g. martinelli - from the standard model to dark matter and beyond: symmetries, masses and mysteries

63
Guido Martinelli SISSA & INFN From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Misteries NIS, Serbia 29/08/2011

Upload: seenet-mtp

Post on 18-Dec-2014

247 views

Category:

Education


0 download

DESCRIPTION

The SEENET-MTP Workshop JW2011 Scientific and Human Legacy of Julius Wess 27-28 August 2011, Donji Milanovac, Serbia

TRANSCRIPT

Page 1: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Guido MartinelliSISSA & INFN

From the Standard Model to DarkMatter and beyond: Symmetries,Masses and Misteries

NIS, Serbia 29/08/2011

Page 2: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Plan of the Talk

1) The UT analysis within the SM2) Beyond the SM: the case of Bs3) Outlook

Page 3: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Lquarks = Lkinetic + Lweak int + Lyukawa

In the Standard Model the quark massmatrix, from which the CKM Matrix andCP originate, is determined by the YukawaLagrangian which couples fermions andHiggs

CP invariant

CP and symmetry breaking are closely related !

Page 4: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Two accidental symmetries:

Absence of FCNC at tree level (& GIMsuppression of FCNC in quantum effects @loops)

NO CP violation @tree level

Flavour Physics is extremely sensitiveto new physics

Page 5: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

QUARK MASSES ARE GENERATED BY DYNAMICAL SYMMETRY BREAKING

Charge -1/3 ∑i,k=1,N [ mu

i,k (uiL uk

R )

+ mdi,k (di

L dkR) + h.c. ]

Charge +2/3

Lyukawa ≡ ∑i,k=1,N [ Yi,k (qi

L HC ) UkR

+ Xi,k (qiL H ) Dk

R + h.c. ]

Page 6: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Diagonalization of the Mass Matrix Up to singular cases, the mass matrix can always be

diagonalized by 2 unitary transformationsui

L UikL uk

L uiR Uik

R ukR

M´= U†L M UR (M´)† = U†

R (M)† ULLmass ≡ mup (uL uR + uR uL ) + mch(cL cR + cR cL )

+ mtop(tL tR + tR tL )

Page 7: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

N(N-1)/2 angles and (N-1)(N-2) /2 phases

N=3 3 angles + 1 phase KMthe phase generates complex couplings i.e. CPviolation;6 masses +3 angles +1 phase = 10 parameters

Vud Vus Vub

Vcd Vcs Vcb

Vtb Vts Vtb

Page 8: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

CP Violation is natural with three quarkgenerations (Kobayashi-Maskawa)

With three generations all CPphenomena are related to the same

unique parameter ( δ )

NO Flavour Changing Neutral Currents (FCNC)at Tree Level

(FCNC processes are good candidates forobserving NEW PHYSICS)

Page 9: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Vud Vus Vub

Vcd Vcs Vcb

Vtd Vts Vtb

Quark masses &Generation Mixing

NeutronProton

νe

e-

downup

W

| Vud |

| Vud | = 0.9735(8)| Vus | = 0.2196(23)| Vcd | = 0.224(16)| Vcs | = 0.970(9)(70)| Vcb | = 0.0406(8)| Vub | = 0.00409(25)| Vtb | = 0.99(29) (0.999)

β-decays

Page 10: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

1 - 1/2 !2 ! A !3(" - i #)

- ! 1 - 1/2 !2 A !2

A !3 $

(1- " - i #) -A !2 1

+ O(λ4)

The Wolfenstein Parametrization

λ ~ 0.2 A ~ 0.8 η ~ 0.2 ρ ~ 0.3

Sin θ12 = λSin θ23 = A λ2

Sin θ13 = A λ3(ρ-i η)

Vtd

Vub

Page 11: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

a1

a2

a3

b1

b2

b3

d1

e1

c3

The Bjorken-Jarlskog Unitarity Triangle| Vij | is invariant under

phase rotationsa1 = V11 V12

* = Vud Vus*

a2 = V21 V22* a3

= V31 V32*

a1 + a2 + a3 = 0(b1 + b2 + b3 = 0 etc.)

