News from High-Energy Cosmic Rays and Neutrinos. Michael Kachelrieß NTNU, Trondheim
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1 News from High-Energy Cosmic Rays and Neutrinos Michael Kachelrieß NTNU, Trondheim []
2 Introduction Outline of the talk 1 Introduction Is progress slow? Results on Composition γ s and ν s as CR secondaries 2 Origin of the CR knee: Escape model Fluxes of groups of CR nuclei Transition to extragalactic CRs Anisotropy 3 IceCube excess Disentangling signal/prompt/background Characteristica of proposed sources 4 Conclusions Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
3 Introduction Outline of the talk 1 Introduction Is progress slow? Results on Composition γ s and ν s as CR secondaries 2 Origin of the CR knee: Escape model Fluxes of groups of CR nuclei Transition to extragalactic CRs Anisotropy 3 IceCube excess Disentangling signal/prompt/background Characteristica of proposed sources 4 Conclusions Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
4 Introduction Outline of the talk 1 Introduction Is progress slow? Results on Composition γ s and ν s as CR secondaries 2 Origin of the CR knee: Escape model Fluxes of groups of CR nuclei Transition to extragalactic CRs Anisotropy 3 IceCube excess Disentangling signal/prompt/background Characteristica of proposed sources 4 Conclusions Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
5 Introduction History 1912: Victor Hess discovers cosmic rays Two key questions what are their sources? how do they accelerate? Hess and Kolhoerster s results: 80 excess ionization altitude/00m Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
6 Introduction History 2 years later: no definite answers yet Why progress has been slow? 1 CRs diffuse in magnetic fields no astronomy possible 2 only indirect detection > 14 ev composition uncertain Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
7 Introduction History 2 years later: no definite answers yet Why progress has been slow? 1 CRs diffuse in magnetic fields no astronomy possible 2 only indirect detection > 14 ev composition uncertain How to overcome these problems? 1 Multi-messenger astronomy, γ: distinguish hadronic from leptonic, only below TeV ν: low event rates requires km 3 detectors Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
8 Introduction History 2 years later: no definite answers yet Why progress has been slow? 1 CRs diffuse in magnetic fields no astronomy possible 2 only indirect detection > 14 ev composition uncertain How to overcome these problems? 1 Multi-messenger astronomy, γ: distinguish hadronic from leptonic, only below TeV ν: low event rates requires km 3 detectors 2 improve experiments: combining different techniques (KASCADE-Grande, PAO, TA) models: new data from LHC (EPOS-LHC, QGSJET-II-04) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
9 Introduction Is Progress slow? Composition of Galactic CRs: traditional view [Gaisser, Stanev, Tilav 13 ] sr -1 s -1 ] 4 3 Proton_total He_total C_total O_total Fe_total Z=53 group Z=80 group dn/de [GeV 2.6 E 1.6 m Pamela Proton Pamela He CreamII Proton CreamII He CreamII C CreamII O CreamII Mg CreamII Si CreamII Fe Primary Energy, E [GeV] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
10 Introduction Is Progress slow? Composition of Galactic CRs: KASCADE-Grande 2013 ) 1.5 sr -1 s -1 ev -2 / (m 2.5 E EAS-TOP (Astrop.Phys.(1999)1) Tibet-III, QGSJET 01 (ApJ678(2008)1165) GAMMA (ICRC 2011) IceTop (arxiv: v1) TUNKA-133 (ICRC 2011) Yakutsk (NewJ.Phys11(2008)065008) KASCADE-Grande, QGSJET II (Astrop.Phys.36(2012)183) Akeno (J.Phys.G18(1992)423) AGASA (ICRC 2003) HiResI (PRL0(2008)11) HiResII (PRL0(2008)11) AUGER (arxiv:17:4809) AUGER AMIGA infill (ICRC 2011) diff. flux dj/de 15 KASCADE, all-part., QGSJET II (see Appendix A) KASCADE, light (p), QGSJET II (see Appendix A) KASCADE, medium (He+C+Si), QGSJET II (see Appendix A) KASCADE, heavy (Fe), QGSJET II (see Appendix A) KASCADE-Grande, all-part., QGSJET II (this work) KASCADE-Grande, light (p), QGSJET II (this work) KASCADE-Grande, medium (He+C+Si), QGSJET II (this work) KASCADE-Grande, heavy (Fe), QGSJET II (this work) primary energy E/eV 18 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
