E6 T signatures and dark matter connectionE6 T signatures and dark matter connection Howard Baer Florida State/ Oklahoma ⋆ Evidence for CDM ⋆ Candidates for CDM ⋆ Neutralino

6ET signatures and dark matter connection

Howard Baer

Florida State/ Oklahoma

⋆ Evidence for CDM

⋆ Candidates for CDM

⋆ Neutralino CDM

• Relic density

• Direct and indirect detection of DM

⋆ NUSUGRA models

⋆ The gravitino problem

⋆ Gravitino CDM

⋆ Axino CDM

H. Baer, TASI 2008: 6ET at LHC and dark matter connection, June 20, 2008 1

Pillars of Big Bang cosmology: Hubble expansion

⋆ Theory: FRW universe

⋆ Hubble expansion

• HST key project

• type Ia supernovae probe

⋆ H0dL = z + 1

2(1 − q0)z

2 + · · ·

⋆ H0 = 72 km/sec/Mpc±10%

⋆ evidence for Λ > 0!

⋆ age of universe: ∼ 13.7 Gyrs


Big Bang nucleosynthesis (BBN)

⋆ Thermal history

of universe:

⋆ Can compute light element

abundances: 4He, D, 3He, 7Li

• match to data:

• ηB ≡ nB

nγ≃ 6 × 10−10

• ηB from BBN

consistent with CMB results @@@ÀÀÀ@@@@@@@@ÀÀÀÀÀÀÀÀ3He/H p

4He

2 3 4 5 6 7 8 9 101

0.01 0.02 0.030.005

CM

B

BB

N

Baryon-to-photon ratio η × 10−10

Baryon density ΩBh2

D___H

0.24

0.23

0.25

0.26

0.27

10−4

10−3

10−5

10−9

10−10

2

57Li/H p

Yp

D/H p @@ÀÀH. Baer, TASI 2008: 6ET at LHC and dark matter connection, June 20, 2008 3

Cosmic microwave background (CMB)

⋆ COBE/WMAP/WMAP3, · · ·

⋆ anisotropies ∼ 10−5

⋆ can extract numerous

cosm. param’s from power spectrum

• flat (k = 0) universe: ρ = ρc

as in inflation models

• contents of universe

∗ ΩΛ ∼ 0.7

∗ Ωbaryons ∼ 0.04

∗ ΩCDM ∼ 0.25

∗ Ων ∼ tiny


Baryogenesis: explaining ηB

⋆ SM electroweak baryogenesis: only if mHSM

<∼ 50 GeV

⋆ MSSM: many more possibilities

• EW baryogenesis: need mt1< mt; mh

<∼ 120 GeV (Carena et al.)

• Affleck-Dine: decay of flat directions: baryo- or leptogenesis

• thermal leptogenesis: (Fukugita, Yanagida; Buchmueller, Plumacher, ...)

∗ natural link to physics of massive neutrinos

∗ due to decay of heavy N states: N → Hℓ 6= N → H†ℓ

∗ lepton asymmetry converted to baryon asymmetry via sphaleron effects

∗ get ηB ∼ 6 × 10−10 if MN ∼ 1010 GeV

∗ need reheat temp TR ∼ 1010 GeV

∗ overproduction of gravitinos if .1<∼ mG

<∼ 10 TeV

• leptogenesis via inflaton decay

⋆ can be constrained by ν/sparticle measurements


Dark Matter in the universe

⋆ Binding of clusters

⋆ Galactic rotation curves

⋆ Gravitational lensing

⋆ Hot gas in clusters

⋆ CMB fluctuations

⋆ Large scale structure

⋆ flatness/BBN


Best fit cosmology: concordance (ΛCDM) model

• ΩBh2 = 0.022 ± 0.001

• Ωνh2 < 0.007 95% CL

• ΩΛh2 ∼ 0.38 ± 0.03

• ΩCDMh2 = 0.105 ± 0.01


Candidates for Dark Matter

⋆ unseen baryons, e.g. BHs, brown dwarves, stellar remnants

– inconsistent with BBN element abundance calc’n

– limits from MACHO, EROS, OGLE

⋆ light neutrinos (= HDM)

⋆ axions/axinos

⋆ WIMPS

⋆ superWIMPS

⋆ Q-balls

⋆ primordial BHs10

-3310

-3010

-2710

-2410

-2110

-1810

-1510

-1210

-910

-610

-310

010

310

610

910

1210

1510

18

mass (GeV)

