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Indirect Dark Matter Detection
Alejandro IbarraTechnische Universität München
ZakopaneMay 2012
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Indirect dark matter searchesAntimatter
Gamma-rays
Neutrinos
Production
Propagation
Detection
of
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hard e+antileptons
quarkssoft e+ p, D
Hard & soft e+ p, DZ0, W
ProductionProduction
Annihilationrate ρ2
hard e+antileptons
quarkssoft e+ p, D
Hard & soft e+ p, DZ0, W
Decayrate ρ
DM
DM
DM
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PropagationPropagation
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PAMELA collaborationarXiv:1007.0821
Experimental results: antiprotons
Fairly good agreement between the measurements and the theoretical predictions from spallation.
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Annihilating dark matter: Lightest SUSY particle
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MIN
MED
MAX
Tran et al.
→ W e, Z e, h e
Decaying dark matter
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Experimental results: positrons
PAMELA collaborationarXiv:0810.4995
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PAMELA collaborationarXiv:0810.4995
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Gast, Schael '09
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PAMELA excess at high energies?Theoretical calculation of the background positron fraction:
Secondary positrons Calculable
Secondary electrons CalculablePrimary electrons To be determined by experiments
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PAMELA excess at high energies?Theoretical calculation of the background positron fraction:
Secondary positrons Calculable
Secondary electrons CalculablePrimary electrons To be determined by experiments
E−2.8
E−2.8E−3.15
E−3.5
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PAMELA excess at high energies?Theoretical calculation of the background positron fraction:
Secondary positrons Calculable
Secondary electrons CalculablePrimary electrons To be determined by experiments Harnik, Kribs '08
E−2.8
E−2.8E−3.15
E−3.5
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Abdo et al.ArXiv:0905.0025
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Present situation:
Evidence for a primary component of positrons
(possibly accompanied by electrons)
Astrophysical sources? Pulsars, SN remnants New particle physics? DM annihilation, DM decay
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Cholis et al.arXiv:0811.3641
Annihilating dark matter
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Cholis et al.arXiv:0811.3641
Annihilating dark matter600 times larger than the thermal cross section
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Cholis et al.arXiv:0811.3641
Annihilating dark matter
5000 <sv>th
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Decaying dark matter
Democratic decay n
Ibarra, Tran, Weniger
mDM=2500 GeV
mDM=600 GeV
Ibarra, Tran, WenigerarXiv:0906.1571
t=1.51026 s
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Conclusion from these plots:Conclusion from these plots: the electron/positron excesses could be explained the electron/positron excesses could be explained by the annihilation/decay of dark matter particles.by the annihilation/decay of dark matter particles.
Conclusion from these plots:Conclusion from these plots: the electron/positron excesses could be explained the electron/positron excesses could be explained by the annihilation/decay of dark matter particles.by the annihilation/decay of dark matter particles.
Is this the first non-gravitational evidence of dark matter?
“Extraordinary claims require extraordinary evidence” Carl Sagan
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High energy positrons are difficult to discriminate from protons.And there are many more protons in cosmic rays than positrons!
Instrumental problem?Instrumental problem?
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PAMELA claims a proton rejection of one part in 105.
Instrumental problem?Instrumental problem?
Schubnell
High energy positrons are difficult to discriminate from protons.And there are many more protons in cosmic rays than positrons!
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• Fermi-LAT has confirmed the positron excess! Fermi coll. arXiv:1109.0521
• More independent measurements soon by AMS-02
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Astrophysical interpretations Astrophysical interpretations
Pulsars Pulsars areare sources sources of high energy of high energy electrons electrons && positrons positrons
Atoyan, Aharonian, Völk;Chi, Cheng, Young;Grimani
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Pulsar explanation I: Geminga + Monogem
Monogem (B0656+14)Geminga
T=370 000 yearsD=157 pc
T=110 000 yearsD=290 pc
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Nice agreement. However, it is not a prediction!● dN
e/dE
e ∝ E
e−1.7 exp(−E
e/1100 GeV)
● Energy output in e+e- pairs: 40% of the spin-down rate (!)
