Predictions of the MSO 10 SM : dark matter and more … Stuart Raby Bonn, Germany August 29, 2005 COSMO 05 w/ R. Dermisek, L. Roszkowski & R.R, de Austri hep-ph/ & hep-ph/o507233

Outline  Minimal SO(10) SUSY Model    analysis  Dark Matter + WMAP data  Light Higgs mass  B s ->      Direct & indirect detection  Conclusions

MSO 10 SM Fit t,b,tau requires TM

Roughly ½ comes from running & EWSB

 Gauge coupling unification  Yukawa unification  Inverted scalar mass hierarchy  Suppresses flavor & CP violation  Nucleon decay MSO 10 SM TM

MSO 10 SM  Extend to 3 family model in 4D ( R. Dermisek & SR, hep-ph/ )  Extend to orbifold GUT in 5D ( H.D. Kim, L. Schradin & SR, hep-ph/ & hep-ph/ )  Extend to heterotic string compactified in 10D compactified on Z 3 xZ 2 orbifold ( T. Kobayashi, SR & R.J. Zhang, hep-ph/ & ) TM

  analysis 11 Parameters : 9 Observables ( included in chi2) :

Results 1. Dark Matter & WMAP 2. B s ->     3. Light Higgs mass - m h 4. Upper bound on m A Lower bound on BR(B s ->     ) 5. Direct & Indirect dark matter detection

Dark Matter & WMAP Neutralino LSP A : broad resonance, m A arbitrary

Results - m 16 & m A fixed Green band consistent with WMAP Light Higgs mass contours

Br( B s ->     ) SM : 3 x MSSM : ~  tan  6 /m A 4 DZero bound < 5.0 x (95% CL) CDF prelim. < 2.0 x (95% CL)

Results - m 16 & m A fixed Constant B s ->     contours Constant   contours

Results - m 16 & m A fixed Constant B s ->     contours

Light Higgs mass |A t | increasesm h decreases Carena, Quiros & Wagner ‘95

Light Higgs mass Needed to fit data M 1/2 increases -A t increases m h decreases

Light Higgs mass contours

m A [max] Br[ B s ->      ][min] Fermilab !!

m A [max] Br[ B s ->      ][min]

Direct Neutralino Detection

Br( B s - >     ) x 10 7 < 5 all < 2 bold Next gen. Exp’ts

Indirect Neutralino Detection

W. deBoer SUSY 05 Within same region of SUSY para. space

Conclusions - MSO 10 SM 1. Gauge & Yukawa unification 2. Suppresses flavor & CP viol. & N decay 3. Dark Matter consistent w/WMAP < m h < 121 GeV 5. m A < 1.3 TeV BR(B s ->    ) > Direct dark matter detection by next generation exp’ts 7. Indirect detection via gammas ?? TM