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

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 Sources p-p p- � γ Photo-hadronic interactions Hadro-nuclear interactions Active Galactic Nuclei Starburst Galaxies Blazars ( 4 — 6 % ) Galaxy clusters Gamma-Ray Bursts � 3

Astrophysical Sources p-p p- � γ Photo-hadronic interactions Hadro-nuclear interactions Active Galactic Nuclei Starburst Galaxies Blazars ( 4 — 6 % ) Galaxy clusters Gamma-Ray Bursts Dark Matter � 4

Neutrino detectors IceCube KM3NeT � 5

Neutrino detectors IceCube • Cubic km of Antarctic ice • Isotropic distribution • Sources unknown • IceCube-Gen2 IceCube Collaboration � 6

Neutrino detectors KM3NeT • Construction phase • Observes Galactic centre � 7

Method Angular power spectrum analysis Monte Carlo method Statistical distribution flux � 8

dF ∝ { F − 2.5 F ⋆ < F dN s Source-flux distribution F − 1.5 F 0 < F < F ⋆ 1st moment 2nd moment Angular Power Spectrum � 9

N ⋆ ∝ I ν Free parameter: � Source-flux distribution F ⋆ 1st moment 2nd moment Angular Power Spectrum � 10

N ⋆ = 10 � 11

N ⋆ = 10 3 � 12

N ⋆ = 10 5 � 13

N ⋆ = ∞ � 14

P-value 2-year IceCube � 15

� � P-value 2-year IceCube 21 observed events E ν > 50 TeV N ⋆ > 82 � 16

10-year exposure assuming � N ⋆ = ∞ KM3NeT IceCube-Gen2 � 17

10-year exposure assuming � N ⋆ = 10 4 KM3NeT IceCube-Gen2 � 18

Heavy Dark Matter J. Stettner, 2019 � 19

Heavy Dark Matter • Tension between HESE (full sky) and Through-Going (Northern hemisphere) J. Stettner, 2019 � 20

Heavy Dark Matter • Tension between HESE (full sky) and Through-Going (Northern hemisphere) • HESE best-fit � γ = 2.89 • 1st order Fermi-acceleration � γ = 2 • 2nd order p—p: � γ ≲ 2.2 • 2-component • DM contributing to Extra-Galactic and Galactic emission J. Stettner, 2019 � 21

• Isotropic astrophysical flux: 7.5-yr HESE Null hypothesis • Isotropic astrophysical flux: 10-yr Through-going Model • Dark matter flux � 22

� � � � � � • Isotropic astrophysical flux: 7.5-yr HESE Null hypothesis • Isotropic astrophysical flux: 10-yr Through-going Model • Dark matter flux Annihilation Decay NFW/isothermal NFW/isothermal Boost factors χ → t ¯ t χχ → t ¯ t χ → τ + τ − χχ → τ + τ − m DM = 400 TeV, 4 PeV m DM = 200 TeV, 2 PeV � 23

• Isotropic astrophysical flux: 7.5-yr HESE Null hypothesis • Isotropic astrophysical flux: 10-yr Through-going Model • Dark matter flux N tot ν = N Astr + N Atm + N DM , EG + N DM , Gal ν ν ν ν Anisotropic Isotropic � 24

� � P-value 6-year IceCube HESE 33 Observed events [60-200 TeV] Model 
 χ → τ + τ − , m DM = 400 TeV 95 % CL χχ → τ + τ − , m DM = 200 TeV NFW density profile Free parameters: Cross section & Lifetime � 25

� � � � � � P-value 6-year IceCube HESE 33 Observed events [60-200 TeV] Model 
 χ → τ + τ − , m DM = 400 TeV 95 % CL χχ → τ + τ − , m DM = 200 TeV NFW density profile Constraints τ DM = 4.7 ⋅ 10 28 [s] < σ v > = 1.2 ⋅ 10 − 22 cm 3 /s [ � ] N ann ∝ ρ 2 N dec ∝ ρ � 26

P-value 10-year IceCube-Gen2 and KM3NeT Annihilation χχ → τ + τ − χ → τ + τ − Decay 95 % CL 95 % CL � 27

P-value 10-year IceCube-Gen2, IceCube, KM3NeT 95 % CL � 28

Decay constraints 10-yr IceCube-Gen2, IceCube DM → τ + τ − DM → t¯ t DM → t ¯ 10 29 t 10 29 IceCube-Gen2 IceCube-Gen2 Dark Matter lifetime, τ DM [s] IceCube Dark Matter lifetime, τ DM [s] IceCube 10 28 10 28 10 27 Preliminary Preliminary 10 26 10 27 10 6 10 7 10 6 10 7 Dark Matter mass, m DM [GeV] Dark Matter mass, m DM [GeV] � 29

Summary - Angular Power Spectrum powerful probe - 2-year of IceCube data with 21 events already constrains � N ⋆ > 82 - 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 � 30

Summary - Angular Power Spectrum powerful probe - 2-year of IceCube data with 21 events already constrains � N ⋆ > 82 - 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 Thank you for your attention � 31

Backup slides � 32

Homogeneous Univers, Source-flux distribution Euclidean space Olber’s paradox � 33

P-value 10-year IceCube-Gen2,KM3NeT � 34

P-value 10-year IceCube-Gen2 Decay � 35

P-value 10-year IceCube-Gen2 Annihilation � 36

Angular power spectrum N ⋆ = 100 � 37

Analysis � 38