10-39

10-36

10-33

10-30

10-27

10-24

10-21

10-18

10-15

10-12

10-9

10-6

10-3

100

103

106

109

1012

1015

1018

1021

1024

σ int (

pb)

Some Dark Matter Candidate Particles

neutrinos neutralino KK photon branonLTP

axion axino

gravitino KK graviton

SuperWIMPs :

wim

pzill

aWIMPs :

Bla

ck H

ole

Rem

nant

Q-ball

fuzzy CDM


Axions

⋆ PQ solution to strong CP problem in QCD

⋆ pseudo-Goldstone boson from

PQ breaking at scale fa

⋆ non-thermally produced

via vacuum mis-alignment

• ma ∼ Λ2QCD/fa ∼ 10−6 − 10−1eV

• Ωah2 ∼ 1

2

[6×10

−6eVma

]7/6

h2

• astro bound: stellar cooling ⇒ ma < 10−1eV

• a couples to EM field: a− γ − γ coupling (Sikivie)

• axion microwave cavity searches

10-6

10-5

10-4

10-3

10-2

10-1

ma ( eV )

10-6

10-5

10-4

10-3

10-2

10-1

100

101

Ωah2

measured : Ωh2 = 0.105 + _ 0.01

axion relic density : vacuum mis-alignment


Axion microwave cavity searches

⋆ ongoing searches: ADMX experiment

• Livermore⇒ U Wash.

• Phase I: probe KSVZ

for ma ∼ 10−6 − 10−5 eV

• Phase II: probe DFSZ

for ma ∼ 10−6 − 10−5 eV

• beyond Phase II:

probe higher values ma


WIMPs: the WIMP miracle!

• Weakly Interacting Massive Particles

• assume in thermal equil’n in early universe

• Boltzman eq’n:

– dn/dt = −3Hn− 〈σvrel〉(n2 − n20)

• Ωh2 = s0

ρc/h2

(45

πg∗

)1/2xf

MP l

1

〈σv〉

• ∼ 0.1 pb〈σv〉 ∼ 0.1

( mwimp

100 GeV

)2

• thermal relic ⇒ new physics at Mweak!


Some WIMP candidates

⋆ 4th gen. Dirac ν (excluded)

⋆ SUSY neutralino (χ or Z1)

⋆ UED excited photon B1µ

⋆ little Higgs photon BH

⋆ little Higgs (theory space) N1 (scalar)

⋆ warped GUTS: LZP KK fermion

⋆ branons

⋆ · · ·


Neutralino dark matter

⋆ Why R-parity? natural in SO(10) SUSYGUTS if properly broken, or broken

via compactification (Mohapatra, Martin, Kawamura, · · ·)

⋆ In thermal equilibrium in early universe

⋆ As universe expands and cools, freeze out

⋆ Number density obtained from Boltzmann eq’n

• dn/dt = −3Hn− 〈σvrel〉(n2 − n20)

• depends critically on thermally averaged annihilation cross section times

velocity

⋆ many thousands of annihilation/co-annihilation diagrams

⋆ several computer codes available

• DarkSUSY, Micromegas, IsaReD (part of Isajet)


Some neutralino (co)annihilation processes


Relic density in minimal SUGRA model

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

Ωh2< 0.0940.094< Ωh2< 0.1290.129< Ωh2< 0.5

NO REWSBLEP2

stau

LS

P

m0 (GeV)

m1/

2 (G

eV)

mSUGRA,tanβ=10,A0=0,µ>0,mtop=175GeV

δaposx1010:30,10,5,1 BF(b→sγ)x104:2,3

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

Ωh2< 0.0940.094< Ωh2< 0.1290.129< Ωh2< 0.5

NO REWSBLEP2

stau

LS

Pm0 (GeV)

m1/

2 (G

eV)

mSUGRA,tanβ=55,A0=0,µ>0,mtop=175GeV

δaposx1010:30,10,5,1 BF(b→sγ)x104:2,3

HB, A. Belyaev, T. Krupovnickas and A. Mustafayev


Main mSUGRA regions consistent with WMAP

⋆ bulk region (low m0, low m1/2)

⋆ stau co-annihilation region (mτ1≃ meZ1

)

⋆ HB/FP region (large m0 where |µ| → small )

