agenda: 1) neutrinos 2) dark matter, axions, lfv search. 3) kaons and b-mesons 4) lep,hera and the...
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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?
M.Calvetti INFN-Laboratori Nazionali di Frascati
and Università di Firenze
MORIOND 2005
What to answer if you are ask:…….what’s new in Moriond?
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Super-Kamiokande atmospheric ’s
For 13~0 and m2~0, a very simple formula fits all SK data (+ MACRO & Soudan2)
1st oscillation dip still visibledespite large L & E smearing
Strong constraints on the parameters (m2, 23)
7
E.Lisi
……
..NEUTRIN
OS……
……
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L.Sulak Super-Kamiokande atmospheric ’s
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SNO’s Three Reactions
-eppd (CC) eCharged Current:
Neutral Current:
npd (NC) xx
Elastic Scattering:
-- ee (ES) xx
•Detect the e-
• energy spectrum
• Weak directional sensitivity
e
•Detect the n through secondary capture
• No directional or neutrino energy info
•Detect the e-
•Mainly sensitive to
•Highly directional
e
K.Miknaitis
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20
Energy Isotropy
Direction Radius
K.Miknaitis
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)syst.()stat.( 35.2
)syst.()stat.( 94.4
)syst.()stat.( 68.1
15.015.0
22.022.0
38.034.0
21.021.0
08.009.0
06.006.0
ES
NC
CC
391- day salt results!
)scm10
of units(In 126
029.0031.0)stat.(023.0340.0
NC
CC
K.Miknaitis
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Ratio of the measured CC,ES,NC reaction rates to the SSM prediction, assuming undistorted CC, ES energy spectra.
SOLARSOLAR SNOSNO
K.Miknaitis
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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 ~2and aMSW~0 excluded Evidence for MSW effects in the Sun
But: expected subleading effect in the Earth (day-night difference) still below experimental uncertainties.
14
What about the neutrino masses? We have only limits…..E.Lisi
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Day-Night Asymmetries (II)
ACC= -0.037 ± 0.063(stat.) ±0.032(syst.)
AES= 0.153 ± 0.198(stat.) ±0.030(syst.)
Constraining ANC to be zero:
In the pure-D2O phase,
(shape constrained, ANC constrained)
013.0012.0e 049.0070.0A
DN
DNA
)(2
Combine with analogous ACC from the salt phase:
Convert Super-Kamiokande AES to Ae, and combine with SNO:
040.0037.0A OD salt 2
027.0035.0A SK SNO
K.Miknaitis
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…..but …do neutrinos oscillate also on earth?
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Bruce Berger
Rencontres de Moriond – March 6, 2005 11
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
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Bruce Berger
Rencontres de Moriond – March 6, 2005 12
L0/E Plot
Goodness of fit:0.7% - decay1.8% - decoherence
11.1% - oscillation(0.4% - constant suppression)
• Data prefer oscillation to otherhypotheses
Data vs.No-oscillationexpectation
Direct observation of the oscillation
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C.Mariani@XLth Rencontres de Moriond (6th March 2005)
K2K experiment
monitormonitor
Near detectors(ND)
+
Target+Horn200m
decay pipe
SK
100m ~250km
12GeV protons
~1011/2.2sec(/10m10m)
~106/2.2sec(/40m40m)
~1 event/2days
Signal of oscillation at K2K Reduction of events Distortion of energy spectrum
(monitor the beam center)
C.Mariani
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C.Mariani@XLth Rencontres de Moriond (6th March 2005)
1KT Flux measurement The same detector technology as Super-K. Sensitive to low energy neutrinos.
KT
SK
KT
SK
KT
SKobsKTSK M
M
dEEE
dEEENN
)()(
)()(exp
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%
expSKN =150.9 N =107+12
-10obsSK
C.Mariani
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C.Mariani@XLth Rencontres de Moriond (6th March 2005)
Erec[GeV]
Best FitKS prob.=36%
m2[e
V2]
sin22
Data are consistent with the oscillation.
preliminary
With 8.9×1019 POT, K2K has confirmedhas confirmed neutrino oscillations at 4.04.0(hep-ex/0411038)(hep-ex/0411038). Disappearance of 3.03.0 Distortion of E spectrum 2.62.6
C.Mariani
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Gordon McGregor
Introducing MiniBooNE:The Booster Neutrino Experiment
•The goal: to check the LSND result.
