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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

UNIFICATION ofFUNDAMENTAL INTERACTIONS

THE G-W-S STANDARD MODEL

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!

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

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

THE ENERGY BUDGET OF THE UNIVERSE (as of Dec.

2007)

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

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

LSS PATTERN AND NEUTRINO MASSES

Cosmological Bounds on the sum of the masses of

the 3 neutrinos from increasingly rich samples of

data sets

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 !!!

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

COSMIC MATTER-ANTIMATTER ASYMMETRY

Murayama

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

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 )

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

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

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

Fundamental COUPLING CONSTANTS are NOT CONSTANT

LOW-ENERGY SUSY AND UNIFICATION

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

ON THE RADIATIVE CORRECTIONS TO THE SCALAR MASSES

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

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

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

HOW TO COPE WITH THE HIERARCHY PROBLEM

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

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)

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)

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.

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)

THE SUSY PATH

LOW-ENERGY SUSY

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)

D. KAZAKOV

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IN SUSY WE NEED TO INTRODUCE AT LEAST TWO HIGGS

DOUBLETS IN ORDER TO PROVIDE A MASS FOR BOTH THE

UP- AND DOWN- QUARKS

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

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

THE SOFT BREAKING TERMS OF THE MINIMAL SUSY SM

(MSSM)

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!

D. kAZAKOV

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

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

124 FREE PARAM.

D. KAZAKOV

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

D. KAZAKOV

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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).

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

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

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

HUNTING FOR DARK MATTER

INDIRECT DM SEARCHES

DIRECT DM SEARCHES

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, )

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

Tightness of the DM constraints in Minimal

Supergravity

Ellis, Olive, Santoso, Spanos

LFV - DM CONSTRAINTS IN MINIMAL SUPERGRAVITY

A.M., Profumo, Vempati, Yaguna

DM SUSYHOW FAR ARE WE IN DIRECT SEARCHES?

Ellis et al.

A.M., PROFUMO, ULLIO

SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS

SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10

TEV

A.M., PROFUMO,ULLIO

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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

NEUTRALINO RELIC ABUNDANCE IN GR AND S-T THEORIES

OF GRAVITY

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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

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!

BACK-UP SLIDES

NO GO AND NO NO-GO ON THE ROAD TO GET A SUSY SM

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Tightness of the DM constraint on minimal

supergravity

Ellis, Olive, Santoso, Spanos

Tightness 3

REACH OF FUTURE FACILITIES FOR NEUTRALINO

DETECTION THROUGH ANTIMATTER SEARCHES WITH

FIXED M1 500 GEV

N03 adiabatically contracted profile

Burkert profile

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