⋆ A-funnel (2meZ1

≃ mA, mH)

⋆ h corridor (2meZ1≃ mh)

⋆ stop co-annihilation region (particular A0 values mt1≃ meZ1

)


Constraints on SUSY models

⋆ LEP2:

– mh > 114.4 GeV for SM-like h

– mfW1

> 103.5 GeV

– meL,R> 99 GeV for mℓ −meZ1

> 10 GeV

⋆ BF (b→ sγ) = (3.55 ± 0.26) × 10−4 (BELLE, CLEO, ALEPH)

– SM theory: BF (b→ sγ) ≃ (3.0 − 3.7) × 10−4

⋆ aµ = (g − 2)µ/2 (Muon g − 2 collaboration)

– ∆aµ = (22 ± 10) × 10−10 (PDG value e+e−)

– ∆aSUSYµ ∝ m2

µµMi tan β

M4

SUSY

⋆ BF (Bs → µ+µ−) < 1.5 × 10−7 (CDF)

– constrains at very large tanβ>∼ 50

⋆ ΩCDMh2 = 0.11 ± 0.01 (WMAP)


Constraints as χ2 on mSUGRA model

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 50

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

mSUGRA, tgβ=10, µ>0, A0=0, mtop=175 GeVe+e- input for δaµ LEP2 excluded

NO REWSB

stau

LS

P

sqrt

(χ2 )

m0 (TeV)

m1/

2 (G

eV)

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 50

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

mSUGRA, tgβ=55, µ>0, A0=0, mtop=175 GeVe+e- input for δaµ LEP2 excluded

NO REWSB

stau

LS

P

sqrt

(χ2 )

m0 (TeV)

m1/

2 (G

eV)


Direct detection of SUSY DM

⋆ Calculate neutralino-nucleus scattering

• calculate Z1 − q or Z1 − g scattering: take v → 0 limit

∗ spin-dependent cross section couples to spin of nucleus: cancel

∗ spin-independent cross section ∝ A2: add

∗ results usually quoted in terms of σSI(Z1p) so results from different

target nuclei can be compared


Current best limit: Xenon-10/CDMS results!

WIMP Mass [GeV/c2]

Cro

ss-s

ectio

n [p

b] (

norm

alis

ed to

nuc

leon

)

080418114601

http://dmtools.brown.edu/ Gaitskell,Mandic,Filippini

101

102

103

10-10

10-9

10-8

10-7

10-6

10-5

080418114601Baer et. al 2003XENON1T (proj)LUX 300 kg LXe Projection (Jul 2007)XENON100 (150 kg) projected sensitivitySuperCDMS (Projected) 25kg (7-ST@Snolab)WARP 140kg (proj)SuperCDMS (Projected) 2-ST@SoudanCDMS Soudan 2007 projectedXENON10 2007 (Net 136 kg-d)CDMS: 2004+2005 (reanalysis) +2008 GeCDMS 2008 GeWARP 2.3L, 96.5 kg-days 55 keV thresholdDAMA 2000 58k kg-days NaI Ann. Mod. 3sigma w/DAMA 1996Edelweiss I final limit, 62 kg-days Ge 2000+2002+2003 limitDATA listed top to bottom on plot


Indirect detection (ID) of SUSY DM: ν-telescopes

⋆ Z1Z1 → bb, etc. in core of sun (or earth): ⇒ νµ → µ in ν telescopes

⋆ flux is largest when σ(Z1p) is largest

– e.g. low mq or HB/FP region for mSUGRA

• experiments: Amanda, Icecube, Antares


ID of SUSY DM: γ and anti-matter searches

• Z1Z1 → qq, etc.→ γ in galactic core or halo

• Z1Z1 → qq, etc.→ e+ in galactic halo

• Z1Z1 → qq, etc.→ p in galactic halo

• Z1Z1 → qq, etc.→ D in galactic halo


Rates for γs, e+s, ps vs. m0 for fixed m1/2 = 550 GeV, tan β = 50

0 1000 2000 3000 4000m0(GeV)

10−5

10−4

10−3

10−2

10−1

100

S/B

(e+

)

0 5 10 15r(kpc)

0

5

10

ρ (G

eV c

m−

3 )

defaultNFWMoore et alKravtsov et al

0 1000 2000 3000 4000m0(GeV)

