Matter effects in upward-going muons and sterile neutrino oscillations

Ambrosio, M.; Antolini, R.; Auriemma, G.; Bakari, D.; Baldini, A.; Barbarino, G. C.; Barish, B.; Battistoni, G.; Becherini, Y.; Bellotti, R.; Bemporad, C.; Bernardini, P.; Bilokon, H.; Bisi, V.; Bloise, C.; Bower, C.; Brigida, M.; Bussino, S.; Cafagna, F.; Calicchio, M.; Campana, D.; Carboni, M.; Caruso, R.; Cecchini, S.; Cei, F.; Chiarella, V.; Choudhary, B. C.; Coutu, S.; Cataldo, G. de; Dekhissi, H.; Marzo, C. De; Mitri, I. De; Derkaoui, J. E.; Vincenzi, M. De; Credico, A. Di; Erriquez, O.; Favuzzi, C.; Forti, C.; Fusco, P.; Giacomelli, G.; Giannini, T.; Giglietto, N.; Giorgini, M.; Grassi, M.; Gray, L.; Grillo, A.; Guarino, F.; Gustavino, C.; Habig, A.; Hanson, K.; Heinz, R.; Iarocci, E.; Katsavounidis, E.; Katsavounidis, I.; Kearns, E.; Kim, H.; Kyriazopoulou, S.; Lamanna, E.; Lane, C.; Levin, D.; Lipari, P.; Longley, N. P.; Longo, M. J.; Loparco, F.; Maaroufi, F.; Mancarella, G.; Mandrioli, G.; Margiotta, A.; Marini, A.; Martello, D.; Marzari‐Chiesa, A.; Mazziotta, M. N.; Michael, D. G.; Mikheyev, S.; Miller, Laura Stephanie; Monacelli, P.; Montaruli, T.; Monteno, M.; Mufson, S.; Musser, J.; Nicoló, D.; Nolty, R.; Orth, C. J.; Osteria, G.; Palamara, O.; Patera, V.; Patrizii, L.; Pazzi, R.; Peck, C. W.; Perrone, L.; Petrera, S.; Pistilli, P.; Popa, V.; Rainò, A.; Reynoldson, J.; Ronga, F.; Rrhioua, Abdeslem; Satriano, C.; Scapparone, E.; Scholberg, K.; Sciubba, A.; Serra, P.; Sioli, M.; Sirri, G.; Sitta, M.; Spinelli, P.; Spinetti, M.; Spurio, M.; Steinberg, R.; Stone, J. L.; Sulak, L.; Surdo, A.; Tarlè, G.; Togo, V.; Vakili, M.; Walter, C. W.; Webb, R.

doi:10.1016/s0370-2693(01)00992-3

Cited by 166 publications

(92 citation statements)

References 33 publications

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“…The Super-Kamiokande data is best fit by the oscillation hypothesis with parameters (sin 2 2θ 23 , ∆m 2 23 ) = (1.0, 2.4×10 −3 eV 2 ) [8,9]; the ranges for these parameters given by the 90% confidence contours of the zenith angle oscillation fit are sin 2 2θ 23 > 0.92 and 1.5 < ∆m 2 23 < 3.4 × 10 −3 eV 2 . The MACRO [13,14] and Soudan 2 [15,16] results are consistent with those obtained by Super-Kamiokande. For the MINOS analysis of atmospheric neutrinos with an interaction vertex in the detector, the parameter ranges are sin 2 2θ 23 > 0.2 and 7 × 10 −5 < ∆m 2 23 < 5 × 10 −2 eV 2 [17].…”

