AGGIORNAMENTO SULLA MATERIA OSCURA

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1 AGGIORNAMENTO SULLA MATERIA OSCURA
Giornata di aggiornamento sulla Fisca Astroparticellare, CNSII, Pisa, 6-7 Aprile 2009 AGGIORNAMENTO SULLA MATERIA OSCURA Antonio Masiero Univ. of Padova e INFN, Padova

2 DM e la Nuova Fisica DM implica nuova fisica al di la’ del SM?
DM implica nuova fisica alla scala elettrodebole ( accessibile a LHC)? Il “miracolo WIMP”e lo spazio dei parametri della nuova fisica nella cosmologia standard e in deviazioni di questa Candidati SUSY WIMP (neutralino, sneutrino, gravitino) a confronto Candidati DM non-SUSY PAMELA, ATIC e Materia Oscura

3 DM  Nuova Fisica oltre il SM SE vale la legge della gravita’
Ωbarioni = ± ** *da CMB ( 5 anni di WMAP) + Type I Supernovae + Baryon Acoustic Oscillations(BAO) **CMB + TypeI SN + BAO in accordo con la Nucleosintesi (BBN)

4 MODIFICARE LA GRAVITA’ (MOND)
DM e’ sempre derivata dalle osservazioni assumendo la validita’ della legge standard della gravita’  possibile evitare l’introduzione di DM se modifico la legge di gravita’ su varie scale astronomiche Possibili problemi per CDM Fit di MOND a >100 curve di rotazione galattiche con successo Problemi a riprodurre i dati relativi alla dinamica di clusters: necessita’ di introdurre materia invisibile (neutrini, barioni oscuri) Versione relativistica di MOND ( Tensor-Vector Scalar Th. - TeVeS) + covarianza ( Bekenstein ’04, Sanders ’05) TeVeS : OK per strong lensing, invece necessita di materia invisibile per riprodurre il weak lensing. Barioni oscuri necessari anche per fenomeni quali il Bullet Cluster ( Milgrom ’08)

5 The BULLET CLUSTER: two colliding clusters of galaxies
Stars, galaxies and putative DM behave differently during collision, allowing for them to be studied separately. In MOND the lensing is expected to follow the baryonic matter, i.e. the X-ray gas. However the lensing is strongest in two separated regions near the visible galaxies most of the mass in the cluster pair is in the form of collisionless DM

6 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 !

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

8 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

9 (Difficili) Condizioni per l’assione per costituire il 100% della DM
Hertzberg, Steigmark, Wilczek Visinelli, Gondolo

10 THE “WIMP MIRACLE” Bergstrom Tante le possibilita’, ma gli WIMP sono speciali : singolare coincidenza tra param. dei MODELLI STANDARD PART. e COSM. per dare validi candidati di DM proprio alla scala eletttrodebole (TeV)

11 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_ COSMO – PARTICLE CONSPIRACY ~ <(annih.) V  > TeV2 From T0 MPlanck ~ 2 / M2  h2 in the range to be cosmologically interesting (for DM) m ~ GeV (weak interaction) h2 ~ !!! THERMAL RELICS (WIMP in thermodyn.equilibrium with the plasma until Tdecoupl)

12 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/ spin spin0 mLSP ~ GeV * 3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + ΩL h2 OK mLKP ~ GeV mLTP ~ GeV * But abandoning gaugino-masss unif Possible to have mLSP down to 7 GeV Bottino, Donato, Fornengo, Scopel

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

14 After LEP: tuning of the SUSY param
After LEP: tuning of the SUSY param. at the % level to correctly reproduce the DM abundance: NEED FOR A “WELL-TEMPERED” NEUTRALINO

15 NEUTRALINO LSP IN THE CONSTRAINED MSSSM: A VERY SPECIAL SELECTION IN THE PARAMETER SPACE?
Favored by gµ -2 Favored by DM Excluded: stau LSP Excluded by bsγ Ellis, Olive, Santoso, Spanos

