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21“…We reanalyze the full WMAP parameter space supplemented by a low-k cutoff for P(k). …”
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22“…Minimal supersymmetric hybrid inflation based on a minimal Kahler potential predicts a spectral index n_s\gsim 0.98. On the other hand, WMAP three year data prefers a central value n_s \approx 0.95. …”
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23“…The first-year WMAP data taken at their face value hint that the Universe might be slightly positively curved and therefore necessarily finite, since all spherical (Clifford-Klein) space forms M^3 = S^3/Gamma, given by the quotient of S^3 by a group Gamma of covering transformations, possess this property. …”
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24“…WMAP observations have accurately determined the position of the first two peaks and dips in the CMB temperature power spectrum. …”
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25por Ade, P.A.R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaglia, P., Battaner, E., Benabed, K., Benoit, A., Benoit-Levy, A., Bernard, J.P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.F., Catalano, A., Chamballu, A., Christensen, P.R., Colombi, S., Colombo, L.P.L., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Dore, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Ensslin, T.A., Eriksen, H.K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Heraud, Y., Gjerlow, E., Gonzalez-Nuevo, J., Gorski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F.K., Hanson, D., Harrison, D.L., Henrot-Versille, S., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J.M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J.A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Norgaard-Nielsen, H.U., Novikov, D., Novikov, I., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G.W., Prezeau, G., Prunet, S., Puget, J.L., Rachen, J.P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, E., Rosset, C., Rossetti, M., Roudier, G., Rubino-Martin, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Sutton, D., Suur-Uski, A.S., Sygnet, J.F., Tauber, J.A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Turler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A.“…Our 2015 LFI analysis provides an independent Solar dipole estimate in excellent agreement with that of HFI and within $1\sigma$ (0.3 % in amplitude) of the WMAP value. This 0.3 % shift in the peak-to-peak dipole temperature from WMAP and a global overhaul of the iterative calibration code increases the overall level of the LFI maps by 0.45 % (30 GHz), 0.64 % (44 GHz), and 0.82 % (70 GHz) in temperature with respect to the 2013 Planck data release, thus reducing the discrepancy with the power spectrum measured by WMAP. …”
Publicado 2015
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26“…Recent cosmological observations of unprecented accuracy, by WMAP in particular, have established a `Standard Model' of cosmology, just as LEP established the Standard Model of particle physics. …”
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27“…If we assume for local f_NL a central value of order 60, according to recent WMAP 5-years estimates, we obtain for Planck a final correction \Delta f_NL = 3. …”
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28“…In this case the overall fine tuning and Higgs mass are only marginally larger for the case SUSY dark matter is subdominant and rises to $\Delta=28.7$ ($m_h=116.98\pm 2$ GeV) for the case of SUSY dark matter saturates the WMAP bound. For a Higgs mass above these values, fine tuning rises exponentially fast. …”
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29por Lubick, N“…Report of the discussions surrounding the release of data from the Wilkinson Microwave Anisotropy Probe (WMAP) at the Inflation '03 conference in Davis, California in March (1 page).…”
Publicado 2003
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30por Huitu, Katri, Kinnunen, Ritva, Laamanen, Jari, Lehti, Sami, Roy, Sourov, Salminen, Tapio“…The allowed parameter space in the light of the WMAP constraints on the cold dark matter relic density is investigated in the above scenarios for gaugino mass parameters. …”
Publicado 2008
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31por Ellis, John R.“…The sneutrino inflation hypothesis makes specific, testable predictions for cosmic microwave background observables, which are compatible with the first release of data from WMAP, and for flavour-violating charged-lepton decays. …”
Publicado 2004
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33por Geralis, T.“…CAST is aiming at surpassing the 1eV WMAP upper limit and possibly revisiting the operation in vacuum with extra sensitive X-ray detectors, while ADMX, using improved extra sensitive SQUID amplifiers will explore the micro-eV mass range.…”
Publicado 2009
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34por Ellis, John R.“…Additionally, a first attempt is made to place in context the exciting new results from the WMAP satellite, which were published shortly after this Meeting. …”
Publicado 2003
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35“…Despite the extra-weak interactions massive particles of this type (XWIMPs) can satisfy the WMAP relic density constraints due to coannihilation if their masses are close to that of the lightest state of the MSSM. …”
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36“…We give parametrizations of WMAP strips with large tan beta and fixed A_0/m_0 > 0 that include portions compatible with m_h = 125 GeV, and present predictions for spin-independent elastic dark matter scattering along these strips. …”
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37“…Extensions of the Standard Model with an extra U'(1) abelian group generically generate terms coming from loops of heavy fermions, leading to three gauge boson couplings, in particular Z'Z gamma. We show that WMAP data constrains the gauge coupling of the group g_D to values comparable with the electro-weak ones, rather independently of the mass of Z'. …”
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38“…We present a specific model for cosmological inflation driven by the Liouville field in a non-critical supersymmetric string framework, in which the departure from criticality is due to open strings stretched between the two moving Type-II 5-branes. We use WMAP and other data on fluctuations in the cosmic microwave background to fix parameters of the model, such as the relative separation and velocity of the 5-branes, respecting also the constraints imposed by data on light propagation from distant gamma-ray bursters. …”
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39por Ade, P.A.R., Aghanim, N., Alves, M.I.R., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartlett, J.G., Bartolo, N., Battaner, E., Benabed, K., Benoit, A., Benoit-Levy, A., Bernard, J.P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.F., Catalano, A., Challinor, A., Chamballu, A., Chary, R.R., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., Couchot, F., Coulais, A., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J.M., Desert, F.X., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Dore, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Ensslin, T.A., Eriksen, H.K., Falgarone, E., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Heraud, Y., Gjerlow, E., Gonzalez-Nuevo, J., Gorski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J.E., Hansen, F.K., Hanson, D., Harrison, D.L., Helou, G., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J.M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Marshall, D.J., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., McGehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschenes, M.A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J.A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Norgaard-Nielsen, H.U., Noviello, F., Novikov, D., Novikov, I., Orlando, E., Oxborrow, C.A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Pratt, G.W., Prezeau, G., Prunet, S., Puget, J.L., Rachen, J.P., Reach, W.T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubino-Martin, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Stompor, R., Strong, A.W., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A.S., Sygnet, J.F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vidal, M., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A.“…(abridged) We discuss the Galactic foreground emission between 20 and 100GHz based on observations by Planck/WMAP. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. …”
Publicado 2015
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40por Giovannini, Massimo“…It is argued that curvature inhomogeneities, compatible with the WMAP 7yr data, shift to lower wavenumbers the magnetic diffusivity scale.…”
Publicado 2011
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