Possibili candidati di materia oscura ai collisori.

Antonio Masiero

Univ. di Padova

INFN, Padova

Ricerca di Materia Oscura a LHC, Padova, 22 Aprile 2008

UNIFICATION ofFUNDAMENTAL INTERACTIONS

THE G-W-S STANDARD MODEL

COLLA NUCLEARE

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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!

WHY TO GO BEYOND THE SM

“OBSERVATIONAL” REASONS

•HIGH ENERGY PHYSICS

(but AFB……)

•FCNC, CPNO (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 bbNO

NO

NO

YES

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

YESStrong CP violation?

MICRO MACROPARTICLE PHYSICS COSMOLOGY

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

Present “Observational” Evidence for New Physics

• NEUTRINO MASSES

• DARK MATTER

• MATTER-ANTIMATTER ASYMMETRY

• INFLATION

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)

Bilancio energetico dell’Universo

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

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 !

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

LSS PATTERN AND NEUTRINO MASSES

(E..g., Ma 1996)

m = 0 eV m = 1 eV

m = 7 eV m = 4 eV

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

TEN COMMANDMENTS TO BE A “GOOD”

DM CANDIDATE • 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”

BERTONE, A.M., TAOSO

WIMPS (Weakly Interacting Massive Particles)

#~# m

# exp(-m/T)# does not change any more

Tdecoupl. typically ~ m /20

depends on particle physics (annih.) and “cosmological” quantities (H, T0, …

h2_ ~ 10-3

<(annih.) V > TeV2

~ 2 / M2 From T0 MPlanck

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)

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

LE “COSTANTI” DI ACCOPPIAMENTO FONDAMENTALI

NON SONO COSTANTI

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

HOW TO COPE WITH THE HIERARCHY PROBLEM

• LOW-ENERGY SUSY

• LARGE EXTRA DIMENSIONS

• DYNAMICAL SYMMETRY BREAKING OF THE ELW. SYMMETRY

• LANDSCAPE APPROACH (ANTHROPIC PRINCIPLE)

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

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)

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)

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

STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS

1) ENLARGEMENT OF THE SM

SUSY EXTRA DIM. LITTLE HIGGS. (x, ) (x, ji) SM part + new part

Anticomm. New bosonic to cancel 2

Coord. Coord. at 1-Loop2) 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 + ΩL h2 OK

* But abandoning gaugino-masss unif. Possible to have mLSP down to 7 GeV

mLSP

~100 - 200

GeV *

mLKP

~600 - 800

GeV

mLTP

~400 - 800

GeV

Bottino, Donato, Fornengo, Scopel

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

HUNTING FOR DARK MATTER

DIRECT DM SEARCHES

INDIRECT DM SEARCHES

Model Independent Annual Modulation ResultModel Independent Annual Modulation Result

experimental single-hit residuals rate vs time and energy DAMA/NaI (7 years) + DAMA/LIBRA (4 years) Total exposure: 300555 kgday = 0.82 tonyr

2-5 keV

2-6 keV

A=(0.0215±0.0026) cpd/kg/keV

2/dof = 51.9/66 8.3 C.L.

2-4 keV

The data favor the presence of a modulated behavior with proper features at The data favor the presence of a modulated behavior with proper features at 8.28.2 C.L. C.L.

A=(0.0176±0.0020) cpd/kg/keV

2/dof = 39.6/66 8.8 C.L.

A=(0.0129±0.0016) cpd/kg/keV

2/dof = 54.3/66 8.2 C.L.

Absence of modulation? No

2/dof=117.7/67 P(A=0) = 1.310-4

Absence of modulation? No

2/dof=116.1/67 P(A=0) = 1.910-4

Absence of modulation? No

2/dof=116.4/67 P(A=0) = 1.810-4

ROM2F/2008/07

Acos[(t-t0)] ; continuous lines: t0 = 152.5 d, T = 1.00 y

ELLIS, OLIVE, SAVAGE

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, Sandick

LHC Sensitivity

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

PROFUMO, A.M., ULLIO

Experimental status and strategy

• Goal ≈ 201810-10 pbarn

• Factor ≈ 300 progress in sensitivity still required compared to best present sensitivities

XENON-10

CDMS

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)

DM DEDO THEY “KNOW” EACH OTHER?

DIRECT INTERACTION (quintessence) WITH DARK MATTER DANGER:

Very LIGHTm ~ H0

-1 ~ 10-33 eVThreat 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

CDM CANDIDATESCATENA, FORNENGO, A.M., PIETRONI, SCHELKE

FCNC, CP ≠, (g-2), ()0 m n …

LINKED TO COSMOLOGICAL EVOLUTION

Possible interplay with dynamical DE

NEWPHYSICS 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