gravitino dark matter
DESCRIPTION
Gravitino Dark matter. the darkest dark matter. Coupling / 1/m pl no signal for direct/indirect DM searches can not be produced at colliders. Shufang Su • U. of Arizona Aspen Winter Conference 2005. New proposal: superWIMP DM. not very exciting. naturally obtain - PowerPoint PPT PresentationTRANSCRIPT
Gravitino Dark matterGravitino Dark matter
Shufang Su • U. of ArizonaShufang Su • U. of Arizona
Aspen Winter Conference 2005Aspen Winter Conference 2005
the darkest dark matterthe darkest dark matter
Coupling Coupling // 1/m 1/mplpl
no signal for direct/indirect DM searchesno signal for direct/indirect DM searches can not be produced at colliderscan not be produced at colliders
not very excitingnot very excitingNew proposal: New proposal: superWIMP superWIMP DMDM naturally obtain naturally obtain
solve BBN solve BBN 77Li anomalyLi anomaly Could be tested at collidersCould be tested at colliders
S. Su Gravitino Dark Matter 3
Gravitino Gravitino
Gravitino: superpartner of gravitonGravitino: superpartner of graviton
Obtain mass when SUSY is spontaneously broken Obtain mass when SUSY is spontaneously broken mmGG »» F/m F/mplpl
Stable when it is LSP Stable when it is LSP - candidate of Dark Matter- candidate of Dark Matter
~~
mmG G »» m mSUSYSUSY
»» GeV – TeV GeV – TeV
coldcold Dark Matter Dark Matter
~~mmGG ¿¿ m mSUSYSUSY
» » keVkeV
warmwarm Dark Matter Dark Matter
~~
S. Su Gravitino Dark Matter 4
Gravitino: warm dark matter Gravitino: warm dark matter
mmG G ¿¿ m mSUSYSUSY (GMSB)(GMSB)
~~ hh22 »» (m (mGG/keV) (100/g/keV) (100/g**))
mmGG »» keV : keV : warmwarm Dark Matter Dark Matter
mmGG keV : keV : problematic !problematic !
gravitino dilution necessarygravitino dilution necessary
stringent bounds on reheating temp. stringent bounds on reheating temp.
~~
~~
Moroi, Murayama and Yamaguchi, PLB303, 289 (1993)
~~
S. Su Gravitino Dark Matter 5
Gravitino cold dark matter Gravitino cold dark matter
mmG G »» m mSUSYSUSY »» GeV – TeV GeV – TeV (supergravity)(supergravity)
~~
thermalthermalLSPLSP vv-1-1
((weak weak coupling)coupling)-2-2
GG~~
~~ ll~~ LSPLSP
WIMPWIMP thermalthermalLSPLSP vv-1-1
((gravitational gravitational coupling)coupling)-2-2
GG~~~~ ll
~~LSPLSP
● vv too smalltoo small
● ththGG too big too big
overclose the Universeoverclose the Universe unless Tunless TRHRH 10 101010 GeV GeV
~~
superWIMPsuperWIMPDMDM
G G LSP + SM LSP + SM
BBN constraints:BBN constraints: TTRHRH 10 1055 – 10 – 1088 GeV GeV
Conflict with thermal leptogenesis:Conflict with thermal leptogenesis: TTRHRH 3 3 ££ 10 1099 GeV GeV
~~
Bolz, Brandenburg and Buchmuller,NPB 606, 518 (2001)
Kawasaki, Kohri and Moroi, asrtro-ph/0402490, astro-ph/0408426
Buchmuller, Bari, Plumacher, NPB665, 445 (2003)
S. Su Gravitino Dark Matter 6
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
S. Su Gravitino Dark Matter 7
SuperWIMP and SUSY WIMP SuperWIMP 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 Gravitino Dark Matter 8
Constraints Constraints
NLSP NLSP G + SM particles G + SM particles~~
Dark matter density Dark matter density GG ·· 0.23 0.23~~
CMB photon energy distributionCMB photon energy distribution
Big bang nucleosynthesisBig bang nucleosynthesis
Late time EM/had injection could Late time EM/had injection could change the BBN prediction of change the BBN prediction of light elements abundanceslight elements abundances
SWIMPSWIMP=(m=(mSWIMPSWIMP/m/mNLSPNLSP) ) ththNLSPNLSP
10-10 = 6.1 0.4
Fields, Sarkar, PDG (2002)
S. Su Gravitino Dark Matter 9
BBN constraints on EM/had injection BBN constraints on EM/had injection
EM,hadEM,had==EM,hadEM,had Br BrEM,hadEM,had YYNLSPNLSP
Decay lifetime Decay lifetime NLSPNLSP
EM/had energy releaseEM/had energy release
» » mmNLSPNLSP-m-mGG~~
Cyburt, Ellis, Fields and Olive, PRD 67, 103521 (2003)
EMEM
EM
(G
eV)
around a yeararound a year
Kawasaki, Kohri and Moroi, astro-ph/0402490
hadhad EMEM
S. Su Gravitino Dark Matter 10
slepton and sneutrino NLSP slepton and sneutrino NLSP
G G = (m= (mGG/m/mNLSPNLSP) ) ththNLSPNLSP~~ ~~
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
J. Feng, F. Takayama, S. Suhep-ph/0404198, 0404231
S. Su Gravitino Dark Matter 11
superWIMP in mSUGRA superWIMP in mSUGRA
BBN EM constraints only
Stau NLSP
Ellis et. al., hep-ph/0312262
superWIMP allowed regionsuperWIMP allowed region
Usual WIMP allowed regionUsual WIMP allowed region
S. Su Gravitino Dark Matter 12
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
GMSB: gravitinoGMSB: gravitino m m »» keV keV warm not cold DMwarm not cold DM
collider searches:collider searches: other sparticle (mass)other sparticle (mass)
(GMSB) (GMSB) ¿¿ (SWIMP):(SWIMP): distinguish experimentallydistinguish experimentally
Distinguish from stau NLSP and gravitino LSP in GMSBDistinguish from stau NLSP and gravitino LSP in GMSB
Feng and Smith, in preparation.
