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Possibili candidati di materia oscura ai collisori.

Ricerca di Materia Oscura a LHC, Padova, 22 Aprile 2008. Possibili candidati di materia oscura ai collisori. Antonio Masiero Univ. di Padova INFN, Padova. UNIFICATION of FUNDAMENTAL INTERACTIONS. THE G-W-S STANDARD MODEL. COLLA NUCLEARE. The HIGGS BOSON CONDENSATE.

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Possibili candidati di materia oscura ai collisori.

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  1. Ricerca di Materia Oscura a LHC, Padova, 22 Aprile 2008 Possibili candidati di materia oscura ai collisori. Antonio Masiero Univ. di Padova INFN, Padova

  2. UNIFICATION ofFUNDAMENTAL INTERACTIONS

  3. THE G-W-S STANDARD MODEL

  4. COLLA NUCLEARE

  5. The HIGGS BOSON CONDENSATE • “SOMETHING” fills the Universe: it “disturbs” Weak interactions making them SHORT-RANGED, while it does NOT affect gravity or electromagnetism. • WHAT IS IT? • Analogy with SUPERCONDUCTIVITY: in a superconductor the magnetic field gets repelled ( Meissner effect) and penetrates only over the “penetration length”, i.e. the magnetic field is short-ranged source which disturbs are the boson condensates, Cooper pairs. • We are “swimming” in Higgs Boson Condensates its value at the minimum of its potential determines the masses of all particles!

  6. 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

  7. 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

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

  9. INDICAZIONI DI NUOVA FISICA AL DI LA’ DEL MODELLO STANDARD • MASSA DEI NEUTRINI • ESISTENZA DI MATERIA OSCURA NON COSTITUITA DALLA “SOLITA” MATERIA (protoni, neutroni) • ASIMMETRIA COSMICA TRA MATERIA E ANTIMATERIA: ESISTENZA DI UNA NUOVA SORGENTE DI VIOLAZIONE DI CP OLTRE A QUELLA PREVISTA DAL MODELLO STANDARD • DOMANDE “FONDAMENTALI” A CUI IL MODELLO STANDARD NON RISPONDE: - UNIFICAZIONE DELLE FORZE FONDAMENTALI - MASSE E MESCOLAMENTI DEI FERMIONI - “STABILITA’” DELLA SCALA DI ENERGIA A CUI I BOSONI W e Z PRENDONO MASSA ( circa 100 GeV)

  10. Bilancio energetico dell’Universo

  11. 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

  12. 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 !

  13. 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

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

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

  16. TEN COMMANDMENTS TO BE A “GOOD” DM CANDIDATE BERTONE, A.M., TAOSO • TO MATCH THE APPROPRIATE RELIC DENSITY • TO BE COLD • TO BE NEUTRAL • TO BE CONSISTENT WITH BBN • TO LEAVE STELLAR EVOLUTION UNCHANGED • TO BE COMPATIBLE WITH CONSTRAINTS ON SELF – INTERACTIONS • TO BE CONSISTENT WITH DIRECT DM SEARCHES • TO BE COMPATIBLE WITH GAMMA – RAY CONSTRAINTS • TO BE COMPATIBLE WITH OTHER ASTROPHYSICAL BOUNDS • “TO BE PROBED EXPERIMENTALLY”

  17. 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)

  18. 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

  19. LE “COSTANTI” DI ACCOPPIAMENTO FONDAMENTALI NON SONO COSTANTI

  20. DA G.U.T. A SUSY G.U.T. Aggiunta di nuove particelle SUSY partner di quelle ordinarie del Modello Standard ad una scala di massa tra 100 e 1000 GeV

  21. HOW TO COPE WITH THE HIERARCHY PROBLEM • LOW-ENERGY SUSY • LARGE EXTRA DIMENSIONS • DYNAMICAL SYMMETRY BREAKING OF THE ELW. SYMMETRY • LANDSCAPE APPROACH (ANTHROPIC PRINCIPLE)

  22. IS THE FINE-TUNING A REAL PROBLEM? • WARNING: THERE EXISTS AN EVEN “LARGER” HIERARCHY OR FINE -TUNING OR NATURALNESS PROBLEM: THE COSMOLOGICAL CONSTANT PROBLEM (“ THE MOTHER” OF ALL NATURALNESS PROBLEMS); SO FAR, WE SIMPLY “ACCEPT” SUCH FINE-TUNING! • (OUTRAGEOUS) POSSIBILITY: THE “THEORY OF EVERYTHING” COULD BE UNIQUE, BUT WITH MANY (INFINITE?) VACUA EACH GIVING RISE TO A DIFFERENT UNI-VERSE ( MULTI-VERSE POSSIBILITY).WE CAN LIVE ONLY IN THE VERY RESTRICTED CLASS OF THE “MULTI-VERSE SPACE” WHERE THE “BOUDARY CONDITIONS” ( FOR INSTANCE, THE VALUE OF THE COSMOLOGICAL CONSTANT OR THE SCALE OF THE ELW.SYMMETRY BREAKING AND, HENCE, THE HIGGS MASS) EXHIBIT VALUES ALLOWING FOR THE CORRECT BBN, LSS,… OUR LIFE! ANTHROPIC PRINCIPLE