10−9

10−8

10−7

10−6

10−5

10−4

dΦ

p− / dE

dΩ (G

eV−

1 cm

−2 s

−1 s

r−1 )

0 1000 2000 3000 4000m0(GeV)

10−12

10−10

10−8

10−6

10−4

Φγ (

cm−

2 s−

1 )

a) b)

c) d)

• rates enhanced in A-funnel and HB/FP region (MHDM)


Direct and indirect detection of neutralino DM

200

400

600

800

1000

1200

1400

1600

0 1000 2000 3000 4000 5000 6000 7000 8000

mSUGRA, A0=0 tanβ=10, µ>0

m0(GeV)

m1/

2(G

eV)

LEP

no REWSB

Z~

1 no

t LS

P

Φ(p-)=3x10-7 GeV-1 cm-2 s-1 sr-1

(S/B)e+=0.01

Φ(γ)=10-10 cm-2 s-1

Φsun(µ)=40 km-2 yr-1

0<Ωh2<0.129

mh=114.4 GeV

σ(Z~

1p)=10-9 pb

LHC

LC1000

LC500

TEV

µD

D

200

400

600

800

1000

1200

1400

1600

0 1000 2000 3000 4000 5000

mSUGRA, A0=0, tanβ=50, µ<0

m0 (GeV)m

1/2

(GeV

)

LEP

no REWSB

Z~

1 no

t LS

P

Φ(p-) 3e-7 GeV-1 cm-2 s-1 sr-1 (S/B)e+=0.01

Φ(γ)=10-10 cm-2 s-1 Φsun(µ)=40 km-2 yr-1

0< Ωh2< 0.129

mh=114.4 GeV

Φearth(µ)=40 km-2 yr-1 σ(Z~

1p)=10-9 pb

LHC

LC1000

LC500

µ

DD

HB, Belyaev, Krupovnickas, O’Farrill


SUGRA models with non-universal scalars

• Normal scalar mass hierarchy NMH: HB, Belyaev, Krupovnickas, Mustafayev

• m0(1) ≃ m0(2) ≪ m0(3) (preserve FCNC bounds)

• motivation: reconcile BF (b→ sγ) with (g − 2)µ anomaly

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 5

200

400

600

800

1000

1200

1400

1600

1800

2000

0.5 1 1.5 2 2.5 3 3.5 4 4.5 50

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

mSUGRA, tgβ=30, µ>0, A0=0, mtop=175 GeV,m01,2=100 GeV

e+e- input for δaµ LEP2 excluded

NO REWSB

stau

LS

P

sqrt

(χ2 )

m03 (TeV)

m1/

2 (G

eV)


SUGRA models with non-universal Higgs mass (NUHM1)

• m2Hu

= m2Hd

≡ m2φ 6= m0: HB, Belyaev, Mustafayev, Profumo, Tata

• motivation: SO(10) SUSYGUTs where Hu,d ∈ φ(10) while matter ∈ ψ(16)

• m2φ ≫ m0 ⇒higgsino DM for any m0, m1/2

• m2φ < 0 ⇒ can have A-funnel for any tan β

10-3

10-2

10-1

1

-3 -2 -1 0 1 2mφ / m0

Ωh

2

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1

-3 -2 -1 0 1 2mφ / m0

m (

TeV

)

m0=300GeV, m1/2=300GeV, tanβ=10, A0=0, µ>0, mt=178GeV

WMAPmA

mχ

µ


NUHM2 (2-parameter case)

• m2Hu

6= m2Hd

6= m0: HB, Belyaev, Mustafayev, Profumo, Tata

• motivation: SU(5) SUSYGUTs where Hu ∈ φ(5), Hd ∈ φ(5)

• can re-parametrize m2Hu, m2

Hd↔ µ, mA (Ellis, Olive, Santoso)

• large S term in RGEs ⇒ light uR, cR squarks, meL< meR

NUHM2: m0=300GeV, m1/2=300GeV, tanβ=10, A0=0, mt=178GeV

100

200

300

400

500

600

700

800

900

0 250 500 750 1000 1250 1500 1750 20000

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

mA (GeV)

µ (G

eV)

LEP2

sqrt

(χ2 )

τ~

1

Ah

NUHM1

HS

mSUGRA

GS


Gaugino mass non-universality

• M1 6= M2 6= M3: HB, TK, AM, EP, SP, XT

• motivation: SUSYGUTs where gauge kinetic function transforms non-trivially

• M2 ∼M1 at MGUT : mixed wino dark matter (MWDM)

