NeutralinoDarkMatter:update NeutralinoDarkMatter:update - - PowerPoint PPT Presentation

NeutralinoDarkMatter:update NeutralinoDarkMatter:update

• ndirectandindirectdetection
• ndirectandindirectdetection

StefanoScopel http://newton.kias.re.kr/~scopel

Outline Outline ofthetalk

• fthetalk

gauginononuniversality&neutralinomass cosmologicallowerboundonmχ from WMAP directsearches indirectsearches

• χ

≤

“γ γ γ γ ”, N.Fornengo,L.PieriandS.Scopel, Phys.Rev.D70,103529(2004) “

• ”,A.Bottino,F.Donato,N.Fornengo,S.

Scopel,Phys.Rev.D70,015005(2004) “”, A. Bottino,F.Donato,N.Fornengo,S.Scopel,Phys.Rev.D69, 037302(2004) “ ”,A.Bottino, F.Donato,N.Fornengo,S.Scopel,Phys.Rev.D68,043506 (2003) “”, A.Bottino,N.Fornengo,S. Scopel,Phys.Rev.D67,063519(2003)

• Theneutralinoisdefinedasthelowest9mass

linearsuperpositionofbinoB,winoW(3) andthe twohiggsinostatesH10,H20:

2 1 1 1 ) 3 ( 2 1

~ ~ ~ ~ H a H a W a B a + + + ≡ χ

neutral,colourless,onlyweak9typeinteractions stable ifR9parityisconserved,thermalrelic nonrelativisticatdecoupling→ ColdDarkMatter (requiredbyCMBdata+structureformation models) relicdensitycanbecompatiblewithcosmological

• bservations: 0.095≤ χh2≤ 0.131

→IDEALCANDIDATEFORCOLDDARKMATTER ~

~

~ ~

MostanalysisontheSUSYmodelassumethat gaugino softmassesunifyattheGUTscale Gaugino massunificationimpliesalowerbound

• ntheneutralino mass:

Howevertheassumptionofgauginomass unificationattheGUTscalemightnotbe justified(forinstance,thegauginounification scalemaybemuchlowerthanthestandard GUTscale)

EffectiveMSSMscheme(effMSSM) EffectiveMSSMscheme(effMSSM)– – Independent Independent parameters parameters

• M1U(1) gauginosoft

breakingterm

• M2SU(2)gauginosoft

breakingterm

• Higgsmixingmass

parameter

• tan β ratiooftwoHiggs

v.e.v.’s

• mAmassofCPoddneutral

Higgsboson(theextended HiggssectorofMSSM includesalsotheneutral scalarsh,H,andthe chargedscalarsH±)

• mq softmasscommon

toallsquarks

• ml softmasscommon

toallsleptons

• Acommon

dimensionlesstrilinear parameterforthe thirdfamily(Ab =At≡ Amq;Aτ ≡ Aml)

• R≡ M1/M2

~ ~

~

~ ~ ~ ~

SUGRA→R=0.5

Lowerlimitontheneutralinomassfrom Lowerlimitontheneutralinomassfrom

GeV 36 ≥

χ

m

!

R

0.5

Experimentalconstraints Experimentalconstraints

acceleratorsdataonsupersymmetricandHiggs bosonsearches(CERNe+e9 colliderLEP2and ColliderDetectorCDFatFermilab) measurementsoftheb→ sγ decay measurementofthemuonanomalousmagnetic moment aµ≡(*µ-/ (weuse ≤ µ

µ µ µ ⋅

⋅ ⋅ ⋅≤ (τ+edata combined), M.Davieretal.,Eur.Phys.J.C31 (2003)503;K.Hagiwaraetal.,hep9ph/0312250) BS→+ - decay,D.Acostaetal.(CDF Collaboration),PRL93,032001(2004),V.M.Abazov etal.(D0Collaboration),PRL94,071802,(2005))

B BS

S→

→

+ +

• decay

decay

SUSYcontributionstronglyenhancedathightanβ andlowmA (∝ (tanβ)6/mA

4)