11 Introduction Is Progress slow? Composition of Galactic CRs: Auger [arxiv: ] 600 Sibyll 2.1 Sibyll 2.1 Sibyll 2.1 Fe N 500 He p Auger 400 log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p = p = QGSJET II-04 QGSJET II-04 QGSJET II log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p < -3 p = EPOS-LHC EPOS-LHC EPOS-LHC log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p = p = X max [g/cm 2 ] X max [g/cm 2 ] X max [g/cm 2 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
12 Introduction Is Progress slow? Composition of Galactic CRs: Auger [arxiv: ] 600 Sibyll 2.1 Sibyll 2.1 Sibyll 2.1 Fe N 500 He p Auger 400 log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p = p = QGSJET II-04 QGSJET II-04 QGSJET II log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p < -3 p = EPOS-LHC EPOS-LHC EPOS-LHC log(e/ev) = log(e/ev) = log(e/ev) = composition ev consistent with N 200 p < -4 p = p = O( 0 50% p, 50% He+N, < 20%Fe ) X max [g/cm 2 ] X max [g/cm 2 ] X max [g/cm 2 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
13 Introduction Is Progress slow? Composition of Galactic CRs: 600 Sibyll 2.1 Sibyll 2.1 Sibyll 2.1 Fe N 500 He p Auger 400 log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p = p = QGSJET II-04 QGSJET II-04 QGSJET II log(e/ev) = log(e/ev) = log(e/ev) = N p < -4 p < -3 p = EPOS-LHC EPOS-LHC EPOS-LHC log(e/ev) = log(e/ev) = log(e/ev) = composition ev consistent with N p < -4 p = p = O( 0 50% p, 50% He+N, < 20%Fe ) early transition X max [g/cm 2 ] from Galactic X max [g/cm to 2 ] extragalactic X max CRs [g/cm 2 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
14 Introduction Is Progress slow? Transition to extragalactic CRs anisotropy limits dipole quadrupole Upper Limit - Dipole Amplitude Z=1 Z=26 1 E [EeV] Upper Limit - Amplitude λ Z=1 Z=26 1 E [EeV] dominant light Galactic composition around E = 18 ev excluded [Giacinti, MK, Semikoz, Sigl ( 12), PAO 13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
15 Introduction Pion peak The pion peak CR scattering on gas or photons: pp mesons, baryons e, γ, ν, p the lightest mesons, π 0 and π ±, are produced most often decays: π 0 2γ and π ± 3ν + e ± Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
16 Introduction Pion peak The pion peak π 0 γ(k 1 ) + γ(k 2 ) at rest: energy conservation: mπ c 2 /2 = E 1 = E 2 momentum conservation: k1 = k 2 moving back-to-back Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
17 Introduction Pion peak The pion peak π 0 γ(k 1 ) + γ(k 2 ) at rest: energy conservation: mπ c 2 /2 = E 1 = E 2 momentum conservation: k1 = k 2 moving back-to-back π 0 is moving: decay isotropic in rest-frame dn/deγ =const. Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
18 Introduction Pion peak The pion peak π 0 γ(k 1 ) + γ(k 2 ) at rest: energy conservation: mπ c 2 /2 = E 1 = E 2 momentum conservation: k1 = k 2 moving back-to-back π 0 is moving: decay isotropic in rest-frame dn/deγ =const. min./max. photon energies Emin max = γ m π 0 2 (1 ± β) = m π ± β 1 β Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
19 Introduction Pion peak The pion peak π 0 γ(k 1 ) + γ(k 2 ) at rest: energy conservation: mπ c 2 /2 = E 1 = E 2 momentum conservation: k1 = k 2 moving back-to-back π 0 is moving: decay isotropic in rest-frame dn/deγ =const. min./max. photon energies Emin max = γ m π 0 2 (1 ± β) = m π 0 2 geometric mean Emin E max = m π ± β 1 β Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
