1. LHC DARK MATTER FLAVOR : the triple alliance hunting for TeV New Physics Antonio Masiero Univ. of Padova and INFN, Padova NIKHEF, MARCH 14 2008

2. LHC and “LOW-ENERGY” NEW PHYSICS LHC discovers NP: difficult, if not impossible, to “reconstruct” the fundamental theory lying behind those signals of NP; LHC does not see any signal of NP: still a NP related to the stabilization of the elw. scale may be present, but with particles whose masses are in the multi-TeV range.

3. ON THE COMPLEMENTARITY OF DM and LFV SEARCHES to DIRECT LHC SEARCHES FOR NP Twofold meaning of such complementarity: i)synergy in “reconstructing” the “fundamental theory” staying behind the signatures of NP; ii) coverage of complementary areas of the NP parameter space ( ex.: multi-TeV SUSY physics)

4. WHY TO GO BEYOND THE SM “OBSERVATIONAL” REASONS HIGH ENERGY PHYSICS (but A FB ……) FCNC, CP  NO (but b sqq penguin …) HIGH PRECISION LOW-EN. NO (but (g-2)  …) NEUTRINO PHYSICS YE m  0,   0 COSMO - PARTICLE PHYSICS YE (DM, ∆ B cos m, INFLAT., DE) Z bb NO YES THEORETICAL REASONS INTRINSIC INCONSISTENCY OF SM AS QFT (spont. broken gauge theory without anomalies) NO ANSWER TO QUESTIONS THAT “WE” CONSIDER “FUNDAMENTAL” QUESTIONS TO BE ANSWERED BY “FUNDAMENTAL” THEORY (hierarchy, unification, flavor) NO YES

5. MICROMACRO PARTICLE PHYSICSCOSMOLOGY GWS STANDARD MODEL HOT BIG BANG STANDARD MODEL HAPPY MARRIAGE Ex: NUCLEOSYNTHESIS BUT ALSO POINTS OF FRICTION -COSMIC MATTER-ANTIMATTER ASYMMETRY -INFLATION - DARK MATTER + DARK ENERGY “OBSERVATIONAL” EVIDENCE FOR NEW PHYSICS BEYOND THE (PARTICLE PHYSICS) STANDARD MODEL

6. Present “Observational” Evidence for New Physics NEUTRINO MASSES DARK MATTER MATTER-ANTIMATTER ASYMMETRY INFLATION

7. The Energy Scale from the “Observational” New Physics neutrino masses dark matter baryogenesis inflation NO NEED FOR THE NP SCALE TO BE CLOSE TO THE ELW. SCALE The Energy Scale from the “Theoretical” New Physics Stabilization of the electroweak symmetry breaking at M W calls for an ULTRAVIOLET COMPLETION of the SM already at the TeV scale + CORRECT GRAND UNIFICATION “CALLS” FOR NEW PARTICLES AT THE ELW. SCALE

8. ELW. SYMM. BREAKING STABILIZATION VS. FLAVOR PROTECTION: THE SCALE TENSION UV SM COMPLETION TO STABILIZE THE ELW. SYMM. BREAKING:  UV ~ O(1 TeV) Isidori

9. FLAVOR BLINDNESS OF THE NP AT THE ELW. SCALE? THREE DECADES OF FLAVOR TESTS ( Redundant determination of the UT triangle verification of the SM, theoretically and experimentally “high precision” FCNC tests, ex. b s + γ, CP violating flavor conserving and flavor changing tests, lepton flavor violating (LFV) processes, …) clearly state that: A) in the HADRONIC SECTOR the CKM flavor pattern of the SM represents the main bulk of the flavor structure and of CP violation; B) in the LEPTONIC SECTOR: although neutrino flavors exhibit large admixtures, LFV, i.e. non – conservation of individual lepton flavor numbers in FCNC transitions among charged leptons, is extremely small: once again the SM is right ( to first approximation) predicting negligibly small LFV

10. UNITARITY TRIANGLE (UT) REDUNDANT DETERMINATION

11. FROM DETERMINATION TO VERIFICATION OF THE CKM PATTERN FOR HADRONIC FLAVOR DESCRIPTION TREE LEVEL ONE - LOOP A. BURAS et al.

12. THE UT - UUT OVERLAP BLANKE, BURAS, GUADAGNOLI, TARANTINO

13. Single channels understood? Allowed to take the avg.?

14. What to make of this triumph of the CKM pattern in hadronic flavor tests? New Physics at the Elw. Scale is Flavor Blind CKM exhausts the flavor changing pattern at the elw. Scale MINIMAL FLAVOR VIOLATION New Physics introduces NEW FLAVOR SOURCES in addition to the CKM pattern. They give rise to contributions which are <20% in the “flavor observables” which have already been observed! MFV : Flavor originates only from the SM Yukawa coupl.

