Probe of New Physics in ILC : Cosmological Connection Yong-Yeon Keum KEK,Japan Yong-Yeon Keum KEK, Japan CHEP Summer-School 2005

Probe of New Physics

in ILC : Cosmological Connection

Yong-Yeon KeumKEK,Japan

Yong-Yeon KeumKEK, Japan

CHEP Summer-School 2005

Beyond the Standard Model

An overview of Astroparticle physics and Cosmology

Cosmological Connection in ILC

Contents:

SUSY and Beyond SM - Supersymmetry: Lost or found: R.Barnett et al. Nucl Phys B267;625 (1986). - Supersymmetry Phenomenology: M.Dine; hep-ph/9612389 - Supersymmetry Phenomenology:H.Murayama;hep-ph/000222

An overview of Astroparticle physics - Astroparticle Physics: I. Tkachev; hep-ph/0405168 - Lecture on Astroparticle Physics: G. Sigl; hep-ph/0408165

References:

A: Beyond the Standard Model

Problems in the Standard Model - couplings and energy scales in field theory - conservation of baryon and lepton number in SM - the hierachy problem - naturally light particles - cannot explain Matter-antiMatter asymmetery (CP-violation in early Universe) etc …


The SM is a very successful theory of particle interactions

Could it be the Final Theory ?

The SM does not include a quantum description of gravity

Ans: NO !!!

The mistery of Quntum Gravity may be lie at energies 1910 !!GeV

Standard Model

The possibility of having makes LHC-ILC physics very exciting:LHC: Hadron collider (Discovery Machine)

ILC: Machine (Precesion measurement)

F TeV

e e


Supersymmetry

What is the Supersymmetry ?? A new class of Symmetry

Bosons Ferminos


Two Higgs doublets:- Gauge anomalies must cancel.

In SM, TrY3=0. SUSY adds extra chiral fermions with Y =-1:

To cancel the anomaly,

add an extra Higgs doublet with Y = 1:

All SUSY Models are at least two Higgs Doublet models.

Higgsdoublet

0 0

0 0;d d u u

d ud u

h H h H

h hH H


Unification of gauge couplings


SM gauge group: GSM=SU(3)xSU(2)xUY(1) GSM= SU(5), SO(10), E6, …..

Unified gauge group:

( 41/10,19 / 6,7)ib

16 5 10 1

32

1

16i

i i

dgb g

dt

Matter unification: Q,U,D,L,E,N -> 16-plet of SO(10)

Gauge coupling constants RG evole:

where t = ln(Qo/Q) Asymptotic freedom : bi > 0 SM:

MSSM: ( 33/ 5, 1,3)ib

Gauge Unification:

No free parameters Requires as measured

at % level. Coupling at unification:

Scale of unification: unif > 1016 GeV [SuperK]

unif < 1018 GeV [QG]

B: An overview of Cosmology

Big Bang Nucleosynthesis (BBN) Cosmic Microwave Background Radiation (CMBR) Dark Matter and Dark Energy Evidence for dark matter candidates and experim

ental status

Astroparticle Physics?Understanding structure and evolution of Universe using

- subatomic particles ( Big Bang model, dark matter)- techniques from particle physics ( analyses)- outer space ( CMB, neutrinos, dark matter)

Particle physics

Astronomy

Astrophysics and cosmology

PARTICLE

ASTROPHYSICS

History of Universe

T (K)

BBN (nuclei)1010

103

1 mn 3.105 y

Recombination (atom)

Time t

1019GeV 1015GeV 1013GeV 100 GeV0.3 MeV

4000 K 10 K 3 K

10-44 s 10-35 s 10-32 s 10-10 s 300 s 3x105 yr 3x109 yr 15x109 yr

Superstringera (?)

GUTEra

Inflationera

Electroweak

era

ParticleEra

Recombinationera

Galaxy & star

formation

Presentera

T(K) ~ 1010 / t(s)

Time

Optical TelescopesGalileo, 1564 - 1642 Hubble telescope, 2001

Multi-wavelength universe

The different faces of the Milky Way

Lecture outline

1) What is Astroparticle Physics ?Big Bang NucleosynthesisCosmic Microwave Background

2) Dark matter, dark energy Evidence for dark matter candidates and

experimental status

3) Supernovae and dark energy

Age < 1s, T > 1 MeVCollisions maintain thermal equilibrium

Proton - neutron conversion

N (neutron)N (proton) = e m/kT ~ 1

(m = 1.3 MeV)

np =

np 0 as T 0 BUT freeze-out

n-p freeze-out- Weak reaction n p rate:

weak = n|v| GF2 T5 (n T3 and GF

2 T2)

- Expansion rate: H = a/a 1/2 with N T4 (Stefan’s law)

so H N1/2 T2

.