20 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
21 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
22 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
23 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
24 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
25 Introduction Pion peak The pion peak n γ ln(m π /2) ln(e γ ) independent of velocity distribution of pions: symmetric photon distribution w.r.t. m π 0/2 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
26 Introduction Pion peak The pion peak: pp interactions n γ ln(m π /2) ln(e γ ) low threshold & approx. Feynman scaling Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec. 14 / 53
27 Introduction Pion peak The pion peak: pp interactions n γ ln(m π /2) ln(e γ ) low threshold & approx. Feynman scaling dn γ /de dn CR /de Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec. 14 / 53
28 Introduction Pion peak The pion peak: pγ interactions n γ ln(m π /2) ln(e γ ) threshold E th > m π m p /ε γ 16 ev with ε γ < ev Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
29 Introduction Pion peak The pion peak: pγ interactions n γ ln(m π /2) ln(e γ ) threshold E th > m π m p /ε γ 16 ev with ε γ < ev dn γ /de { E 1 dn CR /de for E < E th for E > E th Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
30 Introduction Pion peak The pion peak: Neutrinos from pp and pγ interactions Only change from px Y γ to px Y ν: two mass scales mπ, m µ two boxes Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
31 Introduction Pion peak The pion peak: Neutrinos from pp and pγ interactions Only change from px Y γ to px Y ν: two mass scales mπ, m µ two boxes for E ν m π, m µ the same picture Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
32 Introduction Pion peak The pion peak: Neutrinos from pp and pγ interactions Only change from px Y γ to px Y ν: two mass scales mπ, m µ two boxes for E ν m π, m µ the same picture for a single source: pp: dnν /de dn CR /de pγ: dn ν /de { E 1 dn CR /de for E < E th for E > E th steeper spectra for pγ as result of Emax distribution and evolution Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
33 Introduction Pion peak Observing the π 0 bump in SNR W44: - W44 s -1 ) -2 dn/de (erg cm 2 E Best-fit broken power law Fermi-LAT AGILE (Giuliani et al. 2011) 0 π -decay Bremsstrahlung Bremsstrahlung with Break 8 9 Energy (ev) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
34 Introduction Pion peak Observing the π 0 bump in SNR W44: - W44 s -1 ) -2 dn/de (erg cm 2 E Best-fit broken power law Fermi-LAT AGILE (Giuliani et al. 2011) π 0 -decay Bremsstrahlung Bremsstrahlung with Break 8 9 Energy (ev) strong evidence for proton acceleration Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
35 Knee explanations Cosmic Ray Knee: steepening γ 0.4 at few 15 ev. ) 1.5 s -1 sr -1 ev -2 J(E) (m RHIC (p-p) HERA (γ-p) Equivalent c.m. energy 3 Tevatron (p-p) 4 7 TeV 14 TeV LHC (p-p) s pp (GeV) 5 HiRes-MIA HiRes I HiRes II Auger Scaled flux E ATIC PROTON RUNJOB KASCADE (QGSJET 01) KASCADE (SIBYLL 2.1) KASCADE-Grande 2009 Tibet ASg (SIBYLL 2.1) Energy 20 (ev/particle) 21 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
36 Knee explanations Cosmic Ray Knee: 3 explanations. ) Equivalent c.m. energy 3 4 s pp (GeV) 5 6 s -1 sr -1 ev -2 J(E) (m RHIC (p-p) HERA (γ-p) Tevatron (p-p) 7 TeV 14 TeV LHC (p-p) HiRes-MIA HiRes I HiRes II Auger Scaled flux E ATIC KASCADE (QGSJET 01) 14 PROTON RUNJOB KASCADE (SIBYLL 2.1) KASCADE-Grande 2009 Tibet ASg (SIBYLL 2.1) Energy (ev/particle) change of interactions at multi-tev energies: excluded by LHC Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