15. ELW. PRECISION TESTS + FLAVOR PRECISION TESTS WE UNDERSTAND THE (GAUGE AND FLAVOR) STRUCTURE OF THE FUNDAMENTAL INTERACTIONS UP TO ENERGIES OF O(100 GEV)

16. What a SuperB can do in testing CMFV L. Silvestrini at SuperB IV

17. SuperB vs. LHC Sensitivity Reach in testing  SUSY SuperB can probe MFV ( with small-moderate tan  ) for TeV squarks; for a generic non-MFV MSSM sensitivity to squark masses > 100 TeV ! Ciuchini, Isidori, Silvestrini

18. SuperB vs. LHC Sensitivity Reach in testing  SUSY SuperB can probe MFV ( with small-moderate tan  ) for TeV squarks; for a generic non-MFV MSSM sensitivity to squark masses > 100 TeV ! L. Silvestrini

19. LFV IN CHARGED LEPTONS FCNC L i - L j transitions through W - neutrinos mediation GIM suppression ( m / M W ) 2 forever invisible New mechanism: replace SM GIM suppression with a new GIM suppression where m is replaced by some ∆M >> m. Ex.: in SUSY L i - L j transitions can be mediated by photino - SLEPTONS exchanges, BUT in CMSSM (MSSM with flavor universality in the SUSY breaking sector) ∆M sleptons is O( m leptons), hence GIM suppression is still too strong. How to further decrease the SUSY GIM suppression power in LFV through slepton exchange?

20. Non-diagonality of the slepton mass matrix in the basis of diagonal lepton mass matrix depends on the unitary matrix U which diagonalizes (f + f ) ~ SUSY SEESAW: Flavor universal SUSY breaking and yet large lepton flavor violation Borzumati, A. M. 1986 (after discussions with W. Marciano and A. Sanda)

21. How Large LFV in SUSY SEESAW? 1) Size of the Dirac neutrino couplings f 2) Size of the diagonalizing matrix U In MSSM seesaw or in SUSY SU(5) (Moroi): not possible to correlate the neutrino Yukawa couplings to know Yukawas; In SUSY SO(10) ( A.M., Vempati, Vives) at least one neutrino Dirac Yukawa coupling has to be of the order of the top Yukawa coupling one large of O(1) f U two “extreme” cases: a) U with “small” entries U = CKM; b) U with “large” entries with the exception of the 13 entry U = PMNS matrix responsible for the diagonalization of the neutrino mass matrix

22. LFV in SUSYGUTs with SEESAW M Pl M GUT M R M W Scale of appearance of the SUSY soft breaking terms resulting from the spontaneous breaking of supergravity Low-energy SUSY has “memory” of all the multi-step RG occurring from such superlarge scale down to M W potentially large LFV Barbieri, Hall; Barbieri, Hall, Strumia; Hisano, Nomura, Yanagida; Hisano, Moroi, Tobe Yamaguchi; Moroi;A.M.,, Vempati, Vives; Carvalho, Ellis, Gomez, Lola; Calibbi, Faccia, A.M, Vempati LFV in MSSMseesaw:  e  Borzumati, A.M.   Blazek, King; General analysis: Casas Ibarra; Lavignac, Masina,Savoy; Hisano, Moroi, Tobe, Yamaguchi; Ellis, Hisano, Raidal, Shimizu; Fukuyama, Kikuchi, Okada; Petcov, Rodejohann, Shindou, Takanishi; Arganda, Herrero; Deppish, Pas, Redelbach, Rueckl; Petcov, Shindou

23. Bright prospects for the experimental sensitivity to LFV Running: BaBar, Belle Upcoming: MEG (2006) Future: SuperKEKB (2011) PRISM/PRIME (next decade) Super Flavour factory (?) Experiments:

