1. ASTROPARTICLES IN THE LHC ERA
NO - VE 2008, Venice, April 15-18, 2008
ASTROPARTICLES IN THE LHC ERA
Antonio Masiero
Univ. of Padova
and
INFN, Padova

2. LHC and “LOW-ENERGY” NEW PHYSICS
LHC discovers NP: difficult, if not impossible, to “reconstruct” the fundamental theory lying behind those signals of NP;
LHC does not see any signal of NP: still a NP related to the stabilization of the elw. scale may be present, but with particles whose masses are in the multi-TeV range.

3. 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
LEPTOGENESIS
NEUTRINO PHYSICS

4. WHY TO GO BEYOND THE SM “OBSERVATIONAL” REASONS THEORETICAL REASONS NO
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 >3σ for NP in
b - s transitions,,,)
HIGH PRECISION LOW-EN.
NO (but (g-2) …)
NEUTRINO PHYSICS
YE m 0, 0
COSMO - PARTICLE PHYSICS
YE (DM, ∆B cosm, INFLAT., DE)
Z bb NO NO NO NO
YES
YES
Strong CP violation?
YES

6. ON THE COMPLEMENTARITY OF DM and LFV SEARCHES to DIRECT LHC SEARCHES FOR NP
Twofold meaning of such complementarity:
synergy in “reconstructing” the “fundamental theory” staying behind the signatures of NP;
ii) coverage of complementary areas of the NP parameter space ( ex.: multi-TeV SUSY physics)

7. 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

8. Present “Observational” Evidence for New Physics
NEUTRINO MASSES
DARK MATTER
MATTER-ANTIMATTER ASYMMETRY
INFLATION

9. SM FAILS TO GIVE RISE TO A SUITABLE COSMIC MATTER-ANTIMATTER ASYMMETRY
SM DOES NOT SATISFY AT LEAST TWO OF THE THREE SACHAROV’S 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 > 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

10. MATTER-ANTIMATTER ASYMMETRY NEUTRINO MASSES CONNECTION: BARYOGENESIS THROUGH LEPTOGENESIS
Key-ingredient of the SEE-SAW mechanism for neutrino masses: large Majorana mass for the 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 )

11. SUSY SEESAW: Flavor universal SUSY breaking and yet large lepton flavor violation Borzumati, A. M (after discussions with W. Marciano and A. Sanda) ~
Non-diagonality of the slepton mass matrix in the basis of diagonal lepton mass matrix depends on the unitary matrix U which diagonalizes (f+ f)
see Isidori’s talk at this meeting

12. µ e+ in SUSYGUT: past and future
Calibbi, Faccia, A. M., Vempati

13. INFLATION COMMON SOLUTION FOR THESE PROBLEMS
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

14. NO ROOM IN THE PARTICLE PHYSICS STANDARD MODEL FOR INFLATION
V=2 2 +  no inflation
But for one solution requiring a non-trivial gymnastics
Need to extend the SM scalar potential
Ex: GUT’s, SUSY GUT’s,…
See Giudice’s talk at this meeting

ENERGY SCALE OF “INFLATIONARY PHYSICS”:
LIKELY TO BE » Mw
DIFFICULT BUT NOT IMPOSSIBLE TO OBTAIN ELECTROWEAK INFLATION IN SM EXTENSIONS

15. 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

16. Mandatory to look for P - DECAY

17. On the Energetic Budget of the Universe
Courtesy of H. Murayama

18. + SuperNova ( HST/GOODS, SNLS)
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

19. 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 !

20. 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

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_ ~
<(annih.) V  > TeV2
From T0 MPlanck
~ 2 / M2 
h2 in the range to be cosmologically interesting (for DM)
m ~ GeV (weak interaction) h2 ~ !!!
THERMAL RELICS (WIMP in thermodyn.equilibrium with the plasma until Tdecoupl)

23. 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/ spin spin0
mLSP
~ GeV *
3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + ΩL h2 OK
mLKP ~
GeV
mLTP ~
GeV
* But abandoning gaugino-masss unif Possible to have mLSP down to 7 GeV
Bottino, Donato, Fornengo, Scopel

24. D. kAZAKOV

25. FROM THE MSSM TO THE CMSSM ( constrained MSSM)
PROLIFERATION OF PARAMETRS IN THE SOFT BREAKING SECTOR OF THE MSSM:
OVERALL NUMBER OF PARAM. IN THE MSSM IS
1 2 4
CMSSM

