Base de données de spectres stellaires POLLUX


The POLLUX database of synthetic stellar spectra has been fully initiated, developed and is maintained by two CNAP astronomers of LUPM (A. Palacios & A. Lèbre) ensuring their “tâches de service” duties within this project.

POLLUX is a service of the Virtual Observatory (V.O.), and is included in the OV-GSO, the regional expert center gathering V.O. oriented services and applications from Bordeaux to Montpellier and led by Toulouse. Within OV- GSO, VOSPECFLOW, an application based on V.O. protocols that intends to make easier the direct comparison between observed stellar spectra (stored in the TBLegacy archive) and high resolution synthetic spectra (stored in POLLUX) has been fully developed by the POLLUX core team with the help of engineers of Service Informatique du LUPM (M. Sanguillon) and of IRAP (P. Maegth).


VO developments: Creation of services based on V.O. protocols and applications, e.g.,

  • “Service de Convolution” (allowing the transformation of a computed spectrum from POLLUX into a useful simulation of a stellar observation)
  • Automatic tool for the determination of accurate stellar parameters of an observed star, based on the theoretical data stored within POLLUX

Completion of the POLLUX database

  • The coverage of the colour-magnitude diagram in terms of effective temperature and gravity (+ metallicity) needs to be improved (see http://pollux.graal.univ- montp2.fr/USER%20GUIDE.pdf), and part of these missing data will be computed within the team “Astrophysique Stellaire” of LUPM.
  • To date the synthetic spectra stored in POLLUX are computed in the visible domain of the electromagnetic spectrum. Taking into account the forthcoming instrument dedicated to High resolution Infrared (IR) Spectroscopy (e.g., CRIRES+@VLT-ESO; SPIROU@CFHT, ..) the introduction of synthetic spectra computed in the IR domain has to be prepared (also within the V.O. context, with, for example, data description).

Données et valorisation

The POLLUX database offers theoretical data (high resolution synthetic spectra and spectral energy distributions), that have been computed using the best-suited codes for hot and massive stars (CMFGEN), intermediate-type stars (ATLAS) and cool stars (MARCS).

These data are accessible through a user- friendly Web interface. They are useful for both stellar physics (determination of fundamental parameters and chemical abundances, tests of model atmospheres) and galactic physics (spectral libraries for stellar population studies, preparation to Gaia).

See data


  • Agnès Lèbre (Laboratoire Univers et Particules de Montpellier)
  • Ana Palacios (Laboratoire Univers et Particules de Montpellier)

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