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Predictions of the MSO10SM :
dark matter and more …
Stuart Raby
Bonn, Germany August 29, 2005
COSMO 05
w/ R. Dermisek, L. Roszkowski & R.R, de Austrihep-ph/0304101 & hep-ph/o507233
Outline Minimal SO(10) SUSY Model analysis Dark Matter + WMAP data Light Higgs mass Bs ->
Direct & indirect detection Conclusions
3 316 1 0 16
t b
0 16 10 16
16 1/ 2 16
2 2
1.2TeV , <<
A m m m
m M m
tan 50
MSO10SM
Fit t,b,tau requires
TM
2 2
2
2
10
13%2
d uH H
H
m mm
m
Roughly ½ comes from running
GM m
20 10Varying , ,
arbitraryH
A
A m m
m
1/ 2 16, << M m & EWSB
Gauge coupling unification Yukawa unification Inverted scalar mass hierarchy Suppresses flavor & CP violation Nucleon decay
MSO10SMTM
MSO10SM1. Extend to 3 family model in 4D ( R. Dermisek & SR,
hep-ph/0507045 )
2. Extend to orbifold GUT in 5D ( H.D. Kim, L. Schradin & SR, hep-ph/0212348 &
hep-ph/0411328 )
3. Extend to heterotic string compactified in
10D compactified on Z3xZ2 orbifold ( T. Kobayashi, SR & R.J. Zhang, hep-ph/0403065 & 0409098 )
TM
analysis
11 Parameters :
3
01 10/ 2 16tanG G
HM m
M
A m m
9 Observables ( included in chi2) :
EM s Z W NEW
t b b
G M M
M m m M
Results
1. Dark Matter & WMAP2. Bs ->
3. Light Higgs mass - mh
4. Upper bound on mA
Lower bound on BR(Bs -> )5. Direct & Indirect dark matter detection
Dark Matter & WMAP
Neutralino LSP
1 1 A f f
tanAb b
A : broad resonance, mA arbitrary
Results - m16 & mA fixed
Green band consistent with WMAP Light Higgs mass contours
Br( Bs -> )
SM : 3 x 10-9
MSSM : ~ tan 6 /mA4
DZero bound < 5.0 x 10-7 (95% CL)
CDF prelim. < 2.0 x 10-7 (95% CL)
Results - m16 & mA fixed
Constant Bs -> contoursConstant contours
Results - m16 & mA fixed
Constant Bs -> contours
Light Higgs mass
|At| increases mh decreases
Carena,Quiros &Wagner ‘95
Light Higgs mass
2
3
2 2
tan tanlog .
2%
g t tb
bb t
b
b
M Am corrm m m
mm
Needed to fit data
M1/2 increases -At increases
mh decreases
Light Higgs mass contours
mA[max] Br[ Bs -> ][min]
Fermilab !!
-8
1.3 TeV
Br( )
10
A
s
m
B
mA[max] Br[ Bs -> ][min]
Direct Neutralino Detection
Direct Neutralino Detection
Br( Bs -> ) x 107
< 5 all
< 2 bold
Next gen.
Exp’ts
Indirect Neutralino Detection
Indirect Neutralino Detection
W. deBoer SUSY 05
1 1 A b b
Within same region ofSUSY para. space
rays
Conclusions - MSO10SM
1. Gauge & Yukawa unification2. Suppresses flavor & CP viol.
& N decay3. Dark Matter consistent
w/WMAP4. 114 < mh < 121 GeV5. mA < 1.3 TeV
BR(Bs -> ) > 10-8
6. Direct dark matter detection
by next generation exp’ts
7. Indirect detection via gammas
??
TM