Indirect Dark Matter Searches Torsten Bringmann, University of - - PowerPoint PPT Presentation
TeV Particle Astrophysics 2010, Paris, 19 - 23 July Indirect Dark Matter Searches Torsten Bringmann, University of Hamburg Outlook Introduction Messengers for indirect DM searches Gamma rays Antimatter ... Multiwavelength/-messenger
Torsten Bringmann, University of Hamburg
TeV Particle Astrophysics 2010, Paris, 19 - 23 July
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
Gamma rays Antimatter ...
2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
3 credit: WMAP
electrically neutral non-baryonic cold ‒ dissipationless and negligible free- streaming effects collisionless ΩCDM = 0.233 ± 0.013 (WMAP)
(dark!) (BBN) (structure formation) (bullet cluster)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
3 credit: WMAP
electrically neutral non-baryonic cold ‒ dissipationless and negligible free- streaming effects collisionless ΩCDM = 0.233 ± 0.013 (WMAP)
(dark!) (BBN) (structure formation) (bullet cluster)
well-motivated from particle physics
[SUSY, EDs, little Higgs, ...]
thermal production “automatically” leads to the right relic abundance
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
4
y
e lic
(thermal average)
dnχ dt + 3Hnχ = −σv
χ − n2
χeq
nχeq
time increasingσv a3nχ
Fig.: Jungman, Kamionkowski & Griest, PR’96
σv:
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
4
y
e lic
(thermal average)
dnχ dt + 3Hnχ = −σv
χ − n2
χeq
nχeq
time increasingσv a3nχ
Fig.: Jungman, Kamionkowski & Griest, PR’96
σv:
“Freeze-out” when annihilation rate falls behind expansion rate
for weak-scale interactions!
(→ a3nχ ∼ const.)
Ωχh2 ∼ 3 · 10−27cm3/s σv ∼ O(0.1)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
5
χ
SM (annihilation)
χ
SM
χ
(scattering)
χ
SM SM
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
5
χ
SM (annihilation)
χ
SM
χ
(scattering)
χ
SM SM chemical decoupling
Tcd ∼ mχ/25
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
5
χ
SM (annihilation)
χ
SM
χ
(scattering)
χ
SM SM kinetic decoupling
Tkd ∼ mχ/(102..105)
chemical decoupling
Tcd ∼ mχ/25
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
5
χ
SM (annihilation)
χ
SM
χ
(scattering)
χ
SM SM kinetic decoupling
Tkd ∼ mχ/(102..105)
chemical decoupling
Tcd ∼ mχ/25
mχ [GeV] Mcut/M
Higgsino (Zg < 0.05) mixed (0.05 ≤ Zg ≤ 0.95) Gaugino (Zg > 0.95)
K I J∗ F∗
50 100 500 1000 5000 10−4 10−6 10−8 10−10 10−12
Mcut ∼ 10−6M⊙
TB, NJP ’09
size of smallest subhalos
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
6
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
6
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
7
! " e
+
DM DM ! e p
_
+
regions of high DM density
low background; clear signatures
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
8
! " e
+
DM DM ! e p
_
+
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
8
! " e
+
DM DM ! e p
_
+
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
8
! " e
+
DM DM ! e p
_
+
maybe most important!
