Analytic approach to the polarization of the cosmic microwave background in flat and open universes

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We develop an analytic method and approximations to compute the polarization induced in the cosmic microwave background radiation on a wide range of angular scales by anisotropic Thomson scattering in the presence of adiabatic scalar (energy-density) linear fluctuations. The formalism is an extensio...

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Autor principal: Zaldarriaga, M.
Otros Autores: Harari, Diego Darío
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 1995
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Zaldarriaga, M. 
245 1 0 |a Analytic approach to the polarization of the cosmic microwave background in flat and open universes 
260 |c 1995 
270 1 0 |m Zaldarriaga, M.; Departamento de Física, Facultad de Ciencias Exactas Y Naturales, Universidad de Buenos Aires, Ciudad Universitaria-Pab.1, 1428 Buenos Aires, Argentina 
504 |a Lubin, P.M., Smoot, G.F., (1983) Astrophys. J., 273, p. L1 
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504 |a Nanos, G.P., Polarization of the blackbody radiation at 3.2 centimeters (1979) The Astrophysical Journal, 232, p. 341 
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504 |a Negroponte, J., Silk, J., (1980) Phys. Rev. Lett., 44, p. 1433 
504 |a Tolman, B.W., Matzner, R.A., (1984) Proc. R. Soc. London, 392 A, p. 1803 
504 |a Tolman, B.W., The polarization of the microwave background in open universes (1985) The Astrophysical Journal, 290, p. 1 
504 |a Bond, J.R., Efstathiou, G., Cosmic background radiation anisotropies in universes dominated by nonbaryonic dark matter (1984) The Astrophysical Journal, 285, p. L45 
504 |a Milaneschi, E., Valdarnini, R., (1986) Astron. Astrophys., 162, p. 5 
504 |a Bond, J.R., Efstathiou, G., The statistics of cosmic background radiation fluctuations (1987) Monthly Notices of the Royal Astronomical Society, 226, p. 655 
504 |a Crittenden, R., Davis, R.L., Steinhardt, P.J., (1993) Astrophys. J., 417, p. L13 
504 |a Harari, D. D, Zaldarriaga, M., (1993) Phys. Lett. B, 319, p. 96 
504 |a Coulson, D., Crittenden, R.G., Turok, N.G., (1994) Phys. Rev. Lett., 73, p. 2390 
504 |a Ng, Ng, (1995) Phys. Rev. D, 51, p. 364 
504 |a Polnarev, A., (1985) Sov. Astron., 29, p. 607 
504 |a Frewin, R.A., Polnarev, A.G., Coles, P., Gravitational waves and the polarization of the cosmic microwave background (1994) Monthly Notices of the Royal Astronomical Society, 266, p. L21 
504 |a Ka Lok Ng and Kin Wang Ng, Astrophys. J. (to be published); Smoot, G.F., Structure in the COBE differential microwave radiometer first-year maps (1992) The Astrophysical Journal, 396, p. L1 
504 |a Hu, W., Sugiyama, N., (1995) Phys. Rev. D, 51, p. 2599 
504 |a Hu, W., Sugiyama, N., (1995) Astrophys. J., 444, p. 489 
504 |a Vittorio, N., Silk, J., Fine-scale anisotropy of the cosmic microwave background in a universe dominated by cold dark matter (1984) The Astrophysical Journal, 285, p. L39 
504 |a Bond, J.R., Crittenden, R., Davis, R.L., Efstathiou, G., Steinhardt, P.J., (1994) Phys. Rev. Lett., 72, p. 13 
504 |a Seljak, U., (1994) Astrophys. J., 435, p. L87 
504 |a Jorgensen, H.E., Kotok, E., Naselsky, P., Novikov, I., (1995) Astron. Astrophys., 294, p. 639 
504 |a Sachs, R., Wolfe, A., Perturbations of a Cosmological Model and Angular Variations of the Microwave Background (1967) The Astrophysical Journal, 147, p. 73 
504 |a Peebles, P.J.E., Yu, J.T., Primeval Adiabatic Perturbation in an Expanding Universe (1970) The Astrophysical Journal, 162, p. 815 
