AGENDA:

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 .whats new in
Moriond?
M.Calvetti INFN-Laboratori Nazionali di
Frascati and Università di Firenze
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Super-Kamiokande atmospheric ?s
For ?130 and ?m20, 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
K.Miknaitis
SNOs Three Reactions
5
K.Miknaitis
Energy
Isotropy
20
Radius
Direction
6
K.Miknaitis
7
SOLAR
SNO
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 aMSW1
( a way of measuring GF through solar
neutrino oscillations )
Results with 2004 data, aMSW1 confirmed within
factor of 2 and aMSW0 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..
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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)
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..but do neutrinos oscillate also on earth?
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First Reactor Antineutrino Result

• Observed neutrino disappearance
• (NobsNBG)/Nno-osc 0.611 ? 0.085 (stat) ?
  0.041 (syst)
• Standard ne propagation ruled out at the
  99.95 confidence level

Rate!
Energy
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L0/E Plot
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

Data vs. No-oscillation expectation
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K2K experiment
1 event/2days
1011 nm/2.2sec (/10m?10m)
106 nm/2.2sec (/40m?40m)
nm
12GeV protons
nt
p
SK
m
TargetHorn
100m
200m decay pipe
250km
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
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1KT Flux measurement

• The same detector technology as Super-K.
• Sensitive to low energy neutrinos.

?Far/Near Ratio (by MC)110-6
M Fiducial mass MSK22,500Kton, MKT25ton e
efficiency eSK-I(II)77.0(78.2), eKT74.5
exp SK
C.Mariani
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Data are consistent with the oscillation.

• With 8.91019 POT, K2K has confirmed neutrino
  oscillations at 4.0s (hep-ex/0411038).
• Disappearance of nm 3.0s
• Distortion of En spectrum 2.6s

preliminary
Dm2eV2
Best Fit KS prob.36
sin22q
EnrecGeV
C.Mariani
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Introducing MiniBooNE
The Booster Neutrino Experiment

• The goal to check the LSND result.

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Conclusions
...best wishes...

• MiniBooNE is running well.
• Currently 4.571020 protons on target.
• ?µ ? ?e appearance results by hopefully late 2005.

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Neutrino masses in 3-neutrino schemes
From present evidences of atmospheric and solar
neutrino oscillations
eV
solar
atm
atm
solar
3 degenerate massive neutrinos Sm? 3m0
S.Pastor
19
Conclusions
Cosmological observables efficiently constrain
some properties of (relic) neutrinos
?
Bounds on the sum of neutrino masses from CMB
2dFGRS or SDSS, and other cosmological data (best
Sm?lt0.42 eV, conservative Sm?lt1 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
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Future sensitivities to Sm? new ideas
galaxy weak lensing and CMB lensing
sensitivity of future weak lensing
survey (4000º)2 to m? s(m?) 0.1 eV Abazajian
Dodelson PRL 91 (2003) 041301
sensitivity of CMB (primary lensing) to
m? s(m?) 0.15 eV (Planck) s(m?) 0.04 eV
(CMBpol) Kaplinghat, Knox Song PRL 91 (2003)
241301
S.Pastor
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Numerical 2? ranges (95 CL for 1dof), 2004 data
See the contribution from B.Kayser on neutrino
future
Note Precise values for ?12 and ?23 relevant for
model building (see talk by Tanimoto)
E.Lisi
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Experiments measuringzeros
Double Beta Decay Proton decay search Dark matter
search Axions Vacuum polarization Lepton Flavour
Violation
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Cu etching, electropolishing and
passivation TeO2 etching and lapping with clean
powders
Assembling with clean materials
S.Capelli
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Total Statistics 10.85 kgxy
reduction of 2 (4) with respect to MiDBD-II (I)
arXivhep-ex/0501034 v1
DBD0? result T1/2130Te ltm?gt lt
0.21.1 eV
gt 1.8 x 1024 y
130Te (DBD0n)
ltmngt lt 0.07 - 0.5 eV
In 5 years
S.Capelli
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CUORE bkg goal 0.001 0.01 c/keV/kg/y

5 years
best wishes.....
very interesting
S.Capelli
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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 (m?eg , t?eg
  , m?eee , m?e)

larger mass scale needed ? SUSY
not observable!
D.Nicolò
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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
  limited could benefit of new high intensity
  pulsed beams

best wishes.....
.to work hard..
D.Nicolò
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Proton life time .a lower limit
PROTONS (do not) DECAY..
L.Sulak
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P life-time
L.Sulak
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CAST 2003 result
Axion exclusion plot