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
9
dΦγ dEγ (Eγ, ∆ψ) = σvann 8πm2
χ
Bf dN f
γ
dEγ ·
dΩ ∆ψ
dℓ(ψ)ρ2(r)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
9
dΦγ dEγ (Eγ, ∆ψ) = σvann 8πm2
χ
Bf dN f
γ
dEγ ·
dΩ ∆ψ
dℓ(ψ)ρ2(r)
particle physics mχ σvann Bf N f
γ
: total annihilation cross section : WIMP mass : branching ratio into channel : number of photons per ann. f
(50 GeV mχ 5 TeV)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
9
dΦγ dEγ (Eγ, ∆ψ) = σvann 8πm2
χ
Bf dN f
γ
dEγ ·
dΩ ∆ψ
dℓ(ψ)ρ2(r)
astrophysics ∆ψ : angular res. of detector D : distance to source
for point-like sources:
≃
−1 d3r ρ2(r)
particle physics mχ σvann Bf N f
γ
: total annihilation cross section : WIMP mass : branching ratio into channel : number of photons per ann. f
(50 GeV mχ 5 TeV)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
9
dΦγ dEγ (Eγ, ∆ψ) = σvann 8πm2
χ
Bf dN f
γ
dEγ ·
dΩ ∆ψ
dℓ(ψ)ρ2(r)
astrophysics ∆ψ : angular res. of detector D : distance to source
for point-like sources:
≃
−1 d3r ρ2(r)
particle physics mχ σvann Bf N f
γ
: total annihilation cross section : WIMP mass : branching ratio into channel : number of photons per ann. f
(50 GeV mχ 5 TeV)
high accuracy spectral information
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
9
dΦγ dEγ (Eγ, ∆ψ) = σvann 8πm2
χ
Bf dN f
γ
dEγ ·
dΩ ∆ψ
dℓ(ψ)ρ2(r)
astrophysics ∆ψ : angular res. of detector D : distance to source
for point-like sources:
≃
−1 d3r ρ2(r)
particle physics mχ σvann Bf N f
γ
: total annihilation cross section : WIMP mass : branching ratio into channel : number of photons per ann. f
(50 GeV mχ 5 TeV)
high accuracy spectral information
large uncertainty in normalization
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
10
a[( r a) α−1]
ρNFW = c r(a + r)2
ρBurkert = c (r + a)(a2 + r2)
ρiso = c (a2 + r2)
rather stable result conflicting observational claims (NB: observation of stars)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
10
a[( r a) α−1]
ρNFW = c r(a + r)2
ρBurkert = c (r + a)(a2 + r2)
ρiso = c (a2 + r2)
rather stable result conflicting observational claims (NB: observation of stars)
(But could also lead to a steepening of the profile!)
(α ≈ 0.17)
see talks by
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
11 Fig.: Bergström, NJP ’09
ΦSM ∝ ρ2
χ = (1 + BF)ρχ2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
11 Fig.: Bergström, NJP ’09
important to include realistic value for !
Mcut
each decade in Msubhalo contributes about the same depends on uncertain form of microhalo profile ( ...) and (large extrapolations necessary!)
cv
dN/dM
e.g. Diemand, Kuhlen & Madau, ApJ ’07
ΦSM ∝ ρ2
χ = (1 + BF)ρχ2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
12
π0 → γγ
0.001 0.01 0.1 0.1 1 1 10 100 1000 0.02 0.05 0.2 0.5
x = E/mχ dNγ/dx
mainly from result in a rather featureless, model-independent spectrum
Bertone et al., astro-ph/0612387
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
12
π0 → γγ
necessarily loop suppressed: smoking-gun signature
χχ → γγ, γZ, γH
O(α2)
Bergström, Ullio & Buckley, ApJ ’98
0.5% 1% 2% mB(1) = 800 GeV (energy resolution as indicated)
1 2 3 4 0.78 0.78 0.79 0.80 0.81Eγ [TeV] dΦ/dEγ [10−8 m−2 s−1 TeV−1]
Bergström, TB, Eriksson & Gustafsson, JCAP ’05
0.001 0.01 0.1 0.1 1 1 10 100 1000 0.02 0.05 0.2 0.5
x = E/mχ dNγ/dx
mainly from result in a rather featureless, model-independent spectrum
Bertone et al., astro-ph/0612387
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
12
π0 → γγ