(C.Bobeth,T.Ewerth,F.KrugerandJ.Urban, PRD64(2001)074014)

tanβ – enhancedSUSYQCDcorrectionstobYukawa couplingincluded

B BS

S→

→

+ +

• decay

decay

Excluded configurations Strongcorrelationwithdirectdetectionsignals (S.Baek, Y.G.Kim,P.Ko,JHEP0502:067,2005;S.Baek,D.G. Cerdeño,Y.G.Kim,P.KoandC.Muñoz,hep9ph/0505019)

Signofb Signofb9 9>s >sγ γ amplitude amplitude

• themeasurementofB(B9>XsP P)issensitivetothe

signoftheb9>sγ amplitudeC7:

• BelleandBABARdatafavouranegativesignofC7(sameof

thestandardmodel) (Gambino,Haisch,Misiak,PRL94,061803(2005))

• sizeableSUSYcorrection(lightstopandchargino,hightan β)

candriveC7 topositivevaluescompatibletoBR(b9>sγ)but potentiallyinconflictwithB(B9>Xs P P) (notinSUGRA)

• b9>sγ decay depends on |C7|2

DarkmatterdensityfromWMAP DarkmatterdensityfromWMAP

• CMBdata,usedincombinationwithothercosmological
• bservations,arenarrowingdowntherangeofthematter

abundanceSmh2andsomeofitsconstituents,Sνh2 andSbh2:

0.095<CDMh2<0.131 0.095<CDMh2<0.131

• Theupperbound(7CDMh2)max establishesastrictupperlimitfor

anyspecificcoldspecies

• Thelowerbound(7CDMh2)maxfixesthevalueoftheaverage

abundancebelowwhichthehalodensityofaspecificcold constituenthastoberescaledascomparedtothetotalCDMhalo density

Rescalingfactor: ξ≡ ρχ/ ρ0 ≡min(1, 7χh2/(7CDMh2)min)

ρχ = localneutralinodensity;ρ0 = totallocaldarkmatterdensity (2σ range)

Cosmologicallowerboundon Cosmologicallowerboundonm mχ

χ (low

(low m mA

A)

)

upperboundon 7CDMh2 scatterplot: fullcalculation curve:analytical approximationfor minimal7CDMh2

Cosmologicallowerboundon Cosmologicallowerboundonm mχ

χ (

(m mA

A > 200 GeV

> 200 GeV) )

upperboundon 7CDMh2 scatterplot: fullcalculation curve:analytical approximationfor minimal7CDMh2

Thebottomline:thecosmologicallowerbound

• n mχ dependsonthevalueofmA:

mχ >6GeVforlightmA mχ >22GeVforheavymA

(7CDMh2)max=0.131 (7CDMh2)max=0.3

SEARCHES SEARCHES

" "

• Directsearches.Elasticscatteringofχ offnuclei

(∝ WIMPlocaldensity) χ + ? → χ + ?

• Indirectsearches.Signalsdueto χ 9 χ annihilations

χ + χ → → ν, ν, γ, p, e+, d − − − g g f f W+W- ZZ HH, hh, AA, hH, hA, HA, H+H- W+H-, W-H+ Zh, ZH, ZA − Annihilationstakingplaceincelestialbodieswhere χ’s havebeenaccumulated: ν’s → up9goingµ’sfromEarth andSun AnnihilationstakingplaceintheHalooftheMilkyWayor thatofexternalgalaxies: enhancedinhighdensityregions (∝ (WIMPdensity)2) ⇒ Galactic center,clumpiness

• Directsearches.Elasticscatteringofχ offnuclei

(∝ WIMPlocaldensity) χ + ? → χ + ?