Pulsar explanation I: Geminga + Monogem Grasso et al.
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● dNe/dE
e ∝ E
e-α exp(−E
e/E
0), 1.5 < α < 1.9, 800 GeV < E0 < 1400 GeV
● Energy output in e+e- pairs: between 10−30% of the spin-down rate
Pulsar explanation II: Multiple pulsars Grasso et al.
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More later about the dark matter explanations tothe electron/positron excesses
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Gamma raysGamma rays
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The gamma ray flux from dark matter annihilation/decay has two components:
• Prompt radiation of gamma rays produced in the annihilation/decay (final state radiation, pion decay...)• May contain spectral features.
• Inverse Compton Scattering radiation of electrons/positrons produced in the annihilation/decay.• Always smooth spectrum.
Production of gamma-raysProduction of gamma-rays
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Inverse Compton Scattering radiation
The inverse Compton scattering of electrons/positrons from dark matter annihilation/decay with the interstellar and extragalactic radiation fields produces gamma rays.
e± from dark matter annihilation/decay
Ee 1 TeV
Interstellar radiation field (starlight,thermal radiation of dust, CMB)
Upscattered photon
This produces Eγ∗ 100 GeV
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Production rate of gamma rays due to IC scattering of e on the ISRF:
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Number density ofphotons of the ISRF
Production rate of gamma rays due to IC scattering of e on the ISRF:
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Number density ofelectrons/positrons.→ Transport equation.
Production rate of gamma rays due to IC scattering of e on the ISRF:
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Number density ofelectrons/positrons.→ Transport equation.
For electrons with E>10 GeV, the transport equation is dominated by theenergy loss term. Therefore
with
Production rate of gamma rays due to IC scattering of e on the ISRF:
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σT=0.67 barn Compton scattering cross section in the Thomson limit.γe= Ee/me Lorentz factor.Γe=4 γe ε/me ,q=Eγ/Γ(Ee−Eγ),
Production rate of gamma rays due to IC scattering of e on the ISRF:
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Production rate of gamma rays due to IC scattering of e on the ISRF:
Finally, the differential flux in the direction (l, b)
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Prompt radiation
Halo component Extragalactic component
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Prompt radiation
Halo component
Annihilation
Decay
Source term(particle physics)
Line-of-sight integral(astrophysics)
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0 50 100 150 deg
1
10
100
1000 ds 2,s
0 50 100 150 deg
1
10
100
1000 ds ,s
NFW
Isothermal
Moore
Einasto
NFW
Isothermal
Moore
Einasto
Bertone, Buchmüller, Covi, AIarXiv:0709.2299
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Prompt radiation: Effect of substructures
Halo component
Annihilation
Decay
Source term(particle physics)
Line-of-sight integral(astrophysics)
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Prompt radiation
Halo component
• Depends on the dark matterprofile. Strong dependence in thedirection of the galactic centerand mild at high latitudes (|b|>10)• Even if the profile is sphericallysymmetric, the flux at Earth depends onthe direction of observation.
Summary:
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Prompt radiation
Extragalactic component
● Isotropic
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Prompt radiation
Extragalactic component
● Isotropic● Redshifted
Decay
Annihilation
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6.8 Gyr ago
12 Gyr ago12.8 Gyr ago
Now
10.3 Gyr ago
3.4 Gyr ago
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Prompt radiation
Extragalactic component
● Isotropic● Redshifted
Decay
Annihilation
Enhancement
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Fermi coll.arXiv:1002.4415
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Prompt radiation
Extragalactic component
● Isotropic● Redshifted● Attenuated due to pair production gge+e−
Decay
Annihilation
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Prompt radiation
Extragalactic component
● Isotropic● Redshifted● Attenuated due to pair production gge+e−
Stecker et al.
