Direct’ditection’of’wino’Dark’Matter’...
Transcript of Direct’ditection’of’wino’Dark’Matter’...
Direct ditection of wino Dark Matter in the High-‐scale SUSY
Natsumi Nagata
Based on J. Hisano, K. Ishiwata, Natsumi Nagata, Phys. Lett. B690, 311 (2010) and 1210.5985 .
2 November, 2012 Na.onal Tsing Hua University
Nagoya University
Outline
1. Introduction
2. Direct detection of Majorana dark matter
3. Calculation & Results
4. Summary
Introduction Observational evidence for dark matter (DM)
Galactic scale
Cosmological scale
Scale of galaxy clusters
About 80% of the matter in the Universe is nonbaryonic dark matter.
Begeman et. al. (1991).
Komatsu et. al. (2010).
hAp://map.gsfc.nasa.gov/
Clowe et. al. (2006).
Introduction Weakly Interacting Massive Particles (WIMPs)
One of the most promising candidates for dark matter is
Weakly Interacting Massive Particles (WIMPs)
• have masses roughly between 10 GeV ~ a few TeV.
• interact only through weak and gravita.onal interac.ons.
• Their thermal relic abundance is naturally consistent with the cosmological observa.ons [thermal relic scenario].
• appear in models beyond the Standard Model.
SUSY SM
Supersymmetric (SUSY) Standard Model (SM)
One of the promising candidates for physics beyond the SM.
LHC results • Stringent limits are imposed on the masses of
SUSY par.cles
• 125 GeV Higgs boson requires sufficient radia.ve correc.ons in the Minimal Supersymmetric Standard Model (MSSM)
High-‐scale SUSY ??
High-‐scale SUSY
High-‐scale SUSY scenario has a lot of fascina.ng aspects from a phenomenological point of view.
125 GeV Higgs boson can be achieved
SUSY CP/flavor problems are relaxed
Gravi.no problem is avoided
Gauge coupling unifica.on
This scenario also accommodates the existence of Dark Matter (DM) .
(sufficient radia.ve correc.ons)
(suppressed by sfermion masses)
(heavy gravi.no)
(sfermions form SU(5) mul.plets)
Assump.on
A chiral supermul.plet X responsible for SUSY is charged under some symmetry.
SUSY is transferred via operators involving X† X
Sob masses of the scalar par.cles arise from
(MPl: the reduced Planck scale)
VEV of X field Scalar/gravi.no mass
Gaugino mass
Anomaly media.on L. Randall and R. Sundrum (1998) G.F. Giudice, M.A. Luty, H. Murayama, R. Rattazzi (1998)
Wino is the lightest in the gaugino sector
Since the field X is charged under some symmetry, the gaugino mass terms are not given by the X field linear terms.
In this case, the gaugino masses are generated by
Higgsinos
We regard the higgsino mass as a free parameter in the following discussion.
(e.g., Peccei-‐Quinn symmetry)
Origin of Higgsino mass is somewhat model-‐dependent.
On the assump.on of a generic Kahler poten.al
It can be suppressed by some symmetry.
Higgsinos can be much lighter than the gravi.no.
Gravi!noScalar Par!cles Higgsinos
Gauginos
Gluino
BinoWino
Mass spectrum
3 TeV
103 TeV
30 TeV 10 TeV
Thermal relic
J. Hisano, S. Matsumoto, M. Nagai, O. Saito, M. Senami (2006).
Higgsinos can be light
Higgs mass
The 125 GeV Higgs boson mass is easily accounted.
mt= 173.2 ± 0.9 GeV M. Ibe, T.T. Yanagida (2012).
tan�50
tan�5
tan�2
tanΒ�1 ΜH � MSUSY
10 100 1000 104110
115
120
125
130
135
140
MSUSY�TeV
mh�GeV
Small tanβ is favored
125 GeV
Mo.va.on
• Although sfermions may be beyond the reach of the LHC, wino DM can be searched in the DM detection experiments. Especially,
• The discovery of 125 GeV Higgs boson allows us to make a robust prediction for the detection rate.
• It is found that both the tree-‐level and the loop-‐level processes give rise to sizable contributions.