• Indirectsearches.Signalsdueto χ 9 χ annihilations

g g f f W+W- ZZ HH, hh, AA, hH, hA, HA, H+H- W+H-, W-H+ Zh, ZH, ZA −

#$ #$ (∝ WIMP(localdensity)2)

χ + χ → keepdirectionality ν, ν γ (continuum) γ line(Zγ) − searchesforrare componentsincosmicrays ( diffusion) p e+ D − _

Neutralinodirectdetection

Elasticrecoilofnonrelativistichaloneutralinosoff thenucleiofanundergrounddetector RecoilenergyofthenucleusinthekeVrange Yearlymodulationeffectduetotherotationofthe EartharoundtheSun(therelativevelocitybetween thehalo,usuallyassumedatrestintheGalactic system,andthedetectorchangesduringtheyear)

c

x

x

Theelasticcrosssectionis boundedfrombelow: → “funnel” atlowmass

Neutralino– nucleoncrosssection

• !
• 7χh2 <0.095

× × × × 7χh2 >0.095

DAMAmodulationregion,likelyhoodfunctionvaluesdistant morethan4σ fromthenullresult(absenceonmodulation) hypothesis,Riv.N.Cim.26n.1(2003)1973, astro9ph/0307403

Neutralino– nucleoncrosssection

• !
• 7χh2 <0.095

× × × × 7χh2 >0.095 Theelasticcrosssectionis boundedfrombelow: → “funnel” atlowmass

Neutralino– nucleoncrosssection

CDMS,D.S.Akeribetal.,PRL93,211301(2004) Edelweiss,A.Benoitetal.,Phys.Lett.B545,43 (2002);V.Sanglardetal.,astro9ph/0503265 Upperlimitsfromdirectsearches assumptions: isothermalsphere, v0=220km/sec, ρ0=0.3GeV/cm3 CRESSTlimit(similartoEdelweiss),Angloheretal.,astro9 ph/0408006

%&'()*+,-(.)/**-

wrongdirection toexplainDAMA

However,sometrivialconsiderations: for mχ ≥ 25 GeV capture on DAMA is dominated by the I target → WIMPS above threshold in DAMA are also above threshold in CDMS - Edelweiss Ge for mχ ≤ 25 Ge captureonDAMAisdominatedbythe Natarget→ WIMPSabovethresholdinDAMAcanbe belowthresholdintheCDMS9 EdelweissGe CompatibilityDAMA CompatibilityDAMA9 9CDMS CDMS9 9Edelweiss? Edelweiss? Nocombinedanalysisofallexperimentsavailable → GelminiandGondolo,hep9ph/0504010,compatibility bothforathermalizedmaxwellian(lightWIMP)andforhigh velocity(extragalactic?)streams(notSgrstream,wrong direction)

GelminiandGondolo,hep9ph/0504010

Compatibleregion

importantparameter:vescape=650km/sec

6GeV<mχ <8GeV,σ(nucleon)

scalar=fewχ 1097nbarn

canwemakeit? compatibleregion: previousslides: 6GeV<mχ <8GeV,σ(nucleon)

scalar≈6χ 1098nbarn

but:

• π9nucleonsigmatermΣ≈64MeV

(Ellis,Olive,Santoso,Spanos,hep9ph/0502001) weusedΣ≈45MeV 9>factorof2enhancement

• inflattenedhalomodelsρloc ≈1GeV/cm3(even

higherforhighvaluesoftherotationalvelocity) 9>factorof3enhancementcomparedtoρloc =0.3 GeV/cm3 hardbutstillpossible

CompatibilitybetweenCDMSandlow CompatibilitybetweenCDMSandlow massneutralinos massneutralinos

x

x

Neutralino– nucleoncrosssection

v0=220km/sec UpperlimitfromCDMSusingadifferentvelocitydistribution assumptions: NFW,anisotropicvelocity dispersion ρ0=0.2GeV/cm3 v0=270km/sec v0=170km/sec

00 " 123&1&# 0#""

modelused inprevious example

modelused inprevious example

Auniversaldistributionfunctionforrelaxed Auniversaldistributionfunctionforrelaxed collisionlessstructures? collisionlessstructures? (S.H.Hansen,B.Moore,M.Zemp

andJ.Stadel,astro9ph/0505420)

• Arecentanalysis(HMZS)has

extractedthevelocitydistribution function(DF)fromalargerangeof numericalsimulations,wherethe initialconfigurationsinclude isotropicandhighlynon9isotropic structures,aswellascosmological CDMstructures.

