dark matter: why, where, what, how?
DESCRIPTION
N. Bernal, P. Binetruy, D. Cerdeno, E. Dudas, A. Falkowski, A. Goudelis, O. Lebedev, C. Munoz, E. Nezri, S. Pokorski, A. Romagnoni. Dark Matter: Why, Where, What, How?. Yann Mambrini Laboratoire de Physique Théorique Orsay, Université Paris XI. - PowerPoint PPT PresentationTRANSCRIPT
Dark Matter:Dark Matter:
Why, Where, What, How? Why, Where, What, How?
Yann Mambrini Laboratoire de Physique Théorique Orsay, Université Paris XI
Krakow, January 6th 2010
N. Bernal, P. Binetruy, D. Cerdeno, E. Dudas, A. Falkowski, A. Goudelis, O. Lebedev, N. Bernal, P. Binetruy, D. Cerdeno, E. Dudas, A. Falkowski, A. Goudelis, O. Lebedev, C. Munoz, E. Nezri, S. Pokorski, A. Romagnoni C. Munoz, E. Nezri, S. Pokorski, A. Romagnoni
IV)IV) Two SUSY candidates : neutralino and gravitinoTwo SUSY candidates : neutralino and gravitino
I)I) The DM puzzleThe DM puzzle
II)II) Direct Detection : principle, experiment and predictionDirect Detection : principle, experiment and prediction
V)V) Complementarity with accelerator physics (LHC, ILC)Complementarity with accelerator physics (LHC, ILC)
III)III) Indirect detection : principle, experiment and predictionIndirect detection : principle, experiment and prediction
OverviewOverview
VII)VII) Conclusions and PerspectivesConclusions and Perspectives
VI)VI) Extra U(1) candidate and sommerfeld effectExtra U(1) candidate and sommerfeld effect
Dark Matter EvidencesDark Matter Evidences
CMB (WMAP)CMB (WMAP) Galactic ScaleGalactic Scale
SUSY : neutralino, gravitino.. SUSY : neutralino, gravitino.. (Jungman)(Jungman)
KK modes (Extra Dim.) KK modes (Extra Dim.) (Servant, Tait)(Servant, Tait)
Extra U(1) boson Extra U(1) boson (Arkani-Ahmed, Weiner)(Arkani-Ahmed, Weiner)
Sterile right handed neutrino Sterile right handed neutrino (Shaposhnikov)(Shaposhnikov)
Weak scale scalar Weak scale scalar (Tytgat)(Tytgat)
Astroparticle (part 0) : data....Astroparticle (part 0) : data....
WMAPWMAP : 0.094 < : 0.094 < hh<<0.1290.129
DAMA excess, direct detection (< 10 GeV DM)DAMA excess, direct detection (< 10 GeV DM)
INTEGRAL : 511 keV line excess (< MeV DM)INTEGRAL : 511 keV line excess (< MeV DM)
HEAT : Positron excess, (100 GeV DM)HEAT : Positron excess, (100 GeV DM)
EGRET : gamma excess (100 GeV DM)EGRET : gamma excess (100 GeV DM)
HESS, gamma excess (10 TeV DM)HESS, gamma excess (10 TeV DM)
PAMELA/ATTIC (> 1 TeV DM)PAMELA/ATTIC (> 1 TeV DM)
CDMS (10-100 GeV DM)CDMS (10-100 GeV DM)
Astroparticle (part I) : Relic Density (Astroparticle (part I) : Relic Density ())
= = -3 H n -3 H n (H = R / R)(H = R / R)..
