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M ACRO.Atmospheric Neutrinos , MMs, ....

M ACRO.Atmospheric Neutrinos , MMs,. G. Giacomelli University of Bologna and INFN Caltech, 21 jan 2005, Peck-Fest. Introduction 2. Early n oscillation analyses 3. Monte Carlos 4. Final oscillation analyses 5. Search for LIV contributions 6. Search for GUT MMs, Nuclearites, ……

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M ACRO.Atmospheric Neutrinos , MMs, ....

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  1. MACRO.AtmosphericNeutrinos, MMs,.... G. Giacomelli University of Bologna and INFN Caltech, 21 jan 2005, Peck-Fest • Introduction • 2. Earlyn oscillation analyses • 3. Monte Carlos • 4. Final oscillation analyses • 5. Search for LIV contributions • 6. Search for GUT MMs, Nuclearites, …… • 7. Conclusions MACRO: Bari, Bologna, Boston, Caltech, Drexel, Frascati, Gran Sasso, Indiana, L’Aquila, Lecce, Michigan, Napoli, Pisa, Roma, Texas, Torino. Oujda

  2. The MACRO experiment 1984 : Proposal 1987 : Construction starts 1989 : First Supermodule ON 4/1994 : Full detector ON 12/2000 : Rest In Peace

  3. Upthroughgoing In up Absorber Streamer Scintillator In down Upstop 1) 4) 3) 2) DATA SAMPLES(measured) (Bartol96 expected) __________________________ Upthrough(1) 857 1169 In up(2) 157 285In down(3)+ Up stop(4) 262 375

  4. 1984 MACRO Proposal

  5. Effects of nmoscillations on upthroughgoing events Flux reduction depending on zenith angle for the high energy events   underground detector Earth From MC: distortion of the angular distribution

  6. 2. Early analyses { Upthrough m only Angular distribution Absolute value (Bartol96 MC) Very earlyPhys.Lett. B357(1995)481 EarlyDm2=0.0025 eV2 Phys.Lett. B434(1998)451 Maximal mixing Phys.Lett. B517(2001)59 Lower energy topologies consistent with upthrough m { nm energy estimate through Multiple Coulomb Scattering of upthroughgoing muonsPhys.Lett. B566(2003)35

  7. 3. Atmospheric n flux. Monte Carlos -Until 2001 Bartol96 (Honda96) -After 2001FLUKA2001-3 (Honda2001-3) Both 3-dimensional improved interaction models new cosmic ray fit, ..... They agree to ~5% But: Predictions of new Honda and FLUKA MCs H.E. 25% low ; L.E. 12% low -Angular distributions of Bartol96, new Honda and FLUKA MCs agree to ~<6% New L3cosmic data favor Bartol96

  8. From the muon zenith angle distribution. L(cosQ=-1)~13000 km L(cosQ=0)~500 km MACRO data MonteCarlos n1

  9. Very early data. Scintillators with PHRASE electronics Agrees with standard procedure and shows “bump”

  10. OSCILLATION HYPOTHESIS Minimum value for nm nt : Rtmin =1.61 Minimum value for nmnsterile : Rstmin =2.03 PROBABILITY FOR R < Rmin : Pt= 7.2% ; Psterile = 0.015% Pt/Psterile = 480 nmnsterile hypothesis disfavoured at 99.8 % C.L. with respect to nm nt nm nt or nmnsterile ? Phys. Lett. B517 (2001) 59 Eur. Phys. J. C36 (2004) 357

  11. MC predictions for nm nt oscillations with the best MACRO parameters L/En distribution From the muon zenith distribution From the measurement of the muon energy using Multiple Coulomb Scattering Upthr. m data IU m data 12% point-to-point syst. error

  12. Low Energy Neutrino Events Internal Up Internal Down + Up-stopping m Measured (points) and expected number (dashed lines: MC Bartol96) of upgoing semicontained events (left) and up-stopping plus downgoing semicontained m (right). Solid lines: oscillations with the best fit parameterssin22Q=1 and Dm2=0.0023 eV2. <En>=2.3 GeV . Monte Carlo scale uncertainty 21%

