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