a1

a2a3

α β

γOnly the orientation dependson the phase convention

Page 12: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Physical quantities correspond to invariantsunder phase reparametrization i.e.|a1 |, |a2 |, … , |e3 | and the area of theUnitary Triangles

a precise knowledge of themoduli (angles) would fix J

Vud*Vub+ Vcd

* Vcb+Vtd

* Vtb = 0

CP ∝ J

J = Im (a1 a2 * ) = |a1 a2 | Sin β

Vud*Vub Vtd

*Vtb

Vcd*Vcb

α

γ βγ = δCKM

Page 13: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

13

VubVud+ VcbVcd+VtbVtd = 0* **

Page 14: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

From A. StocchiICHEP 2002

Page 15: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

For details see:UTfit Collaboration

http://www.utfit.org

Page 16: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

sin 2β is measured directly from B J/ψ Ksdecays at Babar & Belle

Γ(Bd0 J/ψ Ks , t) - Γ(Bd

0 J/ψ Ks , t)AJ/ψ Ks =Γ(Bd

0 J/ψ Ks , t) + Γ(Bd0 J/ψ Ks , t)

AJ/ψ Ks = sin 2β sin (Δmd t)

Page 17: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

DIFFERENT LEVELS OF THEORETICALUNCERTAINTIES (STRONG INTERACTIONS)

1) First class quantities, with reduced or negligible theor.uncertainties

2) Second class quantities, with theoretical errors of O(10%)or less that can be

reliably estimated

3) Third class quantities, for which theoretical predictionsare model dependent (BBNS, charming, etc.)

In case of discrepacies we cannottell whether is new physics orwe must blame the model

Page 18: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

K0 - K0

mixing

UnitaryTriangle SM

B0d,s - B0

d,s mixing Bd Asymmetry

2005

semileptonic decays

Page 19: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Classical Quantities used in the Standard UT Analysis

beforeonly a lower bound

Inclusive vs ExclusiveOpportunity for lattice QCDsee later

Vub/Vcb εK Δmd Δmd/Δms

levels @68% (95%) CL

f+,F

BK

fBBB1/2 ξ

Page 20: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

New Quantities used in the UT Analysis

sin 2β cos 2β α γ sin (2β + γ)

B→J/Ψ K0 B→J/Ψ K*0 B→ππ,ρρ B→D(*)K B→D(*)π,Dρ

Page 21: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 22: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 23: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 24: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Repeat with several fCP final states

Page 25: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

THECKM

Page 26: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Global Fit within the SM SM Fit

CKM matrix is the dominant source of flavour mixing and CP violation

In thehadronicsector,the SMCKMpatternrepresentstheprincipalpart of theflavourstructureand of CPviolation

ρ = 0.132 ± 0.020

η = 0.353 ± 0.014

Consistence on anover constrained fit

of the CKM parameters

α = (88 ± 3)0

sin2β = 0.695 ±0.025??

β = (22 ±1)0

γ= (69 ± 3)0

Page 27: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Vincenzo Vagnoni ICHEP 06, Moscow, 28th July 2006

The The UT-angles fit does not depend UT-angles fit does not depend onontheoretical calculations theoretical calculations ((treatement treatement ofof

errors is not an issueerrors is not an issue))

η = 0.340± 0.016

η = 0.404 ± 0.039

ANGLES VS LATTICE 2011

ρ = 0.129 ± 0.027

Still imperfectagreement in η dueto sin2β and Vubtension

Comparable accuracydue to the precise sin2βvalue and substantialimprovement due tothe new Δmsmeasurement

Crucial to improvemeasurements of theangles, in particular γ(tree level NP-freedetermination)

UT-angles UT-lattice

ρ = 0.155 ± 0.038

Page 28: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

SM predictionsof Δms

SM expectationΔms = (18.3 ± 1.3 ) ps-1

agreement between the predicted values and the measurements at better than :

5σ3σ

Legenda

Δms

10

Prediction “era” Monitoring “era”

ExpΔms = (17.77 ± 0.12 ) ps-1

Page 29: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Theoretical predictions of Sin 2 βin the years predictions

exist since '95

experiments

sin 2 βUTA = 0.65 ± 0.12Prediction 1995 fromCiuchini,Franco,G.M.,Reina,Silvestrini

Page 30: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

1) Possible tensions in the present SM Fit ?2) Fit of NP-ΔF=2 parameters in a Model “independent” way3) “Scale” analysis in ΔF=2

Is the present picture showing a Model StandardissimoStandardissimo ?