  23. STRADE PER ANDARE AL DI LA’ DEL MODELLO STANDARD 1) NON ESISTE NESSUNA SCALA DI ENERGIA OLTRE QUELLA DEL MS: la gravita’ e’ una forza molto debole perche’ esistono NUOVE DIMENSIONI oltre alle 3+1 spazio-temporali “nostre” VISIBILITA’ A LHC: ESISTONO STATI ECCITATI ( DI KALUZA-KLEIN) ED ALCUNI SONO A SCALA ACCESSIBILE A LHC ( il piu’ leggero KK puo’ essere una particella stabile e costituire la materia oscura)

  24. STRADE OLTRE SM (II) • 2)NON ESISTE IL PROBLEMA DI “TRATTENERE” LA MASSA DEL BOSONE DI HIGGS A 100 GEV PERCHE’ L’HIGGS E’ UN OGGETTO COMPOSTO VISIBILITA’ A LHC: NUOVE INTERAZIONI CHE PRODUCONO IL CONDENSATO DI FERMIONI CHE CHIAMIAMO HIGGS ( nuove risonanze, nuovi stati legati, una nuova QCD a 1 TeV)

  25. STRADE OLTRE SM (III) • 3) LA MASSA DELL’HIGGS E’ “PROTETTA” A 100 – 1000 GEV PERCHE’ ESISTE UNA NUOVA SIMMETRIA, LA SUPERSIMMETRIA VISIBILITA’ A LHC: VEDREMO LE PARTICELLE SUPERSIMMETRICHE E LE LORO INTERAZIONI. LA PIU’ LEGGERA PARTICELLA SUSY PUO’ ESSERE STABILE E COSTITUIRE LA MATERIA OSCURA. AL TEMPO STESSO POTREMMO SCOPRIRE SUSY E LA SORGENTE DEL 90% DELLA MATERIA PRESENTE NELL’UNIVERSO

  26. 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

  27. WIMPs: proviamo a “fabbricarli” anche noi ! L’IPOTESI “WIMPS” MATERIA OSCURA COSTITUITA DA PARTICELLE “NUOVE” CON MASSA TRA 100 E 1000 GEV CHE INTERAGISCONO SOLO DEBOLMENTE LHC, ILC (LINEAR COLLIDER ) POSSONO PRODURRE WIMPS WIMPS scappano dal rivelatore “FIRMA” DELL’HIGGS: ENERGIA MANCANTE DALLA MISURA DI MATERIA OSCURA POSSO RISALIRE A QUANTO GLI WIMPS INTERAGISCANO CON LA MATERIA ORDINARIA E QUINDI PREDIRE LA QUANTITA’ DI WIMPS CHE PRODURRO’ A LHC O A ILC

  28. HUNTING FOR DARK MATTER INDIRECT DM SEARCHES DIRECT DM SEARCHES

  29. 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.

  30. 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

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

  32. Experimental status and strategy • Goal ≈ 201810-10 pbarn • Factor ≈ 300 progress in sensitivity still required compared to best present sensitivities CDMS XENON-10

  33. RICERCA INDIRETTA DI MATERIA OSCURA • ANNICHILAZIONE WIMP-ANTIWIMP • RILEVANTI PRODOTTI DELL’ANNICHILAZIONE : I) FOTONI AD ALTA ENERGIA II) NEUTRINI AD ALTA ENERGIA III) ANTIMATERIA I) ASTRONOMIA GAMMA: telescopi a terra ( es. MAGIC alle Canarie) o nello spazio ( es. AGILE e GLAST) II) TELESCOPI DI NEUTRINI: sotto il ghiaccio del polo (AMANDA), o sotto il mare ( ANTARES, Marsiglia, in futuro NEMO, Capo Passero, Sicilia) III) ANTIMATERIA: ricerche di eccessi di antiprotoni o positroni in esperimenti spaziali (PAMELA su razzo russo, AMS sulla ISS)

  34. 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”,… INFLUENCE OF  ON THE NATURE AND THE ABUNDANCE OF CDM Modifications of the standard picture of WIMPs FREEZE - OUT CATENA, FORNENGO, A.M., PIETRONI, SCHELKE CDM CANDIDATES

  35. 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

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