whenever charged final states are present: characteristic signature (details model-dependent!) usually dominant at high energies
O(α)
Birkedal, Matchev, Perelstein & Spray, hep-ph/0507194
TB, Bergström & Edsjö, JHEP ’08
necessarily loop suppressed: smoking-gun signature
χχ → γγ, γZ, γH
O(α2)
Bergström, Ullio & Buckley, ApJ ’98
0.5% 1% 2% mB(1) = 800 GeV (energy resolution as indicated)
1 2 3 4 0.78 0.78 0.79 0.80 0.81Eγ [TeV] dΦ/dEγ [10−8 m−2 s−1 TeV−1]
Bergström, TB, Eriksson & Gustafsson, JCAP ’05
0.001 0.01 0.1 0.1 1 1 10 100 1000 0.02 0.05 0.2 0.5
x = E/mχ dNγ/dx
mainly from result in a rather featureless, model-independent spectrum
Bertone et al., astro-ph/0612387
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
13
focus point region (mχ = 1926 GeV)
0.01 0.1
x = Eγ/mχ x2dN γ,tot/dx
Total Secondary gammas Internal Bremsstrahlung
0.4 0.6 0.8 1 0.001 1 0.2
BM4
bulk region (mχ = 141 GeV)
x = Eγ/mχ x2dN γ,tot/dx
Total Secondary gammas Internal Bremsstrahlung
0.4 0.6 0.8 1 1 0.01 0.1 0.2
I’
.
coannihilation region (mχ = 233 GeV)
0.01 0.1
x = Eγ/mχ x2dN γ,tot/dx
Total Secondary gammas Internal Bremsstrahlung
0.4 0.6 0.8 1 0.001 1 10 0.2
BM3
funnel region (mχ = 565 GeV)
x = Eγ/mχ x2dN γ,tot/dx
Total Secondary gammas Internal Bremsstrahlung
0.4 0.6 0.8 1 1 0.01 0.1 0.2
K’
.
(benchmarks taken from TB, Edsjö & Bergström, JHEP ’08 and Battaglia et al., EPJC ’03)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
14
0.2 0.4 0.6 0.8 1.0 1.2 0.001 0.01 0.1 1
x = Eγ/mχ
x2dN/dx
B M 3 – c
n n i h i l a t i
( 2 3 ) BM4 – focus point (10.9) I ’ – b u l k ( 3 . 6 ) K ’ – f u n n e l
TB, PoS ’08
Example: mSUGRA benchmarks (assume energy resolution of 10%)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
14
Bergström et al., ’06
Example: Higgsino vs KK-DM (about same mass; assume ) ∆E = 15%
Eγ[TeV] E2
γ d(σv)γ/dEγ [10−29cm3s−1TeV]
10 102 103 0.1 0.5 1 2
Higgsino B(1)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
15
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
15
IB boosts effective sensitivity by a factor of up to ~10 CTA could see a DM signal from Willman 1 for a large class of models (less optimistic prospects for Draco)
∆E/E = 10%
TB, Doro & Fornasa, JCAP ’09 Cannoni et al., PRD ’10
TB, Doro & Fornasa, JCAP ’09
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
15
IB boosts effective sensitivity by a factor of up to ~10 CTA could see a DM signal from Willman 1 for a large class of models (less optimistic prospects for Draco)
∆E/E = 10%
TB, Doro & Fornasa, JCAP ’09 Cannoni et al., PRD ’10
TB, Doro & Fornasa, JCAP ’09
important to include also for other targets!
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Galactic center
brightest DM source in sky large background contributions
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Galactic center
brightest DM source in sky large background contributions
Galactic halo
good statistics, angular information galactic backgrounds?
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Galactic center
brightest DM source in sky large background contributions
Dwarf Galaxies
DM dominated, M/L~1000 fluxes soon in reach!
Galactic halo
good statistics, angular information galactic backgrounds?
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Galactic center
brightest DM source in sky large background contributions
DM clumps
easy discrimination (once found) bright enough?
Dwarf Galaxies
DM dominated, M/L~1000 fluxes soon in reach!
Galactic halo
good statistics, angular information galactic backgrounds?
