MORIOND 2005
AGENDA:
1) Neutrinos
2) Dark matter, Axions, LFV search.
3) Kaons and B-mesons
What to answer if you are ask:
4) LEP,Hera and the Tevatron …….what’s new in Moriond?
5) Hints of new physics?
M.Calvetti
INFN-Laboratori Nazionali di Frascati
and Università di Firenze
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 Strong constraints on the
despite large L & E smearing parameters (m2, 23)
E.Lisi
L.Sulak Super-Kamiokande atmospheric ’s
K.Miknaitis
SNO’s Three Reactions
•Detect the e-
Charged Current:
• e energy spectrum
(CC) e d p p e -
• Weak directional
sensitivity
Neutral Current: •Detect the n through
secondary capture
(NC) x d x p n • No directional or
neutrino energy info
•Detect the e-
Elastic Scattering:
•Mainly sensitive to e
(ES) x e- x e- •Highly directional
K.Miknaitis
Energy Isotropy
20
Direction Radius
K.Miknaitis
391- day salt results!
CC 1.68 0.06
0.06 (stat.) 0..09 (syst.)
0 08
CC
NC 4.94 0.21
(stat.) 0.38
(syst.) 0.340 0.023(stat.) 0..031
0 029
0.21 0.34
NC
ES 2.35 0.22
0.22 (stat.) 0..15 (syst.)
0 15
(In units of
10 6 cm 2s 1 )
SOLAR SNO
K.Miknaitis
Ratio of the measured CC,ES,NC reaction rates to the
SSM prediction, assuming undistorted CC, ES energy spectra.
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…..
2( N D)
Day-Night Asymmetries (II) A
K.Miknaitis ND
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
In the pure-D2O the salt phase:
phase,
0.013 A salt D O 0.037 0.040
Ae 0.070 0.049 0.012
2
Convert Super-Kamiokande AES to
(shape constrained, Ae, and combine with SNO:
ANC constrained) A SNO SK 0.035 0.027
…..but …do neutrinos oscillate also on earth?
First Reactor Antineutrino Result
• Observed neutrino disappearance:
(Nobs–NBG)/Nno-osc = 0.611 0.085 (stat) 0.041 (syst)
• “Standard” e propagation ruled out at the 99.95% confidence level
Rate!
Energy
Bruce Berger Rencontres de Moriond – March 6, 2005 11
Direct observation of the oscillation
Goodness of fit:
0.7% - decay
1.8% - decoherence
11.1% - oscillation
(0.4% - constant suppression)
• Data prefer oscillation to other
hypotheses
L0/E Plot
Data vs.
No-oscillation
expectation
Bruce Berger Rencontres de Moriond – March 6, 2005 12
K2K experiment
~1 event/2days
~1011 m/2.2sec ~106 m/2.2sec
12GeV protons (/10m10m) m (/40m40m)
p+ m SK
Target+Horn
200m 100m ~250km
decay pipe
p monitor
Near detectors
m monitor (ND)
(monitor the beam center)
Signal of oscillation at K2K
Reduction of m events
Distortion of m energy spectrum
C.Mariani@XLth Rencontres de Moriond (6th March 2005)
C.Mariani
1KT Flux measurement
The same detector technology as Super-K.
Sensitive to low energy neutrinos.
N exp
N obs
SK ( E ) ( E )dE
M SK SK
KT ( E ) ( E ) dE
M KT KT
SK KT
Far/Near Ratio (by MC)~1×10-6
M: Fiducial mass MSK=22,500Kton, MKT=25ton
: efficiency SK-I(II)=77.0(78.2)%, KT=74.5%
obs
N
exp
SK =150.9 +12
-10 N SK =107
C.Mariani@XLth Rencontres de Moriond (6th March 2005) C.Mariani
Data are consistent with the oscillation.
With 8.9×1019 POT, K2K has confirmed neutrino oscillations at 4.0
(hep-ex/0411038).
Disappearance of m 3.0
Distortion of E spectrum 2.6
preliminary
m2[eV2]
Best Fit
KS prob.=36%
sin22
Erec[GeV]
C.Mariani@XLth Rencontres de Moriond (6th March 2005) C.Mariani
Introducing MiniBooNE:
The Booster Neutrino Experiment
LMC
m+
?
K+
8GeV p+ m
νμ→νe
Booster
magnetic horn decay pipe 450 m dirt detector
and target 25 or 50 m
•The goal: to check the LSND result.
Gordon McGregor
Conclusions
• MiniBooNE is running well.
• Currently 4.57×1020 protons on target.
• νμ νe appearance results by hopefully late 2005.
