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SUSY AND ASTROPARTICLE PHYSICS

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THE G-W-S STANDARD MODEL. The HIGGS BOSON CONDENSATE ' ... (isotropy of CMBR) FLATNESS ( close to 1 today) AGE OF THE UNIV. PRIMORDIAL MONOPOLES ... – PowerPoint PPT presentation

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Title: SUSY AND ASTROPARTICLE PHYSICS


1
SUSY AND ASTROPARTICLE PHYSICS
X ROMA3 TOPICAL SEMINAR ON SUBNUCLEAR PHYSICS
SUSY TODAY TH. AND EXP. LIMITS ONE YEAR BEFORE
LHC, Univ. ROMA TRE, DEC. 13, 2007
  • Antonio Masiero
  • Univ. di Padova
  • INFN, Padova

2
UNIFICATION ofFUNDAMENTAL INTERACTIONS
3
THE G-W-S STANDARD MODEL
4
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!

5
Where all masses come from the HIGGS mechanism
THE HIGGS MECHANISM CAN BE REALIZED BY THE
PRESENCE OF AN ELEMENTARY HIGGS PARTICLE
The Higgs has already shown up as a VIRTUAL
particle in electroweak radiative effects
6
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
7
THE ENERGY BUDGET OF THE UNIVERSE (as of Dec.
2007)
8
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 !

9
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

10
LSS PATTERN AND NEUTRINO MASSES
11
Cosmological Bounds on the sum of the masses of
the 3 neutrinos from increasingly rich samples of
data sets
12
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 Mplaeli
?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 !!!
13
THE COSMIC MATTER-ANTIMATTER ASYMMETRY
PUZZLE-why only baryons -why
Nbaryons/Nphoton 10-10
  • NO EVIDENCE OF ANTIMATTER WITHIN THE SOLAR SYSTEM
  • ANTIPROTONS IN COSMIC RAYS IN AGREEMENT WITH
    PRODUCTION AS SECONDARIES IN COLLISIONS
  • IF IN CLUSTER OF GALAXIES WE HAD AN ADMIXTURE OF
    GALAXIES MADE OF MATTER AND ANTIMATTER
    THE PHOTON FLUX PRODUCED BY
    MATTER-ANTIMATTER ANNIHILATION IN THE CLUSTER
    WOULD EXCEED THE OBSERVED GAMMA FLUX
  • IF Nba . Nantibar AND NO SEPARATION WELL
    BEFORE THEY DECOUPLE . WE WOULD BE
    LEFT WITH Nbar./Nphoton ltlt 10-10
  • IF BARYONS-ANTIBARYONS ARE SEPARATED EARLIER
    DOMAINS OF BARYONS AND
    ANTIBARYONS ARE TOO SMALL SMALL TODAY TO EXPLAIN
    SEPARATIONS LARGER THAN THE SUPERCLUSTER SIZE

ONLY MATTER IS PRESENT HOW TO DYNAMICALLY PRODUCE
A BARYON-ANTIBARYON ASYMMETRY STARTING FROM A
SYMMETRIC SITUATION
14
COSMIC MATTER-ANTIMATTER ASYMMETRY
Murayama
15
SM FAILS TO GIVE RISE TO A SUITABLE COSMIC
MATTER-ANTIMATTER ASYMMETRY
  • SM DOES NOT SATISFY AT LEAST TWO OF THE THREE
    SACHAROVS NECESSARY CONDITIONS FOR A DYNAMICAL
    BARYOGENESIS
  • NOT ENOUGH CP VIOLATION IN THE SM
    NEED FOR NEW SOURCES OF CPV IN ADDITION TO THE
    PHASE PRESENT IN THE CKM MIXING MATRIX
  • FOR MHIGGS gt 80 GeV THE ELW. PHASE TRANSITION OF
    THE SM IS A SMOOTH CROSSOVER

