High-Energy Neutrinos Michael Kachelrie NTNU, Trondheim [] - - PowerPoint PPT Presentation

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High-Energy Neutrinos Michael Kachelrie NTNU, Trondheim [] - - PowerPoint PPT Presentation

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High-Energy Neutrinos Michael Kachelrie NTNU, Trondheim [] Introduction Outline of the talk 1 Introduction 2 IceCube events properties implications 3 Astrophysical sources point sources versus diffuse flux Galactic sources

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SLIDE 1

[]

High-Energy Neutrinos

Michael Kachelrieß NTNU, Trondheim

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SLIDE 2

Introduction

Outline of the talk

1 Introduction 2 IceCube events ◮ properties ◮ implications 3 Astrophysical sources ◮ point sources versus diffuse flux ◮ Galactic sources versus extragalactic 4 PeV dark matter 5 Summary Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 2 / 33

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SLIDE 3

Introduction

Outline of the talk

1 Introduction 2 IceCube events ◮ properties ◮ implications ◮ or better speculations. . . 3 Astrophysical sources ◮ point sources versus diffuse flux ◮ Galactic sources versus extragalactic 4 PeV dark matter 5 Summary Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 2 / 33

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SLIDE 4

Introduction

Outline of the talk

1 Introduction 2 IceCube events ◮ properties ◮ implications ◮ or better speculations. . . 3 Astrophysical sources ◮ point sources versus diffuse flux ◮ Galactic sources versus extragalactic 4 PeV dark matter 5 Summary Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 2 / 33

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SLIDE 5

Introduction

Outline of the talk

1 Introduction 2 IceCube events ◮ properties ◮ implications ◮ or better speculations. . . 3 Astrophysical sources ◮ point sources versus diffuse flux ◮ Galactic sources versus extragalactic 4 PeV dark matter 5 Summary Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 2 / 33

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SLIDE 6

Introduction

Outline of the talk

1 Introduction 2 IceCube events ◮ properties ◮ implications ◮ or better speculations. . . 3 Astrophysical sources ◮ point sources versus diffuse flux ◮ Galactic sources versus extragalactic 4 PeV dark matter 5 Summary Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 2 / 33

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SLIDE 7

Introduction

1912: Victor Hess discovers cosmic rays

  • 10

20 40 60 80 1 2 3 4 5 6 7 8 9 excess ionization altitude/1000m Hess’ and Kolhoerster’s results:

“The results are most easily ex- plained by the assumption that ra- diation with very high penetrating power enters the atmosphere from above; the Sun can hardly be con- sidered as the source.”

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 3 / 33

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Introduction

1912: Victor Hess discovers cosmic rays

  • 10

20 40 60 80 1 2 3 4 5 6 7 8 9 excess ionization altitude/1000m Hess’ and Kolhoerster’s results:

Two main questions

what are they? what are their sources?

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 3 / 33

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SLIDE 9

Introduction

What do we know 100 years later?

solar modulation →

LHC ⇑

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 4 / 33

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SLIDE 10

Introduction

What do we know 100 years later?

solar modulation →

LHC ⇑

Basic information:

energy density ρcr ∼ 0.8eV/cm3 non-thermal power-law spectrum, dN/dE ∝ 1/Eα nuclear composition, few e−, γ isotropic flux for E < ∼ 1018 eV

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 4 / 33

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Introduction

The CR–γ–ν connection:

HE neutrinos and photons are unavoidable byproducts of HECRs astrophysical models, cosmogenic flux:

◮ ratio Iν/Ip determined by nuclear composition of UHECRs and source

evolution

◮ ratio Iν/Iγ determined by isospin Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 5 / 33

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SLIDE 12

Introduction

The CR–γ–ν connection:

HE neutrinos and photons are unavoidable byproducts of HECRs astrophysical models, cosmogenic flux:

◮ ratio Iν/Ip determined by nuclear composition of UHECRs and source

evolution

◮ ratio Iν/Iγ determined by isospin

astrophysical models, direct flux:

