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Testing the Standard Model and Beyond Shufang Su • U. of Shufang Su • U. of Arizona Arizona DOE Review 2004 • • Progress Report
Testing the Standard Model and Beyond
Testing the Standard Model and Beyond
Shufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of Arizona
DOE Review 2004 •• Progress Report
S. Su DOE Review, 2004 2
Research and Collaborations Research and Collaborations
New candidate of dark matter (DM) : superWIMPNew candidate of dark matter (DM) : superWIMP J. Feng, F. Takayama (UC Irvine)
Model independent study of collider DM searchesModel independent study of collider DM searches J. Feng, F. Takayama (UC Irvine)
Precision study of SUGRA, GMSB and AMSBPrecision study of SUGRA, GMSB and AMSB S. Heinemeyer (CERN), G. Weiglein (IPPP, Durham)
Propagation of high energy stauPropagation of high energy stau M. H. Reno (U. IOWA), I. Sarcevic (UA)
Phenomenology of warped SUSY GUT modelPhenomenology of warped SUSY GUT model C.W. Chiang (NCU), T. Han (U. Wisconsin), L.T. Wang (Harvard)
MSSM contribution to precision observablesMSSM contribution to precision observables M. Ramsey-Musolf (Caltech)
S. Su DOE Review, 2004 3
WIMPWIMP
SWIMPSWIMP(DM)(DM)
SMSM
101066
SuperWIMP Dark Matter SuperWIMP Dark Matter
FRT hep-ph/0302215, 0306024
101044 s s t t 10 1088 s s
Gravitino LSPGravitino LSP
LKK gravitonLKK graviton
WIMP WIMP SWIMP + SM particle SWIMP + SM particle
J. Feng, F. Takayama (UC Irvine)
WIMPWIMP
S. Su DOE Review, 2004 4
SWIMP and SUSY WIMP SWIMP and SUSY WIMP
SUSY caseSUSY case
NLSP NLSP G + SM particles G + SM particles~~
SWIMP: G (LSP) WIMP: NLSP SWIMP: G (LSP) WIMP: NLSP mmGG »» m mNLSPNLSP~~
nneutralino/eutralino/cchargino hargino NLSPNLSP
ssleptonlepton/sneutrino/sneutrino NLSP NLSP
BBBBNN
EMEM
hahadd
BrBrhadhad O(0.01) O(0.01) BrBrhadhad O(10 O(10-3-3))
101044 s s t t 10 1088 s s
Ellis et. al., hep-ph/0312262; Wang and Yang, hep-ph/0405186.
~~
S. Su DOE Review, 2004 5
Viable Parameter Space Viable Parameter Space
apply CMB and BBN constraints on (apply CMB and BBN constraints on (NLSPNLSP, , EM/hadEM/had ) )
viable parameter spaceviable parameter space
NLSPNLSP, , EM,hadEM,had==EM,hadEM,had B BEM,hadEM,had Y YNLSPNLSP
m m ·· 80 80 »» 300 GeV 300 GeV200 GeV 200 GeV ·· m m ·· 400 400 »» 1500 GeV 1500 GeVmmGG ¸̧ 200 GeV 200 GeV
~~
S. Su DOE Review, 2004 6
Collider Phenomenology Collider Phenomenology
SWIMP Dark MatterSWIMP Dark Matter
no signals in direct / indirect dark matter searchesno signals in direct / indirect dark matter searches
SUSY NLSP:SUSY NLSP: rich collider phenomenologyrich collider phenomenology
NLSPNLSP in SWIMP in SWIMP: : long lifetime long lifetime stable inside the detectorstable inside the detector
Charged slepton Charged slepton highly ionizing track, almost background freehighly ionizing track, almost background free
Distinguish from stau NLSP and gravitino LSP in GMSBDistinguish from stau NLSP and gravitino LSP in GMSB ssneutrino neutrino and neutralino and neutralino NLSP NLSP missing energymissing energy
ssignal: energetic jets/leptons + missing energyignal: energetic jets/leptons + missing energy
Does it decay into gravitino or not?Does it decay into gravitino or not?
Is Is the lightest SM superpartner sneutrino or neutralino?the lightest SM superpartner sneutrino or neutralino?