Direct detec.on experiments are promising
• Xenon100 collabora.on gives a stringent constraint on spin-‐independent elas.c WIMP-‐nucleon scaAering cross sec.on.
• Ton-‐scale detectors for direct detec.on experiments are expected to yield significantly improved sensi.vi.es.
Introduction Direct Detection Experiments
]2WIMP Mass [GeV/c6 7 8 910 20 30 40 50 100 200 300 400 1000
]2W
IMP-
Nuc
leon
Cro
ss S
ectio
n [c
m
-4510
-4410
-4310
-4210
-4110
-4010
-3910
]2WIMP Mass [GeV/c6 7 8 910 20 30 40 50 100 200 300 400 1000
]2W
IMP-
Nuc
leon
Cro
ss S
ectio
n [c
m
-4510
-4410
-4310
-4210
-4110
-4010
-3910
DAMA/I
DAMA/Na
CoGeNT
CDMS
EDELWEISS
XENON100 (2010)
XENON100 (2011) Buchmueller et al.
(for WIMPs of mass 50 GeV)
[XENON100 collabora.on, arXiv: 1104. 2549]
WIMP DM
Nucleus
Recoil energy
Effective Lagrangian for Majorana Dark Matter
χ̃0 : DM mq : quark mass M : DM mass
€
LG = fG ¯̃χ0χ̃0GaµνG
aµν
+fqmq¯̃χ0χ̃0q̄q
Spin-‐dependent interac.on
Spin-‐independent interac.on
Twist-‐2 operator Scalar-‐type interaction
• Couplings of DM with “nucleon mass”
• Nucleon matrix element is evaluated with lattice simulations
• Couplings of DM with “quark momentum”
• Parton Distribution Functions (PDF)
Twist-‐2-‐type interac.on
Gluon contribution
The gluon contribu.on turns out to be comparable to the quark contribu.on even if the DM-‐gluon interac.on is induced by higher loop diagrams.
Scalar-‐type interac.ons, , induce fqmqχ̄χq̄q fGχ̄χGaµνG
aµν
The couplings of DM with “nucleon mass”
Nucleon matrix elements:
mN : nucleon mass
1−�
q=u,d,s
fTq ≡ fTG
By using the trace anomaly of the energy momentum tensor in QCD,
This enhancement originates from the large gluon contribu.on to the nucleon mass.
gluon
u sd
Mass frac.ons for proton
Diagrams Tree-‐level
!̃0 q
q!̃0
h
!̃0
!̃0
g
g
! Higgsh
Q
!̃0 q
q!̃0
Z
! axial-tree``Higgs” contribu.on
Effec.ve coupling
(Zij: Neutralino mixing matrix)
The SI effective interaction is not suppressed even if the Wino mass is much larger than the W boson mass.
χ̃− : charged winoWµ : W boson
g2 : weak coupling constant
Pure Wino DM Quark contribution | 1-‐loop
h0
!" 0 !" 0 !" 0 !" 0!"# !"#
W- W- W-
q q’ q
(a) (b)
q q
J. Hisano, S. Matsumoto, M. Nojiri, O. Saito, Phys. Rev. D 71 (2005) 015007.
Lint = −g2( ¯̃χ0γµχ̃−W †
µ + h.c.)
The gauge interaction:
χ̃0 : DM
1-‐loop diagrams:
Remark:
(a) ``Scalar” (b) ``twist-‐2”
!" 0 !" 0!"#
Q/q
Q’/q’W- W -
g g
!" 0 !" 0!"#
W- W-
QQ’
g g
(b) (c)
h0
!" 0 !" 0!"#
W-
(a)
Qg g
Pure Wino DM Gluon contribution | 2-‐loop
J. Hisano, K. Ishiwata, and N. Nagata, Phys. LeA. B 690 (2010) 311.
2-‐loop diagrams:
``Gluon” contribu.on
Results
-2
-1.5
-1
-0.5
0
0.5
1
1 10 100 1000
f p (1
0-9 G
eV-2
)
| | - M2 (TeV)
Wino-like DM (M2 = 3 TeV, lattice)
1 10 100 1000| | - M2 (TeV)
scalartwist-2gluonHiggs
! !