◮ model dependent fluxes: ∝ target density, . . . Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 5 / 33

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SLIDE 13

Introduction

The CR–γ–ν connection:

HE neutrinos and photons are unavoidable byproducts of HECRs astrophysical models, cosmogenic flux:

◮ ratio Iν/Ip determined by nuclear composition of UHECRs and source

evolution

◮ ratio Iν/Iγ determined by isospin

astrophysical models, direct flux:

◮ model dependent fluxes: ∝ target density, . . .

top-down DM models:

◮ large fluxes with Iν ≫ Ip ◮ ratio Iν/Ip fixed by fragmentation Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 5 / 33

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Introduction

The CR–γ–ν connection:

HE neutrinos and photons are unavoidable byproducts of HECRs astrophysical models, cosmogenic flux:

◮ ratio Iν/Ip determined by nuclear composition of UHECRs and source

evolution

◮ ratio Iν/Iγ determined by isospin

astrophysical models, direct flux:

◮ model dependent fluxes: ∝ target density, . . .

top-down DM models:

◮ large fluxes with Iν ≫ Ip ◮ ratio Iν/Ip fixed by fragmentation

prizes to win:

◮ astronomy above 100 TeV ◮ identification of CR sources ◮ determination galactic–extragalactic transition of CRs ◮ test/discover new particle physics Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 5 / 33

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SLIDE 15

Introduction

What is the bonus of HE neutrino astronomy?

astronomy with VHE photons restricted to few Mpc:

10 12 14 16 18 20 22 Gpc 100Mpc 10Mpc Mpc 100kpc 10kpc kpc log10(E/eV)

photon horizon γγ → e+e− CMB IR radio

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 6 / 33

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SLIDE 16

Introduction

What is the bonus of HE neutrino astronomy?

astronomy with VHE photons restricted to few Mpc:

10 12 14 16 18 20 22 Gpc 100Mpc 10Mpc Mpc 100kpc 10kpc kpc log10(E/eV)

photon horizon γγ → e+e− CMB IR radio ambiguity: leptonic/hadronic origin

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 6 / 33

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SLIDE 17

Introduction

HE neutrino astronomy vs UHECRs?

10 12 14 16 18 20 22 Gpc 100Mpc 10Mpc Mpc 100kpc 10kpc kpc log10(E/eV)

proton horizon photon horizon γγ → e+e− CMB IR Virgo ⇓

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 7 / 33

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SLIDE 18

Introduction

HE neutrino astronomy vs UHECRs?

10 12 14 16 18 20 22 Gpc 100Mpc 10Mpc Mpc 100kpc 10kpc kpc log10(E/eV)

proton horizon photon horizon γγ → e+e− CMB IR Virgo ⇓

◮ large statistics of UHECRs, well-suited horizon scale ◮ but no conclusive evidence that qB is small enough Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 7 / 33

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Introduction

What is the bonus of HE neutrino astronomy?

Neutrino astronomy: small σνN large λν but also “large” uncertainty δϑ > ∼ 0.1◦ − 1◦

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 8 / 33

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SLIDE 20

Introduction

What is the bonus of HE neutrino astronomy?

Neutrino astronomy: small σνN large λν but also “large” uncertainty δϑ > ∼ 0.1◦ − 1◦ small event numbers: ∼ 1/yr for PAO or ICECUBE

103 102 10 1 10-1 1022 1021 1020 1019 1018 1017 1016 j(E) E2 [eV cm-2 s-1 sr-1] E [eV] WB max 0.2 CR flux

⇒ identification of steady sources challenging

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 8 / 33

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SLIDE 21

Introduction

What is the bonus of HE neutrino astronomy?