Section: Pacs Numberssupporting

confidence: 82%

Charge-separated atmospheric neutrino-induced muons in the MINOS far detector

Adamson¹,

Andreopoulos²,

Arms³

et al. 2007

Phys. Rev. D

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We found 140 neutrino-induced muons in 854.24 live days in the MINOS far detector, which has an acceptance for neutrino-induced muons of 6.91 × 10 6 cm 2 sr. We looked for evidence of neutrino disappearance in this data set by computing the ratio of the number of low momentum muons to the sum of the number of high momentum and unknown momentum muons for both data and Monte Carlo expectation in the absence of neutrino oscillations. The ratio of data and Monte Carlo ratios, R, is R = 0.65 +0.15 −0.12 (stat) ± 0.09(syst), a result that is consistent with an oscillation signal. A fit to the data for the oscillation parameters sin 2 2θ23 and ∆m 2 23 excludes the null oscillation hypothesis at the 94% confidence level. We separated the muons into µ − and µ + in both the data and Monte Carlo events and found the ratio of the total number of µ − to µ + in both samples. The ratio of those ratios,RCP T , is a test of CPT conservation. The resultR CP T = 0.72 +0.24 −0.18 (stat) +0.08 −0.04 (syst), is consistent with CPT conservation.

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Section: Pacs Numberssupporting

confidence: 82%

Charge-separated atmospheric neutrino-induced muons in the MINOS far detector

Adamson¹,

Andreopoulos²,

Arms³

et al. 2007

Phys. Rev. D

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“…The exact nature of the dark matter in the Universe is still unknown. Relic neutrinos are abundant in the Universe, and from the observations of oscillations of solar and atmospheric neutrinos we know that neutrinos have a mass [2,3,4,5,6,7,8] and will make up a fraction of the dark matter. However, the oscillation experiments can only measure differences in the squared masses of the neutrinos, and not the absolute mass scale, so they cannot tell us how much of the dark matter is in neutrinos.…”

Section: Introductionmentioning

confidence: 99%

Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors

Elgarøy¹,

Lahav²

2003

J. Cosmol. Astropart. Phys.

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Abstract. Solar, atmospheric, and reactor neutrino experiments have confirmed neutrino oscillations, implying that neutrinos have non-zero mass, but without pinning down their absolute masses. While it is established that the effect of neutrinos on the evolution of cosmic structure is small, the upper limits derived from large-scale structure could help significantly to constrain the absolute scale of the neutrino masses. In a recent paper the 2dF Galaxy Redshift Survey (2dFGRS) team provided an upper limit m ν,tot < 2.2 eV , i.e. approximately 0.7 eV for each of the three neutrino flavours, or phrased in terms of their contribution to the matter density, Ω ν /Ω m < 0.16. Here we discuss this analysis in greater detail, considering issues of assumed 'priors' like the matter density Ω m and the bias of the galaxy distribution with respect to the dark matter distribution. As the suppression of the power spectrum depends on the ratio Ω ν /Ω m , we find that the out-of-fashion Mixed Dark Matter model, with Ω ν = 0.2, Ω m = 1 and no cosmological constant, fits both the 2dFGRS power spectrum and the CMB data reasonably well, but only for a Hubble constant H 0 < 50 km s −1 Mpc −1 . As a consequence, excluding low values of the Hubble constant, e.g. with the HST Key Project, is important in order to get a strong upper limit on the neutrino masses. We also comment on the improved limit obtained by the WMAP team, and point out that the main neutrino signature comes from the 2dFGRS and the Lyman α forest.PACS numbers: 95.35.+d, 14.60.Pq, 98.62.Py, 98.80.Es Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors 2

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“…Although the Karlsruhe Rutherford Medium Energy Neutrino Experiment (KARMEN) observed no evidence for neutrino oscillations [2], a joint analysis [3] showed compatibility at 64% CL. Evidence for neutrino oscillations also comes from solar-neutrino [4,5,6,7,8] and reactor-antineutrino experiments [9], which have observed ν e disappearance at ∆m 2 ∼ 8×10 −5 eV 2 , and atmospheric-neutrino [10,11,12,13] and longbaseline accelerator-neutrino experiments [14,15], which have observed ν µ disappearance at ∆m 2 ∼ 3 × 10 −3 eV 2 .…”

mentioning

confidence: 99%