- Freeze-out when weak ~ H with ~weak

H

0.8 MeV

3

drop-out of equilibrium at T ~ 0.8 MeV

np= e m/kT = 0.18

Deuterium bottleneck

nB / n ~ 10-10

Binding Energy (D) = 2.2 MeV

E

Tail of high energy photons preventsformation of Deuterium until T ~ 0.1 MeV

D photo-disintegrated

nB small 2-body reactions only

Formation of D-

-

-

energy distribution

+ n

t=1-3 mn, T=0.3-0.1 MeV- neutron decay: n/p ~ 1/7

- Deuterium (all n):

- Helium (all D ie all n + equal number of p):

Helium abundance ~ ~ 0.252nn+p H abundance ~ 0.75

Heavier elements - BBN

No A=5, A=8 stable nuclei +

2-body reactions only

Trace amounts of 3Li7, 4Be7 :

BBN essentially STOPS at He4

Li5 He4+pHe5 He4+nBe8 He4+He4

He4+H3 Li7+He4+He3 Be7+Be7 + Li7+p

Heavier elements - Stars

Produced in stars(high densities triple alpha reactions allowed)

Spread in ISM by SN explosions

Crab nebula

Observational constraints- Stars are net producers of He4 and metals

use metal poor stars upper limit on primordial abundance of He4 (and on )

- D weakly bound measure in ISMlower limit on primordial abundance of D (upper limit on )

- D burnt to He3 and He3 produced by stars D+He3 increases with time upper limit on D+He3 ie lower limit on

- Li7 very fragile, burnt in stars use old metal poor stars, require Li6 (more fragile)

Abundances

Agreement of abundancesover 10 orders of magnitude

Major success of Big-Bang

Observational concordance

CMB: n= 411 cm-3

= nB/n= (41).10-10

B = =B

c

nBmB

3H2/8G

B h702 ~ 0.04

BBN and neutrinos

H N1/2 T2 (remember?)

so N H sooner freeze-out n/p He4

He m

ass f

racti

on

N = 3

upper limiton He4

# of light neutrinos in LEP

N = 2.994 0.012

Lecture outline


2) Dark matter, dark energy Evidence for dark matter Candidates and experimental status

Supernovae and Dark Energy

Back to thermal historyDensity perturbations (inflation?)

Nucleosynthesis

t = 10-35 s

t ~ 1 mn

t ~ 300000 yrs

Matter: Gravitational collapse

Photons: Free propagation

observable

observable

Galaxies, clusters CMB

Recombination: p+e- H+

End of opaque Universe

Cannotseefurtherback

Multiple scatterings of on e- produces “thermal”spectrum at T = 3000 K

(z ~ 1000 = R0 / Rrec)

“Uniform” background atT0 = 2.7 K

Discovery of CMBR

Discovered in 1965as “excess noise”

(Nobble Prize in 1978)

Bell Labs

Wilson Penzias

25 years later

Bell Labs

COBE 1992

(+ Robert Dicke,Peebles)

FirstAccidental

Prove G.Gamov’s HBB Theory:His estimation is ~5 0K

The First (unrecognized) Direct measurement of CMBR:T.Shmaonov and Pulkovo in 1955; 3.5 0K

CMB = 25 % of TV noise

COBE sky maps

T = 2.7 K

T = 3.4 mK(after subtraction of constant emission)

T = 18 K(after subtraction of dipole)

COBE sky maps

scale 0-4 K: very homogeneous!

Yet, regions > 1° apart neverin causal contact

Inflation ?

