Possibili candidati di materia oscura ai collisori.

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

• Antonio Masiero
• Univ. di Padova
• INFN, Padova

2
UNIFICATION ofFUNDAMENTAL INTERACTIONS
3
THE G-W-S STANDARD MODEL
4
(No Transcript)
5
(No Transcript)
6
COLLA NUCLEARE
7
(No Transcript)
8
(No Transcript)
9
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!

10
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 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
11
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
12
(No Transcript)
13
Present Observational Evidence for New Physics

• NEUTRINO MASSES
• DARK MATTER
• MATTER-ANTIMATTER ASYMMETRY
• INFLATION

14
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)

15
Bilancio energetico dellUniverso
16
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
17
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 !

18
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
  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

19
LSS PATTERN AND NEUTRINO MASSES
20
Cosmological Bounds on the sum of the masses of
the 3 neutrinos from increasingly rich samples of
data sets
21
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

22
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_

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)
23
The 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
24
LE COSTANTI DI ACCOPPIAMENTO FONDAMENTALI
NON SONO COSTANTI
25
(No Transcript)
26
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
27
HOW TO COPE WITH THE HIERARCHY PROBLEM

• LOW-ENERGY SUSY
• LARGE EXTRA DIMENSIONS
• DYNAMICAL SYMMETRY BREAKING OF THE ELW. SYMMETRY
• LANDSCAPE APPROACH (ANTHROPIC PRINCIPLE)

28
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

29
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 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)

30
(No Transcript)
31
STRADE 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)

32
STRADE 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

33
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 ?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
35
HUNTING FOR DARK MATTER
INDIRECT DM SEARCHES
DIRECT DM SEARCHES
36
(No Transcript)
37
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 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.
38
Neutralino-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
39
SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS
SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10
TEV
PROFUMO, A.M., ULLIO
40
(No Transcript)
41
(No Transcript)
42
Experimental status and strategy

• Goal  201810-10 pbarn
• Factor  300 progress in sensitivity still
  required compared to best present sensitivities

CDMS
XENON-10
43
RICERCA 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)

44
(No Transcript)
45
(No Transcript)
46
(No Transcript)
47
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
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
NEUTRINO PHYSICS
LEPTOGENESIS