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Extragalactic background
DM contribution from all z background difficult to model
Galactic center
brightest DM source in sky large background contributions
DM clumps
easy discrimination (once found) bright enough?
Dwarf Galaxies
DM dominated, M/L~1000 fluxes soon in reach!
Galactic halo
good statistics, angular information galactic backgrounds?
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
16
Diemand, Kuhlen & Madau, ApJ ’07
Extragalactic background
DM contribution from all z background difficult to model
Galaxy clusters
cosmic ray contamination better in multi-wavelength?
Galactic center
brightest DM source in sky large background contributions
DM clumps
easy discrimination (once found) bright enough?
Dwarf Galaxies
DM dominated, M/L~1000 fluxes soon in reach!
Galactic halo
good statistics, angular information galactic backgrounds?
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
17
−10
50 h 5 σ 10 events
Energy [ TeV ]
MAGIC II GLAST (1 yr) GLAST (5 yrs) 1 C.U. 0.001 C.U. VERITAS MAGIC
−11 −12 −13 −14
stereo
Integral flux limit [ 1 / (s cm ) ]
2
H.E.S.S.
10 0.01 0.1 1 10 100 9−tel. at 2000 m 10 10 10 10 41−tel. system 4 large + 85
Bernlöhr et al., ’07
large eff. Area (~km2) small field of view lower threshold 40 GeV
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
17
−10
50 h 5 σ 10 events
Energy [ TeV ]
MAGIC II GLAST (1 yr) GLAST (5 yrs) 1 C.U. 0.001 C.U. VERITAS MAGIC
−11 −12 −13 −14
stereo
Integral flux limit [ 1 / (s cm ) ]
2
H.E.S.S.
10 0.01 0.1 1 10 100 9−tel. at 2000 m 10 10 10 10 41−tel. system 4 large + 85
Bernlöhr et al., ’07
large eff. Area (~km2) small field of view lower threshold 40 GeV
small eff. Area (~m2) large field of view upper bound on resolvable Eγ
(from the LAT webpage)
Fermi
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Fermi - Clusters, 1002.2239
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Fermi - Clusters, 1002.2239 Fermi - line search, 1002.2239
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Fermi - Clusters, 1002.2239 Fermi - line search, 1002.2239 Fermi - dwarfs, 1001.4531
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Fermi - Clusters, 1002.2239 Fermi - line search, 1002.2239 Fermi - dwarfs, 1001.4531 VERITAS - dwarfs, 1006.5955
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
18
Fermi - Clusters, 1002.2239 Fermi - line search, 1002.2239 Fermi - dwarfs, 1001.4531 VERITAS - dwarfs, 1006.5955
S.Murgia, B. Cañadas (Fermi), M. Vivier (VERITAS), ...
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
19
! " e
+
DM DM ! e p
_
+
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
19
! " e
+
DM DM ! e p
_
+
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.) Diffusion coefficient, usually D ∝ β(E/q)δ
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.) Diffusion coefficient, usually D ∝ β(E/q)δ convection
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.) Diffusion coefficient, usually D ∝ β(E/q)δ convection energy losses
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.) Diffusion coefficient, usually D ∝ β(E/q)δ convection energy losses diffusive reacceleration
K ∝ v2
ap2/D
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
20
∂t − ∇ · (D∇ − vc)ψ + ∂ ∂pblossψ − ∂ ∂pK ∂ ∂pψ = qsource
(stationary conf.) Diffusion coefficient, usually D ∝ β(E/q)δ convection energy losses diffusive reacceleration
K ∝ v2
ap2/D
Sources (primary & secondary)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
21
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
21
3D possible any magnetic field model realistic gas distribution, full energy losses computations time-consuming “black box” + + + ‒ ‒
Strong, Moskalenko, …
DRAGON
Evoli, Gaggero, Grasso & Maccione
e.g.