• M2 ≃ −M1 at MGUT : bino-wino co-annihilation (BWCA)

-600 -400 -200 0 200 400 600

M1 (GeV)10

-5

10-4

10-3

10-2

10-1

100

101

102

103

104

Ωh2

m0=300 GeV, m1/2=300 GeV, tanβ=10, A0=0, µ>0, mt=178 GeV

-600 -400 -200 0 200 400 600

M1 (GeV)

0

0.2

0.4

0.6

0.8

1

RB~ ,W

~

w~B~

a) b)

WMAP

mSUGRA MWDMBWCA BWCA mSUGRA MWDM


Gaugino mass non-universality: low M3 case

• M3 < M1 ∼M2: HB, TK, AM, EP, SP, XT

• motivation: mixed-moduli AMSB models

• lower M3 → low mq → low µ→ mixed higgsino DM

-400 -200 0 200 400

M3 (GeV)10

-4

10-3

10-2

10-1

100

101

102

Ωh2

m0=300 GeV, m1/2=300 GeV, tanβ=10, A0=0, µ>0, mt=175 GeV

-400 -200 0 200 400

M3 (GeV)

0

0.2

0.4

0.6

0.8

1

RH~

a) b)

WMAP

mSUGRA mSUGRAMHDM1 MHDM1

LEP2

Excluded

LEP2

Excluded

MHDM2 MHDM2


Mixed higgsino DM from a high M2 (HM2DM)

m0 =300GeV, m1/2 =300GeV, tanβ=10, A0 =0, µ >0, mt =171.4GeV

10-2

10-1

1

-3 -2 -1 0 1 2 3

2007/07/07 11.40

WMAP

Ωh

2

00.10.20.30.40.50.60.70.80.9

1

-3 -2 -1 0 1 2 3

r2 = M2 / m1/2

RH

• high M2 ⇒ low |µ| so get mixed higgsino DM but high mqL

• HB, Mustafayev, Summy, Tata


Direct DM detection: well-tempered Z1 models

Spin-independent Direct Detection

10-14

10-13

10-12

10-11

10-10

10-9

10-8

10-7

10-6

10-5

200 400 600 800 1000 1200 1400

----⋅-⋅-⋅⋅⋅⋅⋅⋅

mSUGRA : µ > 0

mSUGRA : µ < 0

NUHM1µ

NUHM1A

MWDM1

MWDM2

BWCA2

LM3DM

HM2DM : M2 > 0

HM2DM : M2 < 0

Xenon-10SuperCDMS 25 kgXenon-100/LUXXenon-1 ton

mz1∼ (GeV)

σ SI (

pb)

• well-tempered Z1 models asymptote at σ(Z1p) ∼ 10−8 pb!


Compressed SUSY (Steve Martin)

• in models with low M3 and A0 ∼ −M1, the t1 becomes quite light

• Martin finds that if

– mt < meZ1

<∼ mt + 100 GeV and

– meZ1+ 25 GeV

<∼ mt1

<∼ meZ1+ 100 GeV, then

• Z1Z1 → tt is dominant dark matter annihilation mechanism in early Universe!

• implications for LHC, DD, IDD: (HB, Box, Park, Tata)

– light mg with t1 = NLSP

– collider signatures depend on whether t1 → cZ1 or bWZ1

– if t1 → cZ1, then large 6ET + jets, but very low isolated lepton rates

– IDD halo annihilation signals enhanced since Z1Z1 → tt→ γs, anti-matter


Mixed modulus-AMSB models

⋆ KKLT model: type IIB superstring compactification with fluxes

• stabilize moduli/dilaton via fluxes and e.g. gaugino condensation on D7

brane

• introduce anti-D3 brane (uplifting potential; de Sitter universe with Λ > 0

• small SUSY breaking due to D3 brane

• mass hierarchy: mmoduli ≫ m3/2 ≫ mSUSY

⋆ MSSM soft terms calculated by Choi, Falkowski, Nilles, Olechowski, Pokorski

⋆ phenomenology: Choi, Jeong, Okumura; Falkowski, Lebedev, Mambrini;

Kitano, Nomura

⋆ see also: HB, E. Park, X. Tata, T. Wang, JHEP0608, 041 (2006); PLB641,

447 (2006); JHEP0706, 033 (2007);


