 169, 83
- TLusty web page
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| | TLUSTY OSTAR2002 | TLUSTY OSTAR2002 Grid: O-type stars, Teff = 27500K - 55000 K
- Hubeny, I., Lanz, T. 1995, ApJ, 439, 875H
- Lanz, T., Hubeny, I. 2003, ApJS, 146, 417
- TLusty web page
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| | 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.
- Hubeny, I., Lanz, T. 1995, ApJ, 439, 875H
- Lanz, T., Hubeny, I. 2003, ApJS, 146, 417
- Lanz, T., Hubeny, I. 2007, ApJS, 169, 83
- TLusty web page
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| | TMAP | | TMAP. Hydrogen+Helium NLTE Models
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| | | TMAP (Grid 2) | | Tubingen NLTE Model Atmosphere Package. Grid for H=1, λmax ~ 4e5 A. 20.000 K < Teff < 150.000 K
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| | TMAP (Grid 3) | | Tubingen NLTE Model Atmosphere Package. Grid for H+He=1, λmax ~ 5e4 A. 50.000 K < Teff < 190.000 K
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| | TMAP (Grid 4) | | Tubingen NLTE Model Atmosphere Package. Grid for H+He=1, ~5 A < λ < ~3 106A. 20.000 K < Teff < 150.000 K
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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.
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| | 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.
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| | 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.
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| | 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.
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| | 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.
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| | SED@ | | Sed@ Evolutionary Sinthesis models results (Cervińo & Luridiana 2006) using
Granada HRES Library and presented in González-Delgado et al. 2005.
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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.
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| | 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.
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| | Kesseli et al. | | An empirical library of stellar spectra created using spectra from the Sloan Digital Sky
Survey’s Baryon Oscillation Spectroscopic Survey (BOSS).
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| | | 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 Ĺ at 2.5 Ĺ (FWHM) spectral resolution
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| | MUSE 1d Spectral Library | | MUSE Spectral Library (MSL), consisting of 35 high-quality spectra of stars covering the Hertzsprung–Russell diagram, and verified the continuum shape of our spectra with synthetic broadband colours.
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| | STELIB | | The objective of the STELIB Stellar Library is to build an homogeneous library of stellar spectra in the visible range (3200 to 9500A), including stars of all spectral types, luminosity classes and metallicity that can be observed from the ground with the current instrumentation.
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| | 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.
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| | | UVES/VLT | | 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)
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Planetary Models | Exogan | | Exogan. Atmospheric Library of Far Away Worlds |
| | Goyal local | | Fully scalable forward model grid of exoplanet transmission spectra. Considering local condensation only.
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| | Goyal rainout | | Fully scalable forward model grid of exoplanet transmission spectra. Considering global condensation and removal of species from the atmospheric column (rainout).
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| | | | Morley2015 Cloudy | | Cloudy models of GJ 1214b “analogs” from Morley et al. 2015. Emission spectra.
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| | | Morley2015 Haze (Soot) | | Hazed (Soot flavour) models of GJ 1214b “analogs” from Morley et al. 2015. Emission spectra.
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