• Combined upper limit obtained (95 C.L.)
• ga??lt1.1610-10 GeV-1

best wishes.....
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CRESST-II Detector Concept
DARK MATTER SEARCH
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
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CDMS II Overview
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
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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
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Egret
CRESST
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...discoveries?..........
1) Egret excess signal. 2) PVLAS
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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
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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.
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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 gt 10? !
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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
r1 for m0100 GeV, M1/2200 GeV
K.Turzynski
43
interesting.but
?
Is it a capital mistake to theorize (too
much) when one has data?
new results coming..
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PVLAS
U.Gastaldi
Laser light
.big discovery!!!... .butdo we belive to it.
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U.Gastaldi
Observed dichroism of Vacuum with infrared Laser
light 1eV
..Spin 0 boson
0 -
m10-3 eV
M5 105 GeV
Axion???? Dark matter???
.to be confirmed..
.to be young lt 60 ..
best wishes.....
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Nice good results.from LEP
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LEP Result
OPAL fit
OPAL fit
b (726 ? 96 ? 70) ? 10-5
G.Abbiendi
49
LEP Results
Slope b (726 ? 96 ? 70 ? 50) ?
10-5 Significance 5.6 s 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 evidence with Significance of
3.0 s including all errors
G.Abbiendi
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-kaons-kaons-kaons-kaons-kaons-
KLOE KTeV NA48 E949
Vus and KS decays from KLOE G.
Lanfranchi LNF/INFN
30

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KL lifetime direct measurement
?We use KL?p0p0p0 events tagged by KS?pp-
events ? tagging and tagged
events are fully decoupled. ?
trigger efficiency is 100, almost flat in the
fiducial volume ? The KL vertex is reconstructed
by TOF, using cluster time/position and KL
momentum (from K S ? pp-) .
(X?,Y?,Z?,T?)
Vus and KS decays from KLOE G. Lanfranchi
LNF/INFN
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KL lifetime final result
Events/0.3 ns
data
Yes, its going down!!
? 14 x 106 events Fit region 6 -26 ns (
40 tL)
t LK/ß?c (ns)
tL (KLOE) (50.87 0.16 (stat) 0.26 (syst))
ns
Vus and KS decays from KLOE G. Lanfranchi
LNF/INFN
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KL lifetime comparison
average tL (50.98 0.21) ns
KLOE direct
KLOE indirect
Vosburgh et al, PRD 6 (1972), 1834
I took my degree in physics in 1972
PDG 2004 (51.8 0.4) ns
Vus and KS decays from KLOE G. Lanfranchi
LNF/INFN
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Step 4 Get the branching ratio
Ordinarily, would measure something like
where the nice mode has high statistics, a
well-known rate, and is similar to Kl3 in the
detector. Sadly, there is no nice mode.
Measure these 5 ratios, use S 1 constraint to
get Br
KTeV- L.Bellantoni
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KL dominant BRs comparison
KL ??e? (no PDG) 0.40450.0009 ?2 5.1
KL ???? 0.27020.0007 ?2 0.3
KLOE NA48 KTeV PDG04
KLOE KTeV PDG04
KL ?pp-?0 0.12550.0006 ?2 0.4
KL ? 3?0 (no PDG) 0.19680.0012 ?21.9
KLOE NA48 KTeV PDG04
KLOE KTeV PDG04
Presented by L.Litov _at_ICHEP04
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Vus from Kl3 decays and tL
Vus?fKp(0)
KLOE
PRD 6 (1972), 1834
KLOE results Vus?fK?(0) (KSe3)
0.2169? 0.0017
Vus?fK?(0) (KLe3) 0.2164? 0.0007
Vus?fK?(0)(KLm3) 0.2174?
0.0009 From Unitarity (1-Vud2)1/2fK?(0)
0.2177? 0.0028
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The KLOE KS beam
KL crash ß?? 0.22 , TOF ? 30 ns
KS tagged by KL interaction in EmC ?
efficiency ? 30 ? KS angular resolution? 1?
(0.3? in ?) ? KS momentum resolution 1 MeV ?
3 105 tags/pb-1
KS ?pe?
KS ?pe?
Vus and KS decays from KLOE G. Lanfranchi
LNF/INFN
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Observation of X0?Sm-n
With 9 events from 99 dataset, no background
events seen in wrong sign, or in 10x MC sample -
Normalized to X0?Lp0, L?pp-
KTeV- L.Bellantoni
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KS ?p0p0p0 upper limit final result
A factor 5 better than the previous limit!
Using the PDG values and our limit we have
h000 lt 1.8 10-2 , 90 CL
90 CL
NA48 (hep-ex/0408053)
Vus and KS decays from KLOE G.
Lanfranchi LNF/INFN

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Search for direct CP-violationin K? ppp
decays by NA48/2
2003 run 50 days 2004 run 60 days Total
statistics in 2 years K?? ????? 4x109 K??
?0?0?? 2x108 200 TB of data recorded
Ivan Mikulec
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Comparison K????-
Ford et al. (1970)
10-2
HyperCP prelim. (2000)
This preliminary result is already an order of
magnitude better than previous experiments
Ag
10-3
NA48/2 prelim. 2003 data
NA48/2 goal 2003-04 data
10-4
10-5
10-6
New physics
SUSY
SM
Ivan Mikulec
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Observation of pp scattering effect in K?3p decays
Charge exchange process ?????0?0 not negligible
under 2mp threshold, destructive interference
generates a cusp in the Dalitz plot,not seen
earlier by lower precision experiments
30M events
MC (no rescattering)
Data
K???0?0
4mp2
4mp2
1 bin 0.00015 GeV2
M(?0?0) GeV/c 2
Ivan Mikulec
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VERY (very) RARE K-DECAYS
A.Ceccucci
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Some BSM Predictions
Compiled by S. Kettel
A.Ceccucci
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K?p nn State of the art
hep-ex/0403036 PRL93 (2004)
AGS
Stopped K 0.1 acceptance