Boltzmann EquationBoltzmann Equation
.. dndn dtdt
I
J
- < - < v> n v> n22[ [ - n- neqeq ] ]22
h ~ ~ 0.1 h ~ ~ 0.1 3.10 cm s 3.10 cm s
< < v > v >
-1-1 33 22 -27-27
XENON (1 evt per kg per year) : 10 kg – 100kg – 1TXENON (1 evt per kg per year) : 10 kg – 100kg – 1T
U U
H
NUCLEUSNUCLEUS
Direct Detection : principleDirect Detection : principle
FERMI (2008)FERMI (2008)
HESS (Namibie, 2004)HESS (Namibie, 2004)
d 1 dN1 dN < < v > v > d d d E d E 2 dE2 dE44 M M
∫∫ dldl22==
(cm , s ) ~ 10(cm , s ) ~ 10 1010 -13-2 -1 < < v > (100 GeV) v > (100 GeV)
10 cm s M10 cm s M22
22
-29-29 33 -1-1 J ∆J ∆
h ~ ~ 0.1 h ~ ~ 0.1 →→~~1010 J J 3.10 cm s 3.10 cm s
< < v > v >
-1-1 33 -11-11 22 -27-27
Indirect detection from GCIndirect detection from GC
Positrons fluxPositrons flux
1 dNe+1 dNe+ 2 dEe+2 dEe+
==QsourceQsource
MM< < v > v >
e+
e-
22
[particle/cm3] df(E,r)[particle/cm3] df(E,r) dtdt
== QQsourcesourceK(E) * K(E) * f(E,r) f(E,r) ++
3 kpc3 kpc
20 kpc20 kpc
Dsource (E) ~ Dsource (E) ~ E*K(E)E*K(E) b(E)b(E)
~ 1.8 (E/1GeV)~ 1.8 (E/1GeV)-0.2-0.2
..db(E)db(E) dEdE
* f(E,r) * f(E,r) ++
[Salati][Salati]
SUSY for dummiesSUSY for dummies
~~Hd (Higgsino down)Hd (Higgsino down)
~~Hu (Higgsino up)Hu (Higgsino up)
~~B ( Bino)B ( Bino)
~~W ( Wino)W ( Wino)
BB
WW
HdHd
HuHu
BosonsBosons FermionsFermions
(Stau)(Stau) LL = M = M11 BB + M BB + M22 WW + WW + Hu Hd Hu Hd
~~~~ ~~ ~~ ~~ ~~
+M+MZZ B Hu + M B Hu + MZZ W Hd + M W Hd + M22staustau ~~ ~~~~~~~~~~
Neutralino : Neutralino : ii= Z= ZiBiB B + Z B + ZiWiW W + Z W + Ziuiu Hu + Z Hu + Zidid Hd Hd
Neutralino Dark MatterNeutralino Dark Matter
M1 M1 0 . . 0 . . 00 M2M2 . . . . . . 0 -μ. . 0 -μ . . . . -μ-μ 0 0
~~ ~~ ~~ ~~WW HdHd HuHu
M=M=
WW~~
HH++~~
BB
M = 2 mM = 2 m
large tanlarge tanBinoBino
AA
AA ff
ff11
StauStau ZZ
tautau
22M ~ mM ~ m
BinoBino
StauStau
++WW
ZZ
33
M ~ mM ~ m
HiggsinoHiggsino
++
The relic density constraintsThe relic density constraints
M0M0
M1/2M1/2
Neutralino Neutralino ≡≡ HiggsinoHiggsino
LightLight
High fluxesHigh fluxes
Neutralino Neutralino ≡≡ BinoBino
M1= M / 2M1= M / 2
High fluxesHigh fluxes
Neutralino Neutralino ≡≡ BinoBino
M1 = M / 2M1 = M / 2
Low fluxesLow fluxes
Complementarity between Complementarity between different detection modes different detection modes
ff
ff
qq qq
e-e-
e+e+
HEATHEATPamelaPamelaAMSAMS
EGRETEGRETHESSHESS
FERMIFERMI
CDMS XENONCDMS XENON
e-e-
e+e+
ILCILC
LHCLHC WMAPWMAP
Application to neutralino DM Application to neutralino DM
Gravitino DM Gravitino DM
In alternative scenario, the gravitino can be the lightest SUSY In alternative scenario, the gravitino can be the lightest SUSY particle (40 % of the SUSY publications in 2009)particle (40 % of the SUSY publications in 2009)
It can happen if the SUSY breaking is not gravitationally mediated It can happen if the SUSY breaking is not gravitationally mediated (Gauge Mediation, sequestred sector..) : the mass of the gravitino (Gauge Mediation, sequestred sector..) : the mass of the gravitino
is “liberated” from the SUSY spectrum is “liberated” from the SUSY spectrum
The gravitino couple only gravitationally with the visible sector : it The gravitino couple only gravitationally with the visible sector : it is stable and is produced in the reheating epoch of the universe : its is stable and is produced in the reheating epoch of the universe : its
thermal relic depends on the reheating temperature, thermal relic depends on the reheating temperature, hh22 ~ T ~ TRR / M / Mgravitinogravitino
BUT the next to lightest SUSY particle is long lived too because can BUT the next to lightest SUSY particle is long lived too because can only decay into SM + gravitino with gravitational type interaction :only decay into SM + gravitino with gravitational type interaction :
It can affect the primordial nucleosynthesis (BBN).It can affect the primordial nucleosynthesis (BBN).