LSS ~ rad ~1°103 x 3.105

14.109

zt LSS

t now

COBE sky maps

Doppler effect due to motion of Earth w.r.t. CMB(v = 370 km/s towards Virgo)

Anisotropies : potential wellsEarly seeds for structure formation?(+ foregrounds)

ResolutionCOBE

(7 degree resolution)WMAP

(0.25 degree resolution)

WMAPWMAP on its way to L2 • Lagrange point L2: position

of co-rotation with Earth Stability of conditions

• Dual system to measure T differences

shield

Back to back primary mirrors

Launched in Jun. 2001First results in 2003

• Very low temperature signal Need shielding from Sun, Earth, Moon, (Jupiter)

• 5 frequency channels (foreground removal)

Cosmological perturbation Universe is not completely homogeneous even on large scales - description of matter inhomogeneities ?? (clusters of galaxies, superclusters)

- description of CMB temperature anisotropies ?? => information on cosmological scenario measurement of cosmological parameters

Max. scale of anisotropies

Max scale relates to total content of Universe tot

Limited by causality (remember?) maximum scale

Power spectrum

tot = 1.02 ± 0.02m= 0.28 ± 0.02 = 0.72 ± 0.04 Bh70

2= 0.045 ± 0.002h70

2 < 0.016 (95%)m < 3 23 eV

CMBfast for the numerical codeU.Seljak and M.Zaldarriaga

Consequences…

- Determinations of B (~ 4%) from BBN (age ~ 1 mn) andCMB (age ~ 300 000 yrs)

agree !

- B (~ 4%) < m (~ 28%) Non baryonic matter

- m (~ 28%) < tot (~ 1) Confirmation of

Next chapter !

B: An overview of Cosmology


2) Dark matter, dark energyEvidence for dark matterCandidates and experimental statusSupernovae and dark energy

Dark matter in clusters

Amas de Coma

Zwicky, 1933

Mass of luminous matter=

10% Gravitational mass

Zwicky

Rotation curves (planets)

Rotation of planetsAssociated

rotation curve

Earth : 1 yr (at 150 106 km) v=30 km/sSaturn : 30 yrs (at 1,4 109 km) v=10 km/s

m =

v = G Mc / r

v2

rG m Mc

r2

Rotation curve of spiral galaxies

Doppler distortion across galaxy velocity distribution Flat rotation curve !

90% of gravitational massis invisible (DARK HALOs)

NGC 3198

Gravitational lensing

Luminous mass ~ 1% Gravitational mass

Einsteinring

Summary of evidence

Dark Energy(~70%)

Stars(~2%)

BaryonicDM

(~3%)

Nonbaryonic

DM(~25%)

= / c

= 1 for k = 0

Dark matter candidates

Baryonic(astrophysical candidates)

Non baryonic(particle candidates)

Molecularclouds

Compactobjects

Planets

Browndwarfs

Reddwarfs

Blackholes

…

Whitedwarfs

Neutronstars

low m

ass objects stel

lar re

sidu

es

Neutrinos

WIMPS

Axions

WIMPZILLA

Dark matter candidates

Baryonic(astrophysical candidates)

Non baryonic(particle candidates)

Molecularclouds

Compactobjects

Neutrinos

WIMPSMicrolensing

Accelerators

Direct search

(10-7 Msun ~10 Msun)

Mass?

tel

esco

pes

AxionsMass?

Principles of microlensing

Angular separation of images ~ 10-3 rad Only 1 (combined) image, amplified

Motion of deflector (220 km/s) Duration tE ~ 90 M/Msun days

Targets (EROS, MACHO)

Event rate : ~ 1 per year per 20 million stars monitored

LCM

SCM

Magellanic clouds : 200 000 ly away (edge of halo?)(Milky Way ~ 70 000 ly in diameter)

Magellanic Clouds Halo

Milky WayEarth

(not to scale)

~30 million stars monitored:- >10 000 variable stars- >100 SN- Microlensing events ?

Final results

Life of a small star (<8 Msun)

White dwarfs

White dwarf = final state of low mass star38 white dwarfs found in old plates

- moving fast belongs to halo (vs. disk)- old (i.e. cold) 1st population of stars in our Galaxy

White dwarfs (~1 Msun) may compose 3 to 35% of the halo

Conclusions on baryonic DM

Favored candidates (compact astrophysical objects)rejected on all mass range

(only small window remaining at ~ 10-100 Msun)

GasCold molecular clouds

…

Non baryonic DM

> 80% of DM is non baryonic

Hot DM ? Cold DM ?

Axions(invoked to solve strong CP violation pb in SM)

Significant only if 10-5 <ma < 10-3 eV(Leave only a narrow window)

WIMPSMv ~ 0.1 eV

M ~ 100 GeV

WIMPZILLA

M ~ 1013 GeV

Initially motivated as a sol. of the GZK-puzzle

in UhE cosmic ray.

Structure formation

HDM wipes outstructure on small scales

Simulations ofDM density maps

CDM createstoo many

sub-structures?

