ダークマターとctacta.scphys.kyoto-u.ac.jp/workshop/20100109/presentations/kohri_cta... ·...
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ダークマターとCTA
Physics Department, Tohoku University Physics Department, Tohoku University
(郡 和範)Kazunori KohriKazunori Kohri
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http://map.gsfc.nasa.gov/media/060916
Dark Matter?
2CDM 0.1Ω ∼h
0
ii
c
ρρ
Ω ≡
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What is Dark Matter?• It is massive (ρ∝a-3)
• It is stable (τ>> 10 18 sec)
• It does not scatter off photons so much( Is it a bound-state?)
• It is neutral (from experiments of sea water m<106 GeV)
• The velocity dispersion is small [cold dark matter (CDM)]
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Candidate of particle (cold) dark matter• Stable or long-lived new particle
• Oscillating scalar field
• Neutralino• Gravitino• Right-handed sneutrino• Axino• …
• Axion• Moduli• …
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Another candidates
• Primordial black hole• Brown dwarf• WIMPZILLA• Integral constant in Horava-Lifshitz gravity• Quark nugget (strange-quark matter)• Solutions in (relativistic-) Modified
Newtonian Dynamics (MOND)• …
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Rotation curve
二間瀬敏史著 「なっとくする宇宙論」
( )M r r∝ Begeman, Broils,Sandars etal (91)
Dark Halo
gas
Stars (visible component)
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Gravitational lens in colliding cluster of galaxies
• Red: Baryon observed by X-ray produced by bremsof thermal electron
• Blue: DM observed by gravitational lens
(2007)
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Time-evolution of fluctuation III
Ma and Bertschinger (95)
See also 松原隆彦 「シリーズ 現代の天文学3 宇宙論 II 宇宙の進化」
-6 -5 -4 -3 -2 -1
Log a
(II) Horizon reentry before matter-radiation equality epoch
∝a
∝a2
aEQ
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Cluster baryon fraction
• Cluster can have a representative distribution in the Universe of both baryon and DM
• Ωbh2 is independently known, fgas was observed by X-ray from Oxygen
Ωm~ 0.2
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Combined Figure
Riess et al (98), Lahav-Liddle PDG (09)
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Fermion Boson
Introduction toIntroduction to SUSYSUSYSupersymmetry (SUSY)
Solving “Hierarchy Problem”
Realizing “Coupling constant unification in GUT”
quark squark
lepton slepton
gravitino graviton
photino photonneutralino
Depending on SUGRA models
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12-13 orders of magnitude !!!
Hierarchy ProblemsHierarchy Problems
≈ 14 1510 - 10 GeVXM
≈ 2 310 -10 GeVWM
GUT-scale
Weak-scale
Higgs mass 22 20 2
2 ( )Wd Vm O Md
ϕϕ υλ
ϕ= ≈ ≈
( )ϕ λ ϕ ϕ υ= −2† 2 /2V
where Higgs’s potential
ϕ
Vϕ
~υc.f) Masses of fermions and vector bosons
ψ ψ ϕ ϕ~ , ~Zm h m g
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Radiative correction to Higgs mass Radiative correction to Higgs mass in Quantum Field Theoryin Quantum Field Theory
ϕδ λΛ + Λ2 2 2 2~m gλϕ ϕ
ϕ
ϕ ϕg g
W
Λ 15Cut off scale ~ ~ 10 GeVXM
+
( )ϕδ22 15~ 10 GeV ?m
Quadratic divergence
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How can we resolve the problem?How can we resolve the problem?Weak scale in the tree level, ( )
( )21
220
2 5
2~ 10 GeV
~ 10 GeV
m
mϕ
ϕ
δ
( )ϕϕ ϕ δ+
222 2 15 0 ~~ 10 GeV ?m mm
To retain the hierarchy, we require an accidental cancellation,
( )ϕ ϕ ϕ ϕδ δ δ+ + + +22 2 2 2 2
0 1 2 3 ... ~ 10 GeV ?m m m m
⎡ ⎤⎣ ⎦215(10 GeV)O
Fine tuning!Fine tuning!