16 LSP NEUTRALINO: THE FREEDOM IN “UN-CONSTRAINED” MSSM
GUTless Model NON-UNIVERSAL HIGGS MODEL ELLIS, OLIVE, SANDICK ELLIS, FALK, OLIVE, SANTOSO

17 CMSSM: Regions of the param.
space favored in a likelihood analysis

18 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

19 SWIMPS (Super Weakly Interacting Massive Particles)
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

20 G. GIUDICE

21 DM and NON-STANDARD COSMOLOGIES BEFORE NUCLEOSYNTHESIS
NEUTRALINO RELIC DENSITY MAY DIFFER FROM ITS STANDARD VALUE, i.e. the value it gets when the expansion rate of the Universe is what is expected in Standard Cosmology WIMPS MAY BE “COLDER”, i.e. they may have smaller typical velocities and, hence, they may lead to smaller masses for the first structures which form GELMINI, GONDOLO

22 DM DE DO THEY “KNOW” EACH OTHER?
DIRECT INTERACTION  (quintessence) WITH DARK MATTER DANGER: Very LIGHT m ~ H0-1 ~ 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, SHELCKE CDM CANDIDATES

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

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

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

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

27 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

28 PROSPECTS FOR DISCOVERING THE CMSSM AT THE LHC IN LIGHT OF WMAP
RED: FULL SAMPLE OF CMMS MODELS BLUE: POINTS COMPATIBLE WITH WMAP GREEN: POINTS ACCESSIBLE TO LHC YELLOW: POINTS ACCESSIBLE TO PRESENT DIRECT DM SEARCHES Ellis et al.

29 PREDICTION OF Ω DM FROM LHC AND ILC FOR TWO DIFFERENT SUSY PARAMETER SETS
BALTZ, BATTAGLIA, PESKIN, WIZANSKY

30

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

32 NEUTRALINO LSP IN SUPERGRAVITY
A.M., PROFUMO, ULLIO

33 A.M., PROFUMO,ULLIO

34

35 WIMPS escape the detector MISSING ENERGY SIGNATURE
SEARCHING FOR WIMPs 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

36 PAMELA PUZZLE ANTIPROTONS POSITRONS

37 ATIC, PPB-BETS, HESS data

38 SMOKING GUN(S) FOR DM? DAMA/LIBRA

39 …bisogna sudare ( o far sudare I teorici) per interpretare i risultati di Pamela in chiave DM
N. WEINER

40 Compilata da A. CIRELLI

41 A. CIRELLI

42 Dalla review di Cirelli a NEUTEL09

43 BOOST richiesto per spiegare I dati di PAMELA e ottenere la corretta abbondanza di DM

44 … da dove viene il possibile boost
ARKANI-AHMED, FINKBEINER, SLATYER, WEINER

45 Slide di A. Cirelli – NEUTEL09

46 Oppure in cosmologie non-standard
El Zant, Khalil, Okada Se la rate di espansione dell’Universo al momento diel disaccoppiamento del WIMP era superiore rispetto a quella della cosmologia standard  possibile “salvare” un’adeguarta popolazione di WIMP pur avendo una sezione di annichilazione piu’ grande ( es. Teorie scalari – tensoriali della gravita’ lavoro in progress di Catena, Fornenfo, A.M., Pietroni)

47 Some final thoughts Very solid evidence of ( a large amount of) NON-BARYONIC COLD DM In the SM NO CANDIDATE FOR COLD DM ( ordinary neutrinos are hot DM; indeed, the best limit on neutrino masses comes from cosmology!) WIMPS: (very) appealing COSMO (HBB SM) – PARTICLE (GWS SM) “conspiracy” in providing the (quantitatively and qualitatively) right DM WIMPS can be part of the NEW PHYSICS at the ELW scale ( link ultraviolet completion of the SM – DM constituents) Possibility of a joint cosmo – and particle – exploration of the TeV New Physics If WIMP is the DM: complementary hunting for TeV New Physics at LHC and in DIRECT and INDIRECT searches of DM

48 I L C TEVATRON LHC 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 INFLATION LEPTOGENESIS NEUTRINO PHYSICS