1 / 87

AGENDA: 1) Neutrinos 2) Dark matter, Axions, LFV search. 3) Kaons and B-mesons

MORIOND 2005. AGENDA: 1) Neutrinos 2) Dark matter, Axions, LFV search. 3) Kaons and B-mesons 4) LEP,Hera and the Tevatron 5) Hints of new physics?. What to answer if you are ask: …….what’s new in Moriond?. M.Calvetti INFN-Laboratori Nazionali di Frascati and Università di Firenze. 7.

gallia
Download Presentation

AGENDA: 1) Neutrinos 2) Dark matter, Axions, LFV search. 3) Kaons and B-mesons

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. MORIOND 2005 AGENDA: 1) Neutrinos 2) Dark matter, Axions, LFV search. 3) Kaons and B-mesons 4) LEP,Hera and the Tevatron 5) Hints of new physics? What to answer if you are ask: …….what’s new in Moriond? M.Calvetti INFN-Laboratori Nazionali di Frascati and Università di Firenze

  2. 7 Super-Kamiokande atmospheric ’s For 13~0 and m2~0, a very simple formula fits all SK data(+ MACRO & Soudan2) 1st oscillation dip still visible despite large L & E smearing Strong constraints on the parameters (m2, 23) ……..NEUTRINOS………… E.Lisi

  3. L.Sulak Super-Kamiokande atmospheric ’s

  4. Charged Current: • Detect the e- • energy spectrum • Weak directional sensitivity • Detect the n through secondary capture • No directional or neutrino energy info Neutral Current: • Detect the e- • Mainly sensitive to • Highly directional Elastic Scattering: K.Miknaitis SNO’s Three Reactions

  5. K.Miknaitis Energy Isotropy 20 Radius Direction

  6. 391- day salt results! K.Miknaitis

  7. SNO SOLAR K.Miknaitis • Ratio of the measured CC,ES,NC reaction rates to the SSM prediction, assuming undistorted CC, ES energy spectra.

  8. 14 Exercise: (1) Change MSW potential “by hand,” V aMSWV (2) Reanalyze all data with (m2,12,aMSW) free (3) Project (m2,12) away and check if aMSW~1 (… a way of “measuring” GF through solar neutrino oscillations …) Results: with 2004 data, aMSW~1 confirmed within factor of ~2 and aMSW~0 excluded Evidence for MSW effects in the Sun But: expected subleading effect in the Earth (day-night difference) still below experimental uncertainties. E.Lisi What about the neutrino masses? We have only limits…..

  9. Day-Night Asymmetries (II) K.Miknaitis Constraining ANC to be zero: ACC= -0.037 ± 0.063(stat.) ±0.032(syst.) AES= 0.153 ± 0.198(stat.) ±0.030(syst.) Combine with analogous ACC from the salt phase: Convert Super-Kamiokande AES to Ae, and combine with SNO: In the pure-D2O phase, (shape constrained, ANC constrained)

  10. …..but …do neutrinos oscillate also on earth?

  11. First Reactor Antineutrino Result • Observed neutrino disappearance: • (Nobs–NBG)/Nno-osc = 0.611  0.085 (stat)  0.041 (syst) • “Standard” ne propagation ruled out at the99.95% confidence level Rate! Energy Rencontres de Moriond – March 6, 2005

  12. Direct observation of the oscillation L0/E Plot • Goodness of fit: • 0.7% - decay • 1.8% - decoherence • 11.1% - oscillation • (0.4% - constant suppression) • Data prefer oscillation to other • hypotheses Data vs. No-oscillation expectation Rencontres de Moriond – March 6, 2005

  13. K2K experiment ~1 event/2days ~1011nm/2.2sec (/10m10m) ~106nm/2.2sec (/40m40m) nm 12GeV protons nt SK p+ m+ Target+Horn 100m ~250km 200m decay pipe p monitor Near n detectors (ND) m monitor (monitor the beam center) • Signal of n oscillation at K2K • Reduction of nm events • Distortion of nm energy spectrum C.Mariani

  14. obs SK N=107 N =150.9 +12 -10 1KT Flux measurement • The same detector technology as Super-K. • Sensitive to low energy neutrinos. Far/Near Ratio (by MC)~1×10-6 M: Fiducial mass MSK=22,500Kton, MKT=25ton e: efficiency eSK-I(II)=77.0(78.2)%, eKT=74.5% exp SK C.Mariani

  15. Data are consistent with the oscillation. • With 8.9×1019 POT, K2K has confirmed neutrino oscillations at 4.0s (hep-ex/0411038). • Disappearance of nm 3.0s • Distortion of En spectrum 2.6s preliminary Dm2[eV2] Best Fit KS prob.=36% sin22q Enrec[GeV] C.Mariani

  16. LMC ? m+ K+ νμ→νe 8GeV p+ nm Booster magnetic horn decay pipe 450 m dirt detector absorber and target 25 or 50 m Introducing MiniBooNE: The Booster Neutrino Experiment • The goal: to check the LSND result.