NEED NEW PHYSICS BEYOND SM. IN PARTICULAR,
FASCINATING POSSIBILITY THE ENTIRE MATTER IN THE
UNIVERSE ORIGINATES FROM THE SAME MECHANISM
RESPONSIBLE FOR THE EXTREME SMALLNESS OF NEUTRINO
MASSES
16
MATTER-ANTIMATTER ASYMMETRY
NEUTRINO MASSES CONNECTION BARYOGENESIS THROUGH
LEPTOGENESIS
  • Key-ingredient of the SEE-SAW mechanism for
    neutrino masses large Majorana mass for
    RIGHT-HANDED neutrino
  • In the early Universe the heavy RH neutrino
    decays with Lepton Number violatiion if these
    decays are accompanied by a new source of CP
    violation in the leptonic sector, then
  • it is possible to create a
    lepton-antilepton asymmetry at the moment RH
    neutrinos decay. Since SM interactions preserve
    Baryon and Lepton numbers at all orders in
    perturbation theory, but violate them at the
    quantum level, such LEPTON ASYMMETRY can be
    converted by these purely quantum effects into a
    BARYON-ANTIBARYON ASYMMETRY (
    Fukugita-Yanagida mechanism for leptogenesis )

17
INFLATION
  • CAUSALITY
  • (isotropy of CMBR)
  • FLATNESS
  • (? close to 1 today)
  • AGE OF THE UNIV.
  • PRIMORDIAL MONOPOLES

SEVERE COSMOGICAL PROBLEMS
COMMON SOLUTION FOR THESE PROBLEMS
VERY FAST (EXPONENTIAL) EXPANSION IN THE UNIV.
?
V(?)
VACUUM ENERGY
? dominated by vacuum en.
TRUE VACUUM
NO WAY TO GET AN INFLATIONARY SCALAR POTENTIAL
IN THE STANDARD MODEL
18
NO ROOM IN THE PARTICLE PHYSICS STANDARD MODEL
FOR INFLATION
V?2 ?2 ??4 no inflation
Need to extend the SM scalar potential Ex GUTs,
SUSY GUTs,
ENERGY SCALE OF INFLATIONARY PHYSICS LIKELY TO
BE Mw DIFFICULT BUT NOT IMPOSSIBLE TO OBTAIN
ELECTROWEAK INFLATION IN SM EXTENSIONS
19
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 b sqq penguin )
  • HIGH PRECISION LOW-EN.
  • NO (but (g-2)? )
  • NEUTRINO PHYSICS
  • YE m? ?0, ???0
  • COSMO - PARTICLE PHYSICS

Z bb
NO
NO
NO
NO
YES
YES
YES
20
Fundamental COUPLING CONSTANTS are NOT CONSTANT
21
LOW-ENERGY SUSY AND UNIFICATION
22
MASS PROTECTION
For FERMIONS, VECTOR (GAUGE) and SCALAR BOSONS
  • FERMIONS chiral symmetry
  • fL fR not invariant
  • under SU(2)x U(1)

SIMMETRY PROTECTION
-VECTOR BOSONS gauge symmetry
FERMIONS and W,Z VECTOR BOSONS can get a mass
only when the elw. symmetry is broken mf, mw ltHgt
NO SYMMETRY PROTECTION FOR SCALAR MASSES
INDUCED MASS PROTECTION
Create a symmetry (SUPERSIMMETRY) Such that
FERMIONS BOSONS So that the fermion
mass protection acts also on bosons as long as
SUSY is exact
SUSY BREAKING SCALE OF 0 (102-103 Gev) LOW
ENERGY SUSY
23
ON THE RADIATIVE CORRECTIONS TO THE SCALAR MASSES
24
DESTABILIZATION OF THE ELW. SYMMETRY BREAKING
SCALE
SCALAR MASSES ARE UNPROTECTED AGAINST LARGE
CORRECTIONS WHICH TEND TO PUSH THEM UP TO THE
LARGEST ENERGY SCALE PRESENT IN THE FULL THEORY
EX
25
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
26
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