24. µ e+  in SUSYGUT: past and future Calibbi, Faccia, A.M., Vempati

25. LFV from SUSY GUTsLorenzo Calibbi and PRISM/PRIME conversion experiment

26. LFV from SUSY GUTsLorenzo Calibbi and the Super B (and Flavour ) factories

27. Antusch, Arganda, Herrero, Teixeira

28. THE COSMIC MATTER-ANTIMATTER ASYMMETRY PUZZLE: -why only baryons -why N baryons /N photon ~ 10 -10 NO EVIDENCE OF ANTIMATTER WITHIN THE SOLAR SYSTEM ANTIPROTONS IN COSMIC RAYS: IN AGREEMENT WITH PRODUCTION AS SECONDARIES IN COLLISIONS IF IN CLUSTER OF GALAXIES WE HAD AN ADMIXTURE OF GALAXIES MADE OF MATTER AND ANTIMATTER THE PHOTON FLUX PRODUCED BY MATTER-ANTIMATTER ANNIHILATION IN THE CLUSTER WOULD EXCEED THE OBSERVED GAMMA FLUX IF N ba. = N antibar AND NO SEPARATION WELL BEFORE THEY DECOUPLE. WE WOULD BE LEFT WITH N bar. /N photon << 10 -10 IF BARYONS-ANTIBARYONS ARE SEPARATED EARLIER DOMAINS OF BARYONS AND ANTIBARYONS ARE TOO SMALL SMALL TODAY TO EXPLAIN SEPARATIONS LARGER THAN THE SUPERCLUSTER SIZE ONLY MATTER IS PRESENT HOW TO DYNAMICALLY PRODUCE A BARYON-ANTIBARYON ASYMMETRY STARTING FROM A SYMMETRIC SITUATION

29. COSMIC MATTER-ANTIMATTER ASYMMETRY Murayama

30. SM FAILS TO GIVE RISE TO A SUITABLE COSMIC MATTER-ANTIMATTER ASYMMETRY SM DOES NOT SATISFY AT LEAST TWO OF THE THREE SACHAROV’S NECESSARY CONDITIONS FOR A DYNAMICAL BARYOGENESIS: NOT ENOUGH CP VIOLATION IN THE SM NEED FOR NEW SOURCES OF CPV IN ADDITION TO THE PHASE PRESENT IN THE CKM MIXING MATRIX FOR M HIGGS > 80 GeV THE ELW. PHASE TRANSITION OF THE SM IS A SMOOTH CROSSOVER NEED NEW PHYSICS BEYOND SM. IN PARTICULAR, FASCINATING POSSIBILITY: THE ENTIRE MATTER IN THE UNIVERSE ORIGINATES FROM THE SAME MECHANISM RESPONSIBLE FOR THE EXTREME SMALLNESS OF NEUTRINO MASSES

31. MATTER-ANTIMATTER ASYMMETRY NEUTRINO MASSES CONNECTION: BARYOGENESIS THROUGH LEPTOGENESIS Key-ingredient of the SEE-SAW mechanism for neutrino masses: large Majorana mass for RIGHT-HANDED neutrino In the early Universe the heavy RH neutrino decays with Lepton Number violatiion; if these decays are accompanied by a new source of CP violation in the leptonic sector, then it is possible to create a lepton-antilepton asymmetry at the moment RH neutrinos decay. Since SM interactions preserve Baryon and Lepton numbers at all orders in perturbation theory, but violate them at the quantum level, such LEPTON ASYMMETRY can be converted by these purely quantum effects into a BARYON-ANTIBARYON ASYMMETRY ( Fukugita-Yanagida mechanism for leptogenesis )

32. Large mixing large b-s transitions in SUSY GUTs In SU(5) d R l L connection in the 5-plet Large (  l 23 ) LL induced by large f of O(f top ) is accompanied by large (  d 23 ) RR In SU(5) assume large f (Moroi) In SO(10) f large because of an underlying Pati-Salam symmetry (Darwin Chang, A.M., Murayama) See also: Akama, Kiyo, Komine, Moroi; Hisano, Moroi, Tobe, Yamaguchi, Yanagida; Hisano, Nomura; Kitano,Koike, Komine, Okada

33. Bounds on the hadronic (  23 ) RR as modified by the inclusion of the LFV correlated bound CMPSVV

34. FCNC HADRON-LEPTON CONNECTION IN SUSYGUT If M Pl M GUT M W soft SUSY breaking terms arise at a scale > M GUT, they have to respect the underlying quark-lepton GU symmetry constraints on  quark from LFV and constraints on  lepton from hadronic FCNC Ciuchini, A.M., Silvestrini, Vempati, Vives PRL general analysis Ciuchini, A.M., Paradisi, Silvestrini, Vempati, Vives

35. DEVIATION from  - e UNIVERSALITY A.M., Paradisi, Petronzio

36. H mediated LFV SUSY contributions to R K Extension to B l deviation from universality Isidori, Paradisi

37. On the Energetic Budget of the Universe

38. DM: the most impressive evidence at the “quantitative” and “qualitative” levels of New Physics beyond SM QUANTITATIVE: Taking into account the latest WMAP data which in combination with LSS data provide stringent bounds on  DM and  B EVIDENCE FOR NON-BARYONIC DM AT MORE THAN 10 STANDARD DEVIATIONS!! THE SM DOES NOT PROVIDE ANY CANDIDATE FOR SUCH NON- BARYONIC DM QUALITATIVE: it is NOT enough to provide a mass to neutrinos to obtain a valid DM candidate; LSS formation requires DM to be COLD NEW PARTICLES NOT INCLUDED IN THE SPECTRUM OF THE FUNDAMENTAL BUILDING BLOCKS OF THE SM !