S. Su DOE Review, 2004 7
Model Independent Study of DM collider searches Model Independent Study of DM collider searches
Charged WIMPCharged WIMP
Two charged track, BG freeTwo charged track, BG free
Guaranteed detectionGuaranteed detection
J. Feng, F. Takayama (UC Irvine)
Dark Matter (DM) relic densityDark Matter (DM) relic density
Annihilation cross section: Annihilation cross section: DM DM !! SM particle) SM particle)
Production cross section: Production cross section: Tevatron: Tevatron: pp pp !! DM) DM)
LHC: LHC: pp pp !! DM) DM)LC: LC: ee++ee-- !! DM) DM)
--
S. Su DOE Review, 2004 8
Model Independent Study of DM collider searches Model Independent Study of DM collider searches
neutral neutral WIMPWIMP
DM: missing energy signalDM: missing energy signal
Much more difficultMuch more difficult
Irreducible background: Irreducible background: +jet (or +jet (or ))
J. Feng, F. Takayama (UC Irvine)
Dark Matter (DM) relic densityDark Matter (DM) relic density
Annihilation cross section: Annihilation cross section: DM DM !! SM particle) SM particle)
Production cross section: Production cross section: Tevatron: Tevatron: pp pp !! DM) DM)
LHC: LHC: pp pp !! DM) DM)LC: LC: ee++ee-- !! DM) DM)
--Production cross section: Production cross section: Tevatron: Tevatron: pp pp !! DM+jet) DM+jet)
LHC: LHC: pp pp !! DM+jet) DM+jet)LC: LC: ee++ee-- !! DM+ DM+))
--
S. Su DOE Review, 2004 9
Precision Study of SUGRA, GMSB and AMSB Precision Study of SUGRA, GMSB and AMSB
Tevatron/LHC/LC could measure sinTevatron/LHC/LC could measure sin22 and m and mWW precisely precisely
SUGRA, GMSB and AMSB contribute differently to sinSUGRA, GMSB and AMSB contribute differently to sin22 and m and mWW
S. Heinemeyer (CERN), G. Weiglein (IPPP, Durham)
SUGRA GMSB
S. Su DOE Review, 2004 10
Phenomenology of Warped SUSY GUT Model Phenomenology of Warped SUSY GUT Model
Rich particle spectra around TeV scaleRich particle spectra around TeV scale
C.W. Chiang (NCU), T. Han (U. Wisconsin), L.T. Wang (Harvard)
How do we know it is warped SUSY GUT?How do we know it is warped SUSY GUT? observe SUSY particleobserve SUSY particle observe GUT particleobserve GUT particle
Goldberger, Nomura and Smith, PRD67, 075021 (2003)Nomura and Smith, PRD 68, 075003 (2003)
MSSMMSSM SUSY SU(5) SUSY SU(5) GUTGUT
Extra-DimExtra-Dim
4D4D
SUSYSUSY
S. Su DOE Review, 2004 11
Phenomenology of Warped SUSY GUT Model Phenomenology of Warped SUSY GUT Model C.W. Chiang (NCU), T. Han (U. Wisconsin), L.T. Wang (Harvard)
A321,Axy
321
q~~
lL~~ llRR !! E ETT + l + l~~ //
xyxy, stable,, stable,tracktrack
S. Su DOE Review, 2004 12
Propagation of High Energy Stau Propagation of High Energy Stau
Long lifetime stau could be produced in high energy cosmic rayLong lifetime stau could be produced in high energy cosmic ray relatively small production cross sectionrelatively small production cross section
It could be detected in current/future neutrino telescopeIt could be detected in current/future neutrino telescope effective detection volume enhanced by its longer effective detection volume enhanced by its longer traveling distancetraveling distance
Photonuclear effectPhotonuclear effect
Pair productionPair production
BremsstrahlungBremsstrahlung
dominatedominate
M. H. Reno(U. IOWA), I. Sarcevic (UA)
Important to understand the energy loss of Important to understand the energy loss of stau when it penetrates the earthstau when it penetrates the earth
Albuquerque, Burdman, Chacko, PRL92, 221802 (2004)
S. Su DOE Review, 2004 13
MSSM Contribution to Precision Observables MSSM Contribution to Precision Observables
SUSY contributes to both high (Z-pole) and low (below Z-pole) SUSY contributes to both high (Z-pole) and low (below Z-pole) precision observablesprecision observables
Oblique parameters for Z-pole observables are not Oblique parameters for Z-pole observables are not good approximation when new physics is near EW scale.good approximation when new physics is near EW scale.
Systematic study of MSSM contribution to Z-pole observablesSystematic study of MSSM contribution to Z-pole observables
Review paper on “Precision Supersymmetry”Review paper on “Precision Supersymmetry”
Z-pole and collider studiesZ-pole and collider studies Neutral Current studies below the Z-poleNeutral Current studies below the Z-pole Charge current universality and weak decayCharge current universality and weak decay Flavor physics and CP violationFlavor physics and CP violation Higgs physicsHiggs physics
M. Ramsey-Musolf (Caltech)
S. Su DOE Review, 2004 14
Research and Collaborations Research and Collaborations
New candidate of dark matter: superWIMPNew candidate of dark matter: superWIMP J. Feng, F. Takayama (UC Irvine)
Model independent study of collider DM searchesModel independent study of collider DM searches J. Feng, F. Takayama (UC Irvine)
Precision study of SUGRA, GMSB and AMSBPrecision study of SUGRA, GMSB and AMSB S. Heinemeyer (CERN), G. Weiglein (IPPP, Durham)
Propagation of high energy stauPropagation of high energy stau M. H. reno (U. of IOWA), I. Sarcevic (UA)
Phenomenology of warped SUSY GUT modelPhenomenology of warped SUSY GUT model C.W. Chiang (NCU), T. Han (U. Wisconsin), L.T. Wang (Harvard)
MSSM contribution to precision observablesMSSM contribution to precision observables M. Ramsey-Musolf (Caltech)