8GeVBooster
?
magnetic hornand target
decay pipe25 or 50 m
LMC
450 m dirt detectorabsorber
νμ→νeK+ +
+
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Gordon McGregor
Conclusions
• MiniBooNE is running well. • Currently 4.57×1020 protons on target.• νμ νe appearance results by hopefully late 2005.
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3 degenerate massive neutrinos Σmν = 3m0
Neutrino masses in 3-neutrino schemes
eV
From present evidences of atmospheric and solar neutrino oscillations
atmatm
solar
solar
eV 0.009 m
eV 0.05m
2sun
2atm
eV
m0
S.Pastor
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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)
Conclusions
Sub-eV sensitivity in the next future (0.1-0.2 eV and better) Test degenerate
mass region and eventually the IH case
ν
Cosmological observables efficiently constrain some properties of (relic) neutrinos
S.Pastor
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Future sensitivities to Σmν: new ideas
galaxy weak lensing and CMB lensing
sensitivity of future weak lensing survey(4000º)2 to mν
σ(mν) ~ 0.1 eV
Abazajian & DodelsonPRL 91 (2003) 041301
sensitivity of CMB(primary + lensing) to mν
σ(mν) = 0.15 eV (Planck)
σ(mν) = 0.04 eV (CMBpol)
Kaplinghat, Knox & SongPRL 91 (2003) 241301
S.Pastor
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Numerical ±2 ranges (95% CL for 1dof), 2004 data:
19
Note: Precise values for 12 and 23 relevant for model building (see talk by Tanimoto) E.Lisi
See the c
ontributio
n from
B.Kayser
on “neutri
no future”
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Experiments measuring……zero’s
Double Beta DecayProton decay searchDark matter searchAxionsVacuum polarizationLepton Flavour Violation
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R&D: Cleaning test R&D: Cleaning test (September-November (September-November
2004)2004)
Cu: etching, electropolishing and passivationTeO2: etching and lapping with clean powders
Assembling with clean materials
S.Capelli
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CUORICINOCUORICINO resultsresults
Total Statistics: 10.85 kgxy
DBD0 result: T1/2
130Te
<m> < [0.2÷1.1] eV
Background (@DBD0):
0.18 ± 0.01 c/keV/kg/y => reduction of ~ 2 (4) with respect to MiDBD-II (I)
130Te (DBD0)
arXiv:hep-ex/0501034 v1
> 1.8 x 1024 y
<m> < 0.07 - 0.5 eV
In 5 years…S.Capelli
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CUORE sensitivityCUORE sensitivity
Sensitivity (1):
b=0.01 c/keV/kg/y=5 keV F0=9.2x1025√t y <m>=0.02÷0.1 eV
b=0.001 c/keV/kg/y=5 keV F0=2.9x1026√t y <m>=0.01÷0.06 eV
CUORE bkg goal: 0.001 ÷ 0.01 c/keV/kg/y
5 years
S.Capelli
eV 0.009 m
eV 0.05m
2sun
2atm
…very interesting……
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LFV in the Standard ModelNeutrino oscillations flavour mixing in lepton sector
•Extensions of SM with massive Dirac neutrinos allow LFV also with charged leptons (e , e , eee , e
55
2
2
22 102sin
2
)e(
)e(
WM
m
not observable!
larger mass scale needed
SUSY
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
D.Nicolò…….to work hard…..
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L.Sulak
Proton life time ….a lower limit…
PROTONS (do not) DECAY……..