Neutrino astronomy: small σνN large λν but also “large” uncertainty δϑ > ∼ 0.1◦ − 1◦ small event numbers: ∼ 1/yr for PAO or ICECUBE

103 102 10 1 10-1 1022 1021 1020 1019 1018 1017 1016 j(E) E2 [eV cm-2 s-1 sr-1] E [eV] WB max 0.2 CR flux

⇒ identification of steady sources challenging correlation with AGN flares, GRBs diffuse flux detected first

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 8 / 33

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SLIDE 22

Introduction

IceCube

[ ]

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 9 / 33

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Introduction

IceCube:Top View

AMANDA SPASE-2 South Pole Dome Skiway 100 m Grid North

IceCube

Counting House

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 10 / 33

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Introduction

IceCube

80 Strings 4800 PMT

1400 m 2400 m

AMANDA

South Pole IceTop Skiway

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 10 / 33

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Introduction Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 10 / 33

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Icecube events

Icecube: 2 events presented at Neutrino 2012

2 cascade events close to Emin = 1015 eV, bg = 0.14

Two events passed the selection criteria

8

Run119316-Event36556705 Jan 3rd 2012 NPE 9.628x104 Number of Optical Sensors 312 Run118545-Event63733662 August 9th 2011 NPE 6.9928x104 Number of Optical Sensors 354

CC/NC interactions in the detector MC 2 events / 672.7 days - background (atm. + conventional atm. ) expectation 0.14 events preliminary p-value: 0.0094 (2.36

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 11 / 33

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Icecube events

Icecube: prompt neutrino analysis

[A. Schukraft, NOW2012 ]

  • Michael Kachelrieß (NTNU Trondheim)

High-Energy Neutrinos Oslo 2014 12 / 33

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Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . .

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 13 / 33

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Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . . anisotropies

◮ event cluster around GC ◮ enhancement close to Galactic plane? Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 13 / 33

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Icecube events

IceCube events: 2 years 28 events

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 14 / 33

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Icecube events

IceCube events: 3 years 36 events

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 14 / 33

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SLIDE 32

Icecube events

KS test for ansiotropy in RA

0.2 0.4 0.6 0.8 1 50 100 150 200 250 300 350 RA C(event) isotropic

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 15 / 33

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SLIDE 33

Icecube events

KS test for ansiotropy in RA

0.2 0.4 0.6 0.8 1 50 100 150 200 250 300 350 RA C(event) isotropic

p = 20% for 2 yr, p = 8% for 3 yr data set

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 15 / 33

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SLIDE 34

Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . . anisotropies

◮ event cluster around GC ◮ enhancement close to Galactic plane gone? Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 16 / 33

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SLIDE 35

Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . . anisotropies

◮ event cluster around GC ◮ enhancement close to Galactic plane gone?

flux is large, close to

◮ Waxman-Bahcall estimate ◮ cascade limit: slope “is steepening”, α ∼ 2.3 − 2.5, conflict? Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 16 / 33

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SLIDE 36

Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . . anisotropies

◮ event cluster around GC ◮ enhancement close to Galactic plane gone?

flux is large, close to

◮ Waxman-Bahcall estimate ◮ cascade limit: slope “is steepening”, α ∼ 2.3 − 2.5, conflict?

CR energies Ep ∼ 20Eν ⇒ up to few×1016 eV,

◮ high for Galactic CRs ◮ lowish for cosmogenic, AGN, GRB Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 16 / 33

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Icecube events

IceCube events: specifications for candidate sources

36 events with ∼ 14 bg: flukes are possible. . . anisotropies

◮ event cluster around GC ◮ enhancement close to Galactic plane gone?

flux is large, close to

◮ Waxman-Bahcall estimate ◮ cascade limit: slope “is steepening”, α ∼ 2.3 − 2.5, conflict?

CR energies Ep ∼ 20Eν ⇒ up to few×1016 eV,

◮ high for Galactic CRs ◮ lowish for cosmogenic, AGN, GRB

initial flavor ratio consistent with 1:1:1 ?