• Allstructureshaveincommonthat

theyhavebeenperturbedviolently (head9onmergers)andsubsequently allowedtorelax,andrangefrom almostsphericaltohighlytriaxial.

• TheauthorsfindthattheDFhasa

universal shape,whichdependsonly

• nonefreeparameter,thetotal

velocitydispersionσtot. q=0.8,k3=0.95

Maxwellian HMZSFit

• “flattopped”shape
• cut9offathighvelocity

12 . 2 1 v

3

≈ − ≤ q k

τοτ

σ

N.Fornengo,S.Scopel,PLB576(2003)189

x

χ χ γ,e+ d p,

4 A

1 m

ann ∝

σ

WIMP indirect detection: annihilations in the halo WIMP indirect detection: annihilations in the halo

= χ f χ f χ f χ

A (Higgs)

f example:

Neutralinoselfannihilationsanddarkmatter densitydistribution

Signalsdependquadraticallyonthedarkmatterdensityρ. Commonparametrization:

=darkmatterlocaldensity a=scalelength

(α,β,γ)=(2,2,0)Isothermal (α,β,γ)=(1,3,1)NFW,∝ r91 inGC (α,β,γ)=(1.5,3,1.5)Mooreetal.,∝ r91.5inGC LargedifferencesinthebehaviourtowardsGC

N.B.Anyway,currentsimulationsnotreliableforradiismallerthan0.1– 1kpc Numericalsimulationsuggestthenon9singularform:(J.F.Navarro etal.,Mon.Not.Roy.Astron.Soc.349,1039(2004 ))

, d(ln(ρ))/d(ln(r)) ρ92≡ ρ(r92) r=r92 =92 α≈0.17

• urreference

model

Gammaraysfromneutralinopairannihilations Gammaraysfromneutralinopairannihilations <σannv>≡annihilationcrosssectiontimerelativevelocity mediatedoverthegalacticvelocitydistribution ,ψ=anglebetweenl.o.s andG.C Integrationalongthelineofsight: Bψ ≡ telescopeaperture strongdependenceonprofile,lessrelevantinotherdirections TowardGC

particlephysics andastrophysics arefactorized

EGRET excess toward GC?

• S. D. Hunter et al., Astrophys. J. 481, 205 (1997)

estimatedbackground,D.L.Bertschetal., Astrophys.J.+(.)587(1993)

Gammafluxduetoneutralino annihilationfromGalacticCenter

lowmass “funnel” nobounds

Gammafluxduetoneutralino annihilationfromGalacticCenter

lowmass “funnel”

• 4

Gammafluxduetoneutralino annihilationfromGalacticCenter

• 4

Backgroundrescaledby10% Neutralinocontribution Signal+background

mχ=30GeV

Ithasalreadybeenshownthatneutralinoswithmχ>50GeV couldexplaintheEGRETexcess (A.Cesarini,F.Fucito, A.Lionetto,A.MorselliandP.Ullio,astro9ph/0305075) CouldtheEGRETexcessbeexplainedalsobylightneutralinos? YES

enhancementrequired comparedtoNFW

mχ=40GeV

Backgroundrescaledby10% Neutralinocontribution Signal+background Ithasalreadybeenshownthatneutralinoswithmχ>50GeV couldexplaintheEGRETexcess (A.Cesarini,F.Fucito, A.Lionetto,A.MorselliandP.Ullio,astro9ph/0305075) CouldtheEGRETexcessbeexplainedalsobylightneutralinos? YES

enhancementrequired comparedtoNFW

EGRETresidualfluxathighlatitudes aftersubtractionofknowncomponents (identifiedsources,spectrumdue tocosmicraysinteractionwith thegalacticdisk) P.Sreekumaretal., Astrophys.J.+5+,523(1998) extragalacticorigin? …orexoticproduction?