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
ROADS TO GO BEYOND THE STANDARD MODEL (I)
  • 1) THERE EXISTS NO NEW PHYSICAL ENERGY SCALE
    ABOVE THE ELW. SCALE gravity is an extremely
    weak force not because of the enormous value of
    the Planck scale, but because of the existence of
    NEW DIMENSIONS beyond the usual 31 space-time
    where (most of) the gravity flux lines get
    dispersed
  • VISIBILITY AT LHC there exist
    excited states of the ordinary particles (
    Kaluza-Klein states) and some of them are
    accessible at LHC (the lightest KK state may be a
    stable particle and it can constitute the DM)

29
ROADS TO GO BEYOND THE STANDARD MODEL (II)
  • 2) NO NEED TO PROTECT THE HIGGS MASS AT THE
    ELW. SCALE THE HIGGS IS A COMPOSITE OBJECT (for
    instance, a fermion condensate) WHOSE
    COMPOSITENESS SCALE IS THE ELW. SCALE (cfr. the
    pion mass case)
  • VISIBILITY AT LHC THERE EXIST NEW
    (STRONG) INTERACTIONS AT THE ELW. SCALE WHICH
    PRODUCE THE HIGGS CONDENSATE ( new resonances,,
    new bound states, a new rescaled QCD at 1 TeV)

30
ROADS TO GO BEYOND THE STANDARD MODEL (III)
  • 3) THE MASS OF THE ELEMENTARY HIGGS BOSON IS
    PROTECTED AT THE ELW. SCALE BECAUSE OF THE
    PRESENCE AT THAT ENERGY OF A NEW SYMMETRY, THE
    SUPERSYMMETRY (SUSY)
  • VISIBILITY AT LHC WELL SEE
    (SOME OF) THE SUSY PARTICLES AND THEIR
    INTERACTIONS. THE LIGHTEST SUSY PARTCILE (LSP) IS
    LIKELY TO BE STABLE AND PROVIDE THE DM. AT THE
    SAME TIME, WE COULD DISCOVER SUSY AND THE SOURCE
    OF 90 OF THE ENTIRRE MATTER PRESENT IN THE
    UNIVERSE.

31
HIERARCHY PROBLEM THE SUSY WAY
SUSY HAS TO BE BROKEN AT A SCALE CLOSE TO 1TeV
LOW ENERGY SUSY
m?2 ? ?2
Scale of susy breaking
F
B
?f
?f
?B
F
?
?
Sm2 ? ( ?B - ?2f ) ?2
16 ?2
m2 B - m2F 1/2 1/vGF
B
In SUSY multiplet
F
SPLITTING IN MASS BETWEEN B and F of O ( ELW.
SCALE)
32
THE SUSY PATH
33
LOW-ENERGY SUSY
34
IS SUSY PRESENT IN NATURE?
  • I think that it is very likely that SUSY is
    present as a fundamental symmetry of Nature it
    is the most general symmetry compatible with a
    good and honest QFT, it is likely to be needed to
    have a consistent STRING theory ( super-string),
    in its local version ( local supersymmetry or
    supergravity) it paves the way to introduce and
    quantize GRAVITY in a unified picture of ALL
    FUNDAMENTAL INTERACTIONS
  • Much more debatable is whether it should be a
    LOW-ENERGY SYMMETRY ( i.e. effectively broken at
    the elw. Scale) or a HIGH-ENERGY SYMMETRY (i.e.
    broken at the Planck scale, or at the string
    compactification scale)

35
D. KAZAKOV
36
(No Transcript)
37
IN SUSY WE NEED TO INTRODUCE AT LEAST TWO HIGGS
DOUBLETS IN ORDER TO PROVIDE A MASS FOR BOTH THE
UP- AND DOWN- QUARKS
38
BREAKING SUSY
  • The world is clearly not supersymmetric
  • for instance, we have not seen a scalar of
    Q1 and a mass of ½ MeV, i.e. the
  • selectron has to be heavier than the electron
    and, hence, SUSU has to be broken