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 16 / 33

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SLIDE 38

Icecube events

Flavour ratio

ratio R = Nsh/Ntr ∼ (Ne + Nτ)/Nµ ∼ 21/7 consistent with 1:1:1 including atm. bg. favors (weakly) 1:0:0 at source

[Mena, Palomares, Vincent ’14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 17 / 33

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SLIDE 39

Icecube events

Flavour ratio

ratio R = Nsh/Ntr ∼ (Ne + Nτ)/Nµ ∼ 21/7 consistent with 1:1:1 including atm. bg. favors (weakly) 1:0:0 at source

[Mena, Palomares, Vincent ’14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 17 / 33

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Astrophysical sources

Sources of high-energy neutrinos

Galactic sources: Galactic plane and bulge SNR hypernova, GRB micro-quasar, . . . Extragalactic sources: diffuse flux from normal/starburst galaxies cosmogenic neutrinos diffuse flux from AGN GRB single AGN, . . . Dark matter decays, topological defects

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 18 / 33

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Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs: “Hillas”

X = 30 g/cm2

0.01 0.1 1 10 100 1011 1012 1013 1014 1015 1016 1017 1018 E2.6 I(E) [GeV1.6 m-2 sr-1 s-1] E/eV p He C O Fe total

[MK, S.Ostapchenko ’14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 19 / 33

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SLIDE 42

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs: “escape” X = 30 g/cm2

0.01 0.1 1 10 100 1000 1011 1012 1013 1014 1015 1016 1017 1018 E2.6 I(E) [GeV1.6 m-2 sr-1 s-1] E/eV p He C O Fe total

[MK, S.Ostapchenko ’14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 19 / 33

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SLIDE 43

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs:

X = 30 g/cm2

0.01 0.1 1 10 100 1000 1011 1012 1013 1014 1015 1016 1017 1018 E2.6 I(E) [GeV1.6 m-2 sr-1 s-1] E/eV Hillas Polygonato Escape

[MK, S.Ostapchenko ’14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 19 / 33

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SLIDE 44

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs:

X = 30 g/cm2

0.01 0.1 1 10 100 1000 1011 1012 1013 1014 1015 1016 1017 1018 E2.6 I(E) [GeV1.6 m-2 sr-1 s-1] E/eV Hillas Polygonato Escape

model dependence impacts background in IceCube

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 19 / 33

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SLIDE 45

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs

gives negligible contribution to IceCube signal τpp is too small even towards GC gas is concentrated as n(z) ∼ n0 exp[−(z|/z12)2] with z12 ∼ 0.2 kpc results apply also to other normal galaxies as starburst galaxies:

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 20 / 33

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SLIDE 46

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs

gives negligible contribution to IceCube signal τpp is too small even towards GC gas is concentrated as n(z) ∼ n0 exp[−(z|/z12)2] with z12 ∼ 0.2 kpc results apply also to other normal galaxies as starburst galaxies: magnetic fields factor 100 higher:

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 20 / 33

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SLIDE 47

Astrophysical sources CR sea interactions in bulge and plane

Neutrinos from Galactic Sea CRs

gives negligible contribution to IceCube signal τpp is too small even towards GC gas is concentrated as n(z) ∼ n0 exp[−(z|/z12)2] with z12 ∼ 0.2 kpc results apply also to other normal galaxies as starburst galaxies: magnetic fields factor 100 higher: if knee is caused by

◮ diffusion: Ecr ∼ B, neutrino knee at few ×1016 eV ◮ source: Emax ∼ BCR, neutrino knee at few ×1014 eV Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 20 / 33

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SLIDE 48

Astrophysical sources Galactic point sources

Galactic sources

at low energies:

◮ many sources, large confinement times Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 21 / 33

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Astrophysical sources Galactic point sources

Galactic sources

at low energies:

◮ many sources, large confinement times

⇒ average CR sea plus few recent sources

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 21 / 33

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SLIDE 50

Astrophysical sources Galactic point sources

Galactic sources

at low energies:

◮ many sources, large confinement times

⇒ average CR sea plus few recent sources

close to the knee:

◮ CRs in PeV range spread fast ◮ few extreme sources Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 21 / 33

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SLIDE 51

Astrophysical sources Galactic point sources

Galactic sources

at low energies:

◮ many sources, large confinement times

⇒ average CR sea plus few recent sources

close to the knee:

