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ASTROPARTICLES IN THE LHC ERA

NO - VE 2008, Venice, April 15-18, 2008. ASTROPARTICLES IN THE LHC ERA. Antonio Masiero Univ. of Padova and INFN, Padova. LHC and “LOW-ENERGY” NEW PHYSICS. LHC discovers NP : difficult, if not impossible, to “reconstruct” the fundamental theory lying behind those signals of NP;

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ASTROPARTICLES IN THE LHC ERA

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  1. NO - VE 2008, Venice, April 15-18, 2008 ASTROPARTICLES IN THE LHC ERA Antonio Masiero Univ. of Padova and INFN, Padova

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

  4. WHY TO GO BEYOND THE SM “OBSERVATIONAL” REASONS 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) • HIGH ENERGY PHYSICS • (but AFB……) • FCNC, CP • NO (but evidence >3σ for NP in • b - s transitions,,,) • HIGH PRECISION LOW-EN. • NO (but (g-2) …) • NEUTRINO PHYSICS • YE m0, 0 • COSMO - PARTICLE PHYSICS • YE (DM, ∆B cosm, INFLAT., DE) Z bb NO NO NO NO YES YES Strong CP violation? YES

  5. ON THE COMPLEMENTARITY OFDM and LFV SEARCHES to DIRECT LHC SEARCHES FOR NP • Twofold meaning of such complementarity: • 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)

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

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

  8. 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 MHIGGS > 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

  9. MATTER-ANTIMATTER ASYMMETRY NEUTRINO MASSES CONNECTION: BARYOGENESIS THROUGH LEPTOGENESIS • Key-ingredient of the SEE-SAW mechanism for neutrino masses: large Majorana mass for the 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 )

  10. SUSY SEESAW: Flavor universal SUSY breaking and yet large lepton flavor violation Borzumati, A. M. 1986 (after discussions with W. Marciano and A. Sanda) ~ 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) see Isidori’s talk at this meeting

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

  12. INFLATION • CAUSALITY (isotropy of CMBR) • FLATNESS ( close to 1 today) • AGE OF THE UNIV. • PRIMORDIAL MONOPOLES SEVERE COSMOGICAL PROBLEMS COMMON SOLUTION FOR THESE PROBLEMS VERY FAST (EXPONENTIAL) EXPANSION IN THE UNIV.  V() VACUUM ENERGY  dominated by vacuum en. TRUE VACUUM NO WAY TO GET AN “INFLATIONARY SCALAR POTENTIAL” IN THE STANDARD MODEL

  13. NO ROOM IN THE PARTICLE PHYSICS STANDARD MODEL FOR INFLATION V=2 2 + 4 no inflation But for one solution requiring a non-trivial gymnastics Need to extend the SM scalar potential Ex: GUT’s, SUSY GUT’s,… See Giudice’s talk at this meeting ENERGY SCALE OF “INFLATIONARY PHYSICS”: LIKELY TO BE » Mw DIFFICULT BUT NOT IMPOSSIBLE TO OBTAINELECTROWEAK INFLATION IN SM EXTENSIONS

  14. 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 MW calls for an ULTRAVIOLET COMPLETION of the SM already at the TeV scale+ CORRECT GRAND UNIFICATION “CALLS” FOR NEW PARTICLES AT THE ELW. SCALE

  15. Mandatory to look for P - DECAY

  16. On the Energetic Budget of the Universe Courtesy of H. Murayama

  17. WMAP3 + small scale CMB exps (BOOMERang, ACBAR, CBI ans VSA) +Large-Scale Structures (SDSS,2dFCRS) +SuperNova ( HST/GOODS, SNLS) CONSISTENT WITH BARYON DENSITY DETERMINATION FROM BIG BANG NUCLEOSYNTHESIS

  18. 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 BEVIDENCE 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 !

  19. 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

  20. WIMPS (Weakly Interacting Massive Particles)  # exp(-m/T) # does not change any more #~# m Tdecoupl. typically ~ m /20    depends on particle physics (annih.) and “cosmological” quantities (H, T0, … 10-3  h2_ ~ <(annih.) V  > TeV2 From T0 MPlanck ~ 2 / M2 h2 in the range 10-2 -10-1 to be cosmologically interesting (for DM) m ~ 102 -103 GeV (weak interaction) h2 ~ 10-2 -10-1 !!! THERMAL RELICS (WIMP in thermodyn.equilibrium with the plasma until Tdecoupl)

  21. STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS SUSY EXTRA DIM. LITTLE HIGGS. 1) ENLARGEMENT OF THE SM (x, ) (x, ji) 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 mLSP ~100 - 200 GeV * mLKP ~600 - 800 GeV 3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + ΩL h2 OK mLTP ~400 - 800 GeV * But abandoning gaugino-masss unif. Possible to have mLSP down to 7 GeV Bottino, Donato, Fornengo, Scopel

