AMS-02 Kazunori Nakayama (University of Tokyo) - - PowerPoint PPT Presentation
AMS-02 Kazunori Nakayama (University of Tokyo) 2015/5/16, Current situation Excess in Positron and Electron flux : PAMELA/AMS-02 and Fermi No excess in gamma-rays : Fermi,
Kazunori Nakayama (University of Tokyo) 2015/5/16, 神戸大学
We are here
Energy (GeV)
0.1 1 10 100
))
+
(e
+
(e
0.01 0.02 0.1 0.2 0.3 0.4
Muller & Tang 1987 MASS 1989 TS93 HEAT94+95 CAPRICE94 AMS98 HEAT00 Clem & Evenson 2007 PAMELA
年 月 日木曜日
年 月 日木曜日
PAMELA Fermi
G.Giesen et al, 1504.04276
Kohri, Ioka, Fujita, Yamazaki, 1505.01236
Energy[GeV]
1 −
10 1 10
2
10
3
10
4
10 /P P
6 −
10
5 −
10
4 −
10
+
Conventional, W
PAMELA2014 AMS-02 background DM+background DM
Jin, Wu, Zhou, 1504.04604
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter)
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind Collision of nucleus
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind Collision of nucleus
Production of i from collision of j
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind Collision of nucleus
Production of i from collision of j
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind Collision of nucleus
Production of i from collision of j
) δ Vc(km/s) 0.85 13.5 0.70 12 0.46 5
L R
Model R(kpc) L(kpc) K0(kpc2/Myr) MIN 20 1 0.0016 MED 20 4 0.0112 MAX 20 15 0.0765
fi(E, x) : Distribution function of species i
∂ ∂tfi(E, x) =K(E)∇2fi(E, x) + ∂ ∂E [b(E)fi(E, x)] + Qi(E, x) − ∂ ∂z[Vc(z)fi(E, x)] − fi(E, x) τi +
Pji τj fj(E, x),
Diffusion due to tangled magnetic field Energy loss due to I.C. and synchrotron Source (Supernova, Dark Matter) Convective wind Collision of nucleus
Production of i from collision of j
Q(T, r) = q( r)dN¯
p(T)
dT
q( r) = 1 2 σv ρDM(| r|) mDM 2 for annihilating DM , q( r) = 1 τDM ρDM(| r|) mDM
p(T)
dT
: energy spectrum of anti-p from DM decay
1 2 σv ) = τDM : DM annihilation cross section, lifetime
,
r|)
: DM density profile in the Galaxy
Propagation of charged particle in tangled magnetic field
λ = K(E) c ∼ 1017cm
1GeV δ ∼ 0.1pc
r ∼
108 yr 1
2
E 1GeV δ
2
Charged particle escapes from diffusion zone after 10^7~10^8 yr. ≡ tesc Electron/positron loses energy before escape due to inverse Compton and synchrotron:
loss =
b(E) ∼ 1.8 kpc 1 GeV E (δ−1)/2
rloss
Primary/Secondary ratio Primary: Produced at Source (Proton, Carbon, ...) Secondary: Produced by primary CR-intersteller medium interaction (Anti-proton, Boron, ...) fprim fsec fsec fprim ∼ tint tesc Prim/Sec ratio determines escape time, but there is a degeneracy on K and L.
R [kpc] L [kpc] δ K0[kpc2/Myr] K0[cm2/s] Vc[km/s] MAX 20.0 15 0.46 0.0765 2.31 × 1028 5 MED 20.0 4 0.70 0.0112 3.38 × 1027 12 MIN 20.0 1 0.85 0.0016 4.83 × 1026 13.5
Anti-p of DM origin is Primary, not Secondary, hence anti-p flux of DM origin significantly depend on L.
Donato et al. (2004)
Jin, Wu, Zhou, 1504.04604
Kinetic Energy[GeV/n]
10
10 1 10
2
10
3
10 B/C
10 B/C
AMS-02 Conventional MIN MED MAX
Energy[GeV]
10 1 10
2
10
3
10 /P P
10
10
10 /P, Background P
PAMELA2014 AMS-02 Conventional MIN MED MAX
Jin, Wu, Zhou, 1504.04604
Anti-proton flux from DM : diffusion model dependence
Hamaguchi, Moroi, KN, 1504.05937
Astro BG Astro BG
tted), 10 (das d 2 × 1027 sec,
long-dashed), while th d 6 × 10−25 cm3/sec, 1 2 σv
τDM
) = mDM = 0.5, 1, 2, 10TeV
mDM = 1, 3, 10, 30TeV
Comparison with AMS-02 data
Wino Dark Matter
2.9TeV 1.7TeV 2.9TeV 1.2TeV Hamaguchi, Moroi, KN, 1504.05937 Ibe,Matsumoto,Shirai,Yanagida, 1504.05554
Wino : Superpartner
Most attractive DM candidate after discovery
Lightest SUSY particle in anomaly-mediation or pure gravity mediation. It can reproduce AMS-02 result with thermal relic DM scenario!!
10−27 10−26 10−25 10−24 10−23 10−22 100 1000 10000 hσvi [cm3s−1] MDM [GeV] 9 5 % U p p e r
n d ( M I N ) MED MAX b e s t fi t ( M I N ) M E D MAX F e r m i γ c
s t r a i n t hσvi(wino) H i g g s i n
Ibe,Matsumoto,Shirai,Yanagida, 1504.05554
Wino Dark Matter
Direct detection of Wino Dark Matter
Hisano, Ishiwata, Nagata, 1504.00915
but still challenging. ~2orders of magnitude below LUX level.
