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dc.contributor.authorZotti, G. de-
dc.contributor.authorGonzález-Nuevo, J.-
dc.contributor.authorLópez-Caniego, M.-
dc.contributor.authorNegrello, Mattia-
dc.contributor.authorCai, Z. Y.-
dc.contributor.authorClemens, M. S.-
dc.contributor.authorDelabrouille, J.-
dc.contributor.authorHerranz, D.-
dc.contributor.authorBonavera, Laura-
dc.contributor.authorMelin, J. B.-
dc.contributor.authorTucci, M.-
dc.contributor.authorSerjeant, S.-
dc.contributor.authorClements, D. L.-
dc.date.accessioned2016-11-07T12:47:03Z-
dc.date.available2016-11-07T12:47:03Z-
dc.date.issued2015-
dc.identifierdoi: 10.1088/1475-7516/2015/06/018-
dc.identifiere-issn: 1475-7516-
dc.identifier.citationJournal of Cosmology and Astroparticle Physics 06: 018 (2015)-
dc.identifier.urihttp://hdl.handle.net/10261/139908-
dc.descriptionarXiv:1501.02170v2.-- et al.-
dc.description.abstractWe discuss the potential of a next generation space-borne CMB experiment for studies of extragalactic sources with reference to COrE+, a project submitted to ESA in response to the call for a Medium-size mission (M4). We consider three possible options for the telescope size: 1 m, 1.5 m and 2 m (although the last option is probably impractical, given the M4 boundary conditions). The proposed instrument will be far more sensitive than Planck and will have a diffraction-limited angular resolution. These properties imply that even the 1 m telescope option will perform substantially better than Planck for studies of extragalactic sources. The source detection limits as a function of frequency have been estimated by means of realistic simulations taking into account all the relevant foregrounds. Predictions for the various classes of extragalactic sources are based on up-to-date models. The most significant improvements over Planck results are presented for each option. COrE+ will provide much larger samples of truly local star-forming galaxies (by about a factor of 8 for the 1 m telescope, of 17 for 1.5 m, of 30 for 2 m), making possible analyses of the properties of galaxies (luminosity functions, dust mass functions, star formation rate functions, dust temperature distributions, etc.) across the Hubble sequence. Even more interestingly, COrE+ will detect, at |b| > 30°, thousands of strongly gravitationally lensed galaxies (about 2,000, 6,000 and 13,000 for the 1 m, 1.5 m and 2 m options, respectively). Such large samples are of extraordinary astrophysical and cosmological value in many fields. Moreover, COrE+ high frequency maps will be optimally suited to pick up proto-clusters of dusty galaxies, i.e. to investigate the evolution of large scale structure at larger redshifts than can be reached by other means. Thanks to its high sensitivity COrE+ will also yield a spectacular advance in the blind detection of extragalactic sources in polarization: we expect that it will detect up to a factor of 40 (1 m option) or of 160 (1.5 m option) more radio sources than can be detected by Planck and, for the first time, from several tens (1 m option) to a few hundreds (1.5 m option) of star forming galaxies. This will open a new window for studies of the global properties of magnetic fields in star forming galaxies and of their relationships with star formation rates.-
dc.description.sponsorshipWork supported in part by ASI/INAF agreement n. 2014-024-R.0. MB acknowledges the financial assistance of the South African National Research Foundation (NRF) and of the Polish National Science Centre under contract #UMO-2012/07/D/ST9/02785.-
dc.publisherInstitute of Physics Publishing-
dc.relation.isversionofPreprint-
dc.rightsopenAccess-
dc.titleExtragalactic sources in Cosmic Microwave Background maps-
dc.typeartículo-
dc.identifier.doihttp://dx.doi.org/10.1088/1475-7516/2015/06/018-
dc.relation.publisherversionhttps:/doi.org/10.1088/1475-7516/2015/06/018-
dc.date.updated2016-11-07T12:47:03Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderIstituto Nazionale di Astrofisica-
dc.contributor.funderSouth African Medical Research Council-
dc.contributor.funderPolish Academy of Sciences-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100005184es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001322es_ES
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