• BR(K ? p nn ) 1.471.30-0.89 10-10
  
• Compatible with SM within errors

A.Ceccucci
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KTeV
K0L?p0ee- and K0L?p0mm-
BR(KL ? p0 ee ) lt 2.8 10-10 _at_90CL
K0S?p0ee- and K0S?p0mm-
BR(KS?p0ee) (5.8 2.8-2.3(stat) 0.8(syst)) ?
10-9
NA48
BR(KS?p0mm) (2.9 1.4-1.2(stat) 0.2(syst)) ?
10-9
Similar physics interest as K0L?p0 nn .
Complicated by long distance contibutions and
radiative backgrounds
A.Ceccucci
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K0L?p0ee (mm) Sensitivity to NP
Isidori, Unterdorfer, Smith
Fleischer et al Ratios of Bd ? Kp modes could
be explained by enhanced electroweak penguins
which, in turn, would enhance the KL BRs
SES of KTeV search

• A. J. Buras, R. Fleischer, S. Recksiegel,
• F. Schwab, hep-ph/0402112, NP B697 (2004)

Kopio-NA48/x-KLOE-KEK (next generation?)
A.Ceccucci
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Tevatron-Tevatron-Tevatron-Tevatron-Tevatron
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Tevatron Long Term Luminosity Plan
Currently expecting delivered luminosity to each
experiment ? 4 - 8 fb-1 by the end of 2009
Increase in number of antiprotons ? key for
higher luminosity Expected peak luminosity ?
3.1032 cm-2sec-1 by 2007
Today
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Cross Section Summary
SM curve C.R. Hamberg, W.L van Neerven and T.
Matsuura, Nucl. Phys.B359, 343 (1991)
F.Deliot
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SM Heavy Higgs H ? WW ? lnln
Search strategy ? 2 high Pt leptons and
missing Et ? WW comes from spin 0
Higgs leptons prefer to point in the same
direction
H
Main Background WW Production
Good agreement with NLO theory 12.0-13.5 pb
Now Measured at the Tevatron by both Experiments
Ohnemus, Campbell, R.K.Ellis
DØ PRL/ hep-ex/0410062
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s(Zb)/s(Zj)

• Disentangle light, c, b contributions
• Use light and b-tagging efficiency from data
• c-tagging efficiency from MC and scaled for
  data/MC difference in b-tagging
• Nc1.69Nb from theory
• Cross checks with
• Soft lepton tagging
• Impact parameter tagging
• 0.024?0.005(stat)?0.005(syst)
• Theory predicts 0.018
• Large part of systematic error from tagging
  efficiency and background estimation

• Apply sec. vertex b-tag
• 42 events with ?1 tag
• 8.3 from QCD background (sideband)

signal
Sec. Vtx displacement/resolution
Submitted to PRL - hep-ex/0410078
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W search in en channel

• W additional charged heavy vector boson
• appears in theories based on the extension of the
  gauge group
• e.g. Left-right symmetric models SU(2)R WR
• assume the neutrino from W decay is light and
  stable.
• signature

high pT electron high ET
MC only
A.Lath
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B-hadrons mass summary
Bs oscillations.???? Wait and see..
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Search for H ? WW
Search in 3 channels H?WW?ll??
with l ee,??,e? ?inclusive
high pT lepton triggers integrated luminosity
184 pb-1 (CDF), 147-177 pb-1(D0)
95 CL for the 3 channels sBR(H?WW) lt 5.7pb
For MH160 GeV
D? Obs 9 evts Bkgnd11.1 ? 3.2 Signal 0.27 ?
0.004 (mH160 GeV)
CDF Obs 8 evts Bkgnd 8.9 ? 1 Signal 0.17 ?
0.02 (mH180 GeV)
Best wishes
x 20?
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AND B-PHYSICS.
the hunt to the new physics continue..
Hints of new physics?
77
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H.Kakuno
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VII Summary and Future
CLEO

• New results on BF D ? mn and fD
• (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
  and
• We have two analysis options available With and
  wo DTag
• (3) Inclusive BF of D ?Xen and D ?Xln, ln 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
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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
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B ? V V tree decay
Diagrams and tables are from presentation of P.J.
Clark_at_FPCP2004
Yes, it is true for trees. fL1
K.Snyo
84
Polarization puzzle in pure penguin decays B ? f
K/0 and B ? r -K0

• Rescattering?
• An enhanced New Standard Model Amplitude?
• New Physics?

Diagrams and tables are from presentation of P.J.
Clark_at_FPCP2004
But, this is not true in B ? f K and r-K0!! fL
deviates from 1 in both Belle and BaBar.
K.Snyo
85
?
86
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Conclusions A lot of work still to be done
Best wishes to you all !!
And..arrivederci!