1 10 100 1000 104 10 50 10 49 10 48 10 47 10 46 10 45 10 44 10 43 10 42 10 41 10 40 10 39 10 38 10 37 WIMP Mass GeV c2 WIMP nucleon cross section cm2
CDMS II Ge (2009) Xenon100 (2012)
CRESST CoGeNT (2012) CDMS Si (2013)
E D E L W E I S S ( 2 1 1 )
DAMA
SIMPLE (2012) ZEPLIN-III (2012) COUPP (2012) LUX (2013) D A M I C ( 2 1 2 ) C D M S l i t e ( 2 1 3 ) 1 N e u t r i n
v e n t s 1 N e u t r i n
v e n t s 1 N e u t r i n
v e n t 3 N e u t r i n
v e n t s 3 N e u t r i n
v e n t s 3 Neutrino Events 1 Neutrino Event 30 Neutrino Events 10 Neutrino Events 100 Neutrino Events
Billard, Figueroa-Faliciano, Strigari, 1307.5458 Wino DM
MIN: Ε 8.8 106 MED:Ε 9.5 106 MAX:Ε 1.0 105
mΧ 2 TeV BG
10 50 100 500 1000 5000 1 5 10 50 100 500 1000
EGeV E3GeV2 m2s1sr1
MIN : v 85 keV MED : v 49 keV MAX : v 38 keV
mΧ 2 TeV
1 5 10 50 100 500 0.1 0.2 0.5 1.0 2.0 5.0 10.0
EkinGeV pp104
Chen, Chiang, Nomura, 1504.07848
Positron and Anti-proton excess can be simultaneously explained by some DM model.
Satellites: Galactic Center:
Pros: Good statistics Cons: confusion, diffuse BG
MW halo:
Pros: very good statistics Pros: Low BG and good source id Cons: low statistics Pros: very good statistics Cons: diffuse BG
Baltz+08
l l Extragalactic:
Pros: very good statistics Cons: diffuse BG, t h i l t i ti
Clusters: Spectral lines:
Pros: no astrophysical uncertainty (Smoking gun) Cons: low statistics
6
/17
astrophysical uncertainties
Clusters:
Pros: low BG and good source id Cons: low statistics, astrophysical uncertainties
Slide from Talk by Tsunefumi Mizuno
TABLE I. Properties of Milky Way dSphs.
Name `a ba Distance log10(Jobs)b (deg) (deg) (kpc) (log10[ GeV2 cm−5]) Bootes I 358.1 69.6 66 18.8 ± 0.22 Canes Venatici II 113.6 82.7 160 17.9 ± 0.25 Carina 260.1 −22.2 105 18.1 ± 0.23 Coma Berenices 241.9 83.6 44 19.0 ± 0.25 Draco 86.4 34.7 76 18.8 ± 0.16 Fornax 237.1 −65.7 147 18.2 ± 0.21 Hercules 28.7 36.9 132 18.1 ± 0.25 Leo II 220.2 67.2 233 17.6 ± 0.18 Leo IV 265.4 56.5 154 17.9 ± 0.28 Sculptor 287.5 −83.2 86 18.6 ± 0.18 Segue 1 220.5 50.4 23 19.5 ± 0.29 Sextans 243.5 42.3 86 18.4 ± 0.27 Ursa Major II 152.5 37.4 32 19.3 ± 0.28 Ursa Minor 105.0 44.8 76 18.8 ± 0.19 Willman 1 158.6 56.8 38 19.1 ± 0.31 Bootes II c 353.7 68.9 42 – Bootes III 35.4 75.4 47 – Canes Venatici I 74.3 79.8 218 17.7 ± 0.26 Canis Major 240.0 −8.0 7 – Leo I 226.0 49.1 254 17.7 ± 0.18 Leo V 261.9 58.5 178 – Pisces II 79.2 −47.1 182 – Sagittarius 5.6 −14.2 26 – Segue 2 149.4 −38.1 35 – Ursa Major I 159.4 54.4 97 18.3 ± 0.24
M.Ackerman et al., 1503.02641
φs(∆Ω) = 1 4π hσvi 2m2
DM
Z Emax
Emin
dNγ dEγ dEγ | {z }
particle physics
⇥ Z
∆Ω
Z
l.o.s.
ρ2
DM(r)dldΩ0
| {z }
Jfactor
.
Gamma-rays from dwarf Spheroidals (dSph)
Fermi constraint on DM ann. from dwarf spheroidal galaxies
M.Ackerman et al., 1503.02641
101 102 103 DM Mass (GeV/c2)
W +W −
10−22 10−23 10−24 10−25 10−26 10−27 hσvi (cm3 s−1)
dSph : DM dominated system, Small uncertainty from DM density profile
CMB constraint
Ando, Ishiwata, 1502.02007 DM mass (GeV) DM lifetime (sec)
For decaying DM, extragalactic gamma-rays gives severe constraint.
Constraint on Wino DM from HESS gamma-ray line search
Baumgart, Rothstein, Vaidya,1412.8698
Constraint from Neutrino
[GeV]
χ
m
2
10
3
10 ]
s
[cm ν σ
10
10
10
10 , Conventinal
DM->W
Isothermal NFW Einasto Moore Fermi-LAT
[GeV]
χ
m
2
10
3
10 ]
s
[cm ν σ
10
10
10
10 , MED
DM->W
Isothermal NFW Einasto Moore Fermi-LAT
[GeV]
χ
m
2
10
3
10 ]
s
[cm ν σ
10
10
10
10 , MIN
DM->W
Isothermal NFW Einasto Moore Fermi-LAT
[GeV]
χ
m
2
10
3
10 ]
s
[cm ν σ
10
10
10
10 , MAX
DM->W
Isothermal NFW Einasto Moore Fermi-LAT
Jin, Wu, Zhou, 1504.04604