Gammafluxduetoneutralinoannihilation fromhighlatitudes

EGRETresidualflux, P.Sreekumaretal.,Astrophys.J.+5+,523(1998) RegionA: |b|>100,|l|>400 100<|b|<300 lowmass “funnel”

RegionB: |b|>860 Re9analysisofEGRETdata, U.Keshet,E.Waxman,A.Loeb,astro9ph/0306442

Gammafluxduetoneutralinoannihilation fromhighlatitudes

"

Clumpiness? γ signalsfromhighaltitudesturnouttobeone

• rderofmagnitudebelowpresentsensitivities.

ContrarytoGC,inthiscaseIBψ ispractically independentonthehaloprofile.

Gammafluxduetoneutralinoannihilation fromhighlatitudes

Effectdiscussedbyseveralauthors,sometimeswithsignal improvementsatthelevelofa fewordersofmagnitude. However,recentanalyticalinvestigationontheproductionof small9scaledarkmatterclumpssuggestthattheclumpiness effectwouldnotbelarge.Enhancementeffectonthe

• annihilationsignalslimitedtoafactorofafew. Similar

conclusionsalsoreachedwithhigh9resolutionnumerical simulations.(V.Berezinsky,etal.,Phys.Rev.D68,103003(2003);F.

Stoheretal.,Mon.Not.Roy.Astron.Soc.,+-,1313(2003)).

Externalgalaxies Externalgalaxies

44LGnearestgalaxiesinGalacticcoordinates. Thesizeofeachsymbolisscaledtotheγ9ray fluxemittedbyahostDMhalowithaMoore profilewithinaviewingangleof1°fromthe halocenter.

(N.Fornengo,L.PieriandS.Scopel,PRD70,103529(2004)) (N.Fornengo,L.PieriandS.Scopel,PRD70,103529(2004)) Fluxvs.anglefromGC

Galacticforeground

Wefocusonthe3most prominentgalaxiesat largeanglesformtheGC, LMC (LargeMagellanic Cloud)M31(Andromeda) andM87(VirgoA)

ModelingDarkMatterHalos

• NFW97, Navarro,Frenk,White,Astrophys.J.490,493(1997)
• M99,Moore,Ghigna,Governato,Lake,Quinn,Stadel,

Tozzi,Astrophys.J.524,L19,(1999)

• M04,Diemand,Moore,Stadel,Mon.Not.Roy.Astron.Soc.

353(2004)624

ModelingDarkMatterHalos

Effect of baryons on the inner parts of galaxies Effect of baryons on the inner parts of galaxies The effect of baryon is still not well known: it may either enhance or disrupt the central cusp:

• adiab-NFW profile includes adiabatic growth of a central

black hole which pulls in DM and enhances an initial NFW profile (Ullio, Zhao, Kamionkowski, PRD64, 043504 (2001))

• but formation of a SBH binary (by merging of halos) leads

to a depletion of the central spike (Merrit at al., PRL88, 191301 (2002))

1 1

• minimalradiusrcut withinwhichthe

selfannihilationrateisequaltothe dynamicaltime(Berezinskietal.,PLB294(1992)221):

1099 ÷ 1098kpc (M99profile) rcut≈ 10914 ÷ 10913kpc(NFW97profile)

• effectofbaryons:presenceofBHerases

DMwithin3× 1099 kpc(MW)and3× 1097 kpc (M87)

• includingothereffects,liketidalinteractions,

thecentralcoreofgalaxiescanreach0.1– 1kpc

numericalsimulationsreliabledownto≈0.1kpc

Integratedgamma Integratedgamma9 9rayflux(galacticcenter,NFW97profile) rayflux(galacticcenter,NFW97profile) Ethreshold=50GeV Ethreshold=100GeV

• NFW97→ Μ99 : fluxesencreasedbyafactor≈ 160
• Ethreshold 50→ 100GeV:fluxesdecrease1orderofmagnitude