α=6, m3/2=12 TeV, tanβ=10, µ >0, mt=175 GeV

200

300

400

500

600

700

800

900

103

105

107

109

1011

1013

1015

1017

M1

M2

M3

a)

Q (GeV)

Mas

s (G

eV)

α=6, m3/2=12 TeV, tanβ=10, µ >0, mt=175 GeV

-600

-400

-200

0

200

400

600

800

103

105

107

109

1011

1013

1015

1017

Hd

Hu

τR

τL

bR

tR

tL

eR ,eL ,

dR,

uR

uL b)

Q (GeV)

sig

n(m

i2 )⋅√

|mi2 |

(G

eV)

• GUT scale AMSB splitting of soft terms cancelled by RGE running:

soft terms unify at “mirage” unification scale

• MM-AMSB contains BWCA, MWDM, LM3DM scenarios!


SO(10) SUSYGUTs: motivation

⋆ In all the excitement of new models, it is easy to neglect the really good ideas

from the past:

⋆ SUSYGUTs with SO(10) → SU(5) → SU(3)C × SU(2)L × U(1)Y :

• unification of forces

• SO(10) naturally anomaly free

• explain ad-hoc SM hypercharge assignments (charge relations: e.g. why

m(proton) = −me

• unification of matter in SO(10): matter ∈ ψ(16), higgs ∈ φ(10)

(simplest models)

• The 16-dim’l spinor rep of SO(10) contains all the matter in a single

generation of the SM, plus a right-handed neutrino state.

• break SO(10): get see-saw νs!

• simplest models: t− b− τ Yukawa unification


YU requires precision calculation of SUSY spectrum:

Hall, Rattazzi, Sarid; Pierce et al. (PBMZ)

• need full 2-loop RGE running

• RG-improved 1-loop effective potential evaluated at optimized scale

• t, b, τ threshold effects

• full set of 1-loop sparticle/Higgs mass corrections

• use Isajet/Isasugra 7.75 spectrum generator


Running of Yukawa couplings: m16 = 10 TeV

1e+00 1e+02 1e+04 1e+06 1e+08 1e+10 1e+12 1e+14 1e+16Q (GeV)

0.4

0.5

0.6

0.7

0.8

0.9

1

f i

fτ

fb

ft

• note shifts at Q = MSUSY !


t − b − τ Yukawa unification in HS model!

• need m16 ∼ 5 − 20 TeV

• need m10 ≃√

2m16

• A0 ≃ −2m16

• tanβ ≃ 50

• m1/2 ≪ m16

• inverted scalar mass hierarchy: Bagger et al.

• split Higgs needed for EWSB: m2Hu

< m2Hd

• Auto, HB, Balazs, Belyaev, Ferrandis, Tata

• HB, Kraml, Sekmen, Summy

• related work: Blazek, Dermisek, Raby (BDR); DRRR uses 1-loop SSB RGEs

and scalar pot’l minimization at Q = MZ


Scan for R ≃ 1 in HS model with µ > 0

• R = max(ft, fb, fτ )/min(ftfb, fτ )


Special SUSY spectrum from Yukawa unified models

• first/second gen. squarks/sleptons ∼ 5 − 20 TeV

• third gen. scalars, µ, mA ∼ 1 − 2 TeV

• gluinos ∼ 350 − 500 GeV

• charginos ∼ 100 − 160 GeV

• Z1 or χ1 ∼ 50 − 80 GeV


Problem: Ω eZ1h2 ∼ 103 − 105× WMAP

• for R ≃ 1, then Ω eZ1

h2 >∼ 102!

• higher than measured value by 103 − 105

• Does this rule out Yukawa-unified SUSY?