An evidence, an evidence, my kingdom for an evidence From Shakespeare's Richard III

Page 31: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Compatibility plotsThey are a procedure to ``measure” the agreement of a singlemeasurement with the indirect determination from the fit

αexp = (91 ± 6)0 γexp = (76 ± 11)0

Page 32: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 33: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 34: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

εΚ

-1.5 σ devation

Three “news” ingredients

(6)

12Imsin

i

K

Me

m

!

!

"

#! " $% &

= +' ()* +

K

1) Buras&Guadagnoli BG&Isidori corrections

Decrease the SM prediction by 6%

2) Improved value for BK BK=0.731±0.07±0.35

3) Brod&Gorbhan charm-top contribution at NNLO enhancement of 3% (not included yet)

Page 35: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 36: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

VUB PUZZLE

Inclusive: uses non perturbative parameters most not from lattice QCD (fitted from the lepton spectrum)

Exclusive: uses non perturbative form factors from LQCD and QCDSR

Page 37: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Vcb & Vub

Vub (excl) = (3.26 ± 0.30) 10-3

Vub (inc) = (4.40 ± 0.31) 10-3

Vub (com) = (3.83 ± 0.57) 10-3

~2σ difference

Vcb (excl) = (39.5 ± 1.0) 10-3

Vcb (inc) = (41.7 ± 0.7) 10-3

Vcb (com) = (41.0 ± 1.0) 10-3

2.4% uncertainty

AFTER EPS-HEP2011

15% uncertainty

Page 38: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

sin2β(excl) = 0.740 ± 0.041 1.6 σ from direct measurement

sin2β(incl) = 0.809 ± 0.036 3.2 σ from direct measurement

no B → τν

Page 39: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

σMeasurementPrediction

+1.318 ±113.55 ±0.28Br(Bll ) 10-9

1.40.731 ±0.0360.88 ±0.09ΒK [103]

0.33.83 ±0.573.63±0.15Vub [103]

2.31.64±0.340.83±0.08Br(Bτ ν) 10-4

1.017.70±0.0819.1±1.5Δms (ps-1)

2.30.667±0.0210.795±0.051sin2β

0.7(91 ± 6)°(85 ± 4)°α

0.9(79 ±10)°(69 ±3)°γ

Summary Table of the Pulls

Page 40: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

What for a ``standardissimo” CKMwhich agrees so well with theexperimental observations?

New Physics at the EWscale is “flavor blind”-> MINIMAL FLAVORVIOLATION, namely flavouroriginates only from theYukawa couplings of the SM

New Physics introduces newsources of flavour, thecontribution of which, atmost < 20 % , should befound in the present data,e.g. in the asymmetries ofBs decays

Page 41: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

INCLUSIVE Vub = (43.1 ± 3.9) 10-4

Model dependent in the threshold region(BLNP, DGE, BLL)But with a different modelling ofthe threshold region [U.Aglietti et al.,0711.0860] Vub = (36.9 ± 1.3 ± 3.9) 10-4

EXCLUSIVE Vub = (34.0 ± 4.0) 10-4

Form factors from LQCD and QCDSR

Page 42: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

…. beyond the Standard Model

Page 43: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Only tree level processes Vub/Vcb and B-> DK(*)

CP VIOLATION PROVEN IN THESM !!

degeneracy of γbroken by ASL

Page 44: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 45: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

In general the mixing mass matrix of the SQuarks(SMM) is not diagonal in flavour space analogouslyto the quark case We may eitherDiagonalize the SMM

z , γ , g

QjLqj

L

FCNC

or Rotate by the samematrices the SUSY partners ofthe u- and d- like quarks(Qj

L )´ = UijL Qj

LUj

LUiL dk

L

g

Page 46: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

In the latter case the Squark MassMatrix is not diagonal

(m2Q )ij = m2average 1ij + Δmij2 δij = Δmij2 / m2average

Page 47: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

New local four-fermion operators are generatedQ1 = (bL

A γµ dLA) (bL

Bγµ dLB) SM

Q2 = (bRA dL

A) (bRB dL

B)Q3 = (bR

A dLB) (bR

B dLA)

Q4 = (bRA dL

A) (bLB dR

B)Q5 = (bR

A dLB) (bL

B dRA)

+ those obtained by L ↔ R

Similarly for the s quark e.g.(sR

A dLA) (sR

B dLB)

Page 48: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Bs mixing , a road to New Physics (NP) ?

