J/A+A/534/A118ivo://CDS.VizieR/J/A+A/534/A118doi:10.26093/cds/vizier.35340118CDSParadis DBernard J.P.Meny C.Gromov V.2011-12-27T13:23:47Z2011-10-18T08:24:32ZCDS support team

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

cds-question@unistra.frinterstellar-mediuminfrared-sourcesmillimeter-astronomysubmillimeter-astronomyIn a previous paper we proposed a new model for the emission by amorphous astronomical dust grains, based on solid-state physics. The model uses a description of the disordered charge distribution (DCD) combined with the presence of two-level systems (TLS) defects in the amorphous solid composing the grains. The goal of this paper is to compare this new model to astronomical observations of different Galactic environments in the far-infrared/ submillimeter, in order to derive a set of canonical model parameters to be used as a Galactic reference to be compared to in future Galactic and extragalactic studies. We compare the TLSmodel with existing astronomical data. We consider the average emission spectrum at high latitudes in our Galaxy as measured with FIRAS and WMAP, as well as the emission from Galactic compact sources observed with the Archeops balloon experiment, for which an inverse relationship between the dust temperature and the emissivity spectral index has been proven.2011A&A...534A.118Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/534/A118CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/534/A118https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/534/A118http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/534/A118https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/534/A118https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/534/A118http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/534/A118GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfraredRadiodefaultJ/A+A/534/A118/table5Predicted emissivities as a function of temperature in the IRAS, Herschel, and Planck photometric bandsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTd[5/100] Dust temperatureKphys.temperatureinte100IPredicted emissivity in the IRAS 100um band (1)cm**2phys.emissivitydoublee160PPredicted emissivity in the PACS 160um band (1)cm**2phys.emissivitydoublee250SPredicted emissivity in the SPIRE 250um band (1)cm**2phys.emissivitydoublee350SPredicted emissivity in the SPIRE 350um band (1)cm**2phys.emissivitydoublee350HPredicted emissivity in the HFI 350um band (1)cm**2phys.emissivitydoublee500SPredicted emissivity in the SPIRE 500um band (1)cm**2phys.emissivitydoublee550HPredicted emissivity in the HFI 550um band (1)cm**2phys.emissivitydoublee850HPredicted emissivity in the HFI 850um band (1)cm**2phys.emissivitydoublee1382HPredicted emissivity in the HFI 1382um band (1)cm**2phys.emissivitydoublee2096HPredicted emissivity in the HFI 2096um band (1)cm**2phys.emissivitydoublee2998HPredicted emissivity in the HFI 2998um band (1)cm**2phys.emissivitydoublee4286LPredicted emissivity in the LFI 4296um band (1)cm**2phys.emissivitydoublee6818LPredicted emissivity in the LFI 6818um band (1)cm**2phys.emissivitydoublee10000LPredicted emissivity in the LFI 10000um band (1)cm**2phys.emissivitydouble