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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
P life-time
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CAST: Principle of detection
• Expected number of photons in the x-ray detector:
L
Transverse magnetic field (B)
X-ray detector
X-ray (same energy and momentum)Axion
[Sikivie PRL 51 (1983)]
aγaa
aγ dEtSP
dE
dΦN a
a
dE
dΦ
γaP
S
t
Differential axion flux at the Earth(cm-2 s -1 keV -1 )
Conversion probability of an axion into photon ( (B×L)2)Magnet bore area (cm2)
Measurement time (s)
For gaγγ =1×1O-10 GeV-
1
t=100 h , S=15 cm2
N γ ≈ 30 events
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CAST 2003 resultAxion exclusion plot
• Combined upper limit obtained (95% C.L.):
gaγγ<1.16×10-10 GeV-1
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CRESST-II Detector Concept
Discrimination of nuclear recoils from radioactive + backgrounds (electron recoils) by simultaneous measurement of phonons and scintillation light
Separate calorimeter as light detector
light reflectorW-thermometer
W-thermometer
300 g scintillatingCaWO4 crystal
proof of principle
En
erg
y in
lig
ht
chan
nel
keV
ee]
Energy in phonon channel [keV]
DMnuclei
DARK MATTER SEARCH
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Ionization Yield EQ/ER
Y~ 1 for electron recoils
Nuclear Recoils (252Cf)
Nuclear Recoils (252Cf)
WIMPS (and neutrons) scatter off nuclei
Identify nuclear recoils event by event!
Y~ 0.3 (Ge) for nuclear recoils
• Events occuring near the surface (<~10 m) have an incomplete charge collection (“dead layer”) and can be misidentified as nuclear recoils
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 m of the surface
Most background sources (electrons, photons) scatter off electrons
Measure simultaneously ionization and athermal phonons
CDMS II Overview
Bulk Electron Recoils (133Ba)
Bulk Electron Recoils (133Ba)
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WIMPs search data with Ge detectors (Run118) Yellow points from neutron calibration
Ch
arg
e Y
ield
Prior to timing cutsAfter timing cuts
Blue points from WIMP search data (Z2, Z3, Z5)
Recoil energy (keV) Recoil energy (keV)
Ch
arg
e Y
ield
Expected background : 0.7 ± 0.35 mis-identified surface electron recoils
Event
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DAMA
CDMS
ZEPLIN
Edelweiss
CDMS_Projections CRESST
Egret
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…..….discoveries?..........
1) Egret excess signal…….
2) PVLAS…………
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 38
DM annihilation in Supersymmetry
Dominant diagram for WMAPcross section in MSSM: + A b bbar quark pair
B-fragmentation well studied at LEP!Yield and spectra of positrons,gammas and antiprotons well known!
f
f
f
f
f
f
Z
Z
W
W 0
f~
A Z
Galaxy = SUPER-B-factory with luminosity some 40 orders of magnitude above man-made B-factories
≈ 37 gammas
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 39
Excess of Diffuse Gamma Rays has same spectrum in all directions compatible with WIMP mass of 50-100 GeV
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.
Egret Excess aboveextrapolated backgroundfrom data below 0.5 GeV
Excess same shape in all regions implying same source everywhere
Statistical errors only
WIMP MASS50 - 100 GeV
65100
Bremsstr.
Extragal.
ICWIM
PS
0
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 40
Diffuse Gamma Rays for different sky regions Good Fits for WIMP masses between 50 and 100 GeV
3 components: galactic background + extragalactic bg + DM annihilation fittedsimultaneously with same WIMP mass and DM normalization in all directions.Boost factor around 70 in all directions and statistical significance > 10 !
A: inner Galaxy B: outer disc C: outer Galaxy
D: low latitude E: intermediate lat. F: galactic poles
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 41
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Instead of conclusions
nonthermal leptogenesis in inflaton decay
masses of 2 singlet neutrinos
degenerate at the GUT scale
(kt,2004)
enhancement of 1 from small mass splittings of singlet neutrinos partly compensated due to
consistency conditions, but leptogenesis OK
e unobservable
large neutrino Yukawa couplings
cancelling out in the seesaw formula(Raidal et al.,2005)
successful leptogenesis from small M1 due to
overcoming DI bound
sneutrino-driven chaotic inflation
e probably observable in the next
round of exps. (Chankowski et al.,2004)
r=1 for m0=100 GeV, M1/2=200 GeV
‘It is a capital mistake to
theorize
before one has data’
K.Turzynski
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 43
……new results coming……..
…interesting….but……
Is it a capital m
istake
to theorize (too much)
when one has data?
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Laser lightPVLAS….big discovery!!!...….but…do we belive to it….
U.Gastaldi
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Observed dichroism of Vacuumwith infrared Laser light 1eV
0 -+
m=10-3 eV
M=5 105 GeV
…..Spin 0 boson……
Axion????Dark matter???
