J/ApJS/214/25ivo://CDS.VizieR/J/ApJS/214/25doi:10.26093/cds/vizier.22140025CDSFreedman R.S.Lustig-Yaeger J.Fortney J.J.Lupu R.E.Marley M.S.,Lodders K.2017-06-19T07:57:17Z2014-10-24T10:05:55ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmosphereschemical-abundancesWe present new calculations of Rosseland and Planck gaseous mean opacities relevant to the atmospheres of giant planets and ultracool dwarfs. Such calculations are used in modeling the atmospheres, interiors, formation, and evolution of these objects. Our calculations are an expansion of those presented in Freedman (2008ApJS..174..504F) to include lower pressures, finer temperature resolution, and also the higher metallicities most relevant for giant planet atmospheres. Calculations span 1{mu}bar to 300bar, and 75-4000K, in a nearly square grid. Opacities at metallicities from solar to 50 times solar abundances are calculated. We also provide an analytic fit to the Rosseland mean opacities over the grid in pressure, temperature, and metallicity. In addition to computing mean opacities at these local temperatures, we also calculate them with weighting functions up to 7000K, to simulate the mean opacities for incident stellar intensities, rather than locally thermally emitted intensities. The chemical equilibrium calculations account for the settling of condensates in a gravitational field and are applicable to cloud-free giant planet and ultracool dwarf atmospheres, but not circumstellar disks. We provide our extensive opacity tables for public use.2014ApJS..214...25Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/214/25CatalogResearchIsServedByTAP VizieR generic servicerelated-toVI/133 : A variationally computed hot NH3 line list - BYTe (Yurchenko+, 2011)J/A+A/562/A133 : Analytical model for atmospheres (Parmentier+, 2014)J/MNRAS/440/1649 : ExoMol line lists for CH4 (Yurchenko+, 2014)J/ApJS/210/21 : Refractive indices of grain materials (Cuzzi+, 2014)J/A+A/494/403 : Low temperature Rosseland opacities (Lederer+, 2009)J/ApJ/382/636 : Rosseland mean free-free Gaunt factor (Itoh+ 1991)http://www.cfa.harvard.edu/hitran/updates.html : HITRAN databasehttp://ether.ipsl.jussieu.fr/etherTypo/?id=950 : GEISA databasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/214/25https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/214/25http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/214/25https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/214/25https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/214/25http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/214/25GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJS/214/25/opacityMean opacities ({kappa}_R_, {kappa}_P_) for atmosphere metallicities [M/H] of 0.0, 0.5, 0.7, 1.0, 1.5, and 1.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[M/H]Metallicity of the atmosphere (0.0, 0.5, 0.7, 1.0, 1.5, or 1.7)log(Sun)phys.abundintnullableT[75/4000] Gas local temperature (planet)Kphys.temperature;pos.lg;pos.lsrintP[1/3e+08] Gas pressure (dyne/cm^2^=dPa={mu}bar)dPasrc.morph.param;phys.pressurefloatrho[0/0.04] Gas density {rho}g.cm**3phys.densitydoubleOpRRosseland mean opacity {kappa}_R_(T,P,{rho}) (1)cm**2.g**-1phys.absorption.coeff;stat.meandoubleOpPPlanck mean opacity {kappa}_P_(T,P,{rho}) (1)cm**2.g**-1phys.absorption.coeff;stat.meandoubleOpR3kRosseland mean opacity {kappa}_R_ using 3000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpP3kPlanck mean opacity {kappa}_P_ using 3000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpR4kRosseland mean opacity {kappa}_R_ using 4000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpP4kPlanck mean opacity {kappa}_P_ using 4000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpR5kRosseland mean opacity {kappa}_R_ using 5000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpP5kPlanck mean opacity {kappa}_P_ using 5000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpR6kRosseland mean opacity {kappa}_R_ using 6000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpP6kPlanck mean opacity {kappa}_P_ using 6000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpR7kRosseland mean opacity {kappa}_R_ using 7000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandoubleOpP7kPlanck mean opacity {kappa}_P_ using 7000K stellar weighting function (1)cm**2.g**-1phys.luminosity.fun;stat.meandouble