Howard Baer- SUSY and cosmology

8/3/2019 Howard Baer- SUSY and cosmology

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SUSY and cosmology

Howard Baer

Florida State University

Cosmology

Baryogenesis

SUSY Dark matter , a, G models

mSUGRA NUSUGRA MM-AMSB

SO(10) SUSYGUTsHowie Baer, Aspen winter conference, January 16, 2008 1


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Pillars of Big Bang cosmology: Hubble expansion

Theory: FRW universe

Hubble expansion HST key project type Ia supernovae probe

H0dL = z + 12 (1 q0)z2 + H0 = 72 km/sec/Mpc10% evidence for > 0!

age of universe: 13.7 Gyrs

Howie Baer, Aspen winter conference, January 16, 2008 2


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Big Bang nucleosynthesis (BBN)

Thermal history

of universe:

Can compute light elementabundances: 4He, D, 3He, 7Li

match to data: B nBn 6 1010 B from BBN

consistent with CMB results

? ? ? ?

? ? ? ?

@ @ @ @

@ @ @ @

3He/H p

4

He

2 3 4 5 6 7 8 9 101

0.01 0.02 0.030.005

CM

B

BBN

Baryon-to-photon ratio 1010

Baryon density Bh2

D___H

0.24

0.23

0.25

0.26

0.27

104

103

105

109

1010

2

5

7Li/H p

Yp

D/H p



4/45

Cosmic microwave background (CMB)

COBE/WMAP/WMAP3,

anisotropies 105 can extract numerous

cosm. params from power spectrum

flat (k = 0) universe: = cas in inflation models

contents of universe

0.7

baryons 0.04 CDM 0.25 tiny



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Baryogenesis: explaining B

SM electroweak baryogenesis: only if mHSM


6/45

Dark Matter in the universe

Binding of clusters

Galactic rotation curves

Gravitational lensing

Hot gas in clusters

CMB fluctuations

Large scale structure

flatness/BBN



7/45

Best fit cosmology: concordance (CDM) model

Bh

2 = 0.022

0.001

h2 < 0.007 95% CL h2 0.38 0.03

CDMh2 = 0.105 0.01



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Candidates for Dark Matter

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

inconsistent with BBN element abundance calcn

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

int

(pb)

Some Dark Matter Candidate Particles

neutrinosneutralinoKK photonbranonLTP

axion axino

gravitinoKK graviton

SuperWIMPs :

wimpz

illaWIMPs :

BlackHoleRem

nant

Q-ball

fuzzy CDM



9/45

Axions

PQ solution to strong CP problem in QCD pseudo-Goldstone boson from

PQ breaking at scale fa

non-thermally producedvia vacuum mis-alignment

ma 2QCD/fa 106 101eV

ah2

12 610

6eVma

7/6

h2

astro bound: stellar cooling ma < 101eV a couples to EM field: a 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

axionh2



10/45

Axion microwave cavity searches

ongoing searches: ADMX experiment

Livermore U Wash. Phase I: probe KSVZ

for ma 106 105 eV

Phase II: probe DFSZfor ma 106 105 eV

beyond Phase II:probe higher values ma



11/45

WIMPs: the WIMP miracle!

Weakly Interacting Massive Particles assume in thermal equiln in early universe Boltzman eqn:

dn/dt = 3Hn vrel(n2 n20) h2 = s0c/h2

45g

1/2xfMPl

1v

0.1 pbv 0.1 mwimp100 GeV 2

thermal relic new physics at Mweak!



12/45

Some WIMP candidates

4th gen. Dirac (excluded)

SUSY neutralino ( or Z1) UED excited photon B1

little Higgs photon BH

little Higgs (theory space) N1 (scalar)

warped GUTS: LZP KK fermion

branons



13/45

Most work done for SUSY theories

SUSY divergence cancellation maintains hierarchy between GUT scaleQ = 1016 GeV and weak scale Q = 100 GeV

gauge coupling unification!

Lightest Higgs mass mh


14/45

Supersymmetry: fermions

bosons

MSSM: doubling of spectra

spin-0 squarks, sleptons

spin-

1

2 charginos, neutralinos, gluino extra Higgses: h, H, A, H

R-parity consn: LSP is stable

LSP candidates sneutrinos (excluded)

gravitinos (superWIMPs)

neutralinos GMSB messengers

hidden sector states

axinos a



15/45

Neutralino dark matter

Why R-parity? natural in SO(10) SUSYGUTS if properly broken, or brokenvia compactification (Mohapatra, Martin, Kawamura, )

In thermal equilibrium in early universe

As universe expands and cools, freeze out

Number density obtained from Boltzmann eqn

dn/dt = 3Hn vrel(n2

n2

0) 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)



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Some neutralino (co)annihilation processes



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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

h2< 0.094

0.094


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Main mSUGRA regions consistent with WMAP

bulk region (low m0, low m1/2) stau co-annihilation region (m1 meZ1) HB/FP region (large m0 where || small )