….to be confirmed……..
….to be young …< 60 …..
U.Gastaldi
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Nice good results…….from
LEP
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LEP Result
00
ln)(
)()(
t
tba
tN
tNtf
MC
data
tδ
δ Δα
ln2
39.1...2 fod8.02
602
372
182
incompatible
b = (726 96 70) 10-5
OPAL fit
OPAL fit
G.Abbiendi
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Slope b = (726 96 70 50) 10-5
Significance: 5.6 including all errors for the total running
5
22
10)304358440(
)GeV811()GeV076(
. .
5
22
10)304358237(
)GeV811()GeV076(
. . hadhad
Hadronic contribution to the running: First Direct Experimental evidence with Significance of 3.0 including all errors
510202 lepsubtracting the precisely calculable leptonic contribution:
SM : 460 10-5 using the Burkhardt-Pietrzyk parameterization
LEP Results
tb
ln
2
contributions to the slope b in our t range are predicted to be in the proportion: e : : hadron ≈ 1 : 1 : 2.5
Most significant direct observation of the running of QED ever achieved
G.Abbiendi
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|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN 30
-kaons-kaons-kaons-kaons-kaons-
KLOE KTeV NA48 E949
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|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN
ctLL
LLLLL
K
KK
/
cos2 222
L Lγ
LK e+ e-
π+
π -
solved for the two variables Lγ, LK
We use KLπ0π0π0 events tagged by KSπ+π- 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 π+π-) .
(Xγ,Yγ,Zγ,Tγ)
KKLL lifetime: direct measurement lifetime: direct measurement
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KKLL lifetime: final result lifetime: final result
τL (KLOE) = (50.87 ±0.16 (stat) ± 0.26 (syst)) ns
|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN
14 x 106 events Fit region = 6 -26 ns ( 40% τL)
t*= LK/βγc (ns)
+ dataYes, it’s going down!!
Eve
nts
/0.3
ns
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KKLL lifetime: comparison lifetime: comparison
|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN
KLOE direct
KLOE indirect
Vosburgh et al, PRD 6 (1972), 1834
average: τL = (50.98 ± 0.21) ns
PDG 2004 = (51.8 ± 0.4) ns
I took my degreein physics in 1972…
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3 Br KL
L
GF
2 mK5
384 3
SEW f
2 t 0 1 Vus
2 ˆ f 2
Step 4: Get the branching ratio
KL KL nice Ordinarily, would measure something like
where the “nice” mode has high statistics, a well-known rate, and is
similar to K3 in the detector. Sadly, there is no “nice” mode.
Measure these 5 ratios, use = 1 constraintto get Br
K3
Ke3
0Ke 3
000Ke3
Ke3
00000
KTeV- L.Bellantoni
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KKLL dominant BR’s: comparison dominant BR’s: comparison
KL e (no PDG) 0.4045±0.0009 χ2 = 5.1
KL 0.2702±0.0007 χ2 = 0.3
KL 30
(no PDG)0.1968±0.0012 χ2=1.9
KL π+π-0
0.1255±0.0006χ2= 0.4
KLOE
NA48
KTeV
PDG04
KLOE
KTeV
PDG04
KLOE
NA48*
KTeV
PDG04
KLOE
KTeV
PDG04
* Presented by L.Litov @ICHEP04 15
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|Vus|f+Kπ(0)
KLOE results: |Vus
|f+
K(0) (KSe3
) = 0.2169 0.0017
|Vus
|f+
K(0) (KLe3
) = 0.2164 0.0007 |V
us|f
+K(0)(K
L3) = 0.2174 0.0009
From Unitarity: (1-|Vud
|2)1/2f+
K(0) = 0.2177 0.0028
|V|Vusus| from K| from Kl3l3 decays decays and and ττLL::
PRD 6 (1972), 1834 KLOE
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The KLOE KThe KLOE KSS “beam”: “beam”:
|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN
KL “crash”βγ 0.22 , TOF 30 ns
KKSS ππee
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
KKSS ππee
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Observation of 0+-
With 9 events from ‘99 dataset,no background events seen in wrong sign, or in 10x MC sample -
Normalized to 00, p
KTeV- L.Bellantoni
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|Vus| and KS decays from KLOE G. Lanfranchi – LNF/INFN
KKSS ππ00ππ00ππ00 upper limit: final result upper limit: final result
Using the PDG values and our limit we have:
KLOE
90 % CL
Nbkg = 3.13 ± 0.82stat± 0.37sys
Nobs = 2
(events with KL tag) = 24.3%
BR(KSπ0π0π0) < 1.2 10-7 @ 90% CL
A(KS 000)
A(KL 000) |000| = < 1.8 10-2 , 90% CL
NA48 (hep-ex/0408053)
A factor 5 better than the previous limit!