37 Knee explanations Cosmic Ray Knee: 3 explanations. change of interactions at multi-tev energies: excluded by LHC change of propagation at R L l coh or E c ZeB l coh : change in diffusion from D(E) E 1/3 to Hall diffusion D(E) E small-angle scattering D(E) E 2 something intermediate? unavoidable effect, but for B few µg and l coh 30 pc at too high energy: E c /Z 15 B l c µg pc Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
38 Knee explanations Cosmic Ray Knee: 3 explanations maximal rigidity of dominant CR sources e.g. Hillas model E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] p He C O Fe total E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
39 Knee explanations Cosmic Ray Knee: 3 explanations maximal rigidity of dominant CR sources e.g. Hillas model E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] p He C O Fe total E/eV i = 1,...,3 types of CR sources, with slopes α A,i, rel. fractions f A,i Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
40 Knee explanations Cosmic Ray Knee: 3 explanations maximal rigidity of dominant CR sources e.g. Hillas model E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] p He C O Fe total E/eV i = 1,...,3 types of CR sources, with slopes α A,i, rel. fractions f A,i no reliable estimate of E max,i, α A,i, and f A,i fit of many-parameter model to two observables: I tot and ln(a) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
41 Knee explanations Cosmic Ray Knee: 3 explanations maximal energy: Gaisser, Stanev & Tilav version [ ] <lna> IC40/IT40 Kascade Tunka-133 HiResMia HiRes Auger TA H4a H3a Global Fit Global Fit with Population Primary Energy, E [GeV] 9 11 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
42 Knee explanations Propagation in turbulent magnetic fields: Galactic magnetic field: regular + turbulent component turbulent: fluctuations on scales l min AU to l max ( 150) pc Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
43 Knee explanations Propagation in turbulent magnetic fields: Galactic magnetic field: regular + turbulent component turbulent: fluctuations on scales l min AU to l max ( 150) pc CRs scatter mainly on field fluctuations B(k) with kr L 1. Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
44 Knee explanations Propagation in turbulent magnetic fields: Galactic magnetic field: regular + turbulent component turbulent: fluctuations on scales l min AU to l max ( 150) pc CRs scatter mainly on field fluctuations B(k) with kr L 1. slope of power spectrum P(k) k α determines energy dependence of diffusion coefficient D(E) E β as β = 2 α: Kolmogorov α = 5/3 β = 1/3 Kraichnan α = 3/2 β = 1/2 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
45 Knee explanations Propagation in turbulent magnetic fields: Galactic magnetic field: regular + turbulent component turbulent: fluctuations on scales l min AU to l max ( 150) pc CRs scatter mainly on field fluctuations B(k) with kr L 1. slope of power spectrum P(k) k α determines energy dependence of diffusion coefficient D(E) E β as β = 2 α: Kolmogorov α = 5/3 β = 1/3 Kraichnan α = 3/2 β = 1/2 observed energy spectrum of primaries: injection: dn/de E α observed: dn/de E α β α = 3/2 and β = 1/2 simplest combination, but degeneracies Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
46 Knee explanations Propagation in turbulent magnetic fields: Galactic magnetic field: regular + turbulent component turbulent: fluctuations on scales l min AU to l max ( 150) pc CRs scatter mainly on field fluctuations B(k) with kr L 1. slope of power spectrum P(k) k α determines energy dependence of diffusion coefficient D(E) E β as β = 2 α: Kolmogorov α = 5/3 β = 1/3 Kraichnan α = 3/2 β = 1/2 observed energy spectrum of primaries: injection: dn/de E α observed: dn/de E α β α = 3/2 and β = 1/2 simplest combination, but degeneracies anisotropy δ = 3D ij i ln(n) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