  17. Conclusions ...best wishes... • MiniBooNE is running well. • Currently 4.57×1020 protons on target. • νμ  νe appearance results by hopefully late 2005.

  18. eV m0 Neutrino masses in 3-neutrino schemes From present evidences of atmospheric and solar neutrino oscillations eV solar atm atm solar 3 degenerate massive neutrinos Σmν = 3m0 S.Pastor

  19. Conclusions Cosmological observables efficiently constrain some properties of (relic) neutrinos ν Bounds on the sum of neutrino masses from CMB + 2dFGRS or SDSS, and other cosmological data (best Σmν<0.42 eV, conservative Σmν<1 eV) Sub-eV sensitivity in the next future (0.1-0.2 eV and better)  Test degenerate mass region and eventually the IH case S.Pastor

  20. galaxy weak lensing and CMB lensing Future sensitivities to Σmν: new ideas sensitivity of future weak lensing survey (4000º)2 to mν σ(mν) ~ 0.1 eV Abazajian & Dodelson PRL 91 (2003) 041301 sensitivity of CMB (primary + lensing) to mν σ(mν) = 0.15 eV (Planck) σ(mν) = 0.04 eV (CMBpol) Kaplinghat, Knox & Song PRL 91 (2003) 241301 S.Pastor

  21. 19 Numerical ±2 ranges (95% CL for 1dof), 2004 data: See the contribution from B.Kayser on “neutrino future” Note: Precise values for 12and 23relevant for model building (see talk by Tanimoto) E.Lisi

  22. Experiments measuring……zero’s Double Beta Decay Proton decay search Dark matter search Axions Vacuum polarization Lepton Flavour Violation

  23. R&D: Cleaning test (September-November 2004) Cu: etching, electropolishing and passivation TeO2: etching and lapping with clean powders Assembling with clean materials S.Capelli

  24. CUORICINOresults Background (@DBD0): 0.18 ± 0.01 c/keV/kg/y => Total Statistics: 10.85 kgxy reduction of ~ 2 (4) with respect to MiDBD-II (I) arXiv:hep-ex/0501034 v1 DBD0 result: T1/2130Te <m> < [0.2÷1.1] eV > 1.8 x 1024 y 130Te (DBD0n) <mn> < 0.07- 0.5 eV In 5 years… S.Capelli

  25. CUORE sensitivity Sensitivity (1): b=0.001 c/keV/kg/y =5 keV F0=2.9x1026√t y <m>=0.01÷0.06 eV b=0.01 c/keV/kg/y =5 keV F0=9.2x1025√t y <m>=0.02÷0.1 eV CUORE bkg goal: 0.001 ÷ 0.01 c/keV/kg/y 5 years best wishes..... …very interesting…… S.Capelli

  26. LFV in the Standard Model • Neutrino oscillations flavour mixing in lepton sector • Extensions of SM with massive Dirac neutrinos allowLFV also with charged leptons (meg , teg , meee , me) larger mass scale needed  SUSY not observable! D.Nicolò

  27. Conclusions •  are sensitive probes of physics beyond the Standard Model • SUSY-SUGRA theories predicts LFV not far from present existing upper limits • Strong case for experimental searches in all channels • +e+results are expected in 2007 (10-13) • -e-conversion search is planned at the level of 10-16 • -e-conversion is not accidental background limitedcould benefit of new high intensity pulsed beams best wishes..... …….to work hard….. D.Nicolò

  28. Proton life time ….a lower limit… PROTONS (do not) DECAY…….. L.Sulak

  29. P life-time IMB limits 45 decay modes ...S-K 7 times bigger than IMB, limits generally 7 times better ...mass is everything!!! MEGATON is needed, 20 times bigger than S-K L.Sulak

  30. CAST: Principle of detection Transverse magnetic field (B) Axion X-ray (same energy and momentum) X-ray detector L [Sikivie PRL 51 (1983)] • Expected number of photons in the x-ray detector: Differential axion flux at the Earth (cm-2 s -1 keV -1 ) Conversion probability of an axion into photon ( (B×L)2) For gaγγ =1×1O-10 GeV-1 t=100 h , S=15 cm2 N γ ≈ 30 events S Magnet bore area (cm2) t Measurement time (s)

  31. CAST 2003 result Axion exclusion plot • Combined upper limit obtained (95% C.L.): gaγγ<1.16×10-10 GeV-1 best wishes.....