◮ CRs in PeV range spread fast ◮ few extreme sources

⇒ inhomogenous CR sea, extended sources ⇒ no clear distinction between point sources

  • vs. Galactic bulge + plane cases

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 21 / 33

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SLIDE 52

Astrophysical sources Galactic point sources

Point source in gamma-ray

source HESS J1825-137

[Neronov, Semikoz, Tchernin ’13 ]

0.00100 0.00150 0.00200 0.00250 0.00300 0.00350 0.00400 0.00450 0.00500 0.00550 0.00600 180.000 225.000 270.000 315.000 0.000 45.000 90.000 135.000

  • 9

.

  • 6

.

  • 3

. 0.000 30.000 6 . 9 .

Kookaburra region HESS J1632 region Galactic Center HESS J1825 region Cygnus region Vela region Crab

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 22 / 33

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SLIDE 53

Astrophysical sources Galactic point sources

Gamma-ray point sources

flux from HESS J1825-137, GC and GP

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 23 / 33

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SLIDE 54

Astrophysical sources Galactic point sources

(Isotropic) photon limits

101 102 103 104 Eγ [TeV] 10−10 10−9 10−8 10−7 10−6 10−5 10−4 E2Jγ [GeV cm−2 s−1 sr−1]

8.5kpc 20kpc 30kpc GRAPES-3 UMC HEGRA EAS-TOP IC-40 (γ) KASCADE GAMMA CASA-MIA

[Ahlers, Murase ’13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 24 / 33

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SLIDE 55

Astrophysical sources Diffuse extragalactic flux

Diffuse ν flux from normal and starburst galaxies

10

3

10

5

10

7

10

9

10

11

10

−9

10

−8

10

−7

10

−6

10

−5

Eν [GeV] E2

ν Φν [GeV/cm2 s sr]

0.1 km2 1 km2 WB Bound Star Bursts AMANDA(νµ); Baikal(νe) Atmospheric→ ← GZK

[Loeb, Waxman ’06 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 25 / 33

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SLIDE 56

Astrophysical sources Diffuse extragalactic flux

Diffuse ν flux from normal and starburst galaxies

10

3

10

5

10

7

10

9

10

11

10

−9

10

−8

10

−7

10

−6

10

−5

Eν [GeV] E2

ν Φν [GeV/cm2 s sr] 0.1 km2 1 km2 WB Bound Star Bursts AMANDA(νµ); Baikal(νe) Atmospheric→ ← GZK

[Loeb, Waxman ’06 ]

too optimistic?

◮ fraction of starbust galaxies? ◮ all calorimetric? Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 25 / 33

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SLIDE 57

Astrophysical sources Cosmogenic neutrinos

Reminder: The photon horizon

10 12 14 16 18 20 22 Gpc 100Mpc 10Mpc Mpc 100kpc 10kpc kpc log10(E/eV)

photon horizon γγ → e+e− CMB IR radio

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 26 / 33

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SLIDE 58

Astrophysical sources Cascade spectrum

Development of the elmag. cascade:

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 27 / 33

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SLIDE 59

Astrophysical sources Cascade spectrum

Development of the elmag. cascade:

analytical estimate:

[Strong ’74, Berezinsky, Smirnov ’75 ]

Jγ(E) =    K(E/εX)−3/2 at E ≤ εX K(E/εX)−2 at εX ≤ E ≤ εa at E > εa three regimes:

◮ Thomson cooling:

Eγ = 4 3 εbbE2

e

m2

e

≈ 100 MeV Ee 1TeV 2

◮ plateau region: ICS Eγ ∼ Ee ◮ above pair-creation threshold smin = 4Eγεbb = 4m2

e:

flux exponentially suppressed

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 27 / 33

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SLIDE 60

Astrophysical sources Cascade spectrum

Fermi limit for cosmogenic neutrinos:

[Berezinsky et al. ’10 ]

