J/A+A/417/827ivo://CDS.VizieR/J/A+A/417/827doi:10.26093/cds/vizier.34170827CDSItoh N.Nozawa S.2017-06-21T08:22:12Z2004-06-08T22:24:15ZCDS support team

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

cds-question@unistra.frgalaxy-clustersastronomical-modelsThese tables contain numerical values for the distortion of the spectral intensity {Delta}I/y defined by the equation {Delta}I/y = 1/y * X^3^/(e^X^-1) * {Delta}n(X)/n0(X) = X^3^/(e^X^-1)*F({theta}_e_,X) The spectral intensity is the function of two variables X and {theta}_e_. Here X={omega}/k_B_*T_0_, {omega} being the photon angular frequency and k_B_*T_0_ being the thermal energy of CMB photons, and {theta}_e_=k_B_*Te/m_e_*c^2^, k_B_*Te being the thermal energy of the electrons and m_e_*c^2^ being the electron rest energy (T_0_ is the temperature of the cosmic microwave background radiation). In these tables, the range for X is taken as 0<X<20 and the range for {theta}_e_ is taken as 0.002<{theta}_e_<0.100.2004A&A...417..827Ihttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/417/827CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/417/827https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/417/827http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/417/827https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/417/827https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/417/827http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/417/827GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/417/827/diValues of {Delta}I/y for {theta}_e_=0.002 to 0.100 (tables 1 to 5 of the paper)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintthetaeValue of {theta}_e_ = k_B_*Te/m_e_*c^2^stat.paramfloatXValue of the variable X = {omega}/k_B_*Torad.s**-1.keV**-1stat.paramfloatDI/yValue of {Delta}I/y for F({theta}_e_,X)stat.paramdouble