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.
The ESO Simple Spectral Access service provides access to the 1D reduced spectra generated either by the principal investigators of ESO observations, or by an unattended ESO processing-pipeline that makes use of certified master calibrations. The spectra are FITS files adhering to the ESO Science Data Product standard, based on the Virtual Observatory Spectral Data Model standard (v1.0 for some spectra, and v2.0 for some others, use the VOCLASS FITS keyword to discern the two).
Science spectra from the HST collection hosted at ESAC/ESA. All public HST observations in calibrated and science-ready form are synchronised with the MAST services for HST reprocessed public data and corresponding metadata. The European HST archive interface can be accessed at https://hst.esac.esa.int/ehst
The Extreme Ultraviolet Explorer (EUVE) was a NASA-funded satellite
launched in June 1992 which obtained extreme ultraviolet spectra (70 - 760 Angstroms)
of over 350 unique astronomical targets. The science payload, was designed and built
at the Space Sciences Laboratory at the University of California, Berkeley, under
the direction of Dr. Roger F. Malina. The program ended in January, 2001. These
particular spectra were extracted by Damian Christian, formerly of the EUVE project,
and reformatted by MAST staff.
The Far Ultraviolet Spectroscopic Explorer (FUSE), launched on June 24, 1999, covers the 905-1187 Å spectral region and obtains high resolution spectra of hot and cool stars, AGNs, supernova remnants, planetary nebulae, solar system objects as well as perform detailed studies of the interstellar medium. This service provides access to the FUSE spectra reprocessed using CalFUSE 3.2 and reformatted to be VO-compatible.
Spectra from the Flash and Heros Echelle spectrographs developed at
Landessternwarte Heidelberg and mounted at La Silla and various other
observatories. The data mostly contains spectra of OB stars. Heros was
the name of the instrument after Flash got a second channel in 1995.
Spectra from the Flash and Heros Echelle spectrographs developed at
Landessternwarte Heidelberg and mounted at La Silla and various other
observatories. The data mostly contains spectra of OB stars. Heros was
the name of the instrument after Flash got a second channel in 1995.
This service exposes about 0.5 million light curves of stars
classified as variable by the Gaia analysis system through the VO SSAP
protocol. The lightcurves are published per-band and are also
available through obscore.
