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.
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.
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. Non equilibrium chemistry (weak). Valid temperature range: 200-2000K. Only for solar metallicity.
Observatoire des Sciences de l'Univers de Besancon (France)
Description:
The model of stellar population synthesis is used to elaborate a global view of the Galaxy including dynamical and evolutionary aspects. Scenarii for the formation and evolution produces theoretical distribution functions which are directly compared with survey observations of different types (photometry, kinematics, abundance distributions) The kinematical and dynamical point of view is linked to an evolution scheme through a key parameter, the stellar ages. The age distribution of stars in the solar neighbourhood is derived from a model of galactic evolution. The stellar populations of the galactic disc are selfconsistently constrained by the Boltzmann and Poisson equations through the potential of the mass model. Observational predictions are thus directly derived from an overall description of galactic structure and evolution.
The model can be used for on-line simulations of line of sights. It produces either star counts or catalogues of stars with photometric data in different systems (Johnson-Cousins, Megacam...) and kinematics (proper motions, radial velocities) according to model hypothesis.
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.
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.
40 fully hydrodynamical numerical simulations of the intergalactic gas that gives rise to the Ly-alpha forest. The available data includes simulated spectra, fields such as temperature and density, and parameter files for the simulation. Links are provided to the simulation software (Enzo). This data is made available as a web supplement to astro-ph/0412557, "A Concordance Model of the Lyman- Alpha Forest at z =1.95".
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.
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).
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
Kurucz ODFNEW /NOVER models. Newly computed ODFs with better opacities and better abundances have been used. (The convective treatment is described in Castelli et al. 1997, AA 318, 841.)
The LCA is dedicated to advancing the state-of-the-art of astrophysical simulation through the development and dissemination of community codes, and through large-scale simulations of astrophysical and cosmological systems. Our community codes include the ZEUS family of astrophysical MHD codes, and ENZO, an adaptive mesh hydrodynamic cosmological code. We also offer a new, elliptic equation, multigrid solver MGMPI. Members and collaborators of the LCA apply ZEUS and ENZO to a wide variety of fluid dynamical probelms in astrophysics and cosmology.
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.
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 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.