Limits on dark matter WIMPs using upward-going muons in the MACRO detector

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

doi:10.1103/physrevd.60.082002

Cited by 82 publications

(20 citation statements)

References 39 publications

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“…To calculate mean pair separation, mean angular separation of muons and the number of muon pairs we applied weighting 1/N p , where N p is the number of independent muon pairs in the bundle: N p = 1 for double muon events and N p = 3 for triple muon events. This has been done to allow easy comparison between our simulations and results of studies of muon bundles detected in underground experiments (see, for example, [9,11]). Only muons with energy more than 1 GeV (a typical threshold in underground experiments) have been taken into account.…”

Section: Resultsmentioning

confidence: 99%

“…Existing deep underground experiments such as MACRO [10] and LVD [9] are also able to search for an excess of narrow muon bundles over the expected number of conventional muon bundles. In fact, evidence for an excess at separation distances less than 3 m has recently been published by the MACRO collaboration [11]. The authors explained the excess as due to production of muon pairs in the rock.…”

Section: Resultsmentioning

confidence: 99%

“…In [6] it was shown that the process should contribute to the number of narrow muon bundles detected in underground experiments, such as LVD [9] and MACRO [10]. The observation of this effect has been recently reported by the MACRO collaboration [11]. However, the cross-section from [7,8] used in [6] was obtained assuming point-like nuclei with complete screening, which is not a reasonable approximation in this case (see [12] for the discussion).…”

Section: Introductionmentioning

confidence: 94%

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Narrow muon bundles from muon pair production in rock

1999

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We revise the process of muon pair production by high-energy muons in rock using the recently published cross-section. The three-dimensional Monte Carlo code MUSIC has been used to obtain the characteristics of the muon bundles initiated via this process. We have compared them with those of conventional muon bundles initiated in the atmosphere and shown that large underground detectors, capable of collecting hundreds of thousands of multiple muon events, can discriminate statistically muon induced bundles from conventional ones. However, we find that the enhancement of the measured muon decoherence function over that predicted at small distances, recently reported by the MACRO experiment, cannot be explained by the effect of muon pair production alone, unless its cross-section is underestimated by a factor of 3.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 94%

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Narrow muon bundles from muon pair production in rock

1999

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“…Slightly weaker constraints have also been placed by Amanda [62], Baksan [63] and Macro [64]. The approximate Super-Kamiokande constraint is shown as a vertical dotted line in the left frame of figure 8.…”

Section: Jhep10(2008)071mentioning

confidence: 92%

Panglossian prospects for detecting neutralino dark matter in light of natural priors?

Allanach

2008

J. High Energy Phys.

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In most global fits of the constrained minimal supersymmetric model (CMSSM) to indirect data, the a priori likelihoods of any two points in tan β are treated as equal, and the more fundamental µ and B Higgs potential parameters are fixed by potential minimization conditions. We find that, if instead a flat ("natural") prior measure on µ and B is placed, a strong preference exists for the focus point region from fits to particle physics and cosmological data. In particular, we find that the lightest neutralino is strongly favored to be a mixed bino-higgsino (∼ 10% higgsino). Such mixed neutralinos have large elastic scattering cross sections with nuclei, leading to extremely promising prospects for both underground direct detection experiments and neutrino telescopes. In particular, the majority of the posterior probability distribution falls within parameter space within an order of magnitude of current direct detection constraints. Furthermore, neutralino annihilations in the sun are predicted to generate thousands of neutrino induced muon events per years at IceCube. Thus, assuming the framework of the CMSSM and using the natural prior measure, modulo caveats regarding astrophysical uncertainties, we are likely to be living in a world with good prospects for the direct and indirect detection of neutralino dark matter.

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“…PET), in physical check-ups and diagnosis as in-vitro inspection (Radioimmunoassay and Enzyme immunoassay as luminescent, fluorescent, Chemiluminescent Immunoassay), biomedicine, industrial application, in environmental measurement equipment (like dust counters used to detect dust contained in air or liquids, and radiation survey monitors used in nuclear power plants). In astroparticle physics, photons detectors play a crucial role in the detection of fundamental physical processes: in particular, most of the future experiments which aimed at the study of very high-energy (GRB, AGN, SNR) or extremely rare phenomena (dark matter, proton decay, zero neutrinosdouble beta decay, neutrinos from astrophysical sources) [3][4][5][6][7] are based on photons detection. The needs of very high sensitivity push the designing of detectors whose sizes should greatly exceed the dimensions of the largest current installations.…”

Section: Introductionmentioning

confidence: 99%