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VESPA - VErsatile SPectral Analysis

Welcome to the VESPA database. VESPA is a code to recover star formation and metallicity histories, dust content and present-day stellar masses from galactic spectra. The algorithm is described in detail in Tojeiro et al. 2007 (MNRAS, 381, 1252).

This database is the main repository for VESPA's results. Currently it holds detailed star formation histories and other parameters for SDSS's latest data release (DR7) of the Main Galaxy Sample (MGS) and the Luminous Red Galaxies (LRG) sample. Details of the catalogue, including description, basic properties and example queries can be found in Tojeiro et al. 2009 (ApJS, 185, 1). Please cite this paper when using data from this catalogue.

Data access is currently via the freeform SQL form. Details of the tables can be found in the schema browser and in Tojeiro et al. 2009.

For questions, support and suggestions please email Rita Tojeiro at rita.tojeiro at port.ac.uk.

News

  • June 17, 2009: Important - the table GalProp had duplicate rows for runids = 3 and 8. These have now been removed.
  • June 16, 2009: We have added the option to load an user-specified list of objects into a temporary table, so that it can be cross-referenced with the VESPA database. Please look at the Freeform SQL page for details.
  • June 16, 2009: Uploaded runID = 5. This corresponds to the run with BC03 models, a one-parameter dust model, on the LRG sample.
  • June 15, 2009: You can now access SDSS' latest data-release (DR7) tables and straightforwardly cross-reference with VESPA's database. Please refer to the schema browser for details.
  • April 27, 2009: Uploaded runID = 1. This corresponds to the run with BC03 models, a one-parameter dust model, on the MGS.
  • April 16, 2009: Uploaded runID = 7. This corresponds to the run with M05 models, a one-parameter dust model, on the LRG sample.
  • April 9, 2009: Uploaded runID = 3. This corresponds to the run with M05 models, a one-parameter dust model, on the MGS.
  • April 5, 2009: Uploaded runIDS = 2, 4, 6 and 8. This corresponds to the runs with a two-parameter dust model, for both samples, and with the BC03 and M05 models



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