Integratedgamma Integratedgamma9 9rayflux(M31,M99profile) rayflux(M31,M99profile) Ethreshold=50GeV Ethreshold=100GeV samefluxlevelasGCwithNFW97,butusingM99profile

5 5σ σ sensitivitycurvesforsatelliteand sensitivitycurvesforsatelliteandČ Čerenkovdetectors erenkovdetectors Galacticcenter Andromeda(M31)

background

NeutralinoNFW97 N e u t r a l i n

• M

9 9 N e u t r a l i n

• M

9 9 extragalacticbackground

Theoreticalcurves:BR(Wbosons)=BR(Higgs)=50%

• highestpossiblesignalfromM31wellbelowexperimental

sensitivityandmerelyatthelevelofbackground

• signalfromCGaccessibletoGLASTandVERITASonlyif

profileharderthanNFW97

Comparisonwithdata(galacticcenter) Comparisonwithdata(galacticcenter)

EGRET CANGAROO

b a c k g r

• u

n d b a c k g r

• u

n d

• excessbothfromEGRET(1GeV<E<20GeV)andfor

CANGAROO(E>200GeV) M99 NFW97

NFW97 M99

M99+NFW97 coudbothexcessesbe explainedatthesame timebyneutralino?

• no. EGRETpossibly

explainedby30<mχ<60 GeV, CANGAROOby1<mχ <2TeV,M99x2.5 needed(spectrumtoo hardforEGRET). coudbothexcessesbe explainedatthesame timebyneutralino?

Comparisonwithdata(galacticcenter) Comparisonwithdata(galacticcenter)

• excessbothfromEGRET(1GeV<E<20GeV)andfor

CANGAROO(E>200GeV) EGRET CANGAROO M99x2.5 HoweverCANGAROO excesscouldpossibly beexplainedwithout conflictwithEGRET

HESSdatafromgalacticcenter HESSdatafromgalacticcenter muchharderspectrum,wouldrequire10TeV<mχ <20TeV

FluxfromM87galaxy FluxfromM87galaxy

whipple (upperlimit)

HEGRA

extragalacticbackground

1

• T

e V

• n

e u t r a l i n

• ,
• M

9 9 no.enhancementofclumpydistributionatmostfactorof 5,neutralinosignalalwaysexpectedbelowbackground possibleexcessdetected,couldbeexplainedbyneutralino?

Conclusions9 1

Relicneutralinoswithmassesmχ < 45GeVare allowedinMSSMmodelswithoutgaugino9mass unificationattheGUTscale. Thecosmologicallowerboundontheneutralinomass fromWMAPCMBdatacombinedwithother measurementsismχ ≥ 6GeV. Formχ < 20GeV variousdirectandindirectneutralino signalsareboundedfrombelow(low9mass ``funnel”). Theseneutralinos,mainlyaB– H1 mixture,are compatiblewiththefinalmodulationresult presentedbytheDAMACollaboration(108000kgday exposure). ~ ~

Conclusions9 2

WIMPdirectexperimentswithcryogenicdetectors providesevereconstraints9 low9massneutralinos windowstillallowed Astrophysicaluncertaintiesmustbetakeninto accountwhencomparingdifferentexperimental results. CurrentdatafromexperimentsofWIMPindirect searches(p's,γ's,up9goingP's),ifinterpreted conservatively,donotyetsetconstraintsonlight neutralinos.

_

Incaseofsteepdistributionsofdarkmatterinthe galacticcenter,neutralinosofmassesaround30940 GeVcouldexplaintheEGRETexcess.

signalfromexternalgalaxies(LMC,M31, M87)possiblyaboveextragalacticbackground, butwellbelowpresentsensitivities CANGAROOexcesstowardGCcanbe explainedby1TeVneutralino,2.5xM99 required,noconflictwithdataatlower energies(EGRET) EGRETandGANGAROOexcesscannotbe explainedatthesametime

Conclusions9 3