J/A+A/688/A197ivo://CDS.VizieR/J/A+A/688/A197doi:10.26093/cds/vizier.36880197CDSMeszaros S.Bohlin R.Allende Prieto C.Cseh B.Kovacs J.Fleming S.W.,Dencs Z.Deustua S.Gordon K.D.Hubeny I.Mezo G.Truszek M.2024-11-29T20:04:51Z2024-08-22T09:25:40ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frspectroscopyastronomical-modelsvisible-astronomyinfrared-astronomyThe modeling of stellar spectra of flux standards observed by the Hubble and James Webb space telescopes requires a large synthetic spectral library that covers a wide atmospheric parameter range. The aim of this paper is to present and describe the calculation methods behind the updated version of the BOSZ synthetic spectral database, which was originally designed to fit the CALSPEC flux standards. These new local thermodynamic equilibrium (LTE) models incorporate both MARCS and ATLAS9 model atmospheres, updated continuous opacities, and 23 new molecular line lists. The new grid was calculated with Synspec using the LTE approximation and covers metallicities [M/H] from -2.5 to 0.75dex, [{alpha}/M] from -0.25 to 0.5dex, and [C/M] from -0.75 to 0.5dex, providing spectra for 336 unique compositions. Calculations for stars between 2800 and 8000K use MARCS model atmospheres, and ATLAS9 is used between 7500 and 16000K. The new BOSZ grid includes 628620 synthetic spectra from 50nm to 32um with models for 495 Teff-logg parameter pairs per composition and per microturbulent velocity. Each spectrum has eight different resolutions spanning a range from R=500 to 50000 as well as the original resolution of the synthesis. The microturbulent velocities are 0, 1, 2, and 4km/s. The new BOSZ grid extends the temperature range to cooler temperatures compared to the original grid because the updated molecular line lists make modeling possible for cooler stars. A publicly available and consistently calculated database of model spectra is important for many astrophysical analyses, for example spectroscopic surveys and the determination of stellar elemental compositions.2024A&A...688A.197Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/688/A197CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/688/A197https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/688/A197http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/688/A197https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/688/A197https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/688/A197http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/688/A197GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/A+A/688/A197/table3Parameters of the missing MARCS modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintloggSurgace gravitylog(cm.s**-2)phys.gravityfloat[M/H]Metallicityphys.abund.Zfloat[C/M]Carbon abundancephys.abundfloat[a/M]alpha abundancephys.abundfloat