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
21
3D possible any magnetic field model realistic gas distribution, full energy losses computations time-consuming “black box” + + + ‒ ‒
Strong, Moskalenko, …
DRAGON
Evoli, Gaggero, Grasso & Maccione
e.g.
Physical insight from analytic solutions fast computations allow to sample full parameter space
simplified gas distribution, energy losses + + ‒ ‒ e.g. Donato, Maurin, Salati, Taillet, ...
2h
R = 20kpc
ISM
L 1kpc
vc
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
22
Maurin, Donato, Taillet & Salati, ApJ ’01
(K0, δ, L, va, vc)
TB & Salati, PRD ’07
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
22
Maurin, Donato, Taillet & Salati, ApJ ’01
(K0, δ, L, va, vc)
TB & Salati, PRD ’07
excellent agreement with new data: BESSpolar 2004 PAMELA 2008
Abe et al., PRL ’08
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
22
Maurin, Donato, Taillet & Salati, ApJ ’01
(K0, δ, L, va, vc)
very nice test for underlying diffusion model!
TB & Salati, PRD ’07
excellent agreement with new data: BESSpolar 2004 PAMELA 2008
Abe et al., PRL ’08
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
23
no significant astrophysical sources for completely diffusion dominated
E¯
p 10 GeV
¯ p
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
23
no significant astrophysical sources for completely diffusion dominated
E¯
p 10 GeV
¯ p
TB & Salati, PRD ’09
up to ~200 from DM profile
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
23
no significant astrophysical sources for completely diffusion dominated
E¯
p 10 GeV
¯ p
TB & Salati, PRD ’09
up to ~200 from DM profile
TB & Salati, PRD ’09
up to ~40 from range of propagation parameters compatible with B/C
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
24
TB & Salati, PRD ’09
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
24
TB & Salati, PRD ’09
+ …but are quite efficient
light SUSY DM non-standard DM profile proposed by deBoer DM explanations for the PAMELA excess “Evidence” for DM seen in Fermi data towards the GC ... e+/e−
Donato et al., PRL ’09 Bottino et al., PRD ’98+05 Bergström et al., JCAP ’06 TB, 0911.1124
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
25
Energy (GeV)
0.1 1 10 100
))
! )+
+
(e ! ) / (
+
(e ! Positron fraction
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
Adriani et al., Nature ’09
(> 500 citations since 10/08!)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
26
σv ∝ m2
ℓ
m2
χ
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
26
σv ∝ m2
ℓ
m2
χ
αem π
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
26
σv ∝ m2
ℓ
m2
χ
Bergström, TB & Edsjö, PRD ’08
first attempt to connect PAMELA to DM
HEAT PAMELA
Ee+ [GeV]
e+/(e+ + e−)
Bergstr¨
background
BM3 (mχ=233 GeV) BM5’ (mχ=132 GeV)
5 10 20 50 100 200 0.01 0.02 0.05 0.1 0.2
χχ → e+e−γ
αem π
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
26
σv ∝ m2
ℓ
m2
χ
Bergström, TB & Edsjö, PRD ’08
first attempt to connect PAMELA to DM
HEAT PAMELA
Ee+ [GeV]
e+/(e+ + e−)
Bergstr¨
background
BM3 (mχ=233 GeV) BM5’ (mχ=132 GeV)
5 10 20 50 100 200 0.01 0.02 0.05 0.1 0.2
χχ → e+e−γ
αem π
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
27
strong constraints on hadronic modes from data favoured large boost factors generic ‒
Bergström, Edsjö & Zaharijas, PRL ’09
¯ p
χχ → e+e− or µ+µ−
O(103)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
27
strong constraints on hadronic modes from data favoured large boost factors generic ‒
Bergström, Edsjö & Zaharijas, PRL ’09
¯ p
χχ → e+e− or µ+µ−
O(103)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
27
strong constraints on hadronic modes from data favoured large boost factors generic ‒
Bergström, Edsjö & Zaharijas, PRL ’09
¯ p
χχ → e+e− or µ+µ−