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2003 run: ~ 50 days2004 run: ~ 60 days
Total statistics in 2 years:
K +: ~4x109
K 00: ~2x108
~ 200 TB of data recorded
Search for direct CP-violationin K± ±+– decays by NA48/2
Ivan Mikulec
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Comparison K±±+-
NA48/2 prelim.: 2003 data
10-6
|Ag|
10-5
10-4
10-3
10-2
SMSM SUSYSUSY
Ford et al. (1970)
HyperCP prelim. (2000)
NA48/2 goal:2003-04 data
NewNewphysicsphysics
This preliminary
result is already an
order of magnitude better than previous
experiments
Ivan Mikulec
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Observation of scattering effect in K→3 decays
1 bin = 0.00015 GeV2
MC (no rescattering)
Data
K±±00
M(00) GeV/c 2
4mπ+2
Charge exchange process +00 not negligible under 2m threshold,destructive interference generates a cusp in the Dalitz plot,
not seen earlier by lower precision experiments
30M events
4mπ+2
Ivan Mikulec
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VERY (very) RARE K-DECAYS
A.Ceccucci
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Some BSM Predictions
SM 8.0 ± 1.1 3.0 ± 0.6
MFVhep-ph/0310208
19.1 9.9
EEWPNP B697 133
7.5 ± 2.1 31 ± 10
EDSQhep-ph/0407021
15 10
MSSMhep-ph/0408142
40 50
0 0 11L( ) 10BR K 11( ) 10BR K
Compiled by S. Kettel
A.Ceccucci
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K+→+ : State of the art
BR(K+ → + ) = 1.47+1.30-0.89 × 10-10
•Compatible with SM within errors
hep-ex/0403036 PRL93 (2004)
Stopped K~0.1 % acceptance
AGS
A.Ceccucci
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KTeVBR(KL → 0 ee ) < 2.8 × 10-10 @90%CL
A.Ceccucci
BR(K0L ) 3.8 10-10 (90% C.L.) [PRL 86, 5425 (2001)]
BR(KS→0ee) =(5.8 +2.8-2.3(stat) ± 0.8(syst)) 10-9
BR(KS→0) = (2.9 +1.4-1.2(stat) ± 0.2(syst)) 10-9
NA48
K0L→0ee and K0
L→0
K0S→0ee and K0
S→0
Similar physics interest asK0
L→0 Complicated by long distance contibutions and radiative backgrounds
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Isidori, Unterdorfer, Smith:
Fleischer et al*:
Ratios of Bd → modes could be explained by enhanced electroweak penguins which, in turn, would enhance the KL BR’s:
•A. J. Buras, R. Fleischer, S. Recksiegel,
F. Schwab, hep-ph/0402112, NP B697 (2004)
0 0L
0 0L
1.6 111.6
0.7 110.7
9.0 10
4.3 10
NP
K e e
NP
K
B
B
0 12L(K ) 10Br
0 12L( ) 10Br e e
K0L→0ee (): Sensitivity to NP
~ SES of KTeVsearch
A.CeccucciKopio-NA48/x-KLOE-KEK (next generation?)