504 |a Doroshkevich, A.G., Zel'dovich, Ya.B., Sunyaev, R.A., (1978) Sov. Astron., 22, p. 523 
504 |a Bardeen, J., (1980) Phys. Rev. D, 22, p. 1882 
504 |a Kodama, H., Sasaki, M., Cosmological Perturbation Theory (1984) Progress of Theoretical Physics Supplement, 78, p. 1 
504 |a Mukhanov, V.F., Feldman, H.A., Brandenberger, R.H., (1992) Phys. Rep., 215, p. 203 
504 |a Notice that our definition of Δ T and Δ P differs by a factor 4 from that of Ref. cite Bond87, while our definition for the polarization correlation function CP turns out to be identical; Notice that our multipole expansion differs from that in Ref. cite Hu94 by a factor (-i)l/(2l+1); Kodama, H., Sasaki, M., EVOLUTION OF ISOCURVATURE PERTURBATIONS I: PHOTON-BARYON UNIVERSE (1986) International Journal of Modern Physics A, 1, p. 265 
504 |a Bond, J.R., (1988) The Early Universe, , edited by, W.G. Unruh, G.W. Semenoff, Reidel, Dordrecht 
504 |a Jones, B.T.J., Wyse, R.F.G., (1985) Astron. Astrophys., 149, p. 144 
504 |a Nasel'skii, P.D., Polnarev, A.G., (1987) Astrophys. J., 26, p. 327 
504 |a Peebles, P.J.E., (1980) The Large Scale Structure of the Universe, , Princeton University Press, Princeton, NJ 
504 |a Silk, J., Cosmic Black-Body Radiation and Galaxy Formation (1968) The Astrophysical Journal, 151, p. 459 
504 |a Kaiser, N., Small-angle anisotropy of the microwave background radiation in the adiabatic theory (1983) Monthly Notices of the Royal Astronomical Society, 202, p. 1169 
504 |a Notice that in order to compare our Figs. 1 and 2 with Figs. (4b) and (7a) of Ref. citeBond87 some adjustments are needed to account for different conventions and normalizations. Our W(k) corresponds to twice what is plotted in (4b). Our definition of the quadrupole anisotropy aT2 is 4 times that used in citeBond87. And finally the value of aT2 used is different; Kamionkowski, M., Spergel, D., (1994) Astrophys. J., 432, p. 7 
506 |2 openaire  |e Política editorial 
520 3 |a We develop an analytic method and approximations to compute the polarization induced in the cosmic microwave background radiation on a wide range of angular scales by anisotropic Thomson scattering in the presence of adiabatic scalar (energy-density) linear fluctuations. The formalism is an extension to the polarized case of the analytic approach recently developed by Hu and Sugiyama to evaluate the (unpolarized) temperature correlation function. The analytic approach helps to highlight the dependence of potentially measurable polarization properties of the cosmic microwave background radiation upon various parameters of the cosmological model. We show, for instance, that the ratio between the multipoles of the temperature and polarization correlation functions depends very sensitively upon the value of 0, the matter density in units of the critical, in an open universe. © 1995 The American Physical Society.  |l eng 
593 |a Departamento de Física, Facultad de Ciencias Exactas Y Naturales, Universidad de Buenos Aires, Ciudad Universitaria-Pab.1, 1428 Buenos Aires, Argentina 
700 1 |a Harari, Diego Darío 
773 0 |d 1995  |g v. 52  |h pp. 3276-3287  |k n. 6  |x 05562821  |w (AR-BaUEN)CENRE-394  |t Physical Review D 
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856 4 0 |u https://doi.org/10.1103/PhysRevD.52.3276  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_05562821_v52_n6_p3276_Zaldarriaga  |y Handle 
856 4 0 |u https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v52_n6_p3276_Zaldarriaga  |y Registro en la Biblioteca Digital 
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