O(103)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
28
secondaries ~ 2-4 primaries ~ 5
Delahaye et al., A&A ’09 Delahaye et al., PRD ’08
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
28
secondaries ~ 2-4 primaries ~ 5
Delahaye et al., A&A ’09 Delahaye et al., PRD ’08
e±
i.e. much better than for primary antiprotons: for , energy loss is dominant must be locally produced (~ kpc) very difficult to explain PAMELA data without primary component
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
28
secondaries ~ 2-4 primaries ~ 5
Delahaye et al., A&A ’09 Delahaye et al., PRD ’08
pulsars
GRB Large arm/interarm difference in SN rate effect of SNR on near dense cloud
Ioka, 0812.4851 Shaviv, Nakir & Piran, PRL ’09 Fujita, Kohri, Yamazaki & Ioka, PRD ’09 Blasi, PRL ’09 Blasi & Serpico, PRL ’09 Grasso et al., ApP ’09 Yüksel, Kistler & Stanev, PRL ’09 Profumo, 0812.4457 Malyshev, Cholis & Gelfand, PRD ’09
e±
i.e. much better than for primary antiprotons: for , energy loss is dominant must be locally produced (~ kpc) very difficult to explain PAMELA data without primary component
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
28
secondaries ~ 2-4 primaries ~ 5
Delahaye et al., A&A ’09 Delahaye et al., PRD ’08
pulsars
GRB Large arm/interarm difference in SN rate effect of SNR on near dense cloud
Ioka, 0812.4851 Shaviv, Nakir & Piran, PRL ’09 Fujita, Kohri, Yamazaki & Ioka, PRD ’09 Blasi, PRL ’09 Blasi & Serpico, PRL ’09 Grasso et al., ApP ’09 Yüksel, Kistler & Stanev, PRL ’09 Profumo, 0812.4457 Malyshev, Cholis & Gelfand, PRD ’09
e±
i.e. much better than for primary antiprotons: for , energy loss is dominant must be locally produced (~ kpc) very difficult to explain PAMELA data without primary component
see talk by
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
29
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
29
wait for upcoming higher statistics experiments ???
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
29
wait for upcoming higher statistics experiments ???
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
30
Arkani-Hamed, Finkbeiner, Slatyer & Weiner, PRD ’09
large annihilation rates (Sommerfeld enhancement) later decay:
mφ 1 GeV
a)
χ χ φ φ φ ... mφ ∼ GeV
φ φ φ
χ χ
φ → e+e− or µ+µ− (kinematics!)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
30
Arkani-Hamed, Finkbeiner, Slatyer & Weiner, PRD ’09
large annihilation rates (Sommerfeld enhancement) later decay:
mφ 1 GeV
a)
χ χ φ φ φ ... mφ ∼ GeV
φ φ φ
χ χ
φ → e+e− or µ+µ− (kinematics!)
Bertone, Bergström, TB, Edsjö & Taoso, PRD ’09
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
31
1 2 3 4 z [kpc] 10
10
10
10
10 !e [MeV cm
~ "
2 (arbitrary normalization)
D M e C R p r i m a r y secondary at source secondary in ISM Ee = 200 GeV R = 8 kpc
Regis & Ullio, PRD ’09
Φe
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
31
1 2 3 4 z [kpc] 10
10
10
10
10 !e [MeV cm
~ "
2 (arbitrary normalization)
D M e C R p r i m a r y secondary at source secondary in ISM Ee = 200 GeV R = 8 kpc
Primary/secondary astrophysical source localized at z=0
Regis & Ullio, PRD ’09
Φe
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
31
1 2 3 4 z [kpc] 10
10
10
10
10 !e [MeV cm
~ "
2 (arbitrary normalization)
D M e C R p r i m a r y secondary at source secondary in ISM Ee = 200 GeV R = 8 kpc
Primary/secondary astrophysical source localized at z=0 DM contribution extended
Regis & Ullio, PRD ’09
Φe
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
31
1 2 3 4 z [kpc] 10
10
10
10
10 !e [MeV cm
~ "
2 (arbitrary normalization)
D M e C R p r i m a r y secondary at source secondary in ISM Ee = 200 GeV R = 8 kpc
Primary/secondary astrophysical source localized at z=0 DM contribution extended handle on this by Fermi/Planck !?