< 0! > 0!
tanβ = 1, 2, 5, 50 tanβ = 1, 2, 5, 50 (from top to boAom) (from boAom to top)
There is a cancellation among these contributions
Effec.ve coupling with a proton
Results
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
|!| - M2 (TeV)
Wino-like DM (M2 = 3 TeV, !>0, lattice)
tan"=1.1
1 10 100 1000|!| - M2 (TeV)
tan"=2
1 10 100 1000|!| - M2 (TeV)
tan"=50TotalTree
ScaAering cross sec.ons with a proton
• Cancellations between tree-‐ and loop-‐level contributions occur at a certain value of μ
• Loop contribution is dominant in a wide range of parameter region
Results
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
|!| - M2 (TeV)
Wino-like DM (M2 = 3 TeV, !<0, lattice)
tan"=1.1
1 10 100 1000|!| - M2 (TeV)
tan"=2
1 10 100 1000|!| - M2 (TeV)
tan"=50TotalTree
ScaAering cross sec.ons with a proton
Tree-‐level contribution interferes constructively to the loop contribution in the case of low tanβ
J. Hisano, K. Ishiwata, and N. Nagata, arXiv:1210.5985.
Summary
• We evaluate the wino-‐DM elastic scattering cross sections in the High-‐scale SUSY scenario.
• Electroweak loop contribu.on is dominant in a wide range of parameter region.
• There is a cancella.on between tree-‐ and loop-‐level contribu.ons and it significantly reduces the scaAering cross sec.ons.
• The resultant cross sec.ons might be within a reach of future experiments.
Split SUSY
N. Arkani-Hamed, S. Dimopoulos (2004).
The SUSY scale is much higher than the EW scale. The spectrum below the SUSY scale contains
The SM par.cles (1 Higgs douplet)
Bino Wino Gluino Higgsino
Gauge coupling unifica.on Existence of DM
SUSY Flavor/CP problem
OK !!
Gauge coupling unifica.on
6 8 10 12 14 16
20
30
40
50
Good enough !!
N. Arkani-Hamed, S. Dimopoulos (2004).
α-‐1
sfermions ・・・ SU(5) mul.plets
do not affect unifica.on @ 1-‐loop
(The other Higgs doublet makes a small contribu.on)
Wino dark maAer
Then, what determines the SUSY scale ??
(Naturalness for the EW scale is not in our hand, any more)
The amount of dark maAer abundance !!
0
0.1
0.2
0.3
1 2 3m (TeV)
Non perturbativePerturbative
WMAP
J. Hisano, S. Matsumoto, M. Nagai, O. Saito, M. Senami (2006).
The second moments of the parton distribu.on func.ons (PDFs)
mN : nucleon mass
Nucleon matrix elements
�N |mq q̄q|N�/mN ≡ fTq ,
• The mass frac.ons ( for the scalar-‐type quark operators)
1−�
q=u,d,s
fTq ≡ fTG
• For the twist-‐2 operators
Trace anomaly of energy-‐momentum tensor in QCD
mQQ̄Q
g g
Q
M. A. Shifman, A. I. Vainshtein and V. I. Zakharov, Phys. LeA. B 78 (1978) 443.
The matrix element of gluon field strength tensor can be evaluated by using the trace anomaly of the energy-‐momentum tensor in QCD
Θµµ =
β(αs)
4αsGa
µνGaµν +
�
q=u,d,s
mq q̄q +�
Q=c,b,t
mQQ̄Q
The trace anomaly of the energy-‐momentum tensor in QCD (Nf=3)
mN
�
q=u,d,s
mNfTq
mNfTG = −9αs
8π�N |Ga
µνGaµν |N�
Heavy quark contribution
Gluon contribution
SI coupling of Majorana DM with nucleon
The effective coupling of DM with nucleon is given as follows:
Leff = fN ¯̃χχ̃N̄N
The gluon contribu.on can be comparable to the quark contribu.on even if the DM-‐gluon interac.on is induced by higher loop diagrams.
