Title: Possibili candidati di materia oscura ai collisori.
1Possibili candidati di materia oscura ai
collisori.
Ricerca di Materia Oscura a LHC, Padova, 22
Aprile 2008
- Antonio Masiero
- Univ. di Padova
- INFN, Padova
2UNIFICATION ofFUNDAMENTAL INTERACTIONS
3THE G-W-S STANDARD MODEL
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6COLLA NUCLEARE
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9The 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!
10WHY 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 gt3s for NP in
- b - s transitions,,,)
- HIGH PRECISION LOW-EN.
- NO (but (g-2)? )
- NEUTRINO PHYSICS
- YE m? ?0, ???0
Z bb
NO
NO
NO
NO
YES
YES
Strong CP violation?
YES
11MICRO
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
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13Present Observational Evidence for New Physics
- NEUTRINO MASSES
- DARK MATTER
- MATTER-ANTIMATTER ASYMMETRY
- INFLATION
14INDICAZIONI 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)
15Bilancio energetico dellUniverso
16WMAP3 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
17DM 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 ! -
18THE 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
massltltdecoupling 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
19LSS PATTERN AND NEUTRINO MASSES
20Cosmological Bounds on the sum of the masses of
the 3 neutrinos from increasingly rich samples of
data sets
21TEN 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
22WIMPS (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_
lt(?annih.) V ? gt 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)
23The Energy Scale from theObservational 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
24LE COSTANTI DI ACCOPPIAMENTO FONDAMENTALI
NON SONO COSTANTI
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26DA 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
27HOW TO COPE WITH THE HIERARCHY PROBLEM
- LOW-ENERGY SUSY
- LARGE EXTRA DIMENSIONS
- DYNAMICAL SYMMETRY BREAKING OF THE ELW. SYMMETRY
- LANDSCAPE APPROACH (ANTHROPIC PRINCIPLE)
28IS 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
29STRADE 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 31 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)
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31STRADE OLTRE SM (II)
- 2) NON ESISTE IL PROBLEMA DI TRATTENERE LA
MASSA DEL BOSONE DI HIGGS A 100 GEV PERCHE
LHIGGS 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)
32STRADE OLTRE SM (III)
- 3) LA MASSA DELLHIGGS 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 NELLUNIVERSO
33STABLE 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 ?L h2 OK
mLTP 400 - 800 GeV
But abandoning gaugino-masss unif.
Possible to have mLSP down to 7 GeV
Bottino, Donato, Fornengo, Scopel
34 WIMPs proviamo a fabbricarli anche noi !
LIPOTESI 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
DELLHIGGS 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
35HUNTING FOR DARK MATTER
INDIRECT DM SEARCHES
DIRECT DM SEARCHES
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37Model Independent Annual Modulation Result
DAMA/NaI (7 years) DAMA/LIBRA (4 years) Total
exposure 300555 kg?day 0.82 ton?yr
experimental single-hit residuals rate vs time
and energy
ROM2F/2008/07
Acosw(t-t0) continuous lines t0 152.5 d,
T 1.00 y
2-4 keV
A(0.02150.0026) cpd/kg/keV ?2/dof 51.9/66
8.3 ? C.L.
Absence of modulation? No ?2/dof117.7/67 ?
P(A0) 1.3?10-4
2-5 keV
A(0.01760.0020) cpd/kg/keV ?2/dof 39.6/66
8.8 ? C.L.
Absence of modulation? No ?2/dof116.1/67 ?
P(A0) 1.9?10-4
2-6 keV
A(0.01290.0016) cpd/kg/keV ?2/dof 54.3/66 8.2
? C.L.
Absence of modulation? No ?2/dof116.4/67 ?
P(A0) 1.8?10-4
The data favor the presence of a modulated
behavior with proper features at 8.2s C.L.
38Neutralino-nucleon scattering cross sections
along the WMAP-allowed coannihilation strip for
tanbeta10 and coannihilation/funnel strip for
tanbeta50 using the hadronic parameters
ELLIS, OLIVE, SAVAGE
Ellis, Olive, Sandick
LHC Sensitivity
39SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS
SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10
TEV
PROFUMO, A.M., ULLIO
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42Experimental status and strategy
- Goal 201810-10 pbarn
- Factor 300 progress in sensitivity still
required compared to best present sensitivities
CDMS
XENON-10
43RICERCA INDIRETTA DI MATERIA OSCURA
- ANNICHILAZIONE WIMP-ANTIWIMP
- RILEVANTI PRODOTTI DELLANNICHILAZIONE
- 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)
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47DM 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
48I 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
NEUTRINO PHYSICS
LEPTOGENESIS