Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove

Planck Collaboration: N. Aghanim , C. Armitage-Caplan , M. Arnaud , M. Ashdown , F. Atrio-Barandela , J. Aumont , A. J. Banday , R. B. Barreiro

show 170 more authors

J. G. Bartlett K. Benabed A. Benoit-L\'evy J.-P. Bernard M. Bersanelli P. Bielewicz J. Bobin J. J. Bock J. R. Bond J. Borrill F. R. Bouchet M. Bridges C. Burigana R. C. Butler J.-F. Cardoso A. Catalano A. Challinor A. Chamballu L.-Y Chiang H. C. Chiang P. R. Christensen D. L. Clements L. P. L. Colombo F. Couchot B. P. Crill F. Cuttaia L. Danese R. D. Davies R. J. Davis P. De Bernardis A. De Rosa G. de Zotti J. Delabrouille J. M. Diego S. Donzelli O. Dor\'e X. Dupac G. Efstathiou T. A. En{\ss}lin H. K. Eriksen F. Finelli O. Forni M. Frailis E. Franceschi S. Galeotta K. Ganga M. Giard G. Giardino J. Gonz\'alez-Nuevo K. M. G\'orski S. Gratton A. Gregorio A. Gruppuso F. K. Hansen D. Hanson D. Harrison G. Helou S. R. Hildebrandt E. Hivon M. Hobson W. A. Holmes W. Hovest K. M. Huffenberger W. C. Jones M. Juvela E. Keih\"anen R. Keskitalo T. S. Kisner J. Knoche L. Knox M. Kunz H. Kurki-Suonio A. L\"ahteenm\"aki J.-M. Lamarre A. Lasenby C. R. Lawrence R. Leonardi A. Lewis M. Liguori P. B. Lilje M. Linden-V{\o}rnle M. L\'opez-Caniego P. M. Lubin J. F. Mac\'ias-P\'erez M. Maris D. J. Marshall P. G. Martin E. Mart\'inez-Gonz\'alez S. Masi S. Matarrese P. Mazzotta P. R. Meinhold A. Melchiorri L. Mendes M. Migliaccio S. Mitra A. Moneti L. Montier G. Morgante D. Mortlock A. Moss D. Munshi P. Naselsky F. Nati P. Natoli H. U. N{\o}rgaard-Nielsen F. Noviello D. Novikov I. Novikov S. Osborne C. A. Oxborrow L. Pagano F. Pajot D. Paoletti F. Pasian G. Patanchon O. Perdereau F. Perrotta F. Piacentini E. Pierpaoli D. Pietrobon S. Plaszczynski E. Pointecouteau G. Polenta N. Ponthieu L. Popa G. W. Pratt G. Pr\'ezeau J.-L. Puget J. P. Rachen W. T. Reach M. Reinecke S. Ricciardi T. Riller I. Ristorcelli G. Rocha C. Rosset J. A. Rubi\~no-Mart\'in B. Rusholme D. Santos G. Savini D. Scott M. D. Seiffert E. P. S. Shellard L. D. Spencer R. Sunyaev F. Sureau A.-S. Suur-Uski J.-F. Sygnet J. A. Tauber D. Tavagnacco L. Terenzi L. Toffolatti M. Tomasi M. Tristram M. Tucci M. T\"urler L. Valenziano J. Valiviita B. Van Tent P. Vielva F. Villa N. Vittorio L. A. Wade B. D. Wandelt M. White D. Yvon A. Zacchei J. P. Zibin A. Zonca

Authors on Pith no claims yet

classification 🌌 astro-ph.CO

keywords temperaturevelocityboostingdipoledopplerfluctuationsplanckwell

0 comments

read the original abstract

Our velocity relative to the rest frame of the cosmic microwave background (CMB) generates a dipole temperature anisotropy on the sky which has been well measured for more than 30 years, and has an accepted amplitude of v/c = 0.00123, or v = 369km/s. In addition to this signal generated by Doppler boosting of the CMB monopole, our motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances). This is an order 0.1% effect applied to fluctuations which are already one part in roughly one hundred thousand, so it is quite small. Nevertheless, it becomes detectable with the all-sky coverage, high angular resolution, and low noise levels of the Planck satellite. Here we report a first measurement of this velocity signature using the aberration and modulation effects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l,b)=(264, 48) [deg], of 384km/s +- 78km/s (stat.) +- 115km/s (syst.). This is a significant confirmation of the expected velocity.

This paper has not been read by Pith yet.

discussion (0)

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Planck 2018 results. X. Constraints on inflation
astro-ph.CO 2018-07 accept novelty 4.0

Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.