39. THE RISE AND FALL OF NEUTRINOS AS DARK MATTER Massive neutrinos: only candidates in the SM to account for DM. From here the “prejudice” of neutrinos of a few eV to correctly account for DM Neutrinos decouple at ~1 MeV ; being their mass<<decoupling temperature, neutrinos remain relativistic for a long time. Being very fast, they smooth out any possible growth of density fluctuation forbidding the formation of proto-structures. The “weight” of neutrinos in the DM budget is severely limited by the observations disfavoring scenarios where first superlarge structures arise and then galaxies originate from their fragmentation

40. LSS PATTERN AND NEUTRINO MASSES (E..g., Ma 1996) m = 0 eVm = 1 eV m = 7 eVm = 4 eV

41. Cosmological Bounds on the sum of the masses of the 3 neutrinos from increasingly rich samples of data sets

42. WIMPS (Weakly Interacting Massive Particles) #  ~#  m  #  exp(-m  /T) #  does not change any more T decoupl. typically ~ m  /20    depends on particle physics (  annih. ) and “cosmological” quantities (H, T 0, …    h 2 _ ~ 10 -3 TeV 2 ~  2 / M 2  From T 0 M plaeli   h 2 in the range 10 -2 -10 -1 to be cosmologically interesting (for DM) m  ~ 10 2 - 10 3 GeV (weak interaction)  h 2 ~ 10 -2 -10 -1 !!!

43. SEARCHING FOR WIMPs WIMPS HYPOTHESIS DM made of particles with mass 10Gev - 1Tev ELW scale With WEAK INTERACT. LHC, ILC may PRODUCE WIMPS WIMPS escape the detector MISSING ENERGY SIGNATURE FROM “KNOWN” COSM. ABUNDANCE OF WIMPs PREDICTION FOR WIMP PRODUCTION AT COLLIDERS WITHOUT SPECYFING THE PART. PHYSICS MODEL OF WIMPs BIRKEDAL, MATCHEV, PERELSTEIN, FENG,SU, TAKAYAMA

44. STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS 1) ENLARGEMENT OF THE SM SUSY EXTRA DIM. LITTLE HIGGS. (x ,  ) (x , j i) SM part + new part Anticomm. New bosonic to cancel  2 Coord. Coord. at 1-Loop 2) SELECTION RULE DISCRETE SYMM. STABLE NEW PART. R-PARITY LSP KK-PARITY LKP T-PARITY LTP Neutralino spin 1/2 spin1 spin0 3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + Ω L h 2 OK * But abandoning gaugino-masss unif. Possible to have m LSP down to 7 GeV m LSP ~100 - 200 GeV * m LKP ~600 - 800 GeV m LTP ~400 - 800 GeV Bottino, Donato, Fornengo, Scopel

45. LFV - DM CONSTRAINTS IN MINIMAL SUPERGRAVITY A.M., Profumo, Vempati, Yaguna

46. A.M., PROFUMO, ULLIO

47. SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10 TEV

48. REACH OF FUTURE FACILITIES FOR NEUTRALINO DETECTION THROUGH ANTIMATTER SEARCHES WITH FIXED M 1 = 500 GEV N03 adiabatically contracted profile Burkert profile

49. A.M., PROFUMO,ULLIO

51. THE “WHY NOW” PROBLEM

52. DMDE DO THEY “KNOW” EACH OTHER? DIRECT INTERACTION  (quintessence) WITH DARK MATTER DANGER:  Very LIGHT m  ~ H 0 -1 ~ 10 -33 eV Threat of violation of the equivalence principle, constancy of the fundamental “constants”, … CARROLL INFLUENCE OF  ON THE NATURE AND THE ABUNDANCE OF CDM Modifications of the standard picture of WIMPs FREEZE - OUT CDM CANDIDATES CATENA, FORNENGO, A.M., PIETRONI, ROSATI, SCHELKE SCALAR-TENSOR THEORIES OF GRAVITY, KINATION, RS II EXTRA DIM.

53. SCHELKE, CATENA, FORNENGO, A.M., PIETRONI

54. NEUTRALINO RELIC ABUNDANCE IN GR AND S-T THEORIES OF GRAVITY

55. CONSTRAINTS ON THE ENHANCEMENT OF THE UNIV.EXPANSION RATE FROM THE LIMITS ON THE ANTIPROTON ABUNDANCE SCFMP

56. FCNC, CP ≠, (g-2), (  ) 0 m  n    … LINKED TO COSMOLOGICAL EVOLUTION Possible interplay with dynamical DE NEW PHYSICS AT THE ELW SCALE DM - FLAVOR for DISCOVERY and/or FUND. TH. RECONSTRUCTION A MAJOR LEAP AHEAD IS NEEDED LFV NEUTRINO PHYSICSLEPTOGENESIS TEVATRON I L C