Gordon McGregor
Neutrino masses in 3-neutrino schemes
From present evidences of atmospheric and solar neutrino oscillations
eV eV
m 2
atm 0.05 eV
msun 0.009 eV
2
solar m0
atm
atm
solar
3 degenerate massive neutrinos
Σmν = 3m0
S.Pastor
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 Σmνreduction of ~ 2 (4) with respect to MiDBD-II (I)
arXiv:hep-ex/0501034 v1
DBD0 result:
T1/2130Te > 1.8 x 1024 y
=0.02÷0.1 eV 5 years =0.01÷0.06 eV
…very interesting……
S.Capelli
LFV in the Standard Model
Neutrino oscillations flavour mixing in lepton sector
•Extensions of SM with massive Dirac neutrinos allow LFV also
with charged leptons (me , e , meee , me)
larger mass scale
needed SUSY
2
( m e ) 2 m 2
sin 2 2 10 55
M not observable!
( m e ) 2p W
D.Nicolò
Conclusions
• m 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
• m+e+ results are expected in 2007 (10-13)
• m-e- conversion search is planned at the level of 10-16
• m-e- conversion is not accidental background limited could benefit of new
high intensity pulsed beams
…….to work hard….. D.Nicolò
Proton life time ….a lower limit…
PROTONS (do not) DECAY……..
L.Sulak
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
CAST: Principle of detection
Axion X-ray (same energy and momentum) X-ray
detector
L
[Sikivie PRL 51 (1983)]
• Expected number of photons in the x-ray
detector:
dΦ a Differential axion flux at the Earth
dΦ a
Nγ Pa γ S t dE a dE a (cm-2 s -1 keV -1 )
dE a Conversion probability of
Pa γ
For gaγγ =1×1O-10 GeV-1 an axion into photon ( (B×L)2)
t=100 h , S=15 cm2 S Magnet bore area (cm2)
N γ ≈ 30 events t Measurement time (s)
CAST 2003 result
Axion exclusion plot
• Combined upper limit
obtained (95% C.L.):
gaγγ 10 !
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 40
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 41
Instead of conclusions
sneutrino-driven me probably
chaotic inflation nonthermal leptogenesis observable in the next
in inflaton decay round of exps.
(Chankowski et al.,2004)
masses of 2 singlet enhancement of 1 from me unobservable
neutrinos small mass splittings of
degenerate at the singlet neutrinos partly
GUT scale compensated due to
(kt,2004) consistency conditions,
but leptogenesis OK
large neutrino successful leptogenesis
Yukawa couplings from small M1 due to
cancelling out in the overcoming DI bound r=1 for m0=100 GeV, M1/2=200 GeV
seesaw formula
(Raidal et al.,2005)
K.Turzynski
…interesting….but……
……new results coming……..
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 43
U.Gastaldi
PVLAS
Laser light
….big discovery!!!...
….but…do we belive to it….
U.Gastaldi
Observed dichroism of Vacuum
with infrared Laser light 1eV
…..Spin 0 boson……
-+
0
-3
m=10 eV
5
M=5 10 GeV
Axion????
Dark matter???
….to be confirmed……..
….to be young … 20 GeV,
ET >25 GeV, (ET , l or j) , veto on jets,
light (
D: Obs: 9 evts; Bkgnd:11.1 3.2
Signal: 0.27 0.004 (mH=160 GeV)
*BR(H→WW)< 5.6pb
For MH=160 GeV
CDF: Obs: 8 evts;
Bkgnd: 8.9 1
Signal: 0.17 0.02
(mH=180 GeV)
Maximum likelihood
limit on the ll
distributions for
x 20? mH=140-180 GeV
Gregorio Bernardi / LPNHE-Paris
AND B-PHYSICS…….
……the hunt to the new physics continue……..
Hints of new physics?
H.Kakuno
VII: Summary and Future CLEO
(1) New results on BF D+ m and fD
BD m ) 3.5 1.4 0.6)104
f D 202 41 17) MeV
(2) Exclusive BF of semileptonic decays coming (pretty) soon.
• With just 60 pb-1, stastistical power of many decay modes already
at the world best.
• The world first events of D 0 e and D e
• We have two analysis options available: With and wo DTag
3) Inclusive BF of D Xe and D Xl, l coming.
(4) Currently we are running at (3770) with 12 “8-pole” wigglers.
More data is coming on (3770), Ds threshold, etc.
fDs
D.Kim
Polarization in B V V decay
Angles in transversity basis
Differential cross section looks so complicated,
but not, actually.
Physics implication and recent experimental results
are reviewed here.
K.Snyo
B V V tree decay
Diagrams and tables are from presentation of P.J. Clark@FPCP2004
Yes, it is true for trees.
fL~1
K.Snyo
Polarization puzzle in pure penguin
decays: B K*±/0 and B K*0
Today
275
275
275
Rescattering?
An enhanced New Standard Model Amplitude?
Diagrams and tables are from presentation of P.J. Clark@FPCP2004
But, this is not true in B K* and K*0!!
New Physics?
K.Snyo
fL deviates from 1 in both Belle and BaBar.
Conclusions:
A lot of work still to be done………
Best wishes to you all !!
And…..arrivederci!