J/A+A/557/A66ivo://CDS.VizieR/J/A+A/557/A66doi:10.26093/cds/vizier.35570066CDSBethermin M.Wang L.Dore O.Lagache G.Sargent M.Daddi E.,Cousin M.Aussel H.2017-06-20T13:16:43Z2013-09-03T08:18:19ZCDS support team

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

cds-question@unistra.frgalaxiesinfrared-sourcesspectral-energy-distributionRecent studies have revealed a strong correlation between the star formation rate (SFR) and stellarmass of the majority of star-forming galaxies, the so-called star-forming main sequence. An empirical modeling approach (the 2-SFM framework) that distinguishes between the main sequence and rarer starburst galaxies is capable of reproducing most statistical properties of infrared galaxies, such as number counts, luminosity functions, and redshift distributions. In this paper, we extend this approach by establishing a connection between stellar mass and halo mass with the technique of abundance matching. Based on a few simple assumptions and a physically motivated formalism, our model successfully predicts the (cross-)power spectra of the cosmic infrared background (CIB), the crosscorrelation between CIB and cosmic microwave background (CMB) lensing, and the correlation functions of bright, resolved infrared galaxies measured by Herschel, Planck, ACT, and SPT.We use this model to infer the redshift distribution of CIB-anisotropies and of the CIBxCMB lensing signal, as well as the level of correlation between CIB-anisotropies at different wavelengths. Material (effective spectral energy distributions, differential emissivities of halos, relations between Mh and SFR) associated to this model is available at http://irfu.cea.fr/Sap/Phocea/Page/index.php?id=5372013A&A...557A..66Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/557/A66CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/713/970 : Low-resolution SED templates for AGNs & galaxies (Assef+, 2010)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/557/A66https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/557/A66http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/557/A66https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/557/A66https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/557/A66http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/557/A66GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/A+A/557/A66/sedTable of the effective SEDsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[5/5000] Wavelength {lambda} ({mu}m)umem.wldoublenuLnu0SED {nu}L_{nu}_({lambda}) at z=0stat.paramdoublenuLnu2SED {nu}L_{nu}_({lambda}) at z=0.2stat.paramdoublenuLnu4SED {nu}L_{nu}_({lambda}) at z=0.4stat.paramdoublenuLnu6SED {nu}L_{nu}_({lambda}) at z=0.6stat.paramdoublenuLnu8SED {nu}L_{nu}_({lambda}) at z=0.8stat.paramdoublenuLnu10SED {nu}L_{nu}_({lambda}) at z=1.0stat.paramdoublenuLnu12SED {nu}L_{nu}_({lambda}) at z=1.2stat.paramdoublenuLnu14SED {nu}L_{nu}_({lambda}) at z=1.4stat.paramdoublenuLnu16SED {nu}L_{nu}_({lambda}) at z=1.6stat.paramdoublenuLnu18SED {nu}L_{nu}_({lambda}) at z=1.8stat.paramdoublenuLnu20SED {nu}L_{nu}_({lambda}) at z=2.0stat.paramdoublenuLnu23SED {nu}L_{nu}_({lambda}) at z=2.33stat.paramdoublenuLnu26SED {nu}L_{nu}_({lambda}) at z=2.66stat.paramdoublenuLnu30SED {nu}L_{nu}_({lambda}) at z=3.0stat.paramdoublenuLnu35SED {nu}L_{nu}_({lambda}) at z=3.5stat.paramdoublenuLnu40SED {nu}L_{nu}_({lambda}) at z=4.0stat.paramdoublenuLnu50SED {nu}L_{nu}_({lambda}) at z=5.0stat.paramdouble