B/pollux POLLUX database of synthetic stellar spectra (Palacios+ 2010-2021) ================================================================================ The POLLUX database of synthetic stellar spectra. Palacios A., Gebran M., Josselin E., Martins F., Plez B., Belmas M., Lebre A. =2010A&A...516A..13P +2021A&A...545A..67B ================================================================================ ADC_Keywords: Spectroscopy ; Models Keywords: astronomical data bases: miscellaneous - stars: general - techniques: spectroscopic Abstract: Synthetic spectra are needed to determine fundamental stellar and wind parameters of all types of stars. They are also used for the construction of theoretical spectral libraries helpful for stellar population synthesis. Therefore, a database of theoretical spectra is required to allow rapid and quantitative comparisons to spectroscopic data. We provide such a database offering an unprecedented coverage of the entire Hertzsprung-Russell diagram. We present the POLLUX database of synthetic stellar spectra. For objects with Teff<=6000K, MARCS atmosphere models are computed and the program TURBOSPECTRUM provides the synthetic spectra. ATLAS12 models are computed for stars with 7000K<=Teff<=15000K. SYNSPEC gives the corresponding spectra. Finally, the code CMFGEN provides atmosphere models for the hottest stars (Teff>25000K). Their spectra are computed with CMF_FLUX_. STAGGER 3D RHD models are computed for stars with 3900K<=Teff<=7000K. OPTIM3D gives the corresponding spectra. MARCS (from the AMBRE project, https://doi.org/10.1051/0004-6361/201219330) and ATLAS12 data consist of high resolution (R>150000) optical spectra in the range 3000 to 12000{AA} for a large variety of metallicities and chemical compositions. The CMFGEN data are high resolution (R > 150000) spectra in the optical, the UV and the IR domains and spectral energy distributions extending from the UV to near-IR ranges at solar metallicity and at the subsolar metallicities of Z=1/5Zsun and Z=1/30Zsun (https://arxiv.org/pdf/2010.13430.pdf). The OPTIM3D-STAGGER data are medium resolution (R=20000) spectra in the optical, the UV and the IR domains from 2000 to 200000{AA}. The OPTIM3D-Gaia data are very high resolution spectra (R=300000) in the Gaia-RVS spectral domain (from 8395{AA} to 8905{AA} ) (https://doi.org/10.1051/0004-6361/201732147). All the spectra cover the HR diagram at various metallicities. We propose a wide variety of synthetic spectra for various types of stars in a format that is compliant with th Virtual Observatory standards. A user-friendly web interface allows an easy selection of spectra and data retrieval. Upcoming developments will include an extension to a large range of metallicities and to the near-IR high resolution spectra, as well as a better coverage of the HR diagram, with the inclusion of models for Wolf-Rayet stars and large datasets for cool stars. The POLLUX database is accessible at http://pollux.oreme.org/ and through the Virtual Observatory. Description: A description of the data (high resolution synthetic spectra and spectral energy distributions) in the POLLUX database is presented in the form of an ascii table providing parameters that can be queried (Teff, logg, code, metallicity) and giving the filename and URL where a fits file can be retrieved. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file sed.dat 173 273 *Spectral energy distributions in the POLLUX database (version 16/03/2021) sshr.dat 173 15307 *High resolution synthetic spectra in the POLLUX database (version 16/03/2021) -------------------------------------------------------------------------------- Note on sed.dat and sshr.dat: Model atmosphere and codes for spectral synthesis used are CMFGEN/CMF_FLUX for O-type stars, ATLAS12/SYNSPEC for A and F-type stars, MARCS/TURBOSPECTRUM for G to M type stars. STAGGER/OPTIM3D spectra based of 3D RHD simulations are also provided for G to M type stars in the optical domain and in the Gaia-RVS spectral domain. -------------------------------------------------------------------------------- See also: http://pollux.oreme.org/ : POLLUX Database Home Page Byte-by-byte Description of file: sed.dat sshr.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 I6 --- Seq Internal Identification number 8-110 A103 --- Shortname Name of the data file in the database (1) 112-115 A4 --- Type Type of Data, "sed" or "spec" (1) 117-125 A9 --- Model ? Code used to compute model atmosphere 127-129 A3 --- domain Spetral domain (UV, VIS or IR) (2) 131-135 I5 K Teff [2000/66450] Effective Temperature 137-141 F5.2 [cm/s2] logg [-1/5.5]? Logarithm of the surface gravity 143-149 F7.3 km/s Vturb [0/50]? Microturbulent velocity 151-155 F5.2 [Sun] [Fe/H] [-5/1] Metallicity 157-163 F7.1 0.1nm lam.min [50/12000] Lower bound of the wavelength domain 165-173 F9.2 0.1nm lam.max [2999/200000] Upper bound of the wavelength domain -------------------------------------------------------------------------------- Note (1): The FITS file for this data can be retrieved at the url: http://pollux.graal.univ-montp2.fr/ssaserver/tsap?Id=.FITS * Files with extension ".spec" refer to high resolution synthetic spectra (R>150000). * Files with extension ".sed" refer to spectral energy distributions. (no such files any more in 15-Mar-2015 version) In both cases, the wavelength coverage is indicated by lamMin and lamMax. Note (2): Spectral domain indicated only for high resolution synthetic spectra. -------------------------------------------------------------------------------- History: * 16-Apr-2010: Original version (1040 spectra) * 06-Jun-2011: Version 2451 spectra * 15-Mar-2015: version 8134 spectra * 13-Nov-2018: new version * 24-Nov-2020: new version * 16-Mar-2021: new version Acknowledging : When using POLLUX data for scientific publication, please quote the reference Palacios A., Gebran M., Josselin E., Martins F., Plez B., Belmas M., Lèbre A., 2010, A&A 516, A13 and mention the following sentence: This research was achieved using the POLLUX database ( http://pollux.oreme.org ) operated at LUPM (Université Montpellier - CNRS, France) with the support of the PNPS and INSU. Acknowledgements: Ana Palacios, univ-montp2.fr Michele Sanguillon, univ-montp2.fr ================================================================================ (End) Ana Palacios [CNRS/UM2, France], Patricia Vannier [CDS] 24-Nov-2020