This data server provides access to the ALHAMBRA Final Catalogue. The ALHAMBRA (Advance Large Homogeneous Area Medium Band Redshift Astronomical) survey (Moles et al. 2008) has observed 8 different regions of the sky, including sections of the COSMOS, DEEP2, ELAIS, GOODS-N, SDSS and Groth fields using a new photometric system with 20 contiguous, non-overlapping, equal width (~ 300A) filters, covering the optical range (3500A-9700A), plus the standard broadband NIR J, H and Ks filters. The observations were carried out with the Calar Alto (CAHA) 3.5m telescope using the wide field, 0.25 deg2 FOV optical camera LAICA and the NIR instrument Omega-2000. The ALHAMBRA survey dataset represents a ~700hrs of total exposure time, gathered in between the 2005 and 2012.Further information on the project can be found at the ALHAMBRA web page.
Access to the results of the unsupervised classification of all galaxy spectra in the seventh and final Sloan Digital Sky Survey data release (SDSS/DR7) as described in Sanchez Almeida et al. (2010 ApJ 714,487S). 99% of the galaxies can be assigned to only 17 major classes, with 11 additional minor classes including the remaining 1%.
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.
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.
CMC15 is an astrometric and photometric catalogue of more than 122.7 million stars in the magnitude range 9 < r' (SDSS) < 17. With a positional accuracy to about 35 mas, the catalogue covers the declination range -40deg to 50deg. The current release comprises all the observations made between March 1999 and March 2011. The catalogue fills the gap between 5h 30m and 10h 30m for declinations south of -15deg of the CMC14 and adds the bans -30deg to -40deg. Some zones north of -30deg have also been re-observed in order to improve their internal errors.
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.
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.)
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.
El Observatorio de Cielo Profundo (ObCP) de la Asociación Astronómica de Cartagena es un observatorio urbano situado en el barrio de Canteras, en Cartagena. Fruto de la colaboración de la asociación con el Ayuntamiento de Cartagena, está situado en la terraza del Centro Juvenil de Canteras.
El observatorio está equipado con un tubo Celestron C14HD y una CCD Moravian G3-11000 con rueda portafiltros, alojado en una cúpula de cuatro metros y controlado todo remotamente.
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.