10 16 10 17 10 18 10 19 10 20 10 21 10 22 10
  • 1
10 10 1 10 2 10 3 10 4 10 5 10 6 1 21 1 2 IceCube 5yr tilted 2.0 RICE Auger diff. E
  • 2
cascade ANITA E 2 J(E), eVcm
  • 2
s
  • 1
sr
  • 1
E, eV ANITA-lite Auger 2.6 nadir JEM-EUSO BAIKAL e = 10 22 m=3

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 28 / 33

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SLIDE 61

Astrophysical sources Cascade spectrum

Cascade limit: α = 2.1

1 10 100 1000 10000 1e+10 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E2 J(E) [eV/cm2 s sr] E/eV gamma nu Fermi EGRB

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 29 / 33

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SLIDE 62

Astrophysical sources Cascade spectrum

Cascade limit: α = 2.3

1 10 100 1000 10000 1e+10 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E2 J(E) [eV/cm2 s sr] E/eV gamma nu Fermi EGRB

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 29 / 33

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SLIDE 63

Astrophysical sources Cascade spectrum

Cascade limit: α = 2.5

1 10 100 1000 10000 1e+10 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E2 J(E) [eV/cm2 s sr] E/eV gamma nu Fermi EGRB

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 29 / 33

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SLIDE 64

Astrophysical sources Cascade spectrum

IceCube limit on GRBs

215 optically detected GRBs stacked

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 30 / 33

slide-65
SLIDE 65

Astrophysical sources Cascade spectrum

IceCube limit on GRBs

215 optically detected GRBs stacked

10

4

10

5

10

6

10

7

Neutrino Energy (GeV) 10

  • 9

10

  • 8

E2 Φν (GeV cm−2 s−1 sr−1 )

Waxman & Bahcall IC40 limit IC40 Guetta et al. IC40+59 Combined limit IC40+59 Guetta et al.

10

  • 1

10 E2 Fν (GeV cm−2 )

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 30 / 33

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SLIDE 66

PeV dark matter

PeV dark matter

re-incarnation of SHDM idea for AGASA excess: non-hermal DM avoids cascacde limit Galactic anisotropy some option to move initial flavor ration 1 : 2 : 0 towards 1 : 0 : 0

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 31 / 33

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SLIDE 67

PeV dark matter

PeV dark matter

re-incarnation of SHDM idea for AGASA excess: non-hermal DM avoids cascacde limit Galactic anisotropy some option to move initial flavor ration 1 : 2 : 0 towards 1 : 0 : 0

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 31 / 33

slide-68
SLIDE 68

PeV dark matter

PeV dark matter

re-incarnation of SHDM idea for AGASA excess: non-hermal DM avoids cascacde limit Galactic anisotropy some option to move initial flavor ration 1 : 2 : 0 towards 1 : 0 : 0

Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 31 / 33

slide-69
SLIDE 69

PeV dark matter

PeV dark matter

DM ΝeΝ e 15, bb 85 DM ΝeΝ e 12, cc 88 DM ee 40, qq 60

1 10 102 103 1011 1010 EΝ TeV EΝ

2dJdEΝ TeV cm2 s1 sr1

[Esmaili, Serpico ’13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 32 / 33

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SLIDE 70

PeV dark matter

PeV dark matter

102 103 0.1 1 10 EΝ TeV eventsbin

DM ΝΝ , qq E2 spec. data

[Esmaili, Serpico ’13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 32 / 33

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SLIDE 71

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33

slide-72
SLIDE 72

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33

slide-73
SLIDE 73

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33

slide-74
SLIDE 74

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33

slide-75
SLIDE 75

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33

slide-76
SLIDE 76

PeV dark matter

Summary

1 excess towards GC, consistent (?) with γ-ray data

⇒ partly Galactic origin

2 no enhancement towards Galactic plane: ◮ gas too narrow, flux too low 3 some tension with (Northern) γ-ray limits 4 extragalactic: ◮ dominant isotropic component ◮ diffuse, difficult to identify ◮ spectrum α = −2.45: cascade limit? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Neutrinos Oslo 2014 33 / 33