  32. DARK MATTER SEARCH CRESST-II Detector Concept Discrimination of nuclear recoils from radioactive + backgrounds (electron recoils) by simultaneous measurement of phonons and scintillation light proof of principle Separate calorimeter as light detector W-thermometer Energy in light channel keVee] 300 g scintillatingCaWO4 crystal DM nuclei W-thermometer Energy in phonon channel [keV] light reflector

  33. CDMS II Overview • WIMPS (and neutrons) scatter off nuclei Identify nuclear recoilsevent by event! Nuclear Recoils (252Cf) Nuclear Recoils (252Cf) • Surface events: • Electrons produced by radioactive beta decays from surface contamination • Electrons ejected from nearby material by high energy x-rays • Gammas interacting within ~10 mm of the surface Y~ 0.3 (Ge) for nuclear recoils Nuclear Recoils (252Cf) Nuclear Recoils (252Cf) • Events occuring near the surface (<~10 mm) have an incomplete charge collection (“dead layer”) and can be misidentified as nuclear recoils Measure simultaneously ionization and athermal phonons • Most background sources (electrons, photons) scatter off electrons Bulk Electron Recoils (133Ba) Bulk Electron Recoils (133Ba) Ionization Yield  EQ/ER Y~ 1 for electron recoils

  34. Yellow points from neutron calibration Event WIMPs search data with Ge detectors (Run118) • Blue points from WIMP search data (Z2, Z3, Z5) After timing cuts Prior to timing cuts Charge Yield Charge Yield Recoil energy (keV) Recoil energy (keV) Expected background : 0.7 ± 0.35 mis-identified surface electron recoils

  35. DAMA ZEPLIN Edelweiss CDMS CDMS_Projections Egret CRESST

  36. …..….discoveries?.......... 1) Egret excess signal……. 2) PVLAS…………

  37.   f f f ~ f A Z    f f f   W Z 0    Z W DM annihilation in Supersymmetry ≈ 37 gammas B-fragmentation well studied at LEP! Yield and spectra of positrons, gammas and antiprotons well known! Dominant diagram for WMAP cross section in MSSM:  +   A  b bbar quark pair Galaxy = SUPER-B-factory with luminosity some 40 orders of magnitude above man-made B-factories

  38. WIMP MASS 50 - 100 GeV 65 100 0 WIMPS IC Extragal. Bremsstr. Excess of Diffuse Gamma Rays has same spectrum in all directions compatible with WIMP mass of 50-100 GeV Egret Excess above extrapolated background from data below 0.5 GeV Statistical errors only Excess same shape in all regions implying same source everywhere Important: if experiment measures gamma rays down to 0.1 GeV, then normalizations of DM annihilation and background can both be left free, so one is not sensitive to abso- lute background estimates, BUT ONLY TO THE SHAPE, which is much better known.

  39. Diffuse Gamma Rays for different sky regions Good Fits for WIMP masses between 50 and 100 GeV A: inner Galaxy B: outer disc C: outer Galaxy E: intermediate lat. F: galactic poles D: low latitude 3 components: galactic background + extragalactic bg + DM annihilation fitted simultaneously with same WIMP mass and DM normalization in all directions. Boost factor around 70 in all directions and statistical significance > 10 !

  40. Instead of conclusions sneutrino-driven chaotic inflation e probably observable in the next round of exps.(Chankowski et al.,2004) nonthermal leptogenesis in inflaton decay ‘It is a capital mistake to theorize before one has data’ enhancement of 1 from small mass splittings of singlet neutrinos partly compensated due to consistency conditions, but leptogenesis OK e unobservable masses of 2 singlet neutrinos degenerate at the GUT scale (kt,2004) large neutrino Yukawa couplings cancelling out in the seesaw formula(Raidal et al.,2005) successful leptogenesis from small M1 due to overcoming DI bound r=1 form0=100 GeV, M1/2=200 GeV K.Turzynski

  41. …interesting….but…… ? Is it a capital mistake to theorize (too much) when one has data? ……new results coming……..

  42. PVLAS U.Gastaldi Laser light ….big discovery!!!... ….but…do we belive to it….

  43. U.Gastaldi Observed dichroism of Vacuum with infrared Laser light 1eV …..Spin 0 boson…… 0 -+ m=10-3 eV M=5 105 GeV Axion???? Dark matter??? ….to be confirmed…….. ….to be young …< 60 ….. best wishes.....

  44. Nice good results…….from LEP

  45. incompatible LEP Result OPAL fit OPAL fit b = (726  96  70)  10-5 G.Abbiendi

  46. LEP Results Slope b = (726  96  70  50)  10-5 Significance:5.6s including all errors for the total running SM : 460  10-5 using the Burkhardt-Pietrzyk parameterization Most significant direct observation of the running of aQED ever achieved contributions to the slope b in our t range are predicted to be in the proportion: e : m : hadron ≈ 1 : 1 : 2.5 subtracting the precisely calculable leptonic contribution: Hadronic contribution to the running: First Direct Experimental evidencewith Significance of 3.0s including all errors G.Abbiendi

  47. NA48 -kaons-kaons-kaons-kaons-kaons- KLOE KTeV NA48 E949 |Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN 30

More Related