  13. Zenithdistribution R2= N(low En) / N(high En) En estimate IU, ID and UGS m R3= N(ID+UGS) / N(IU) No oscillation hypothesis ruled out by ~ 5 s Best fit parameters for nm nt Dm2 = 2.3 10-3 eV2 ; sin2 2q =1 Eur. Phys. J. C36(2004)357 4. Final oscillation analyses Use ratios with uncertainties of ~5%, indep of MCs { R1= N(cos Q < -0.7) /N(cosQ > -0.4) H.E. L.E. Absolute values referred to Bartol96 MC : R4=(Data/MC)H.E. ; R5=(Data/MC)L.E. With these informations, the no oscillation hypothesis is ruled out by ~ 6 s

  14. MACRO D q

  15. Exotic oscillations Lorentz invariance violation (LIV) Mixing between flavor and velocity eigenstates (asymptotic vn different from c)  dependence LEn  LIV is not dominant We computed upper limits of LIV parameters dv/2=(v3-v2)/2 , sin2 2θv using the formalism of Coleman-Glashow PL B405(1997)249; hep-ph/0407087 , taking the Nlow, Nhigh samples of low and high energy upthroughgoing data, fixing n mass oscillation parameters to the MACRO values and using the Feldman-Cousin procedure Violation of the equivalence principle Similar results as for LIV, but with parameter fDg [ Dg= difference of coupling constants of n to grav pot f] Fogli hep-ph/9904248

  16. L=10000 km , Dm2=0.0023 eV2 , sin22θm=1 , sin22θv=1

  17. )

  18. Flux upper limits for GUT MMs EPJ C25 (2002) 511 -5 -4 Direct searches , g = gD , isotropic flux , scat < 1 mb

  19. The Lab in Hall B (to the tune of House at Pooh Corner) Christopher Walter and I rode along On the road to the Fiordigigli Posing our questions to Sciubba and PeckOn our way to get tortelliniBut we spent more time schmoozing Today than we had And we've got to get back To the external lab So help me if you can, I've got to get Back there to catch the navetta by one You'd be surprised there's so much to be done: Clean up the oil that we've spilled Fix all the tubes that we've killedBack to the lab beneath the Gran Sasso Back to the slab beneath the Gran SassoBack to the lab in Hall B Back to the lab in Hall B Return to the Macro song parodies home page nolty_r@caltech.edu

  20. Catalysis of proton decay GUT MM – p interaction may violate baryon and lepton number conservation M + p M + e+ + p0 If sB0 ~ score ~ 10-56 cm2 ~ negligible Rubakov-Callan mechanism If sB0 ~ sstrong could see a string of p decays along MM trajectory sB0 ~ s0/b (or s0/b2) p-decay detectors IMB  < 13 10-15 cm-2 sr-1 s-1 10-5< b < 10-1 Kamiokande 5 10-5 < b < 10-3 n-telescopes Lake Baikal  < 6 10-17 cm-2 sr-1 s-1b ~ 10-5

  21. e+ MM • s= 5 10-25 cm 2 s= 10-24 cm 2 MACRO: dedicated search for MM induced p decay using the streamer tube system S = 4250 m2sr , t = 70,000 hours Look for Slow MM track Fast e+ track EPJ C26 (2002) 163

  22. Magnetic Monopole searches • GUT MM, mM˜1016 GeV • Sensitivity well below the Parker bound, 10-15 cm -2s -1sr –1 • Good efficiency for • ~5x10-5 <b=v/c<1 • Redundancy: 3 different sub-detectors • Sensitivity for catalysis of nucleon-decay induced by MM • NO Candidates

  23. uud u d u d u d u d d u s s u d udd < < uud udd quark matter (non strange) nuclearites nuclei NUCLEARITESE. Witten, Phys. Rev. D30 (1984) 272A. De Rujula, S. L. Glashow, Nature 312 (1984) 734 • Aggregates of u, d, s quarks + electrons , ne=2/3 nu –1/3 nd –1/3 ns • Ground state of nuclear matter; stable for any barion number A :300 < A < 1057 • Z~A1/3 ?, ~A2/3 ? ; Z/A << 1 , rN3.5 x 10 14 g cm-3(rnuclei 1014 g cm-3) Produced in Early Universe:candidates for cold Dark Matter Searched for in CR reaching the Earth [black points are electrons] RN = 102 fm 103 fm 104 fm 105 fm 106 fm MN = 106 GeV109GeV1012 GeV1015 GeV

  24. High Mass Nuclearites: present situation: White Mountain 4800 m a.s.l. Mt. Norikura 2000 m a.s.l. Ohya : 100 hg/cm2 undergr. MACRO : 3700 hg/cm2 undergr.

  25. NATO ARW, Oujda, spring 2001

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