new physics beyond the sm astroparticle lhc synergy n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
NEW PHYSICS BEYOND THE SM: ASTROPARTICLE – LHC SYNERGY PowerPoint Presentation
Download Presentation
NEW PHYSICS BEYOND THE SM: ASTROPARTICLE – LHC SYNERGY

Loading in 2 Seconds...

play fullscreen
1 / 56

NEW PHYSICS BEYOND THE SM: ASTROPARTICLE – LHC SYNERGY - PowerPoint PPT Presentation


  • 136 Views
  • Uploaded on

Workshop on PAMELA PHYSICS, Rome, 11 –12 May, 2009. NEW PHYSICS BEYOND THE SM: ASTROPARTICLE – LHC SYNERGY. Antonio Masiero Univ. of Padova INFN, Padova. WHY TO GO BEYOND THE SM. “OBSERVATIONAL” REASONS. THEORETICAL REASONS. INTRINSIC INCONSISTENCY OF SM AS QFT

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

NEW PHYSICS BEYOND THE SM: ASTROPARTICLE – LHC SYNERGY


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
new physics beyond the sm astroparticle lhc synergy

Workshop on PAMELA PHYSICS,

Rome, 11 –12 May, 2009

NEW PHYSICS BEYOND THE SM:ASTROPARTICLE – LHC SYNERGY

Antonio Masiero

Univ. of Padova

INFN, Padova

why to go beyond the sm
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
  • YE (DM, ∆B cosm, INFLAT., DE)

Z bb

NO

NO

NO

NO

YES

YES

Strong CP violation?

YES

slide4

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

inflation
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 SM

no room in the particle physics standard model for inflation
NO ROOM IN THE PARTICLE PHYSICS STANDARD MODEL FOR INFLATION

V=2 2 + 4 no inflation

Need to extend the SM scalar potential

Ex: GUT’s, SUSY GUT’s,…

ENERGY SCALE OF “INFLATIONARY PHYSICS”:

LIKELY TO BE » Mw

DIFFICULT BUT NOT IMPOSSIBLE TO OBTAINELECTROWEAK INFLATION IN SM EXTENSIONS

the cosmic matter antimatter asymmetry puzzle why only baryons why n baryons n photon 10 10
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 << 10-10
  • IF BARYONS-ANTIBARYONS ARE SEPARATED EARLIER DOMAINS OF BARYONS AND ANTIBARYONS ARE TOO 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

sm fails to give rise to a suitable cosmic matter antimatter asymmetry
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

matter antimatter asymmetry neutrino masses connection baryogenesis through leptogenesis
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 )

susy see saw
UV COMPLETION OF THE SM TO STABILIZE THE ELW. SCALE:

LOW-ENERGY

SUSY

COMPLETION OF THE SM FERMIONIC SPECTRUM TO ALLOW FOR NEUTRINO MASSES: NATURALLY SMALL PHYSICAL NEUTRINO MASSES WITH RIGHT-HANDED NEUTRINO WITH A LARGE MAJORANA MASS

SEE-SAW

SUSY SEE-SAW
slide12

SUSY SEESAW: Flavor universal SUSY breaking and yet large lepton flavor violation Borzumati, A. M. 1986 (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)

e in susygut past and future
µ e+ in SUSYGUT: past and future

CATENA, FACCIA, A.M., VEMPATI

baryogenesis at the electroweak scale
BARYOGENESIS AT THE ELECTROWEAK SCALE ?

In the MSSM:

-light stop:

-light Higgs

-large SUSY masses

CARENA, NARDINI, QUIROS, WAGNER

dm new physics beyond the particle physics sm if newton is right at scales size of the solar system
DM  NEW PHYSICS BEYOND THE ( PARTICLE PHYSICS ) SM - if Newton is right at scales>size of the Solar System
  • ΩDM= 0.233 ± 0.013 *
  • Ωbaryons = 0.0462 ± 0.0015 **

*from CMB ( 5 yrs. of WMAP) + Type I Supernovae + Baryon Acoustic Oscillations (BAO)

