The Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data provide stringent limits on deviations from the minimal, six-parameter Λ cold dark matter model. We report these limits and use them to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature. We also constrain models of dark energy via its equation of state, parity-violating interaction, and neutrino properties, such as mass and the number of species. We detect no convincing deviations from the minimal model. The six parameters and the corresponding 68% uncertainties, derived from the WMAP data combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO) in the distribution of galaxies, are: Ω b h 2 = 0.02267+0.00058 –0.00059, Ω c h 2 = 0.1131 ± 0.0034, ΩΛ = 0.726 ± 0.015, ns = 0.960 ± 0.013, τ = 0.084 ± 0.016, and at k = 0.002 Mpc-1. From these, we derive σ8 = 0.812 ± 0.026, H 0 = 70.5 ± 1.3 km s-1 Mpc–1, Ω b = 0.0456 ± 0.0015, Ω c = 0.228 ± 0.013, Ω m h 2 = 0.1358+0.0037 –0.0036, z reion = 10.9 ± 1.4, and t 0 = 13.72 ± 0.12 Gyr. With the WMAP data combined with BAO and SN, we find the limit on the tensor-to-scalar ratio of r 1 is disfavored even when gravitational waves are included, which constrains the models of inflation that can produce significant gravitational waves, such as chaotic or power-law inflation models, or a blue spectrum, such as hybrid inflation models. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: –0.14 < 1 + w < 0.12(95%CL) and –0.0179 < Ω k < 0.0081(95%CL). We provide a set of WMAP distance priors, to test a variety of dark energy models with spatial curvature. We test a time-dependent w with a present value constrained as –0.33 < 1 + w 0 < 0.21 (95% CL). Temperature and dark matter fluctuations are found to obey the adiabatic relation to within 8.9% and 2.1% for the axion-type and curvaton-type dark matter, respectively. The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than –59 < Δα < 24 (95% CL) between the decoupling and the present epoch. We find the limit on the total mass of massive neutrinos of ∑m ν < 0.67 eV(95%CL), which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom (dof), expressed in units of the effective number of neutrino species, is constrained as N eff = 4.4 ± 1.5 (68%), consistent with the standard value of 3.04. Finally, quantitative limits on physically-motivated primordial non-Gaussianity parameters are –9 < f local NL < 111 (95% CL) and –151 < f equil NL < 253 (95% CL) for the local and equilateral models, respectively.

https://iopscience.iop.org/article/10.1088/0067-0049/180/2/330/pdf

Five-year wilkinson microwave anisotropy probe observations: cosmological interpretation

Strong constraints on the cosmic star formation history (SFH) have recently been established using ultraviolet and far-infrared measurements, refining the results of numerous measurements over the past decade. The data show a compellingly consistent picture of the SFH out to redshift z ≈ 6, with especially tight constraints for z 1. We fit these data with simple analytical forms and derive conservative uncertainties. Since the z 1 SFH data are quite precise, we investigate the sequence of assumptions and corrections that together affect the SFH normalization to test their accuracy, both in this redshift range and beyond. As lower limits on this normalization, we consider the evolution in stellar and metal mass densities, and supernova rate density, finding it unlikely that the SFH normalization is much lower than indicated by our direct fit. As a corresponding upper limit on the SFH normalization, we consider the Super-Kamiokande limit on the electron antineutrino (e) flux from past core-collapse supernovae, which applies primarily to z 1. We find consistency with the SFH only if the neutrino temperatures from supernova events are relatively modest. Constraints on the assumed initial mass function (IMF) also become apparent. The traditional Salpeter IMF, assumed for convenience by many authors, is known to be a poor representation at low stellar masses (1 M☉), and we show that recently favored IMFs are also constrained. In particular, somewhat shallow, or top-heavy, IMFs may be preferred, although they cannot be too top-heavy. To resolve the outstanding issues, improved data are called for on the supernova rate density evolution, the ranges of stellar masses leading to core-collapse and type Ia supernovae, and the antineutrino and neutrino backgrounds from core-collapse supernovae.

https://iopscience.iop.org/article/10.1086/506610/pdf

On the Normalization of the Cosmic Star Formation History

Tri-bimaximal mixing and the neutrino oscillation data

We update the constraints on the fraction of the Universe going into primordial black holes in the mass range ${10}^{9}--{10}^{17}\text{ }\text{ }\mathrm{g}$ associated with the effects of their evaporations on big bang nucleosynthesis and the extragalactic photon background. We include for the first time all the effects of quark and gluon emission by black holes on these constraints and account for the latest observational developments. We then discuss the other constraints in this mass range and show that these are weaker than the nucleosynthesis and photon background limits, apart from a small range ${10}^{13}--{10}^{14}\text{ }\text{ }\mathrm{g}$, where the damping of cosmic microwave background anisotropies dominates. Finally we review the gravitational and astrophysical effects of nonevaporating primordial black holes, updating constraints over the broader mass range $1--{10}^{50}\text{ }\text{ }\mathrm{g}$.