  22. D. kAZAKOV

  23. FROM THE MSSM TO THE CMSSM ( constrained MSSM) PROLIFERATION OF PARAMETRS IN THE SOFT BREAKING SECTOR OF THE MSSM: OVERALL NUMBER OF PARAM. IN THE MSSM IS 1 2 4 CMSSM

  24. WHICH SUSY HIDDEN SECTOR SUSY BREAKING AT SCALE F F = (105 - 106) GeV F = MW MPl GRAVITY GAUGE INTERACTIONS MESSENGERS Mgravitino~ F/MPl ~ (102 -103) eV Mgravitino ~ F/MPl ~ (102 -103) GeV OBSERVABLE SECTOR SM + superpartners MSSM : minimal content of superfields

  25. GRAVITINO LSP? • GAUGE MEDIATED SUSY BREAKING (GMSB) : LSP likely to be the GRAVITINO ( it can be so light that it is more a warm DM than a cold DM candidate ) Although we cannot directly detect the gravitino, there could be interesting signatures from the next to the LSP ( NLSP) : for instance the s-tau could decay into tau and gravitino, Possibly with a very long life time, even of the order of days or months

  26. DIFFERENT FROM THE THERMAL HISTORY OF WIMPS SWIMPS(Super Weakly Interacting Massive Particles) • - LSP Gravitino in SUSY • - First excitation of the graviton in UED … They inherit the appropriate relic density through the decay of a more massive thermal species that has earlier decoupled from the thermal bath

  27. ELLIS, OLIVE,SANTOSO,SPANOS

  28. THE “WHY NOW” PROBLEM

  29. DM DE DO THEY “KNOW” EACH OTHER? DIRECT INTERACTION  (quintessence) WITH DARK MATTER • DANGER: • Very LIGHT m ~ H0-1 ~ 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 SCALAR-TENSOR THEORIES OF GRAVITY, KINATION, RS II EXTRA DIM. Modifications of the standard picture of WIMPs FREEZE - OUT CATENA, FORNENGO, A.M., PIETRONI, ROSATI, SCHELKE CDM CANDIDATES

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

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

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

  33. SEARCHING FORWIMPs LHC, ILC may PRODUCE WIMPS WIMPS escape the detector MISSING ENERGY SIGNATURE WIMPS HYPOTHESIS DM made of particles with mass 10Gev - 1Tev ELW scale With WEAK INTERACT. 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

  34. Model Independent Annual Modulation Result DAMA/NaI (7 years) + DAMA/LIBRA (4 years) Total exposure: 300555 kgday = 0.82 tonyr experimental single-hit residualsratevstime and energy ROM2F/2008/07 Acos[w(t-t0)] ; continuous lines: t0 = 152.5 d, T = 1.00 y 2-4 keV A=(0.0215±0.0026) cpd/kg/keV 2/dof = 51.9/66 8.3  C.L. Absence of modulation? No 2/dof=117.7/67  P(A=0) = 1.310-4 2-5 keV A=(0.0176±0.0020) cpd/kg/keV 2/dof = 39.6/66 8.8  C.L. Absence of modulation? No 2/dof=116.1/67  P(A=0) = 1.910-4 2-6 keV A=(0.0129±0.0016) cpd/kg/keV 2/dof = 54.3/66 8.2  C.L. Absence of modulation? No 2/dof=116.4/67  P(A=0) = 1.810-4 The data favor the presence of a modulated behavior with proper features at 8.2s C.L.

  35. Neutralino-nucleon scattering cross sections along the WMAP-allowed coannihilation strip for tanbeta=10 and coannihilation/funnel strip for tanbeta=50 using the hadronic parameters ELLIS, OLIVE, SAVAGE Ellis, Olive, Sandick LHC Sensitivity

  36. SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10 TEV PROFUMO, A.M., ULLIO

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

  38. INDIRECT SEARCHES OF DM • WIMPs collected inside celestial bodies ( Earth, Sun): their annihilations produce energetic neutrinos • WIMPs in the DM halo: WIMP annihilations can take place ( in particular, their rate can be enhanced with there exists a CLUMPY distribution of DM as computer simulations of the DM distribution in the galaxies seem to suggest. From the WIMP annihilation: -- energetic neutrinos ( under-ice, under-water exps Amanda, Antares, Nemo, Antares, …) --photons in tens of GeV range ( gamma astronomy on ground Magic, Hess, … or in space Glast…) --antimatter: look for an excess of antimatter w.r.t. what is expected in cosmic rays ( space exps. Pamela, AMS, …)

  39. Roszkowski, Ruiz, Silk, Trotta

  40. CIRELLI, STRUMIA, TAMBURINI 2008

  41. A.M., PROFUMO, ULLIO

  42. A.M., PROFUMO,ULLIO

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