**CMB + TypeI SN + BAO in agreement with Nucleosynthesis (BBN)

slide18

The BULLET CLUSTER: two colliding clusters of galaxies

Stars, galaxies and putative DM behave differently during collision, allowing for them to be studied separately. In MOND the lensing is expected to follow the baryonic matter, i.e. the X-ray gas. However the lensing is strongest in two separated regions near the visible galaxies most of the mass in the cluster pair is in the form of collisionless DM

dm the most impressive evidence at the quantitative and qualitative levels of new physics beyond sm
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 BEVIDENCE 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 energy scale from the observational new physics
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

difficult conditions for the axion to constitute 100 of dm
(Difficult) Conditions for the axion to constitute 100% of DM

Hertzberg, Steigmark, Wilczek

Visinelli, Gondolo

the wimp miracle
THE “WIMP MIRACLE”

Bergstrom

Many possibilities, but WIMPs are singled out by an exceptional “coincidence”: parameters of the STANDARD MODELS of PARTICLE PHYSICS and COSMOLOGY conspire to provide a viable cold DM candidate at the ELECTROWEAK SCALE

wimps weakly interacting massive particles
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_

COSMO – PARTICLE

CONSPIRACY

~

<(annih.) V  > 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)

stable elw scale wimps from particle physics
STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS

SUSYEXTRA 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 + ΩL h2 OK

mLTP

~400 - 800

GeV

* But abandoning gaugino-masss unif. Possible to have mLSP down to 7 GeV

Bottino, Donato, Fornengo, Scopel

which susy
WHICH SUSY

HIDDEN

SECTOR SUSY

BREAKING AT

SCALE F

F = (105 - 106) GeV

F = MW MPl

GRAVITY

GAUGE INTERACTIONS

MESSENGERS

Mgravitino~ F/MPl ~

(102 -103) eV

Mgravitino ~ F/MPl ~

(102 -103) GeV

OBSERVABLE

SECTOR

SM + superpartners

MSSM : minimal content

of superfields

slide26
After LEP: tuning of the SUSY param. at the % level to correctly reproduce the DM abundance: NEED FOR A “WELL-TEMPERED” NEUTRALINO
neutralino lsp in the constrained msssm a very special selection in the parameter space
NEUTRALINO LSP IN THE CONSTRAINED MSSSM: A VERY SPECIAL SELECTION IN THE PARAMETER SPACE?

Favored by gµ -2

Favored by DM

Excluded: stau LSP

Excluded by bsγ

Ellis, Olive, Santoso, Spanos

lsp neutralino the freedom in un constrained mssm
LSP NEUTRALINO: THE FREEDOM IN “UN-CONSTRAINED” MSSM

NON-UNIVERSAL HIGGS MODEL

GUTless Model

ELLIS, OLIVE, SANDICK

ELLIS, FALK, OLIVE, SANTOSO

slide29

CMSSM: Regions of the param.

space favored in a likelihood analysis

gravitino lsp
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

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

dm and non standard cosmologies before nucleosynthesis
DM and NON-STANDARD COSMOLOGIES BEFORE NUCLEOSYNTHESIS
  • NEUTRALINO RELIC DENSITY MAY DIFFER FROM ITS STANDARD VALUE, i.e. the value it gets when the expansion rate of the Universe is what is expected in Standard Cosmology (EX.: SCALAR-TENSOR THEORIES OF GRAVITY, KINATION, EXTRA-DIM. RANDALL-SUNDRUM TYPE II MODEL, ETC.)
  • WIMPS MAY BE “COLDER”, i.e. they may have smaller typical velocities and, hence, they may lead to smaller masses for the first structures which form

GELMINI, GONDOLO

dm de
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

EX.: SCALAR-TENSOR GRAVITY

CATENA, FORNENGO, A.M., PIETRONI, SHELCKE

CDM CANDIDATES

slide37

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

SCFMP

larger wimp annihilation cross section in non standard cosmologies
LARGER WIMP ANNIHILATION CROSS-SECTION IN NON-STANDARD COSMOLOGIES
  • Having a Universe expansion rate at the WIMP freeze-out larger than in Standard Cosmology possible to provide a DM adequate WIMP population even in the presence of a larger annihilation cross-section ( Catena, Fornengo, A.M., Pietroni)
  • Possible application to increase the present DM annihilation rate to account for the PAMELA results in the DM interpretation (instead of other mechanisms like the Sommerfeld effect or a nearby resonance)

