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
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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
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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
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Dark Matter in the universe
Binding of clusters
Galactic rotation curves
Gravitational lensing
Hot gas in clusters
CMB fluctuations
Large scale structure
flatness/BBN
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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
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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
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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
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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!
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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
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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
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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
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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?
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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
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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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( ) ( )
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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
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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
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MCMC scan: compromise solution with m16 3 TeV
Z1 Z1 annihilate through h resonance
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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!
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