J/A+A/531/A12ivo://CDS.VizieR/J/A+A/531/A12doi:10.26093/cds/vizier.35310012CDSSchaerer D.Hayes M.Verhamme A.Teyssier R.2011-08-01T21:08:10Z2011-05-31T09:01:14ZCDS support team

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

cds-question@unistra.frastronomical-modelsinterstellar-mediumultraviolet-astronomyLy{alpha} is a key diagnostic for numerous observations of distant star-forming galaxies, but detailed radiation transfer models are required for interpreting them. We provide an extensive grid of 3D radiation transfer models that simulate the Ly{alpha} and UV continuum radiation transfer in the interstellar medium of star-forming galaxies. We have improved our Monte Carlo MCLya code and used it to compute a grid of 6240 radiation transfer models for homogeneous spherical shells containing HI and dust surrounding a central source. The simulations cover a wide range of parameter space. We present the detailed predictions from our models including in particular the Ly{alpha} escape fraction fesc, the continuum attenuation, and detailed Ly{alpha} line profiles. The Ly{alpha} escape fraction is shown to depend strongly on dust content, but also on other parameters (HI column density and radial velocity). The predicted line profiles show a wide diversity of morphologies, ranging from broad absorption lines to emission lines with complex features. The results from our simulations are distributed in electronic format. Our models should be of use for interpreting observations from distant galaxies, for other simulations, and should also serve as an important basis for comparison for future, more refined, radiation transfer models.2011A&A...531A..12Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/531/A12CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/531/A12https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/531/A12http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/531/A12https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/531/A12https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/531/A12http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/531/A12GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapUVdefaultJ/A+A/531/A12/table2Predicted Ly{alpha} and continuum escape fraction for all radiation transfer modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintb[10/160] HI velocity dispersion in the shellkm/sphys.veloc.dispersionfloattau.a[0/4] Dust absorption optical depthphys.absorption.opticalDepthfloatlog(NHI)[16/21.7] logarithm (dec.) of HI column densitylog(cm**-2)phys.columnDensityfloatVexp[0/700] Expansion velocitykm/sphys.veloc.expansionfloatFWHM[50/1000] Full width at half maximum of input Ly{alpha} emission linekm/sspect.line.widthfloatFesc[0/1] Ly{alpha} escape fractionstat.fit.paramdoubleFesc-c[0/1] UV continuum escape fraction close to Ly{alpha}stat.fit.paramdoubleW(Lya)Ly{alpha} absorption equivalent width predicted for a flat UV continuum0.1nmspect.line.eqWidthdouble