The Cosmic Microwave Background Dipole as a Cosmological Effect

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dc.creatorJaroszynski, M.
dc.creatorPaczynski, B.
dc.date1994-11-29
dc.date.accessioned2026-07-07T02:19:36Z
dc.date.available2026-07-07T02:19:36Z
dc.descriptionA conventional explanation of the dipole anisotropy of the cosmic microwave background (CMB) radiation is in terms of the Doppler effect: our galaxy is moving with respect to CMB frame with $ \sim 600 ~ km ~ s^{-1} $. However, as the deep redshift surveys fail to reveal a convergence of the large scale flow to zero at distances as large as $ d \sim H^{-1} 15,000 ~ km ~ s^{-1} $ (Lauer & Postman, 1994), the uniqueness of the conventional interpretation has to be investigated. A possible alternative might be a cosmological entropy gradient, as suggested by Paczyński & Piran (1990). We find that contrary to that suggestion a quadrupole anisotropy is generically of the same order of magnitude as the dipole anisotropy (or larger) not only for adiabatic but also for iso-curvature initial perturbations. Hence, the observed dipole cannot be explained with a very large scale perturbation which was initially iso-curvature.
dc.description14 pages, plain TEX Submitted to ApJ The full postscript version with 3 figures at ftp://astro.princeton.edu/library/preprints/pop602.ps.Z (88kB, compressed). e-mails: mj@orion.astrouw.edu.pl, bp@astro.princeton.edu
dc.identifierhttps://arxiv.org/abs/astro-ph/9411111
dc.identifierhttp://arxiv.org/abs/astro-ph/9411111
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/9932
dc.subjectAstrophysics
dc.titleThe Cosmic Microwave Background Dipole as a Cosmological Effect
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