The Standard Model contributionto CP violation in Bs mixing iswell predicted and rather small

The phase of the mixing amplitudes can be extractedfrom Bs ->J/Ψ φ with a relatively small th.

uncertainty. A phase very different from 0.04 impliesNP in Bs mixing

2009

Page 49: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Main Ingredients and General Parametrizations

Neutral Kaon Mixing

Page 50: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Bd and Bs mixing

CqPen and φq

Pen parametrize possible NP contributions to Γq

12 from b -> s penguins

Page 51: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Physical observables

Page 52: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Experimental measurements

Page 53: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 54: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

XXACP (J/Ψ Κ)

XXASL(Bs)

XXεK

XXτ(Βs), ΔΓs/Γs

XXXXACH

CεK

X

ϕs

XXACP (Dπ(ρ),DKπ)

XXASL

XXα (ρρ,ρπ,ππ)

Xγ (DΚ)

~XACP (J/Ψ φ)

XΔms

ϕd

X

Cd Csρ , η

XΔmd

XVub/VcbTree

processes

1↔3 family

2↔3 family

1↔2familiy

0

( , , , ..)

( / , ) sin(2 2 ) ( , , )

( , , )

| | | |

d d

d d

d d

EXP SM

d B d B

CP B B

EXP SM

B B

EXP SM

K K

m C m f C QCD

A J K f

f

C!

" #

$ % " # %

& & % " # %

! !

' = '

( = +

= )

= ( , , , ..)

( , , , ..)

( / , ) sin(2 2 ) ( , , )

...

s

s s

EXP SM

s B s Bs

CP s B B

f C QCD

m C m f C QCD

A J f

!" #

" #

% $ % " # %

' = '

( = )

ΔF=2NP model independent Fit

Parametrizing NP physics in ΔF=2 processes

2 2 2

2

NP SM

i B B

SM

B

A Ae

A

! = ! =

! =

+=

qC döCBqe2iφBq

Page 55: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

η = 0.346 ± 0.015

ρ = 0.129 ± 0.022

η = 0.389 ± 0.054

ρ = 0.145 ± 0.045

SM analysis NP-ΔF=2 analysis

ρ,η fit quite precisely in NP-ΔF=2 analysis and consistent with the one obtained on the SM analysis

[error double](main contributors tree-level γ and Vub)

5 new free parameters Cs,ϕs Bs mixing Cd,ϕd Bd mixing CεK K mixing

Today : fit is overcontrained

Possible to fit 7 free parameters (ρ, η, Cd,ϕd ,Cs,ϕs, CεK)

Please consider these numbers when you want to get CKM parametersin presence of NP in ΔF=2 amplitudes (all sectors 1-2,1-3,2-3)

Page 56: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 57: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

Effective Theory Analysis ΔF=2

2( )

( )

j

j

j

jC

LF F

C

L= !" ="

""

L is loop factor and should be : L=1 tree/strong int. NPL=α2

s or α2W for stron/weak perturb. NP

C(Λ) coefficients are extracted from data

F1=FSM=(VtqVtb*)2

Fj=1=0 MFV

|Fj | =FSMarbitrary phases NMFV

|Fj | =1 arbitrary phases

Flavour generic

Effective Hamiltonian in the mixing amplitudes

Page 58: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

From Kaon sector @ 95% [TeV]

~14000~47000~470000Generic

3.211107NMFV

MFV

αW loopαs loopStrong/treeScenario

From Bd&Bs sector @ 95% [TeV]

1003303300Generic

0.250.88NMFV

MFV

αW loopαs loopStrong/treeScenario

Main contribution to present lower bound on NP scale come fromΔΦ=2 chirality-flipping operators ( Q4) which are RG enhanced

Page 59: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

b s & τ µγ in SUSY GUTS

ΔMs msq=500 GeV

Φs

Limits from Belle and Babar <4.5 & 6.8 10-8

Page 60: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries
Page 61: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

We can consider simultaneously LFV, g-2e EDM,e.g. Isidori, Mescia, Paradisi, Temes in MSSM

Page 62: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

FCNC in rare K decays

Page 63: G. Martinelli - From the Standard Model to Dark Matter and beyond: Symmetries, Masses and Mysteries

1) CKM matrix is the dominant source of flavour mixing and CPviolation σ(ρ)~15% & σ(η) ~4%

2) There are tensions that should be understood : sin2β, εK , Br(Bτ ν)

3) Estraction of SM predictions with different possibilities:inclusive vs exclusive

4) The suggestion of a large Bs mixing phase has survived formore than two years but could be killed by LHCbmeasurements.

CONCLUSIONS