Hubble Deep Field

Neutrinos as HDM

- exist as relic from Big Bang (~ 115 cm-3);- (now) known to have mass: neutrino oscillations

1 2 3

Solar

Atm.

1

10-1

10-2

10-3

10-4

10-5

masses (eV) from oscillations

(most likely solution)

contribution to matter density: v ~ m / 46 eVm ~ 0.05 eV v ~ 0.003

3

11vn n

Weakly Interacting Massive ParticlesIf SUSY exists - production of sparticles in early universe - all decay except LSP (conservation of R-parity) relic from Big Bang - m ~ 30 GeV (accelerator) - annihilate throughX X - relic density ~ 0.3 for typical weak annihilation rates

actual abundance

equilibrium abundance

Increasing

<Av>Freezeout

Neq e-m/T

X = m/T (time)Next chapter !

Direct detection of WIMPS

If halo DM made of WIMPS~ 500 WIMPS/m3 with v ~ 220 km/s > 10 000 WIMPs/cm2/s on Earth (from -vsun)

Requirement : High mass detectorsLow radioactive background (discrimination)

Experimental signature : nuclear recoil (vs. electronic “recoil”)

e- e-

n WIMP

Main sourceof background(radioactivity)

n WIMP

Edelweiss: detector

Dilution cryostat low background

(temperature ~15mK)

Archeological lead shielding

In Modane undergroundlaboratory

Negligible neutron background(~ 0,01 evt/kg/day)

Detectors3 x 320g

bolometers

Conclusions on direct detection

Regions ofWIMPs models

Regions above the curves

excluded byexperiments

Indirect detection of WIMPs

Energy loss by elastic scatteringwith massive bodies

(halos, Earth, Sun, galactic center)

Gravitational capture + annihilation

Earth, Sun, GC telescopes XSuperK, Baksan, IMB, MACRO

AMANDA, ANTARES, Baïkal…

Halo High energy astronomy AMS, GLAST, VERITAS, BESS,

CELESTE, CAPRICE, MILAGRO…

Lecture outline


2) Dark matter, dark energyEvidence for dark matterCandidates and experimental status

Baryonic (EROS, MACHO)Exotic (Edelweiss, DAMA, Antares)

Supernovae and dark energy

White dwarfs in binary systems

SN Ia

Very luminous (L ~ 1010 Lsun), out to high zStandard candles (1.4 Msun)~ 1 to 2 / century / galaxy

Geometry of the Universe

1 = k(t) + ∑x(t) + (t)

Curvature

Energy density of components(matter, radiation)

Wg ~ 2.47 x 10-5

Density of dark energy

Expansion vs geometry: qO = m / 2 -

ClosedUniverse

FlatUniverse

OpenUniverse

Measurement of the geometry

AT A GIVEN DISTANCEKnown physical size angle depends on geometry Known luminosity flux depends on geometry

CMB

SN Ia

Hubble diagram:

Redshift z

m = - 2.5 log F + cst = 5 log (H0 DL) + M - 5 log H0 + 25

H0DL czz 0 mesure de H0 z grand : mesure de m,

Mag

nit

ud

e m

older

fain

ter

1+z = a(tobs)/a(tem)

At a given z

Calan TololoHamuy et al.,A.J.1996

SupernovaCosmologyProject

Accelerated expansion= smaller rate in the past

= more time to reach a given z= larger distance of propagation of the photons= smaller flux

SN 1a residual Hubble Diagram

Initial constraints (1998)

42 supernovae

q0 = M/2 - < 0 :Accelerating Universe

If flat (tot = 1) :M = 0.28 = 0.72

Concordance

CMB

LSS

2000 2002

Expected precision with JDEM (>2010)

Outstanding Questions:

Dark Matter: What is it ?

How is it distributed ? Dark Energy: What is it ? Does it evolve or not ? Why not

Baryons: Why not

Ultra-HE Cosmic Rays: What are they ?

Where do they come from ?

1200 or 10 ?

0?B

What kind of tools do we need to address these ?

Dark Energy vs Accelerating Universe Dark Matter - WIMP - SuperWIMP Neutralino Dark Matter in mSURGA Important stratege in ILC and LHC

C: Cosmological Connection in ILC

Dark Energy vs Accelerating Univ.