S. Su Gravitino Dark Matter 13
Guaranteed signal at colliders Guaranteed signal at colliders
Birkedal, matchev, Perelstein, PRD 70, 077701 (2004).
Model independent approach: Model independent approach: DMDM < < v> v>annann productionproduction
Feng, SS, Takayama, in preparation
superWIMP:superWIMP: promising event rates at LHC/LC.promising event rates at LHC/LC.
Usual WIMP:Usual WIMP: missing energy + jet or photonmissing energy + jet or photon irreducible SM backgroundirreducible SM background
preliminarypreliminary preliminarypreliminary
S. Su Gravitino Dark Matter 14
Sneutrino and neutralino NLSP Sneutrino and neutralino NLSP
ssneutrino neutrino and neutralino and neutralino NLSP NLSP missing energymissing energy
ssignal: energetic jets/leptons + missing energyignal: energetic jets/leptons + missing energy
angular distribution of events angular distribution of events (LC)(LC)
Does it decay into gravitino or not?Does it decay into gravitino or not?
sneutrino case: sneutrino case: most likely gravitino is LSPmost likely gravitino is LSP
neutralino case: neutralino case: most likely neutralino LSPmost likely neutralino LSP
vs.vs.
Is Is the lightest SM superpartner sneutrino or neutralino?the lightest SM superpartner sneutrino or neutralino?
direct/indirect dark matter searchdirect/indirect dark matter search positive detection positive detection disfavor gravitino LSP disfavor gravitino LSP
precision determination of SUSY parameter: precision determination of SUSY parameter: thth,,
,, 0.23 0.23 favor gravitino LSP favor gravitino LSP
S. Su Gravitino Dark Matter 15
NLSPNLSP
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
NLSPNLSPSMSM
~~GG
SMSM
Buchmuller et. al., hep-ph/0402179Hamaguchi and Ibarra, hep-ph/0412229Feng et. al., Hep-ph/0405248
Slepton trapping:Slepton trapping:Hamaguchi et. al. hep-ph/0409248Feng and Smith, hep-ph/0409278
● Decay life time Decay life time
● SM particle energy/angularSM particle energy/angular distributiondistribution……
mmGG
mmplpl
LFV LFV
… …
~ ~
S. Su Gravitino Dark Matter 16
Slepton trapping Slepton trapping
Slepton could live for a year, so Slepton could live for a year, so can be trapped then moved can be trapped then moved to a quiet environment to to a quiet environment to observe decaysobserve decays
Courtesy of J. Feng
LHC: 10LHC: 1066 slepton/yr possible, but slepton/yr possible, but most are fast. By optimizing trap most are fast. By optimizing trap location and shape, can catch location and shape, can catch »» 100/yr in 1000m100/yr in 1000m33 water water
LC: tune beam energy to LC: tune beam energy to produce slow sleptons, can catch produce slow sleptons, can catch 1000/yr in 1000m1000/yr in 1000m33 water water
Feng and Smith, hep-ph/0409278
S. Su Gravitino Dark Matter 17
ConclusionsConclusions
Gravitino could be Gravitino could be warmwarm DM: DM: m m »» keV keV
Gravitino could be Gravitino could be coldcold DM: DM: m m »» few hundred GeV few hundred GeV
thermal production: Tthermal production: TRHRH 10 101010 GeV GeV Non-thermal production: superWIMPNon-thermal production: superWIMP
SuperWIMP:SuperWIMP: gravitinogravitino LSP LSP WIMP:WIMP: sleptonslepton/sneutrino//sneutrino/neutralinoneutralino
Constraints from BBN: EM injection and Constraints from BBN: EM injection and hadronichadronic injectioninjection
viable parameter spaceviable parameter space
Rich collider phenomenologyRich collider phenomenology (no direct/indirect DM (no direct/indirect DM signal)signal) ccharged slepton:harged slepton: highly ionizing trackhighly ionizing track ssneutrinoneutrino/neutralino/neutralino:: missing energymissing energy
Slepton trappingSlepton trapping
WIMP WIMP superWIMP + SM superWIMP + SM particleparticle