• English
    • Norsk
  • English 
    • English
    • Norsk
  • Administration
View Item 
  •   Home
  • Øvrige samlinger
  • Høstingsarkiver
  • CRIStin høstingsarkiv
  • View Item
  •   Home
  • Øvrige samlinger
  • Høstingsarkiver
  • CRIStin høstingsarkiv
  • View Item
JavaScript is disabled for your browser. Some features of this site may not work without it.

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

Aghanim, N; Armitage-Caplan, C; Arnaud, M; Ashdown, M; Atrio-Barandela, F; Aumont, J; Baccigalupi, C; Banday, AJ; Barreiro, RB; Bartlett, JG; Benabed, K; Benoit-Levy, A; Bernard, JP; Bersanelli, M; Bielewicz, P; Bobin, J; Bock, JJ; Bond, JR; Borrill, J; Bouchet, FR; Bridges, M; Burigana, C; Butler, RC; Cardoso, JF; Catalano, A; Challinor, A; Chamballu, A; Chiang, HC; Chiang, LY; Christensen, PR; Clements, DL; Colombo, LPL; Couchot, F; Crill, BP; Curto, A; Cuttaia, F; Danese, L; Davies, RD; Davis, RJ; De Bernardis, P; De Rosa, A; De Zotti, G; Delabrouille, J; Diego, JM; Donzelli, S; Dore, O; Dupac, X; Efstathiou, G; Enßlin, TA; Eriksen, Hans Kristian Kamfjord; Finelli, F; Forni, O; Frailis, M; Franceschi, E; Galeotta, S; Ganga, K; Giard, M; Giardino, G; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gregorio, A; Gruppuso, A; Hansen, Frode Kristian; Hanson, D; Harrison, DL; Helou, G; Hildebrandt, SR; Hivon, E; Hobson, M; Holmes, WA; Hovest, W; Huffenberger, KM; Jones, WC; Juvela, M; Keihänen, E; Keskitalo, R; Kisner, TS; Knoche, J; Knox, L; Kunz, M; Kurki-Suonio, H; Lähteenmäki, A; Lamarre, JM; Lasenby, A; Laureijs, RJ; Lawrence, CR; Leonardi, R; Lewis, A; Liguori, M; Lilje, Per Barth; Linden-Vørnle, M; Lopez-Caniego, M; Lubin, PM; Macias-Perez, JF; Mandolesi, N; Maris, M; Marshall, DJ; Martin, PG; Martinez-Gonzalez, E; Masi, S; Massardi, M; Matarrese, S; Mazzotta, P; Meinhold, PR; Melchiorri, A; Mendes, L; Migliaccio, M; Mitra, S; Moneti, A; Montier, L; Morgante, G; Mortlock, D; Moss, A; Munshi, D; Naselsky, P; Nati, F; Natoli, P; Nørgaard-Nielsen, HU; Noviello, F; Novikov, D; Novikov, I; Osborne, S; Oxborrow, CA; Pagano, L; Pajot, F; Paoletti, D; Pasian, F; Patanchon, G; Perdereau, O; Perrotta, F; Piacentini, F; Pierpaoli, E; Pietrobon, D; Plaszczynski, S; Pointecouteau, E; Polenta, G; Ponthieu, N; Popa, L; Pratt, GW; Prezeau, G; Puget, JL; Rachen, JP; Reach, WT; Reinecke, M; Ricciardi, S; Riller, T; Ristorcelli, I; Rocha, G; Rosset, C; Rubino-Martin, JA; Rusholme, B; Santos, D; Savini, G; Scott, D; Seiffert, MD; Shellard, EPS; Spencer, LD; Sunyaev, R; Sureau, F; Suur-Uski, AS; Sygnet, JF; Tauber, JA; Tavagnacco, D; Terenzi, L; Toffolatti, L; Tomasi, M; Tristram, M; Tucci, M; Turler, M; Valenziano, L; Väliviita, Jussi-Pekka; Van Tent, B; Vielva, P; Villa, F; Vittorio, N; Wade, LA; Wandelt, BD; White, M; Yvon, D; Zacchei, A; Zibin, JP; Zonca, A
Journal article; PublishedVersion; Peer reviewed
View/Open
Paper27.pdf (1.398Mb)
Year
2014
Permanent link
http://urn.nb.no/URN:NBN:no-46739

CRIStin
1213456

Metadata
Show metadata
Appears in the following Collection
  • Institutt for teoretisk astrofysikk [873]
  • CRIStin høstingsarkiv [22066]
Original version
Astronomy and Astrophysics. 2014, 571, DOI: http://dx.doi.org/10.1051/0004-6361/201321556
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 = 1.23 × 10-3, or v = 369. 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 10-3 effect applied to fluctuations which are already one part in roughly 105, 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°), of 384 km s-1 ± 78 km s-1 (stat.) ± 115 km s-1 (syst.). This is a significant confirmation of the expected velocity.

Reproduced with permission from Astronomy & Astrophysics, © ESO 2014
 
Responsible for this website 
University of Oslo Library


Contact Us 
duo-hjelp@ub.uio.no


Privacy policy
 

 

For students / employeesSubmit master thesisAccess to restricted material

Browse

All of DUOCommunities & CollectionsBy Issue DateAuthorsTitlesThis CollectionBy Issue DateAuthorsTitles

For library staff

Login
RSS Feeds
 
Responsible for this website 
University of Oslo Library


Contact Us 
duo-hjelp@ub.uio.no


Privacy policy