Negative pressure:

Smoothly distributed, (almost ) not clustering Candidates A: Cosmological constant (or vacuum energy)

B: Dynamical field: Qunitessence,K-essence,Phantom etc…

)3(3

4/ p

Gaa

0a 3/1/ 03 pwp

g

GT

8

1/ pw eV10~m

)102(8

3-

43

eVG

p

)(2

1QVQQL

VQpVQ QQ 22

2

1,

2

1

11 Qw

however: , cosmological constant problem!12010~/ obth

DMDM h h22=0.112 ± 0.009=0.112 ± 0.009 Non-Non-baryonicbaryonic StableStable NeutralNeutral ColdCold

WIMPWIMP

appear in particle physics models motivated independentlyappear in particle physics models motivated independently by attempts to solve EWSB by attempts to solve EWSB

relic density are determined by Mrelic density are determined by Mplpl and M and Mweakweak

naturally around the observed valuenaturally around the observed value no need to introduce and adjust new energy scaleno need to introduce and adjust new energy scale

superWIMPsuperWIMP

Dark Matter (DM)

Among the many model of dark metter,there is a generic classin which the dark matter particle is a thermal relic (WIMP).

A WIMP is a heavy, neutral stable particle that was in thermalequilibrium in the early universe.

Due to the expansion of the universe, such particles eventually cannot find partners to annihilate.

Thus , a WIMP has a calculable density today.

andand

Neutral WIMPNeutral WIMP

mmWIMPWIMP»» M Mweakweak

anan »» weakweak22 M Mweakweak

-2-2

WIMPWIMP »» hh ananv v ii-1-1

naturally around naturally around the observed valuethe observed value

e.g. neutralino LSPe.g. neutralino LSP

WIMPWIMP

WIMP Initially, in thermal equilibrium

f f

Cooling Universe:

/m TEQN N e

s freeze out: N ~ Const.

SUSY : - Superpartners - R-parity (R-sneutrino) - Neutralino; Gravitino super-WIMP Extra Dimensions: - KK partners (KK-photon,KK-neutrino) - KK graviton super-WIMP Branes: - Brane fluctuations - Branons Little Higgs: use T-parity, etc…

WIMP Dark Matter Candidates:

SWIMPSWIMPSMSM

101066

101044 s s t t 10 1088 s s

superWIMPsuperWIMP

e.g. Gravitino LSPe.g. Gravitino LSP LKK gravitonLKK graviton

WIMPWIMP neutralneutral chargedcharged

WIMP WIMP superWIMP + SM particles superWIMP + SM particles

WIMPWIMP

SuperWIMP Feng et al. hepph/0302215,0306024

Ex: Neutralino

LCC1: Bulk regionAnnihilation through slepton exchange

NN depends on the light sleptonmasses and couplings

LCC2: Focus point regionAnnihilation to WW,ZZ

NN depends on

M1,M2,tan

LCC3: Coannihilation regionAnnihilation of stau is actually dominant

depends on

LCC4: A funnel regionAnnihilation through A resonance

NN depends on

Focus Point Results

Experimentally we can find WIMPs in the jet + missing energy signal. Typical cross section: ~ 100 pb for M < 1 TeV. LHC can discover the new physics signal at the very early s

tage. However LHC cannot prove SUSY, because the jet+ missin

g energy signal is generic in WIMP models. The connection to dark matter would make it very important

to find out which options is correct. We ultimately need a precision measurement in ILC.

Important stratege in ILC vs LHC

Important stratege in ILC vs LHC

Once we identified the dark matter particle, we have to see whether we can quantitatively account for the relic density.

The relic density depends on the annihilation cross section, which is very model-dependent.

Fortunately, the cross section depends mainly on the masses and couplings of the lightest

states of the new sector.

The determination of these quantities is the forte of the ILC.

Now Cosmology and Astroparticles provide many unsolved problems which are among the most outstanding in basic science today.

We need new particle physics beyond SM, cannot be solved by cosmology tools alone.

In many cases, ILC can provides an essential tool for discovering the answers.

Conclusion: Why ILC is so important ?

On the way of the discovering of WIMPs,

1) Observe dark matter as missing energy at a collider. 2) Determine qualitatively which model is correct. 3) Determine whether that model explains quantitatively the relic dens

ity. 4) Determine the cross sections relavant to astrophysical dark matter

observations.

LHC is crucial only for #1, After that, the tasks are beyond the reach of LHC and call for ILC .

Conclusion: Why ILC is so important ?

Thanks !Thanks !

Documents

Probe of New Physics in ILC : Cosmological Connection Yong-Yeon Keum KEK,Japan Yong-Yeon Keum KEK, Japan CHEP Summer-School 2005