El Zant, Khalil, Okada

slide40

SPIN - INDEPENDENT NEUTRALINO - PROTON CROSS SECTION FOR ONE OF THE SUSY PARAM. FIXED AT 10 TEV

PROFUMO, A.M., ULLIO

slide41

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

prospects for discovering the cmssm at the lhc in light of wmap
PROSPECTS FOR DISCOVERING THE CMSSM AT THE LHC IN LIGHT OF WMAP

RED: FULL SAMPLE OF CMMS MODELS

BLUE: POINTS COMPATIBLE WITH WMAP

GREEN: POINTS ACCESSIBLE TO LHC

YELLOW: POINTS ACCESSIBLE TO PRESENT DIRECT DM SEARCHES

Ellis et al.

slide44

PREDICTION OF Ω DM FROM LHC AND ILC FOR TWO DIFFERENT SUSY PARAMETER SETS

BALTZ, BATTAGLIA, PESKIN, WIZANSKY

lfv dm constraints in minimal supergravity
LFV - DM CONSTRAINTS IN MINIMAL SUPERGRAVITY

A.M., Profumo, Vempati, Yaguna

slide46

NEUTRALINO LSP IN SUPERGRAVITY

A.M., PROFUMO, ULLIO

searching for wimps
SEARCHING FORWIMPs

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

smoking gun s for dm
SMOKING GUN(S) FOR DM?

N. Weiner, La Thuile March ‘09

DAMA/LIBRA

tev dm
TeV DM?
  • PAMELA anti-proton and positron fractions
  • FERMI and HESS electron+positron flux
  • FERMI (preliminary) diffuse γ rays
  • HESS and VERITAS observations of γ raysfrom the Galactic Center ( with new –preliminary - HESS data), the Galactic Ridge and dwarf galaxies
  • SuperKamiokande up-going neutrino-induced muon flux

PAMELA, FERMI and HESS observations point to non-conventional DM models with

-- Leptophilic final states

-- Large “Event rates” in our galaxy

-- High mass scale of O(TeV)

slide52
Absence of any sharp feature at low scale in the new FERMI data  DM LIGHTER THAN ABOUT A TeV IS NOW EXCLUDED AS AN INTERPRETATION OF THE PAMELA EXCESS  PAMELA should find a greater positron fraction at higher energies
  • TeV DM: if the electron-positron excess is everywhere in the DM halo, the Inverse Compton Scattering on ambient light produces a gamma-excess above 10 GeV that can be tested by FERMI gamma observations

Maede, Papucci, Strumia and Volansky 0905.0480

some final thoughts
Some final thoughts
  • Very solid evidence of ( a large amount of) NON-BARYONIC COLD DM
  • In the SM NO CANDIDATE FORCOLD DM ( ordinary neutrinos are hot DM; indeed, the best limit on neutrino masses comes from cosmology!)
  • WIMPS: (very) appealing COSMO (HBB SM) – PARTICLE (GWS SM) “conspiracy” in providing the (quantitatively and qualitatively) right DM
  • WIMPS can be part of the NEW PHYSICS at the ELW scale ( link ultraviolet completion of the SM – DM constituents)
  • Possibility of a joint cosmo – and particle – exploration of the TeV New Physics
  • If WIMP is the DM: complementary hunting for TeV New Physics at LHC and in DIRECT and INDIRECT searches of DM
on the lhc dm fcnc cooperation to corner tev new physics
ON THE LHC – DM –FCNC COOPERATION TO CORNER TeV NEW PHYSICS
  • The traditional competition between direct and indirect (DM,FCNC, CPV) searches to establish who is going to see the new physics first is no longer the priority, rather
  • COMPLEMENTARITY between direct and indirect searches for New Physics is the key-word
  • 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)

SLOW “DECOUPLING” of NEW PHYSICS EFFECTS in DM and FCNC SEARCHES w.r.t. the DIRECT ACCELERATOR SEARCHES.