26. WHICH SUSY F = (105 - 106) GeV F = MW MPl MESSENGERS GRAVITY
HIDDEN
SECTOR SUSY
BREAKING AT
SCALE F
F = ( ) GeV
F = MW MPl
GRAVITY
MESSENGERS
GAUGE INTERACTIONS
Mgravitino ~ F/MPl ~
( ) eV
Mgravitino ~ F/MPl ~
( ) GeV
OBSERVABLE
SECTOR
SM + superpartners
MSSM : minimal content
of superfields

27. 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

28. SWIMPS (Super Weakly Interacting Massive Particles)
DIFFERENT FROM THE THERMAL HISTORY OF WIMPS
SWIMPS (Super Weakly Interacting Massive Particles)
- LSP Gravitino in SUSY
- First excitation of the graviton in UED …
They inherit the appropriate relic density through the decay of a more massive thermal species that has earlier decoupled from the thermal bath

29. ELLIS, OLIVE,SANTOSO,SPANOS

31. THE “WHY NOW” PROBLEM

32. DM DE DO THEY “KNOW” EACH OTHER?
DIRECT INTERACTION  (quintessence) WITH DARK MATTER
DANGER:
Very LIGHT
m ~ H0-1 ~ eV
Threat of violation of the equivalence principle, constancy of the fundamental “constants”, …CARROLL
INFLUENCE OF  ON THE NATURE AND THE ABUNDANCE OF CDM
SCALAR-TENSOR THEORIES OF GRAVITY, KINATION, RS II EXTRA DIM.
Modifications of the standard picture of
WIMPs FREEZE - OUT
CATENA, FORNENGO, A.M., PIETRONI, ROSATI, SCHELKE
CDM CANDIDATES

33. SCHELKE, CATENA, FORNENGO, A.M., PIETRONI

34. NEUTRALINO RELIC ABUNDANCE IN GR AND S-T THEORIES OF GRAVITY

35. CONSTRAINTS ON THE ENHANCEMENT OF THE UNIV
CONSTRAINTS ON THE ENHANCEMENT OF THE UNIV.EXPANSION RATE FROM THE LIMITS ON THE ANTIPROTON ABUNDANCE
SCFMP

36. WIMPS escape the detector MISSING ENERGY SIGNATURE
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

38. Model Independent Annual Modulation Result
DAMA/NaI (7 years) + DAMA/LIBRA (4 years) Total exposure: kgday = 0.82 tonyr
experimental single-hit residuals rate vs time and energy
ROM2F/2008/07
Acos[w(t-t0)] ; continuous lines: t0 = d, T = 1.00 y
2-4 keV
A=(0.0215±0.0026) cpd/kg/keV
2/dof = 51.9/  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/  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/  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 8.2s C.L.

39. 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

40. SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10 TEV
PROFUMO, A.M., ULLIO

42. LFV - DM CONSTRAINTS IN MINIMAL SUPERGRAVITY
A.M., Profumo, Vempati, Yaguna

43. 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, …)
--photons in tens of GeV range ( gamma astronomy on ground Magic, Hess, … or in space Glast…)
--antimatter: look for an excess of antimatter w.r.t. what is expected in cosmic rays ( space exps. Pamela, AMS, …)

46. Roszkowski, Ruiz,
Silk, Trotta

47. CIRELLI, STRUMIA, TAMBURINI 2008

48. A.M., PROFUMO, ULLIO

49. A.M., PROFUMO,ULLIO

51. S. Katsanevas ASPERA

52. C. SPIERING, APPEC - ASPERA ROADMAP
2013
2011
2009
2007
2008
2018
2016
2014
2012
2010
2017
2015
Auger North
30 M€ (from 85)
CTA
> 2/3 from M€
KM3NeT
250 M€
Megaton M€
Grav Wave 3rd generation
300 M€
DM search 1 ton M€ M€ M€
Double Beta 1 ton M€
C. SPIERING, APPEC - ASPERA ROADMAP

53. CTA Auger North KM3NeT Megaton Grav Wave 3rd generation
2013
2011
2009
2007
2008
2018
2016
2014
2012
2010
2017
2015
Auger North
30 M€ (from 85)
CTA
> 2/3 from M€
KM3NeT
250 M€
Megaton M€
Grav Wave 3rd generation
300 M€
DM search 1 ton M€ M€ M€
Double Beta 1 ton M€
add 300 M€ for running
experiments, upgrades,
new methods
~ 950 M€

54. 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
LEPTOGENESIS
NEUTRINO PHYSICS