Exploring cosmic origins with CORE: effects of observer peculiar motion
Creators: name: Burigana, C.
name: Carvalho, C. S.
name: Trombetti, T.
name: Notari, A.
name: Quartin, M.
name: De Gasperis, G.
name: Buzzelli, A.
name: Vittorio, N.
name: De Zotti, G.
name: de Bernardis, P.
name: Chluba, J.
name: Bilicki, M.
name: Danese, L.
name: Delabrouille, J.
name: Toffolatti, L.
name: Lapi, A.
name: Negrello, M.
name: Mazzotta, P.
name: Scott, D.
name: Contreras, D.
name: Achucarro, A.
name: Ade, P.
name: Allison, R.
name: Ashdown, M.
name: Ballardini, M.
name: Banday, A. J.
name: Banerji, R.
name: Bartlett, J.
name: Bartolo, N.
name: Basak, S.
name: Bersanelli, M.
name: Bonaldi, A.
name: Bonato, M.
name: Borrill, J.
name: Bouchet, F.
name: Boulanger, F.
name: Brinckmann, T.
name: Bucher, M.
name: Cabella, P.
name: Cai, Z. -Y.
name: Calvo, M.
name: Castellano, G.
name: Challinor, A.
name: Clesse, S.
name: Colantoni, I.
name: Coppolecchia, A.
name: Crook, M.
name: D'Alessandro, G.
name: Diego, J. -M.
name: Di Marco, A.
name: Di Valentino, E.
name: Errard, J.
name: Feeney, S.
name: Fernandez-Cobos, R.
name: Ferraro, S.
name: Finelli, F.
name: Forastieri, F.
name: Galli, S.
name: Genova-Santos, R.
name: Gerbino, M.
name: Gonzalez-Nuevo, J.
name: Grandis, S.
name: Greenslade, J.
name: Hagstotz, S.
name: Hanany, S.
name: Handley, W.
name: Hernandez-Monteagudo, C.
name: Hervias-Caimapo, C.
name: Hills, M.
name: Hivon, E.
name: Kiiveri, K.
name: Kisner, T.
name: Kitching, T.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Lamagna, L.
name: Lasenby, A.
name: Lattanzi, M.
name: Lesgourgues, J.
name: Liguori, M.
name: Lindholm, V.
name: Lopez-Caniego, M.
name: Luzzi, G.
name: Maffei, B.
name: Mandolesi, N.
name: Martinez-Gonzalez, E.
name: Martins, C. J. A. P.
name: Masi, S.
name: McCarthy, D.
name: Melchiorri, A.
name: Melin, J. -B.
name: Molinari, D.
name: Monfardini, A.
name: Natoli, P.
name: Paiella, A.
name: Paoletti, D.
name: Patanchon, G.
name: Piat, M.
name: Pisano, G.
name: Polastri, L.
name: Polenta, G.
name: Pollo, A.
name: Poulin, V.
name: Remazeilles, M.
name: Roman, M.
name: Rubino-Martin, J. -A.
name: Salvati, L.
name: Tartari, A.
name: Tomasi, M.
name: Tramonte, D.
name: Trappe, N.
name: Tucker, C.
name: Valiviita, J.
name: Van de Weijgaert, R.
name: van Tent, B.
name: Vennin, V.
name: Vielva, P.
name: Young, K.
name: Zannoni, M.
Publisher: name: arXiv
Year: 2017
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We discuss the effects on the CMB, CIB, and thermal SZ effect due to the peculiar motion of an observer with respect to the CMB rest frame, which induces boosting effects. We investigate the scientific perspectives opened by future CMB space missions, focussing on the CORE proposal. The improvements in sensitivity offered by a mission like CORE, together with its high resolution over a wide frequency range, will provide a more accurate estimate of the CMB dipole. The extension of boosting effects to polarization and cross-correlations will enable a more robust determination of purely velocity-driven effects that are not degenerate with the intrinsic CMB dipole, allowing us to achieve a S/N ratio of 13; this improves on the Planck detection and essentially equals that of an ideal cosmic-variance-limited experiment up to a multipole l of 2000. Precise inter-frequency calibration will offer the opportunity to constrain or even detect CMB spectral distortions, particularly from the cosmological reionization, because of the frequency dependence of the dipole spectrum, without resorting to precise absolute calibration. The expected improvement with respect to COBE-FIRAS in the recovery of distortion parameters (in principle, a factor of several hundred for an ideal experiment with the CORE configuration) ranges from a factor of several up to about 50, depending on the quality of foreground removal and relative calibration. Even for 1% accuracy in both foreground removal and relative calibration at an angular scale of 1 deg, we find that dipole analyses for a mission like CORE will be able to improve the recovery of the CIB spectrum amplitude by a factor of 17 in comparison with current results based on FIRAS. In addition to the scientific potential of a mission like CORE for these analyses, synergies with other planned and ongoing projects are also discussed.
description: 61+5 pages, 17 figures, 25 tables, 8 sections, 5 appendices. In press on JCAP - Version 3 - Minor changes, affiliations fixed, references updated - version in line with corrected proofs