SUSY HAS TO BE BROKEN AT A SCALE gt 100 GeV SINCE
NO SUSY PARTNERS HAVE BEEN SEEN UP TO THOSE
ENERGIES, roughly COLORED S-PARTICLE MASSES gt
200 GeV UNCOLORED S- PARTICLE MASSES gt 100 GeV
39
WHICH SUSY
HIDDEN SECTOR SUSY BREAKING AT SCALE ?F
F (105 - 106) GeV
F MW MPl
GRAVITY
MESSENGERS
GAUGE INTERACTIONS
Mgravitino F/MPl (102 - 103)eV
Mgravitino F/MPl (102 -103) GeV
OBSERVABLE SECTOR SM superpartners MSSM
minimal content of superfields
40
THE SOFT BREAKING TERMS OF THE MINIMAL SUSY SM
(MSSM)
41
THE FATE OF B AND L IN THE SM AND MSSM
  • IN THE SM B AND L ARE AUTOMATIC SYMMETRIES NO
    B or L VIOLATING OPERATOR OF DIM.4 INVARIANT
    UNDER THE GAUGE SIMMETRY SU(3) X SU(2) X U(1) IS
    ALLOWED ( B AND L ARE CONSERVED AT ANY ORDER IN
    PERTURBATION THEORY, BUT ARE VIOLATED AT THE
    QUANTUM LEVEL (ONLY B L IS EXACTLY PRESERVED
    )
  • IN THE MSSM, THANKS TO THE EXTENDED PARTICLE
    SPECTRUM WITH NEW SUSY PARTNERS CARRYING B AND L,
    IT IS POSSIBLE TO WRITE ( RENORMALIZABLE)
    OPERATORS WHICH VIOLATE EITHER B OR L
  • IF BOTH B AND L
    VIOLATING OPERATORS ARE PRESENT, GIVEN THAT SUSY
    PARTNER MASSES ARE OF O(TEV), THERE IS NO WAY TO
    PREVENT A TOO FAST PROTON DECAY UNLESS THE YUKAWA
    COUPLINGS ARE INCREDIBLY SMALL!

42
D. kAZAKOV
43
ADDITIONAL DISCRETE SYMMETRY IN THE MSSM TO SLOW
DOWN P - DECAY
  • SIMPLEST (and nicest) SOLUTION ADD A SYMMETRY
    WHICH FORBIDS ALL B AND L VIOLATING OPERATORS
  • R PARITY
  • SINCE B AND L 4-DIM. OPERATORS INVOLVE 2 ORDINARY
    FERMIONS AND A SUSY SCALAR PARTICLE, THE SIMPLEST
    WAY TO ELIMINATE ALL OF THEM
  • R 1 FOR ORDINARY PARTICLES
  • R - 1 FOR SUSY PARTNERS
  • IMPLICATIONS OF IMPOSING R PARITY
  • i) The superpartners are created or destroyed in
    pairs
  • ii) THE LIGHTEST SUPERPARTNER IS ABSOLUTELY STABLE

44
BROKEN R PARITY
  • PROTON DECAY REQUIRES THE VIOLATION OF BOTH B AND
    L
  • NOT NECESSARY TO HAVE R
    PARITY TO KILL B AND L VIOLATING OPERATORS
  • ENOUGH TO IMPOSE
    AN ADDITIONAL DISCRETE SYMMETRY TO FORBID EITHER
    B OR L VIOLATING OPERATORS RESTRICTIONS ON THE
    YUKAWA COUPLINGS OF THE SURVIVING B OR L
    VIOLATING OPERATORS