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Einasto
isothermal
Impact of attenuation: decaying dark matter
Ibarra, Tran, WenigerarXiv:0909.3514
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PropagationPropagation
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Where to look for annihilating dark matter
Kuhlen, Diemand, Madau
Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
Galactic centerGalactic center Very good statistics Source confusions Uncertainties in diffuse background modelling
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
SatellitesSatellites Low background Good source identification Low statistics
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
Galactic haloGalactic halo Very good statistics Uncertainties in diffuse background modelling
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
Extragalactic backgroundExtragalactic background Good statistics Uncertainties in diffuse background modelling Astrophysical uncertainties
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
Galaxy clustersGalaxy clusters Good source identification Low background Low statistics
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Kuhlen, Diemand, Madau
Spectral featuresSpectral features No astrophysical uncertainties “Smoking gun” Potentially low statistics.
Where to look for annihilating dark matter Baltz et al.arXiv:0806.2911
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Diffuse Galactic emissionDiffuse Galactic emission
Divide the sky in different regions:
3°3°
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Diffuse Galactic emissionDiffuse Galactic emission
5°30°
Divide the sky in different regions:
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Diffuse Galactic emissionDiffuse Galactic emission
10°20°
Divide the sky in different regions:
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Diffuse Galactic emissionDiffuse Galactic emission
Galactic poles
Divide the sky in different regions:
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Background I: sources
But beware of backgrounds when searching for dark matter...
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Inverse compton
bremmstrahlung
p0-decay
Background II: modelling of the diffuse emission
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Cirelli, Panci, Serpico
Conservative approach: demand that the flux from dark matter annihilations does not exceed the measured flux
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Cirelli, Panci, Serpico
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Dwarf spheroidal galaxiesDwarf spheroidal galaxies
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High mass-to-light ratio:dwarf galaxies contain large amounts of dark matter
Relatively close
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Assume a Navarro-Frenk-White dark matter halo profile insidethe tidal radius:
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Flux upper limits
Fermi coll.arXiv:1001.4531
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Constraints on annihilating WIMPs
Fermi coll.arXiv:1001.4531
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Closing in light WIMP scenarios from dwarf galaxy observations
Geringer-Sameth, Koushiappas '11
MDM> 40 GeV for DM DM → b b
MDM> 19 GeV for DM DM → τ+ τ−
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Gamma-ray featuresGamma-ray features
Strategy: search for a feature in the gamma-ray spectrum whichcannot be mimicked by any (known) astrophysical source:
• If not observed strong limits on models → (background substraction very efficient)• If observed, unequivocal sign of dark matter
Gamma-ray lines Virtual InternalBremsstrahlungGamma-ray boxes
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• Inert Higgs
Gustafsson, Lundström, Bergström, Edsjö
Gamma-ray linesGamma-ray lines
Predicted to be fairly intense in some concrete models
Produced in the annihilation DM DM → g g
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Gamma-ray linesGamma-ray lines
Predicted to be fairly intense in some concrete models
Jackson et al.arXiv: 0912.0004
• Dirac fermion coupled to a Z'
Produced in the annihilation DM DM → g g
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Fermi collaborationarXiv:1002.2239
Gamma-ray linesGamma-ray lines
Fermi coll. arXiv:1001.4836
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Gamma-ray linesGamma-ray lines
Vertongen, WenigerarXiv:1101.2610
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Gamma-ray linesGamma-ray lines
arXiv:1204.2797
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Gamma-ray linesGamma-ray lines
arXiv:1204.2797
mDM=129 GeV
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Gamma-ray linesGamma-ray lines
4.6 s (3.3 s including LEE)
For Einasto halo profile,
arXiv:1204.2797
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Gamma-ray boxesGamma-ray boxes
Consider the cascade decay: DM DM → f f
f g g→
AI, Lopez-Gehler, PatoarXiv:1205.0007
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Gamma-ray boxesGamma-ray boxes
Consider the cascade decay: DM DM → f f
f g g→
AI, Lopez-Gehler, PatoarXiv:1205.0007
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Virtual internal BremsstrahlungVirtual internal Bremsstrahlung BergströmFlores, Olive, Rudaz
Bringmann et al.arXiv:1203.1312
VIB FSR FSR
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Virtual internal BremsstrahlungVirtual internal Bremsstrahlung
Bringmann et al.arXiv:1203.1312
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Virtual internal BremsstrahlungVirtual internal Bremsstrahlung
4.3 s (3.1 s with LEE)
Bringmann et al.arXiv:1203.1312
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Where to look for decaying dark matter Bertone et al.arXiv:0709.2299
A priori, same targets as for annihilating dark matter:
• Diffuse galactic background (galactic center, galactic halo)• Dwarf galaxies. • Clusters of galaxies.• Isotropic (“extragalactic”) background.• Gamma-ray lines.
