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B/pollux POLLUX database of synthetic stellar spectra (Palacios+ 2010-2021)
The following files can be converted to FITS (extension .fit or fit.gz)
sed.dat sshrflux.dat sshrint.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=B/pollux
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drwxr-xr-x 4 cats archive 4096 Jan 19 17:30 [TAR file]
-rw-r--r-- 1 cats archive 483 May 29 2023 .message
-r--r--r-- 1 cats archive 9945 May 26 2023 ReadMe
-r--r--r-- 1 cats archive 132 May 26 2023 custom.htx
-r--r--r-- 1 cats archive 67328 May 25 2023 sed.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 205702 May 25 2023 sshrflux.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 59927 May 25 2023 sshrint.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :B/pollux POLLUX database of synthetic stellar spectra (Palacios+ 2010-2021)
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The POLLUX database of synthetic stellar spectra.
Palacios A., Gebran M., Josselin E., Martins F., Plez B., Belmas M.,
Lebre A.
<Astron. Astrophys. 516, A13 (2010); 545 A67 (2021)>
=2010A&A...516A..13P
+2021A&A...545A..67B
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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 12000AA 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 200000AA. The OPTIM3D-Gaia data are
very high resolution spectra (R=300000) in the Gaia-RVS spectral
domain (from 8395AA to 8905AA )
(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.