s uper wimp dark matter
DESCRIPTION
S uper WIMP Dark matter. Gravitino from Slepton and Sneutrino Decays. Shufang Su • U. of Arizona. J. Feng, F. Takayama, S. Su Hep-ph/0404198. Outline. -. SWIMP dark matter and gravitino LSP Late time energy injection and BBN Slepton and sneutrino NLSP - PowerPoint PPT PresentationTRANSCRIPT
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SuperWIMP Dark matterSuperWIMP Dark matter
Shufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of ArizonaShufang Su • U. of Arizona
J. Feng, F. Takayama, S. SuHep-ph/0404198
Gravitino from Slepton and Sneutrino Decays
Gravitino from Slepton and Sneutrino Decays
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S. Su SWIMP 2
Outline Outline
SWIMP dark matter and SWIMP dark matter and gravitino LSPgravitino LSP
Late time energy injection and BBN Late time energy injection and BBN
Slepton Slepton and sneutrino and sneutrino NLSPNLSP– Dominant two body EM decay Dominant two body EM decay l l !! l+G l+G– Subdominant 3-body hadronic decaySubdominant 3-body hadronic decay– Viable parameter spaceViable parameter space
ConclusionConclusion
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S. Su SWIMP 3
Why gravitino not considered as CDM usually?
Why gravitino not considered as CDM usually?
ththGG vv-1-1 ( (gravitional gravitional coupling)coupling)-2 -2
(comparig to WIMP of (comparig to WIMP of weakweak coupling strength) coupling strength)
● vv too smalltoo small
● ththGG too big, overclose the Universe too big, overclose the Universe
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However, gravitino can get relic density by other However, gravitino can get relic density by other meansmeans
SuperWIMPSuperWIMP
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S. Su SWIMP 4
WIMPWIMP
SWIMPSWIMPSMSM
101066
WIMP SWIMP + SM particle WIMP SWIMP + SM particle
FRT hep-ph/0302215, 0306024
101044 s s t t 10 1088 s s
Gravitino LSPGravitino LSP
LKK gravitonLKK graviton
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S. Su SWIMP 5
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~~
Neutralino/Chargino Neutralino/Chargino NLSPNLSP
Slepton NLSP Slepton NLSP
BBNBBNEMEM
hadhad
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
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S. Su SWIMP 6
Different approach to gravitino superWIMP Different approach to gravitino superWIMP
NLSP NLSP G + SM particles G + SM particles~~
my talkmy talk Takayama’s talkTakayama’s talk
SWIMPSWIMP close universe close universe SWIMPSWIMP maybe maybe insiginificantinsiginificant
nnNLSPNLSP NLSPNLSP/m/mNLSPNLSP
1/m1/mSUSYSUSY
ththNLSPNLSP vv-1-1 m m22
SUSYSUSY
nnNLSPNLSP m mSUSYSUSY
NLSP: slepton,sneutrinoNLSP: slepton,sneutrino NLSP: slepton, NLSP: slepton, sneutrino, sneutrino,
neutralinoneutralino
fix fix SWIMP SWIMP = 0.23= 0.23 SWIMP SWIMP = m= mGG/m/mNLSP NLSP thth
NLSPNLSP~~
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S. Su SWIMP 7
Late time energy injection and BBN Late time energy injection and BBN
Fields, Sarkar, PDG (2002)
10-10 = 6.1 0.4
?? EM,hadEM,had==EM,hadEM,had B BEM,hadEM,had Y YNLSPNLSPEM, had energy injection:EM, had energy injection:
» » mmNLSPNLSP-m-mGG
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S. Su SWIMP 8
EM and Had BBN constraints EM and Had BBN constraints
Cyburt, Ellis, Fields and Olive, PRD 67, 103521 (2003)
Kawasaki, Kohri and Moroi,astro-ph/0402490
EM BBN constraintsEM BBN constraints had BBN constraintshad BBN constraints EM BBNEM BBN
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S. Su SWIMP 9
Slepton NLSP lifetime and EM injection
Slepton NLSP lifetime and EM injection
Decay lifetime Decay lifetime (sec)(sec)
l l G + l G + l, , !! G + G + ~~ ~~~~~~
EM energy injection EM energy injection EM EM (GeV)(GeV)
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S. Su SWIMP 10
Hadronic decay branching ratio Hadronic decay branching ratio
l l lZlZGG,,WGWG , , !! ZG, lWGZG, lWG~~ ~~~~~~ ~~ ~~
meson contribution
mNLSP
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S. Su SWIMP 12
Viable Parameter space Viable Parameter space
negligible EM BBN constraintsnegligible EM BBN constraints
200 GeV 200 GeV ·· m m ·· 400 400 »» 1500 GeV 1500 GeVmmGG ¸̧ 200 GeV 200 GeV
m m ·· 80 80 »» 300 GeV 300 GeV~~
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S. Su SWIMP 13
ConclusionsConclusions
SSuperuperWIMP is possible candidate for dark matterWIMP is possible candidate for dark matter
SUSY models: gravitino LSP (SWIMP) slepton NLSP (WIMP)SUSY models: gravitino LSP (SWIMP) slepton NLSP (WIMP)
Constraints from BBN: EM injection and hadronic injectionConstraints from BBN: EM injection and hadronic injection
need updated studies of BBN constraints on hadronic/EM injectionneed updated studies of BBN constraints on hadronic/EM injection
Favored mass region: (enlarged if Favored mass region: (enlarged if SWIMPSWIMP<0.23)<0.23)
Sneutrino:Sneutrino: m m 880-0-3300 GeV00 GeV m m 100 GeV 100 GeV
Charged Charged RR:: 200 GeV 200 GeV ·· m m ·· 1500 GeV, m 1500 GeV, mGG ¸̧ 200 GeV 200 GeV
500 GeV 500 GeV m mRR
• Rich collider phenomenologyRich collider phenomenology (no direct/indirect DM signal)(no direct/indirect DM signal) Charged slepton:Charged slepton: highly ionizing trackhighly ionizing track Sneutrino:Sneutrino: missing energymissing energy
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S. Su SWIMP 14
NLSPNLSP
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
SMSM
● Decay life time Decay life time m mplpl
● SM energy distributionSM energy distribution
mmGG
SUSY breaking scaleSUSY breaking scale
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