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Where to look for decaying dark matter Bertone et al.arXiv:0709.2299
A priori, same targets as for annihilating dark matter:
• Diffuse galactic background (galactic center, galactic halo)• Dwarf galaxies. • Clusters of galaxies.• Isotropic (“extragalactic”) background.• Gamma-ray lines.
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Fermi coll.arXiv:1002.3603
Isotropic (“extragalactic”) backgroundIsotropic (“extragalactic”) background
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m=3000 GeV, τ=2.11026 s.
Average flux, excluding galactic disk
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Zhang et al.
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Clusters of galaxiesClusters of galaxies
Huang et al.
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Gamma-ray linesGamma-ray lines
Inequivocal sign of dark matter. No (known) astrophysical source canproduce a gamma-ray line
Predicted to be fairly intense in some concrete models
● Gravitino in general SUSY models (without imposing R-parity conservation)
Buchmüller et al.
m=200 GeVτ=7×1026 s
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Gamma-ray linesGamma-ray lines
Inequivocal sign of dark matter. No (known) astrophysical source canproduce a gamma-ray line
Predicted to be fairly intense in some concrete models
● Vector of a hidden SU(2).
m=600 GeVt=1.11027 s
Arina, Hambye,AI, Weniger
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Gamma-ray linesGamma-ray lines
Inequivocal sign of dark matter. No (known) astrophysical source canproduce a gamma-ray line
Predicted to be fairly intense in some concrete models
● Vector of a hidden SU(2).
m=1550 GeVt=1.61027 s
Arina, Hambye,AI, Weniger
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1030
1029
1028
1027
mDM (GeV)100 1000
t DM
(s)
Gamma-ray linesGamma-ray lines
Fermi coll. arXiv:1001.4836
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Gamma-ray linesGamma-ray lines
Vertongen, Weniger1101.2610
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Gamma-ray linesGamma-ray lines
Vertongen, Weniger1101.2610
Garny et al.1011.3786
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Gamma-ray linesGamma-ray lines
Inequivocal sign of dark matter. No (known) astrophysical source canproduce a gamma-ray line
Predicted to be fairly intense in some concrete models
● Gravitino in general SUSY models (without imposing R-parity conservation)
Buchmüller et al.
m=200 GeVτ=7×1026 s
Ruled out
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ConclusionsConclusions
We have entered an era where indirect searches provide strong constraints on the dark matter properties. Or from the optimistic point of view, there exists (perhaps for the first time) a discovery potential.
1996 2010
Jungman, Kamionkowski, Griest
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ConclusionsConclusions
We have entered an era where indirect searches provide strong constraints on the dark matter properties. Or from the optimistic point of view, there exists (perhaps for the first time) a discovery potential.
A few anomalies have been reported, which can be interpretedas originated from dark matter annihilations/decays. Very exciting, but caution should prevail over excitement. Look for smoking gunsand for correlations in signals in different channels/energies.
Bright future in indirect dark matter searches: AMS-02, IceCube,CTA... New surprises (and new challenges) are surely awaiting us.