A-funnel (2meZ1 mA, mH) h corridor (2meZ1 mh) stop co-annihilation region (particular A0 values mt1

meZ1

)



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SUSY reach of all colliders and relic density

200

400

600

800

1000

1200

1400

1600

0 1000 2000 3000 4000 5000 6000 7000 8000

mSugra with tan = 10, A0

= 0, > 0

m0

(GeV)

m1/2

(GeV)

LHC

Tevatron

LC 500

LC 1000

G h2< 0.129

G LEP2 excluded

200

400

600

800

1000

1200

1400

1600

0 1000 2000 3000 4000 5000 6000 7000

mSugra with tan = 45, A0

= 0, < 0

m0

(GeV)

m1/2

(GeV)

LHC

Tevatron

LC 500

LC 1000

G h2< 0.129

G LEP2 excluded

HB, Belyaev, Krupovnickas, Tata



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International linear e+e collider (ILC)

A linear e+e collider with

s = 0.5 1 TeV is highest priority project forHEP beyond LHC! Why?

All beam energy

collision (aside from brem/beamstrahlung losses)

beam energy known clean collision environment

low (electroweak) background levels

adjustable beam energy (threshold scans) e and possibly e+ beam polarization

ILC will be ideal machine to perform precision spectroscopy of any new (EWinteracting) matter states (provided they are kinematically accessible)!

timeline: decision-2012; ready-2020



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Precision sparticle measurements at a e+e linear collider



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Role of ILC in DM physics

Baltz, Battaglia, Peskin, Wizansky analysis fit all sparticle measurements to determine underlying SUSY parameters then plug in to theory to find relic density does eZ1h2 saturate measured value? possible mixed dark matter? Z1 decay to gravitino or axino?



23/45

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 SI( Z1p) so results from different

target nuclei can be compared



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Current best limit: new Xenon-10 result!

WIMP Mass [GeV/c2]

Cross-section[pb](n

ormalisedtonucleo

n)

071107122201

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

101

102

103

10-10

10-9

10-8

10-7

10-6

10-5

071107122201

Baer et. al 2003XENON1T (proj)LUX 300 kg LXe Projection (Jul 2007)SuperCDMS (Projected) 25kg (7-ST@Snolab)WARP 140kg (proj)DEAP CLEAN 150kg FV (proj)SuperCDMS (Projected) 2-ST@SoudanXENON10 2007 (Net 136 kg-d)CDMS (Soudan) 2004 + 2005 Ge (7 keV threshold)DAMA 2000 58k kg-days NaI Ann.Mod. 3sigma,w/o DAMA 1996 limitDATA listed top to bottom on plot



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Indirect detection (ID) of SUSY DM: -telescopes

Z1Z1 bb, etc. in core of sun (or earth): in telescopes

flux is largest when ( Z1p) is largest e.g. low mq or HB/FP region for mSUGRA

experiments: Amanda, Icecube, Antares



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ID of SUSY DM: and anti-matter searches

Z1Z1 qq, etc. 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



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

0 1000 2000 3000 4000

m0(GeV)

105

104

103

102

101

100

S/B(e+)

0 5 10 15

r(kpc)

0

5

10

(G

eVcm

3)

default

NFW

Moore et al

Kravtsov et al

0 1000 2000 3000 4000

m0(GeV)

109

108

107

106

105

104

d

p/dEd(

GeV

1c

m

2s

1

sr

1)

0 1000 2000 3000 4000

m0(GeV)

1012

1010

108

106

104

(c

m

2s

1)

a) b)

c) d)

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



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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 tan=10, >0

m0(GeV)

m1/2

(Ge

V)

LEP

no REWSB

Z~1notLSP

(p-)=3x10

-7GeV

-1cm

-2s

-1sr

-1

(S/B)e+=0.01

()=10-10

cm-2

s-1

sun

()=40 km

-2

yr

-1

G 0


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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: NLSPh

2

Z1 hG, ZG, G or 1 G possible lifetime NLSP 104 108 sec constraints from BBN, CMB not too severe

DM relic density is then G =mG

mNLSPNLSP + TP

G (TR) Feng, Rajaraman, Su, Takayama; Ellis et al; Buchmuller et al. G undetectable via direct/indirect DM searches

unique collider signatures:

1=NLSP: stable charged tracks can collect NLSPs in e.g. water (slepton trapping) monitor for NLSP G decays



30/45

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

s) with (g

2) 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 5

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

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

e+e

-input for a G LEP2 excluded

NO REWSB

stau

LSP

sqrt

(2)

m03 (TeV)

m1/2

(Ge

V)