MMstaustau
MMgravitinogravitino
BBN constraints BBN constraints
NLSP NLSP (stau)(stau)
SMSM(tau)(tau)
LSP LSP (gravitino)(gravitino)
1 / M1 / Mplanckplanck
=> Long lived NLSP => Long lived NLSP (> 5000 seconds)(> 5000 seconds)
tautau
neutrinoneutrino
BBNBBN
TTRR=10=1099 GeV GeV
TTRR=10=1077 GeV GeV
BBNBBN (5000 seconds)(5000 seconds)
Extra U(1) candidates
Sommerfeld Enhancement
ConclusionsConclusions
Several candidates can respect WMAP Several candidates can respect WMAP constraintsconstraints
Different experiments reach different parts of Different experiments reach different parts of the parameter space the parameter space
Strong correlation/complementarityStrong correlation/complementarity
Future sensitivity will be able to test 80 Future sensitivity will be able to test 80 percent of SUSY parameter spacepercent of SUSY parameter space
MMii ( r ( ri i ) r) rii = [ M = [ MCDMCDM ( r ( rff ) + M ) + Mbb (r (rf f )] r)] rff
N-Body simulationN-Body simulation(NFW, Moore..)(NFW, Moore..)
Today baryon Today baryon distributiondistribution??????
Baryon fall in the Galactic CenterBaryon fall in the Galactic Center
Redistribution of mass Redistribution of mass in the gravitational potentialin the gravitational potential
BaryonsBaryons
NeutralinosNeutralinos
(r) ~ 1/r (r) ~ 1/r (NFW (NFW compressed)compressed)
1.51.5
Baryon falls in the central region Baryon falls in the central region to form galaxyto form galaxy
ReReReReRedistribution of masses Redistribution of masses
in the gravitational potentialin the gravitational potential
( r )( r )arb. unitsarb. units
200200
100100
LogLog1010 ( r( r )) 00 11-1-1-2-2-3-3
NFWNFW
NFW NFW compressedcompressed
Adiabatique CompressionAdiabatique Compression
(r) ~ 1/r (r) ~ 1/r
Indirect detection : Mass measurementIndirect detection : Mass measurement
GLAST, 3yrsGLAST, 3yrs
XENON, 3 yrsXENON, 3 yrs
Complementarity Direct,Complementarity Direct,Indirect and ILCIndirect and ILC
SummarySummary
MasseMasse
50 GeV50 GeV
100 GeV100 GeV
175 GeV175 GeV
500 GeV500 GeV
Direct Direct detectiondetection
Indirect Indirect detectiondetection
LeptonicLeptoniccollidercollider
+/- 5 GeV+/- 5 GeV +/- 10 GeV+/- 10 GeV
+/- 10 GeV+/- 10 GeV +/- 20 GeV+/- 20 GeV +/- 40 GeV+/- 40 GeV
+/- 25 GeV+/- 25 GeV+/- 60 GeV+/- 60 GeV +/- 90 GeV+/- 90 GeV
The background The background
e-e-
e+e+
BackgroundBackgroundEE
Nbr evtsNbr evts
A leptonic collider as aA leptonic collider as aDark Matter detectorDark Matter detector
e-e-
e+e+
e-e-
e+e+ILCILCWMAPWMAP
KeKe
annann prodprod
Colinear or soft-gamma approximationColinear or soft-gamma approximation
Direct Detection : the backgroundDirect Detection : the background
XENON XENON
SUSYSUSY