Transcript Slide 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
UNIFICATION of
FUNDAMENTAL 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
Z
bb
NO (but AFB……)
•FCNC, CP
NO
NO (but evidence >3σ for NP in
b - s transitions,,,)
•HIGH PRECISION LOW-EN.
NO
NO (but (g-2) …)
•NEUTRINO PHYSICS
YES
YE m
0,  0

•COSMO - PARTICLE PHYSICS
YES
YE (DM, ∆B cosm, INFLAT., DE)
THEORETICAL REASONS
•INTRINSIC INCONSISTENCY OF
SM AS QFT
NO (spont. broken gauge theory
without anomalies)
•NO ANSWER TO QUESTIONS
THAT “WE” CONSIDER
“FUNDAMENTAL” QUESTIONS TO
BE ANSWERED BY
“FUNDAMENTAL” THEORY
YES (hierarchy, unification, flavor)
Strong CP violation?
MICRO
MACRO
PARTICLE PHYSICS
GWS STANDARD MODEL
COSMOLOGY
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 NONBARYONIC 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
m = 0 eV
m = 1 eV
m = 7 eV
m = 4 eV
(E..g., Ma 1996)
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
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”
WIMPS (Weakly Interacting Massive Particles)
# exp(-m/T)

#~#
# does not change any more
m
Tdecoupl. typically ~ m /20
 ) and “cosmological” quantities (H, T , …
  depends on particle physics (annih.
0
 h2_~
10-3
<(annih.) V  > TeV2
~
2 /
M 2
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
PHYSICS
1) ENLARGEMENT
OF THE SM
SUSY
(x, )
EXTRA DIM.
(x, ji)
Anticomm.
Coord.
2) SELECTION
RULE
DISCRETE SYMM.
PARTICLE
New bosonic
Coord.
LITTLE HIGGS.
SM part + new part
to cancel 2
at 1-Loop
R-PARITY LSP
KK-PARITY LKP
T-PARITY LTP
Neutralino spin 1/2
spin1
spin0
STABLE NEW
PART.
3) FIND REGION (S)
PARAM. SPACE
WHERE THE “L” NEW
PART. IS NEUTRAL +
ΩL h2 OK
mLSP
mLKP
mLTP
~100 - 200
~600 - 800
~400 - 800
GeV *
GeV
GeV
* But abandoning gaugino-masss unif.
Possible to have mLSP down to 7 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
INDIRECT DM SEARCHES
DIRECT DM SEARCHES
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
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 8.2 C.L.
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
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 ≈ 2018
10-10 pbarn
• Factor ≈ 300
progress in
sensitivity still
required compared
to best present
sensitivities
CDMS
XENON-10
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
DE
DO THEY “KNOW” EACH OTHER?
DIRECT INTERACTION  (quintessence) WITH DARK
DANGER:
MATTER
 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
CDM CANDIDATES
CATENA, FORNENGO, A.M.,
PIETRONI, SCHELKE
ILC
TEVATRON
DM - FLAVOR
A MAJOR
LEAP AHEAD
IS NEEDED
for DISCOVERY
and/or FUND. TH.
RECONSTRUCTION
NEW
PHYSICS AT
THE ELW
SCALE
m n …
FCNC, CP ≠, (g-2), ()0
LINKED TO COSMOLOGICAL EVOLUTION
LFV
NEUTRINO PHYSICS
Possible interplay with dynamical DE
LEPTOGENESIS