In total,
$ 10,110,087,734,958.95-) $ 10,110,087,734,957.70
$ 1.25
GDP in USA (2002)?
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Solution in SUSYSolution in SUSYIn exact SUSY, the quadratic divergence is canceled by both boson and fermion loops.
2thϕ ϕ
t
+ 0=ϕ ϕ
tth th
Exact SUSY2 2
2
1(4 ) thπ
Λ2 22
1 (4 ) thπ
− Λ
Even if SUSY,
ϕδπ
⎛ ⎞Λ⎜ ⎟⎜ ⎟⎝ ⎠
∼ 2
2
22 2
2
1ln
(4 )t
t
th m
mm
We don’t need a fine tuning when
∼ ∼ ∼2 2 2... ( )t Wb
mm OM
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SUSY GUTSUSY GUT
The coupling constants are unified at
≈ 1610 GeVXM
A lot of new particles ,which do not obey the asymptotic free, appear at
μ ≥ 210 GeVMartin, ”A Supersymmetry Primer”
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Lightest SUSY particle (LSP)• R-parity conservation
i)Decay
ii) Pair annihilation/production
τ χ τ→ +
χ χ+ ↔ +f f
(-1) (-1)×
(-1)× (-1)
(+1)
(+1) ×(+1)
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Thermal freezeoutBoltzmann equation
frezeout
3χ σ∼ Hn
v
( )2
20.10.1
TeVχ
σ⎛ ⎞⎜ ⎟Ω ⎜ ⎟⎜ ⎟⎝ ⎠
∼v
h
Freezeout / 30χ∼T m
Ωχ does not depend on mχ
Kolb & Turner
Predicting TeV Physics!!! 26 33 10 /v cm sσ −= ×
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Positron Excess (PAMELA satellite reported)
Adriani et al, arXiv:0810.4995v1 [astro-ph]
/ ( ~0.6 proton diffusion)e e E δ δ+ − −∝
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Electron and positron flux by ATIC2
Chang et al (08)
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Electron and positron flux by Fermi
Abdo et al, Fermi LAT Collaboration, arXiv:0905.0025, PRL102 (09) 181101
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Hisano, Kawasaki,
Kohri, Moroi, Nakayama (09)
Positron excess
in DM annihilation
Diffusion model
Fitted to B/C ratio
24 23 310 10 /v cm sσ − −−∼
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Hisano, Kawasaki,
Kohri, Moroi, Nakayama (09)
Electron/positron cutoff
in DM annihilation
23 310 /v cm sσ −∼
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Kawasaki, Kohri, Nakayama (09)Gamma-ray signal from GC by DM annihilation
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Kawasaki, Kohri, Nakayama (09)
Extragalactic diffuse Gamma-ray by DM annihilation
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Fitting by Papucci and StrumiaPapucci, Strumia, arXiv:0912.0742 [hep-ph]
See also Chen, Mandal and F. Takahashi, arXiv:0910.2639 [hep-ph]
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CTA?
Courtesy of Kazunori Nakayama
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Result of Papucci and StrumiaPapucci, Strumia, arXiv:0912.0742v1 [hep-ph]
Extragalactic diffuse-gamma
CTA?
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Direct detection by CDMSII
2recoil
1~ ~ (10)keV2μE v O
-3~ 220km/s (v/c~10 )v
Ge DM
Ge DM
~ m mm m
μ+
Ge 72.6 um =
Ge DMm m
arXiv:0912.3592v1 [astro-ph.CO]
M < O(100) GeV? (Farina et al)
Background
0.8 ±0.1(stat) ±0.2(syst)
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arXiv:0912.5038v1 [hep-ph]Marco Farina, Duccio Pappadopulo, Alessandro Strumia
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ConclusionConclusion• Fermi may not exclude the possible scenarios
for the positron/electron excess by the DM annihilation/decay because of the upper limit on the sensitivity (<300 GeV)
• CTA will be able to verify those scenarios
• CTA may have a sufficient sensitivity to detect gamma-rays associated with DM annihilation even with its canonical annihilation cross section (~3×10-26 cm3/s)