Regis & Ullio, PRD ’09
Φe
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
31
1 2 3 4 z [kpc] 10
10
10
10
10 !e [MeV cm
~ "
2 (arbitrary normalization)
D M e C R p r i m a r y secondary at source secondary in ISM Ee = 200 GeV R = 8 kpc
Primary/secondary astrophysical source localized at z=0 DM contribution extended handle on this by Fermi/Planck !?
Regis & Ullio, PRD ’09
10
1
10
2
10
3
10
4
10
5
10
6
E [MeV] 10
10
10
10
E
2 J [Mev cm
CR total EGB DM! DM! DMe
component could be seen against diffuse background Φe
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
32
Borriello, Cuoco & Miele, PRL ’09
Already EGRET data in some tension with annihilating WIMP explanation of PAMELA Prediction for Fermi: even decaying DM could be excluded!
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
32
Borriello, Cuoco & Miele, PRL ’09
Already EGRET data in some tension with annihilating WIMP explanation of PAMELA Prediction for Fermi: even decaying DM could be excluded!
102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec
FERMI 10° 20° FERMI Gal. Poles Isotropic
Cirelli, Panci & Serpico, 0912.0663
After 1yr Fermi PAMELA +Fermi +Hess
ψ → µ+µ−, Einasto
τdec[s]
mψ [GeV]
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
33
Regis & Ullio, PRD ’08 _ _ _ _ _ _ __
_
10
8
10
10
10
12
10
14
10
16
10
18
10
20
10
22
10
24
10
26
10
28
!![Hz] 10
10
10
10
10
! S"!#![erg s
10
10
10
10 10
2
10
4
10
6
10
8
10
10
10
12
10
14
E [eV] EGRET HESS CHANDRA VLT Narayan et al.
Melia & Falcke
J1746-2851 J1745-290
10
1
10
2
10
3
10
4
M! [GeV] 10
10
10
10
"v [cm
3s
VLA (D configuration) G L A S T C T A
Nsp b - b _
VLA (LaRosa et al)
excluded by IR/NIR/XR !
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
34
small eff. areas (Fermi) relatively short observation times (HESS, VERITAS, MAGIC, …)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
34
small eff. areas (Fermi) relatively short observation times (HESS, VERITAS, MAGIC, …)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
DMA ≈ 10 GeV
(cf. “5@5”)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
DMA = 5000 h 5 y
DMA ≈ 10 GeV
(cf. “5@5”)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
DMA = 5000 h 5 y
DMA ≈ 10 GeV
(cf. “5@5”)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
35
DMA ∼ 10 × Aeff CTA 10 km2
DMA = 5000 h 5 y
DMA ≈ 10 GeV
(cf. “5@5”)
Maybe… But should be investigated further!
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
36
MSSM+mSUGRA scan: ~106 models, 3 WMAP, all collider bounds OK
σ
preliminary!
CDMS excl. SuperCDMS XENON 1t
6 5 4 3 2 1 1 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5
Bergström, Bringmann & Edsjö 2010
log10ΣvmΧ2 1030cm3s1GeV2
log10ΣSI pb
(Bergström, TB & Edsjö, in prep.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
36
MSSM+mSUGRA scan: ~106 models, 3 WMAP, all collider bounds OK
σ
preliminary!