Suppressed by αs
gluon
u sd
Mass frac.ons for proton
Elastic scattering cross section
mT : the mass of the target nucleusnp : the number of protonnn : the number of neutron
From now on, we just show the results for the SI cross sec.on of WIMP DM with a proton as a reference value.
One can derive the SI cross section by using the SI effective couplings as follows :
Loop contribu.ons only
10-48
10-47
10-46
10-45
100 1000
SI cr
oss s
ectio
n (cm
2 )
Wino mass (GeV)
Wino DM
130GeV
115GeV
J. Hisano, K. Ishiwata, and N. Nagata, Phys. LeA. B 690 (2010) 311.
The SI cross section is almost independent of the wino mass.
Results Wino LSP
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
|!| - M2 (TeV)
Wino-like DM (M2 = 200 GeV, !<0, lattice)
tan"=1.1
1 10 100 1000|!| - M2 (TeV)
tan"=2
1 10 100 1000|!| - M2 (TeV)
tan"=50TotalTree
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
|!| - M2 (TeV)
Wino-like DM (M2 = 200 GeV, !>0, lattice)
tan"=1.1
1 10 100 1000|!| - M2 (TeV)
tan"=2
1 10 100 1000|!| - M2 (TeV)
tan"=50TotalTree
Results Higgsino LSP
-2
-1.5
-1
-0.5
0
0.5
1
1 10 100 1000
f p (1
0-9 G
eV-2
)
M2 - | | (TeV)
Higgsino-like DM (| | = 1 TeV, lattice)
1 10 100 1000M2 - | | (TeV)
scalartwist-2gluonHiggs
! !
< 0! > 0!
!
tanβ = 1, 2, 5, 50 tanβ = 1, 2, 5, 50 (from top to boAom) (from boAom to top)
Results Higgsino LSP
10-50
10-49
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
M2 - |!| (TeV)
Higgsino-like DM (|!| = 1 TeV, !<0, lattice)
tan"=1.1
1 10 100 1000M2 - |!| (TeV)
tan"=2
1 10 100 1000M2 - |!| (TeV)
tan"=50TotalTree
10-50
10-49
10-48
10-47
10-46
10-45
1 10 100 1000
SI cr
oss s
ectio
n (cm
2 )
M2 - |!| (TeV)
Higgsino-like DM (|!| = 1 TeV, !>0, lattice)
tan"=1.1
1 10 100 1000M2 - |!| (TeV)
!
tan"=2
1 10 100 1000M2 - |!| (TeV)
!
tan"=50TotalTree
Results
1
10
100
1 10 100
M2 (
TeV)
|!| (TeV)
!<0, lattice tan"=1.1
1 10 100|!| (TeV)
tan"=2
1 10 100|!| (TeV)
tan"=50!
10 44-10 45-
10 47-
10 47-10 44- 10 46-10 45-10 47-
10 48-
10 46-
10 48-
10 48-10 45-
10 46-
10 45-
10 46-
10 48-
10 47-
10 46-10 45-
10 47-
10 47-
10 48-
10 46- 10 48-
10 46-10 47- 10 48-
10 46-10 47- 10 48-
10 48-
10 47-
XENON10010 47-@60GeV
10 48- @60GeV
1
10
100
1 10 100
M2 (
TeV)
|!| (TeV)
!>0, lattice tan"=1.1
1 10 100|!| (TeV)
tan"=2
1 10 100|!| (TeV)
tan"=50!
10 44-10 45-
10 47-
10 47-10 48-10 44- 10 46-10 45- 10 47-10 48-
10 46-
10 48-
10 44-10 45-
10 47-
10 47-10 48-10 44- 10 46-10 45- 10 47-10 48-
10 46-
10 48-
10 44-10 45-
10 47-
10 47-10 44- 10 46-10 45-10 47-
10 48-
10 46-
10 48-
10 48-
10 47-
10 47-
10 48-
10 46- 10 48- 10 47-
10 47-
10 48-
10 46- 10 48-10 47-
10 47-
10 48-
10 46- 10 48-
XENON100
10 47- @60GeV
10 48- @60GeV