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Referencias:

• Lubin, P.M., Smoot, G.F., (1983) Astrophys. J., 273, p. L1
• Rees, M., Polarization and Spectrum of the Primeval Radiation in an Anisotropic Universe (1968) The Astrophysical Journal, 153, p. L1
• Chandrasekar, S., (1950) Radiative Transfer, , Oxford University Press, Oxford, England
• Nanos, G.P., Polarization of the blackbody radiation at 3.2 centimeters (1979) The Astrophysical Journal, 232, p. 341
• Basko, M., Polnarev, A., (1979) Sov. Astron., 24, p. 3
• Negroponte, J., Silk, J., (1980) Phys. Rev. Lett., 44, p. 1433
• Tolman, B.W., Matzner, R.A., (1984) Proc. R. Soc. London, 392 A, p. 1803
• Tolman, B.W., The polarization of the microwave background in open universes (1985) The Astrophysical Journal, 290, p. 1
• Bond, J.R., Efstathiou, G., Cosmic background radiation anisotropies in universes dominated by nonbaryonic dark matter (1984) The Astrophysical Journal, 285, p. L45
• Milaneschi, E., Valdarnini, R., (1986) Astron. Astrophys., 162, p. 5
• Bond, J.R., Efstathiou, G., The statistics of cosmic background radiation fluctuations (1987) Monthly Notices of the Royal Astronomical Society, 226, p. 655
• Crittenden, R., Davis, R.L., Steinhardt, P.J., (1993) Astrophys. J., 417, p. L13
• Harari, D. D, Zaldarriaga, M., (1993) Phys. Lett. B, 319, p. 96
• Coulson, D., Crittenden, R.G., Turok, N.G., (1994) Phys. Rev. Lett., 73, p. 2390
• Ng, Ng, (1995) Phys. Rev. D, 51, p. 364
• Polnarev, A., (1985) Sov. Astron., 29, p. 607
• 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
• 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
• Hu, W., Sugiyama, N., (1995) Phys. Rev. D, 51, p. 2599
• Hu, W., Sugiyama, N., (1995) Astrophys. J., 444, p. 489
• 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
• Bond, J.R., Crittenden, R., Davis, R.L., Efstathiou, G., Steinhardt, P.J., (1994) Phys. Rev. Lett., 72, p. 13
• Seljak, U., (1994) Astrophys. J., 435, p. L87
• Jorgensen, H.E., Kotok, E., Naselsky, P., Novikov, I., (1995) Astron. Astrophys., 294, p. 639
• Sachs, R., Wolfe, A., Perturbations of a Cosmological Model and Angular Variations of the Microwave Background (1967) The Astrophysical Journal, 147, p. 73
• Peebles, P.J.E., Yu, J.T., Primeval Adiabatic Perturbation in an Expanding Universe (1970) The Astrophysical Journal, 162, p. 815
• Doroshkevich, A.G., Zel'dovich, Ya.B., Sunyaev, R.A., (1978) Sov. Astron., 22, p. 523
• Bardeen, J., (1980) Phys. Rev. D, 22, p. 1882
• Kodama, H., Sasaki, M., Cosmological Perturbation Theory (1984) Progress of Theoretical Physics Supplement, 78, p. 1
• Mukhanov, V.F., Feldman, H.A., Brandenberger, R.H., (1992) Phys. Rep., 215, p. 203
• 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
• Bond, J.R., (1988) The Early Universe, , edited by, W.G. Unruh, G.W. Semenoff, Reidel, Dordrecht
• Jones, B.T.J., Wyse, R.F.G., (1985) Astron. Astrophys., 149, p. 144
• Nasel'skii, P.D., Polnarev, A.G., (1987) Astrophys. J., 26, p. 327
• Peebles, P.J.E., (1980) The Large Scale Structure of the Universe, , Princeton University Press, Princeton, NJ
• Silk, J., Cosmic Black-Body Radiation and Galaxy Formation (1968) The Astrophysical Journal, 151, p. 459
• 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
• 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

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