10 orders of magnitude often “missing” in exclusion plots from direct detection! {
CDMS excl. SuperCDMS XENON 1t
6 5 4 3 2 1 1 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5
Bergström, Bringmann & Edsjö 2010
log10ΣvmΧ2 1030cm3s1GeV2
log10ΣSI pb
(Bergström, TB & Edsjö, in prep.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
36
MSSM+mSUGRA scan: ~106 models, 3 WMAP, all collider bounds OK
σ
preliminary!
10 orders of magnitude often “missing” in exclusion plots from direct detection! { CTA/DMA:
assume that angular resolution is good enough to distinguish HESS source from GC; take Fermi background model
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 6 5 4 3 2 1 1 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5
Bergström, Bringmann & Edsjö 2010
log10ΣvmΧ2 1030cm3s1GeV2
log10ΣSI pb
CTA DMA
5y
(Bergström, TB & Edsjö, in prep.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
36
MSSM+mSUGRA scan: ~106 models, 3 WMAP, all collider bounds OK
σ
preliminary!
10 orders of magnitude often “missing” in exclusion plots from direct detection! { CTA/DMA:
assume that angular resolution is good enough to distinguish HESS source from GC; take Fermi background model
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW BF10 6 5 4 3 2 1 1 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5
Bergström, Bringmann & Edsjö 2010
log10ΣvmΧ2 1030cm3s1GeV2
log10ΣSI pb
CTA DMA
5y
(Bergström, TB & Edsjö, in prep.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
36
MSSM+mSUGRA scan: ~106 models, 3 WMAP, all collider bounds OK
σ
preliminary!
10 orders of magnitude often “missing” in exclusion plots from direct detection! { CTA/DMA:
assume that angular resolution is good enough to distinguish HESS source from GC; take Fermi background model
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW adiab. contr. 6 5 4 3 2 1 1 20 19 18 17 16 15 14 13 12 11 10 9 8 7 6 5
Bergström, Bringmann & Edsjö 2010
log10ΣvmΧ2 1030cm3s1GeV2
log10ΣSI pb
CTA DMA
5y
(Bergström, TB & Edsjö, in prep.)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
5y
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
mixed neutralinos: well suited for direct searches
5y
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
pure Higgsinos: accessible by indirect searches (DMA!) mixed neutralinos: well suited for direct searches
5y
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
high-mass Gauginos: more difficult, but indirect searches OK for favorable DM distributions pure Higgsinos: accessible by indirect searches (DMA!) mixed neutralinos: well suited for direct searches
5y
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
high-mass Gauginos: more difficult, but indirect searches OK for favorable DM distributions pure Higgsinos: accessible by indirect searches (DMA!) mixed neutralinos: well suited for direct searches
5y
NB! Sommerfeld effect important in this region not yet included...
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
37
CDMS excl. SuperCDMS XENON 1t Fermi CTA DMA
GC, NFW no boost 100 1000 6 5 4 3 2 1 1 2 3 4 5 6
Bergström, Bringmann & Edsjö 2010
mΧ GeV
log10 Zg1Zg
preliminary! (Bergström, TB & Edsjö, in prep.)
high-mass Gauginos: more difficult, but indirect searches OK for favorable DM distributions pure Higgsinos: accessible by indirect searches (DMA!) mixed neutralinos: well suited for direct searches
5y
NB! Sommerfeld effect important in this region not yet included...
(Bruch ’10)
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
38
So far, we have (probably) not seen a real signal but indirect detection experiments seriously start to probe the parameter space of realistic WIMP models
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
38
So far, we have (probably) not seen a real signal but indirect detection experiments seriously start to probe the parameter space of realistic WIMP models
make use of complementarity of the different approaches - synergy!
Torsten Bringmann, University of Hamburg ‒ Indirect Dark Matter Searches
38
So far, we have (probably) not seen a real signal but indirect detection experiments seriously start to probe the parameter space of realistic WIMP models
make use of complementarity of the different approaches - synergy!
fully exploit the potential of indirect searches (especially when combined with multiwavelength/-messenger techniques) cover a large part of the parameter space that neither direct nor accelerator searches could hope to reach!