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SUGRA models with non-universal Higgs mass (NUHM1)

m2Hu = m2Hd m2 = m0: HB, Belyaev, Mustafayev, Profumo, Tata motivation: SO(10) SUSYGUTs where Hu,d (10) while matter (16)

m2

m0 higgsino DM for any m0, m1/2 m2 < 0 can have A-funnel for any tan

10-3

10-2

10-1

1

-3 -2 -1 0 1 2 m / m0

h2

0

0.1

0.20.3

0.4

0.5

0.6

0.7

0.8

0.9

1

-3 -2 -1 0 1 2 m / m0

m(TeV)

m0=300GeV, m

1/2=300GeV, tan=10, A

0=0, >0, m

t=178GeV

WMAPm

A

m



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NUHM2 (2-parameter case)

m2Hu = m2Hd = m0: HB, Belyaev, Mustafayev, Profumo, Tata motivation: SU(5) SUSYGUTs where Hu (5), Hd (5)

can re-parametrize m2Hu , m

2Hd

, mA (Ellis, Olive, Santoso)

large S term in RGEs light uR, cR squarks, meL < meRNUHM2: m

0=300GeV, m

1/2=300GeV, tan=10, A

0=0, m

t=178GeV

100

200

300

400

500

600

700

800

900

0 250 500 750 1000 1250 1500 1750 2000

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

mA

(GeV)

(GeV)

LEP2

sqrt(2)

~

1

Ah

NUHM1

HS

mSUGRA

GS



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Gaugino mass non-universality

M1 = M2 = 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

10

4

h

2

m0=300 GeV, m

1/2=300 GeV, tan=10, A

0=0, >0, m

t=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



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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 mixed higgsino DM

-400 -200 0 200 400

M3

(GeV)

10-4

10

-3

10-2

10-1

100

101

102

h

2

m0=300 GeV, m

1/2=300 GeV, tan=10, A

0=0, >0, m

t=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



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Mixed higgsino DM from a high M2 (HM2DM)

m0

=300GeV, m1/2

=300GeV, tan=10, A0

=0, >0, mt=171.4GeV

10-2

10 -1

1

-3 -2 -1 0 1 2 3

2007/07/07 11.40

WMAP

h2

00.10.20.30.40.50.6

0.70.80.9

1

-3 -2 -1 0 1 2 3

r2

= M2

/ m1/2

RH

high M2 low || so get mixed higgsino DM but high mqL HB, Mustafayev, Summy, Tata



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Compressed SUSY (Steve Martin)

in models with low M3 and A0 M1, the t1 becomes quite light Martin finds that if

mt < meZ1 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);



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=6, m3/2

=12 TeV, tan=10, >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)

Mass(GeV)

=6, m3/2

=12 TeV, tan=10, >0, mt=175 GeV

-600

-400

-200

0

200

400

600

800

103

105

107

109

1011

1013

1015

1017

Hd

Hu

R

L

bR

tR

tL

eR

,e

L,

dR,

uR

uL b)

Q (GeV)

sign(mi2

)|mi2

|(Ge

V)

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!


( ) ( )


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SO(10) SUSYGUTs and t b Yukawa unification (YU)

superpotential: f f 161610 +

YU not possible in mSUGRA YU can work in NUHM2 model! need A20 = 2m210 = 4m216

inverted scalar mass hierarchy: BFPZ

split Higgs: m2Hu < m2Hd mq,(1, 2) 10 TeV mt1 , mA,

1

2 TeV

mg 350 500 GeV see Baer et al; Blazek et al.

g1

g2

g3

fb

ft

f

MZ

MG

Co u p li n

g s

0.0

0.2

0.4

0.6

0.8

1.0

1.2

1.4

tLtR

bR

LR

uL,R

,dR

eR

eL

At

Ab

A

Hu

Hd

Q (GeV)

S o ftPa r a

me te r s

( Te V)

10

15

5

0

-5

-10

-15

-20

1 10 10 10 10 10 10 10 10 102 4 6 8 10 12 14 16 18



40/45

Top-down scan of NUHM2 p-space

New analysis: MCMC approach (HB, Kraml, Sekmen, Summy)



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Problem reconciling DM with Yukawa unification

one solution: axino DM instead of neutralino

ah2

mam eZ1

eZ1h2

: warm DM also thermal component depending on TR: CDM



42/45

MCMC scan: compromise solution with m16 3 TeV

Z1 Z1 annihilate through h resonance



43/45

Can generate BDR solutions with both WS/GS BCs

Z1 Z1 annihilate through A resonance comb. large tan 50 and low mA: excluded by Bs +



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Prediction of new physics at LHC from SO(10) SUSYGUTs:

gluino pair production with mg 350 450 GeV high b-jet multiplicity meZ2 meZ1 50 75 GeV dilepon mas edge



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Conclusions

Baryogenesis scenarios: constrained by /sparticle searches

Overwhelming evidence for CDM in the universe: identity unknown

Numerous candidate CDM particles from theory WIMPs: thermal relic from Big Bang

SUSY

Z1 is favored WIMP candidate, but many others

Detection at colliders: Tevatron, LHC, ILC; direct/indirect DM

SuperWIMPs: G in SUSY; G in UED

models: mSUGRA; NUSUGRA; MMAMSB; SO(10) with YU

We are on our way to unveiling the mysteries of baryogenesis and DarkMatter in next several years!


Howard Baer- SUSY and cosmology

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