Convolution of normalized synthetic stellar spectra.
Up to 3 successive convolutions are allowed on a adjustable portion of a synthetic spectrum, in order to mimic an observable.
These convolutions acount for macroturbulence velocity, rotational velocity and instrumental profile.
Finally, the output can be Doppler-shifted in order to take into account a stellar radial velocity.
This catalogue is a simulation of the Gaia DR2 stellar content using
Galaxia (a tool to sample stars from a Besancon-like Milky Way model),
3d dust extinction maps and the latest PARSEC Isochrones. It is
mimicking the Gaia DR2 data model and an apparent magnitude limit of
g=20,7. Extinctions and photometry in different bands have also been
included in a supplementary table as well as uncertainty estimates
using a scaled nominal error model.
This catalogue is a simulation of the Gaia EDR3 stellar content using
Galaxia (a tool to sample stars from a Besancon-like Milky Way model),
3d dust extinction maps and the latest PARSEC Isochrones. It is
mimicking the Gaia DR2 data model and an apparent magnitude limit of
G=20,7. Extinctions and photometry in different bands have also been
included in a supplementary table as well as uncertainty estimates
using scaled GDR2 errors. Additional magnitude limit per HEALpix maps
are provided, based on the mode in the magnitude distribution of Gaia
DR2 data.
Fully scalable forward model grid of exoplanet transmission spectra. Considering global condensation and removal of species from the atmospheric column (rainout).
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.
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.
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.
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.
Simulated non-Gaussian temperature and polarization CMB maps. The
non-Gaussian simulations have been generated using the algorithm described in
:bibcode:`2009ApJS..184..264E` up to a multipole moment of l_max = 1024. The
transfer functions were computed with CAMB version February 2009 and RECFAST
1.5.
TheoSSA provides spectral energy distributions based on model
atmosphere calculations. Currently, we serve results obtained using
the Tübingen NLTE Model Atmosphere Package (TMAP) for hot compact
stars.
TheoSSA provides spectral energy distributions based on model
atmosphere calculations. Currently, we serve results obtained using
the Tübingen NLTE Model Atmosphere Package (TMAP) for hot compact
stars.
TMAW -- Tübingen Model Atmosphere Package WWW Interface
Short Name:
TMAW
Date:
23 Mar 2022 13:13:07
Publisher:
The GAVO DC team
Description:
The Tübingen NLTE Model-Atmosphere Package (`TMAP
<http://astro.uni-tuebingen.de/%7ETMAP/TMAP.html>`_) is a tool to calculate
stellar atmospheres in spherical or plane-parallel geometry in hydrostatic
and radiative equilibrium allowing departures from local thermodynamic
equilibrium (LTE) for the population of atomic levels./TMAP/ is based on
the so-called Accelerated Lambda Iteration (ALI) method and is able to
account for line blanketing by metals. All elements from hydrogen to nickel
may be included in the calculation with model atoms which are tailored for
the aims of the user.
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.
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.
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.
The NextGen Model grid of theoretical spectra; Gas phase only, valid for Teff > 2700 K. Updated opacities. Wavelengths have been converted to air wavelengths.
The NextGen Model grid of theoretical spectra; Gas phase only, valid for Teff > 2700 K. Updated opacities. Wavelengths have been converted to air wavelengths.
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.
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.
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.
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 (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
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.