45
124 FREE PARAM.
D. KAZAKOV
46
CMSSM RADIATIVE ELW. BREAKING A 4 PARAMETER
WORLD
  • FREE PARAM. IN THE CMSSM

IMPOSING THE RAD. BREAKING OF THE ELW. SYMMETRY
ONE ESTABLISHES A RELATION BETWEEN THE ELW.
BREAKING SCALE AND THE SOFT SUSY PARAMETERS
FURTHER REDUCING THE NUMBER OF THE FREE PARAM. IN
THE CMSSM TO FOUR , FOR INSTANCE THE FIRST FOUR
PARAM. ABOVE THE SIGN OF µ ( THE ELW. SYMM.
BREAKING FIXES ONLY THE SQUARE OF µ
47
D. KAZAKOV
48
(No Transcript)
49
(No Transcript)
50
(No Transcript)
51
SUSY DM a successful marriage
  • Supersymmetrizing the SM does not lead
    necessarily to a stable SUSY particle to be a DM
    candidate.
  • However, the mere SUSY version of the SM is known
    to lead to a too fast p-decay. Hence,
    necessarily, the SUSY version of the SM has to be
    supplemented with some additional ( ad hoc?)
    symmetry to prevent the p-decay catastrophe.
  • Certainly the simplest and maybe also the most
    attractive solution is to impose the discrete
    R-parity symmetry
  • MSSM R PARITY LIGHTEST SUSY
    PARTICLE (LSP) IS STABLE .
  • The LSP can constitute an interesting DM
    candidate in several interesting realizations of
    the MSSM ( i.e., with different SUSY breaking
    mechanisms including gravity, gaugino, gauge,
    anomaly mediations, and in various regions of the
    parameter space).

52
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
53
WHO IS THE LSP?
  • SUPERGRAVITY ( transmission of the SUSY breaking
    from the hidden to the obsevable sector occurring
    via gravitational interactions) best candidate
    to play the role of LSP
  • NEUTRALINO ( i.e., the lightest of the four
    eigenstates of the 4x4 neutralino mass matrix)
  • In CMSSM the LSP neutralino is almost entirely a
    BINO

54
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

55
HUNTING FOR DARK MATTER
INDIRECT DM SEARCHES
DIRECT DM SEARCHES
56
INDIRECT SEARCHES OF DM
  • WIMPs collected inside celestial bodies ( Earth,
    Sun) their annihilations produce energetic
    neutrinos
  • WIMPs in the DM halo WIMP annihilations can take
    place ( in particular, their rate can be enhanced
    with there exists a CLUMPY distribution of DM as
    computer simulations of the DM distribution in
    the galaxies seem to suggest. From the WIMP
    annihilation
  • -- energetic neutrinos ( under-ice, under-water
    exps Amanda, Antares, Nemo, Antares,Nestor
    future IceCube, KM3 )
  • --photons in tens of GeV range ( gamma astronomy
    on ground Magic, Hess, future ACT , Argo or in
    space Agile, Glast)
  • --antimatter look for an excess of antimatter
    w.r.t. what is expected in cosmic rays ( space
    exps. Pamela, AMS, )

57
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
58
Tightness of the DM constraints in Minimal
Supergravity
Ellis, Olive, Santoso, Spanos
59
LFV - DM CONSTRAINTS IN MINIMAL SUPERGRAVITY
A.M., Profumo, Vempati, Yaguna
60
DM SUSYHOW FAR ARE WE IN DIRECT SEARCHES?
Ellis et al.
61
A.M., PROFUMO, ULLIO
62
SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS
SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10
TEV
63
A.M., PROFUMO,ULLIO
64
(No Transcript)
65
(No Transcript)
66
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, SHELCKE
CDM CANDIDATES
67
NEUTRALINO RELIC ABUNDANCE IN GR AND S-T THEORIES
OF GRAVITY
68
(No Transcript)
69
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
INFLATION
70
ON THE SUSY BET
  • Dialogue between a professor and a student at a
    summer school
  • Q professor, what is the most likely NP?
  • A no doubt, SUSY (MSSM)
  • Q professor, what is the probability that SUSY
    is the right NP at the TeV scale?
  • A lets say, 5 or so
  • Q But, professor, you said that SUSY is the most
    likely NP, and now you say that it has 5 chance
    to be it?
  • A yes, but you should consider that all the rest
    has been proposed as NP has 5 per mille
    probability to be right!

71
BACK-UP SLIDES
72
NO GO AND NO NO-GO ON THE ROAD TO GET A SUSY SM
73
(No Transcript)
74
Tightness of the DM constraint on minimal
supergravity
Ellis, Olive, Santoso, Spanos
75
Tightness 3
76
REACH OF FUTURE FACILITIES FOR NEUTRALINO
DETECTION THROUGH ANTIMATTER SEARCHES WITH
FIXED M1 500 GEV
N03 adiabatically contracted profile
Burkert profile
77
(No Transcript)
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