Solution: axino a dark matter

• invoke axion solution to strong CP problem

• axino is spin 1

2element of saxion/axion/axino supermultiplet

• 10−6 eV < ma < 10−2 eV

• 100 keV < ma <∼ 10 GeV

• for our case, Z1 → aγ with τeZ1∼ 0.03 sec

• can shed large factors of relic density:

• Ωah2 ∼ ma

m eZ1

Ω eZ1

h2: ⇒ warm DM for ma < 1 − 10 GeV (JLM)

• also generate thermal component for axino DM depending on TR: ⇒ CDM


Consistent cosmology for SUSY SO(10): gravitino problem

• gravitino problem in generic SUGRA models: overproduction of G followed by

late G decay can destroy successful BBN predictons: upper bound on TR

(see Kohri, Moroi, Yotsuyanagi; Cybert, Ellis, Fields, Olive)


Leptogenesis via inflaton decay

• Upper bound on TR from BBN is below that for successful thermal

leptogenesis: need TR>∼ 1010 GeV (Buchmuller, Plumacher)

• Alternatively, one may have non-thermal leptogenesis where inflaton

φ→ NiNi decay (Lazarides,Shafi; Kumekawa, Moroi, Yanagida)

• additional source of Ni in early universe allows lower TR:

nB

s≃ 8.2 × 10−11 ×

(TR

106 GeV

) (2mN1

mφ

) ( mν3

0.05 eV

)δeff (1)

• WMAP observation: nb/s ∼ 0.9 × 10−10 ⇒ TR>∼ 106 GeV


Cold and warm axino DM in the universe

• Non-thermal axino production via Z1 → aγ decay:

⇒ warm DM for ma<∼ 1 GeV (Jedamzik, Lemoine, Moultaka)

• thermal production of a: cold DM for ma > .1 MeV

(Brandenberg, Steffen)

ΩTPa h2 ≃ 5.5g6

s ln

(1.108

gs

)(1011 GeV

fa/N

)2 ( ma

0.1 GeV

) (TR

104 GeV

)(2)

• with 0.1 ≃ Ωah2 = ΩTP

a h2 + ma

m eZ1

Ω eZh2, can calculate value of TR needed

given a PQ breaking scale fa/N ∼ 1011 GeV


Consistent cosmology for SO(10) SUSY GUTs with a DM

• Happily, TR falls into the right range to give cold axino DM with a small

admixture of warm axino DM, preserve BBN predictions (solving the gravitino

problem) and have non-thermal leptogenesis!

• See HB and H. Summy, arXiv:0803.0510 (2008)

1e-05 0.0001 0.001 0.01m

a~ (GeV)

1e+06

1e+07

1e+08

1e+09

TR (

GeV

) BBN/gravitino

NT leptogenesis

warm a~DM


SuperWIMPs (e.g. G in SUGRA or G in UED)

⋆ mG = F/√

3M∗ ∼ TeV in Supergravity models

• usually G decouples (but see Moroi et al. for BBN constraints)

• if G is LSP, then calculate NLSP abundance as a thermal relic: ΩNLSPh2

• Z1 → hG, ZG, γG or τ1 → τG possible

∗ lifetime τNLSP ∼ 104 − 108 sec

∗ constraints from BBN, CMB not too severe

∗ DM relic density is then ΩG =mG

mNLSPΩNLSP + ΩTP

G(TR)

∗ Feng, Rajaraman, Su, Takayama; Ellis et al; Buchmuller et al.

• G undetectable via direct/indirect DM searches

• unique collider signatures:

∗ τ1=NLSP: stable charged tracks

∗ can collect NLSPs in e.g. water (slepton trapping)

∗ monitor for NLSP → G decays


SUGRA models beyond MSSM: NMSSM

⋆ Add extra singlet SF S

• motivation: introduce µ parameter via SUSY breaking

• 3 neutral scalar higgs, 2 pseudoscalars and 5 neutralinos

0 200 400 600 800µ [GeV]

0

200

400

600

800

M2

[GeV

]

WM

AP

Ωh2= 1

Ωh2= 0.02

Belanger, Boudjema, Hugonie, Pukhov, Semenov


Conclusions

⋆ Overwhelming evidence for CDM in the universe

⋆ Numerous candidate CDM particles

• Axions: searches ongoing (ADMX group)

⋆ SUSY LSP: thermal relic from Big Bang

⋆ Various regions ⇒ distinct collider/DM signatures

⋆ Direct/ indirect DM detection prospects

⋆ Detection at colliders: Tevatron, LHC, ILC

⋆ Beyond mSUGRA:

• NMH, NUHM1, NUHM2, MWDM, BWCA, low M3, high M2, comp.

SUSY, SO(10)

• axino a or gravitino G as dark matter

• NMSSM


Documents

E6 T signatures and dark matter connectionE6 T signatures and dark matter connection Howard Baer Florida State/ Oklahoma ⋆ Evidence for CDM ⋆ Candidates for CDM ⋆ Neutralino