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Tevatron-Tevatron-Tevatron-Tevatron-Tevatron
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Gregorio Bernardi / LPNHE-Paris
CDFTevatron Long Term Luminosity
PlanCurrently expecting
delivered luminosity to each
experiment
4 - 8 fb-1
by the end of 2009 Integrated Weekly Luminosity (pb-1)
0
10
20
30
40
50
60
10/1/03 9/30/04 9/30/05 9/30/06 9/30/07 9/29/08 9/29/09
electron cooling
stacktail bandwidth upgradeDesign
Base
Total Luminosity (fb-1)
0
1
2
3
4
5
6
7
8
9
10/1/03 9/30/04 9/30/05 9/30/06 9/30/07 9/29/08 9/29/09
Design
BaseToday
Increase in number of antiprotons
key for higher luminosity
Expected peak luminosity 3.1032 cm-2sec-1 by 2007
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Cross Section SummaryCross Section Summary
SM curve: C.R. Hamberg, W.L van Neerven and T. Matsuura, Nucl. Phys.B359, 343 (1991)SM curve: C.R. Hamberg, W.L van Neerven and T. Matsuura, Nucl. Phys.B359, 343 (1991)
F.Deliot
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Gregorio Bernardi / LPNHE-Paris
CDFSM “Heavy” Higgs: H WW
llSearch strategy:
2 high Pt leptons and missing Et
WW comes from spin 0 Higgs:leptons prefer to point in the same
directionW+ e+
W- e-
H
Main Background: WW ProductionGood agreement with NLO theory: 12.0-13.5 pb
Ohnemus, Campbell, R.K.EllisNow Measured at the Tevatron by both ExperimentsDØ: PRL/ hep-ex/0410062
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Gregorio Bernardi / LPNHE-Paris
CDF (Z+b)/(Z+j)
Apply sec. vertex b-tag42 events with 1 tag8.3 from QCD
background (sideband)
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
– Nc=1.69Nb from theory
Cross checks with– Soft lepton tagging– Impact parameter tagging
0.0240.005(stat)0.005(syst)
– Theory predicts 0.018– Large part of systematic error
from tagging efficiency and background estimation
Sec. Vtx displacement/resolutionSubmitted to PRL - hep-ex/0410078
signal
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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:
W’ search in e channel
MC onlyhigh pT electron + high ET
A.Lath
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Moriond
Saverio D’Auria University of Glasgow
B-hadrons mass summary
New for Moriond EW 05
Bs oscillations….???? Wait and see…..
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Gregorio Bernardi / LPNHE-Paris
CDF
Search in 3 channels: HWW*ll with l = ee,,e inclusive high pT lepton triggers: integrated luminosity 184 pb-1 (CDF), 147-177 pb-1(D0)
CDF: Obs: 8 evts; Bkgnd: 8.9 1 Signal: 0.17 0.02 (mH=180
GeV)
Search for H WW*
Data Selection: two isolated leptons with opposite charges with pT > 20 GeV, >25 GeV, ( , l or j) , veto on jets, light (<MH/2) invariant dilepton mass
TE TE
Maximum likelihood limit on the ll distributions for mH=140-180 GeV
*BR(H→WW)< 5.6pb For MH=160 GeV
95% CL for the 3 channels*BR(H→WW) < 5.7pb For MH=160 GeV
D: Obs: 9 evts; Bkgnd:11.1 3.2 Signal: 0.27 0.004 (mH=160
GeV)
x 20?
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AND B-PHYSICS…….
……the hunt to the new physics continue……..
Hints of new physics?
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H.Kakuno
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(1) New results on BF D+ 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 Xeand D Xllcoming.
(4) Currently we are running at (3770) with 12 “8-pole” wigglers.
More data is coming on (3770), Ds threshold, etc.
VII: Summary and Future
MeV 1741202
106.04.15.3 4
Df
DB
0D e D e
fDs
D.Kim
CLEO
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Polarization in B Polarization in B V V decay V V decayAngles in transversity basis
Physics implication and recent experimental results are reviewed here.
Differential cross section looks so complicated,but not, actually.
K.Snyo
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B B V V V V treetree decay decay
Yes, it is true for trees.fL~1
Diagrams and tables are from presentation of P.J. Clark@FPCP2004
K.Snyo
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Polarization puzzle in pure penguin Polarization puzzle in pure penguin decays: decays: B B KK*±/0*±/0 and B and B KK*0*0
But, this is not true in B K* and K*0!!fL deviates from 1 in both Belle and BaBar.
Today
275
275
275
Diagrams and tables are from presentation of P.J. Clark@FPCP2004
Rescattering?An enhanced New Standard Model Amplitude?New Physics?
K.Snyo
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Best wishes to you all !!
Conclusions:
A lot of work still to be done………
And…..arrivederci!