New cosmological constraints on primordial black holes

R-Parity-violating supersymmetry

Y.Fukuda, K.Ishihara, Y.Itow, T.Kajita, J.Kameda, S.Kasuga, K.Kobayashi, Y.Kobayashi, Y.Koshio, M.Miura, M.Nakahata, S.Nakayama, Y.Obayashi, A.Okada, K.Okumura, N.Sakurai, M.Shiozawa, Y.Suzuki, H.Takeuchi, Y.Takeuchi, Y.Totsuka, S.Yamada, M.Earl, A.Habig, E.Kearns, M.D.Messier, K.Scholberg, J.L.Stone, L.R.Sulak, C.W.Walter, M.Goldhaber, T.Barszczak, D.Casper, W.Gajewski, W.R.Kropp, S.Mine, L.R.Price, M.Smy, H.W.Sobel, M.R.Vagins, K.S.Ganezer, W.E.Keig, R.W.Ellsworth , S.Tasaka, A.Kibayashi, J.G.Learned, S.Matsuno, V.J.Stenger, D.Takemori, T.Ishii, H.Ishino, T.Kobayashi, K.Nakamura, Y.Oyama, A.Sakai, M.Sakuda, O.Sasaki, S.Echigo, M.Kohama, A.T.Suzuki , T.Inagaki, K.Nishikawa, T.J.Haines, E.Blaufuss, B.K.Kim, R.Sanford, R.Svoboda, M.L.Chen, J.A.Goodman, G.W.Sullivan, J.Hill, C.K.Jung, K.Martens, C.Mauger, C.McGrew, E.Sharkey, B.Viren, C.Yanagisawa, W.Doki, M.Kirisawa, S.Inaba, K.Miyano, H.Okazawa, C.Saji, M.Takahashi, M.Takahata, K.Higuchi, Y.Nagashima, M.Takita, T.Yamaguchi, M.Yoshida, S.B.Kim, M.Etoh, A.Hasegawa, T.Hasegawa, S.Hatakeyama, K.Inoue, T.Iwamoto, M.Koga, T.Maruyama, H.Ogawa, J.Shirai, A.Suzuki, F.Tsushima, M.Koshiba, Y.Hatakeyama, M.Koike, M.Nemoto, K.Nishijima, H.Fujiyasu, T.Futagami, Y.Hayato, Y.Kanaya, K.Kaneyuki, Y.Watanabe, D.Kielczewska, J.S.George, A.L.Stachyra, R.J.Wilkes, K.K.Young Institute for Cosmic Ray Research, University of Tokyo, Tanashi, Tokyo 188-8502, Japan Department of Physics, Boston University, Boston, MA 02215, USA Physics Department, Brookhaven National Laboratory, Upton, NY 11973, USA Department of Physics and Astronomy, University of California, Irvine, Irvine, CA 92697-4575, USA Department of Physics, California State University, Dominguez Hills, Carson, CA 90747, USA Department of Physics, George Mason University, Fairfax, VA 22030, USA Department of Physics, Gifu University, Gifu, Gifu 501-1193, Japan Department of Physics and Astronomy, University of Hawaii, Honolulu, HI 96822, USA Inst. of Particle and Nuclear Studies, High Energy Accelerator Research Org. (KEK), Tsukuba, Ibaraki 305-0801, Japan Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan Department of Physics, Kyoto University, Kyoto 606-8502, Japan Physics Division, P-23, Los Alamos National Laboratory, Los Alamos, NM 87544, USA Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA Department of Physics, University of Maryland, College Park, MD 20742, USA Department of Physics and Astronomy, State University of New York, Stony Brook, NY 11794-3800, USA Department of Physics, Niigata University, Niigata, Niigata 950-2181, Japan Department of Physics, Osaka University, Toyonaka, Osaka 560-0043, Japan Department of Physics, Seoul National University, Seoul 151-742, Korea Department of Physics, Tohoku University, Sendai, Miyagi 980-8578, Japan The University of Tokyo, Tokyo 113-0033, Japan Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan Department of Physics, Tokyo Institute for Technology, Meguro, Tokyo 152-8551, Japan Institute of Experimental Physics, Warsaw University, 00-681 Warsaw, Poland Department of Physics, University of Washington, Seattle, WA 98195-1560, USA

T. Ishii

Papers

99 08 04 9 v 3 1 D ec 1 99 9 Neutrino-induced upward stopping muons in Super-Kamiokande ( March 25 , 2022 ) The Super-Kamiokande Collaboration