Angular power spectrum analysis on current and future high-energy - - PowerPoint PPT Presentation

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Angular power spectrum analysis on current and future high-energy - - PowerPoint PPT Presentation

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Angular power spectrum analysis on current and future high-energy neutrino data Ariane Dekker TAUP 2019 A. Dekker, S. Ando, JCAP 02 (2019) 002 A. Dekker, M. Chianese, S. Ando, arXiv:1909.XXXXX 1 Credits: IceCube/NASA 2 Astrophysical

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Angular power spectrum analysis on current and future high-energy neutrino data

Ariane Dekker TAUP 2019

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  • A. Dekker, S. Ando, JCAP 02 (2019) 002
  • A. Dekker, M. Chianese, S. Ando, arXiv:1909.XXXXX
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Credits: IceCube/NASA

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Astrophysical Sources

p-γ p-p

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Photo-hadronic interactions Active Galactic Nuclei Blazars ( 4 — 6 % ) Gamma-Ray Bursts Hadro-nuclear interactions Starburst Galaxies Galaxy clusters

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Astrophysical Sources

p-γ p-p

Photo-hadronic interactions Active Galactic Nuclei Blazars ( 4 — 6 % ) Gamma-Ray Bursts Hadro-nuclear interactions Starburst Galaxies Galaxy clusters

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Dark Matter

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IceCube KM3NeT

Neutrino detectors

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Neutrino detectors

  • Cubic km of Antarctic ice
  • Isotropic distribution
  • Sources unknown
  • IceCube-Gen2

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IceCube

IceCube Collaboration

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Neutrino detectors

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  • Construction phase
  • Observes Galactic centre

KM3NeT

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Angular power spectrum analysis Monte Carlo method Statistical distribution flux

Method

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Source-flux distribution

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1st moment 2nd moment Angular Power Spectrum

dNs dF ∝ { F−2.5 F⋆ < F F−1.5 F0 < F < F⋆

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Source-flux distribution

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1st moment 2nd moment Angular Power Spectrum

Free parameter:

N⋆ ∝ Iν F⋆

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N⋆ = 10

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N⋆ = 103

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N⋆ = 105

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N⋆ = ∞

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P-value 2-year IceCube

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P-value 2-year IceCube

21 observed events

  • Eν > 50 TeV

N⋆ > 82

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10-year exposure assuming N⋆ = ∞

IceCube-Gen2

KM3NeT

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10-year exposure assuming N⋆ = 104

IceCube-Gen2

KM3NeT

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Heavy Dark Matter

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  • J. Stettner, 2019
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Heavy Dark Matter

  • Tension between HESE (full sky) and

Through-Going (Northern hemisphere)

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  • J. Stettner, 2019
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SLIDE 21
  • Tension between HESE (full sky) and

Through-Going (Northern hemisphere)

  • HESE best-fit
  • 1st order Fermi-acceleration
  • 2nd order

p—p:

  • 2-component
  • DM contributing to Extra-Galactic

and Galactic emission

γ = 2.89 γ = 2 γ ≲ 2.2

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  • J. Stettner, 2019

Heavy Dark Matter

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Null hypothesis

  • Isotropic astrophysical flux: 7.5-yr HESE

Model

  • Isotropic astrophysical flux: 10-yr Through-going
  • Dark matter flux

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Decay

NFW/isothermal

  • χ → t¯

t χ → τ+τ− mDM = 400 TeV, 4 PeV

Annihilation

NFW/isothermal Boost factors

  • χχ → t¯

t χχ → τ+τ− mDM = 200 TeV, 2 PeV

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Model Null hypothesis

  • Isotropic astrophysical flux: 7.5-yr HESE
  • Isotropic astrophysical flux: 10-yr Through-going
  • Dark matter flux
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Ntot

ν = NAstr ν

+ NAtm

ν

+ NDM,EG

ν

+ NDM,Gal

ν

Isotropic Anisotropic

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Null hypothesis Model

  • Isotropic astrophysical flux: 7.5-yr HESE
  • Isotropic astrophysical flux: 10-yr Through-going
  • Dark matter flux
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P-value 6-year IceCube HESE

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33 Observed events [60-200 TeV] Model


  • NFW density profile

Free parameters: Cross section & Lifetime

χ → τ+τ−, mDM = 400 TeV χχ → τ+τ−, mDM = 200 TeV

95 % CL

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P-value 6-year IceCube HESE

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33 Observed events [60-200 TeV] Model


  • NFW density profile

Constraints

  • [s]
  • [

]

  • χ → τ+τ−, mDM = 400 TeV

χχ → τ+τ−, mDM = 200 TeV τDM = 4.7 ⋅ 1028 < σv > = 1.2 ⋅ 10−22 cm3/s Nann ∝ ρ2 Ndec ∝ ρ

95 % CL

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P-value 10-year IceCube-Gen2 and KM3NeT

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95 % CL 95 % CL

Decay Annihilation χχ → τ+τ−

χ → τ+τ−

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P-value 10-year IceCube-Gen2, IceCube, KM3NeT

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95 % CL

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106 107 Dark Matter mass, mDM [GeV] 1027 1028 1029 Dark Matter lifetime, τDM [s]

IceCube-Gen2 IceCube

106 107 Dark Matter mass, mDM [GeV] 1026 1027 1028 1029 Dark Matter lifetime, τDM [s]

DM → t¯ t

IceCube-Gen2 IceCube

Preliminary Preliminary

DM → t¯ t DM → τ+τ−

Decay constraints 10-yr IceCube-Gen2, IceCube

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Summary

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  • Angular Power Spectrum powerful probe
  • 2-year of IceCube data with 21 events already constrains
  • With 10-yr IceCube-Gen2 & KM3NeT exposure we can constrain bright sources
  • The tension between HESE and Through-Going datasets
  • Look for DM signal using IceCube HESE and TG KM3NeT exposure

N⋆ > 82

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Summary

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Thank you for your attention

  • Angular Power Spectrum powerful probe
  • 2-year of IceCube data with 21 events already constrains
  • With 10-yr IceCube-Gen2 & KM3NeT exposure we can constrain bright sources
  • The tension between HESE and Through-Going datasets
  • Look for DM signal using IceCube HESE and TG KM3NeT exposure

N⋆ > 82

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Backup slides

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Source-flux distribution

Olber’s paradox Homogeneous Univers, Euclidean space

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P-value 10-year IceCube-Gen2,KM3NeT

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P-value 10-year IceCube-Gen2 Decay

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P-value 10-year IceCube-Gen2 Annihilation

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Angular power spectrum

N⋆ = 100

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Analysis