47 Knee explanations Our approach: use model for Galactic magnetic field calculate trajectories x(t) via F L = qv B. Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
48 Knee explanations Our approach: use model for Galactic magnetic field calculate trajectories x(t) via F L = qv B. as preparation, let s calculate diffusion tensor in pure, isotropic turbulent magnetic field Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
49 Knee explanations Eigenvalues of D ij = x i x j /(2t) for E = 15 ev D(1PeV) (cm 2 /s) 1e+29 1e+28 d 3 d 2 d 1D Time (kyr) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
50 Knee explanations Eigenvalues of D ij = x i x j /(2t) for E = 15 ev D(1PeV) (cm 2 /s) 1e+29 1e+28 d 3 d 2 d 1D Time (kyr) asymptotic value is smaller than extrapolated Galprop value [Giacinti, MK, Semikoz ( 12) ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
51 Knee explanations Knee from Cosmic Ray Escape l coh and regular field B(x) fixed from observations LOFAR: lcoh < pc in disc determine magnitude of random B rms (x) from grammage X(E) Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
52 Knee explanations Knee from Cosmic Ray Escape l coh and regular field B(x) fixed from observations LOFAR: lcoh < pc in disc determine magnitude of random B rms (x) from grammage X(E) X(E) in g/cm β=1, L=pc β=0.1, L=pc 0.01 β=1/8, L=25pc δ=1/3 AMS-02 (a) AMS-02 (b) Jones E/Z in ev Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
53 Knee explanations Knee from Cosmic Ray Escape l coh and regular field B(x) fixed from observations LOFAR: lcoh < pc in disc determine magnitude of random B rms (x) from grammage X(E) X(E) in g/cm β=1, L=pc β=0.1, L=pc 0.01 β=1/8, L=25pc δ=1/3 AMS-02 (a) AMS-02 (b) Jones E/Z in ev prefers weak random fields fluxes I A (E) of all isotopes fixed by low-energy data Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
54 Knee explanations Galactic CRs: KASCADE-Grande 2013 ) 1.5 sr -1 s -1 ev -2 / (m EAS-TOP (Astrop.Phys.(1999)1) Tibet-III, QGSJET 01 (ApJ678(2008)1165) GAMMA (ICRC 2011) IceTop (arxiv: v1) TUNKA-133 (ICRC 2011) Yakutsk (NewJ.Phys11(2008)065008) KASCADE-Grande, QGSJET II (Astrop.Phys.36(2012)183) Akeno (J.Phys.G18(1992)423) AGASA (ICRC 2003) HiResI (PRL0(2008)11) HiResII (PRL0(2008)11) AUGER (arxiv:17:4809) AUGER AMIGA infill (ICRC 2011) diff. flux dj/de E KASCADE, all-part., QGSJET II (see Appendix A) KASCADE, light (p), QGSJET II (see Appendix A) KASCADE, medium (He+C+Si), QGSJET II (see Appendix A) KASCADE, heavy (Fe), QGSJET II (see Appendix A) KASCADE-Grande, all-part., QGSJET II (this work) KASCADE-Grande, light (p), QGSJET II (this work) KASCADE-Grande, medium (He+C+Si), QGSJET II (this work) KASCADE-Grande, heavy (Fe), QGSJET II (this work) primary energy E/eV 18 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
55 Knee explanations Knee from Cosmic Ray Escape: energy spectra protons from X(E): E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] B=0.1 B=1 KASCADE-Grande 0 1e+15 1e+16 1e+17 E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
56 Knee explanations Knee from Cosmic Ray Escape: He energy spectra 13 E 2.5 F(E) [ev 2.5 /cm 2 /s/sr] PAMELA 2011 CREAM-2011 KASCADE Grande KASCADE 2013 He 5 pc e+ 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E [ev] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
57 Knee explanations Knee from Cosmic Ray Escape: CNO energy spectra 13 E 2.5 F(E) [ev 2.5 /cm 2 /s/sr] KASCADE Grande CNO KASCADE 2013 CREAM C+O 9 CNO 25 pc e+12 1e+13 1e+14 1e+15 1e+16 1e+17 1e+18 1e+19 E [ev] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
58 Knee explanations Knee from Cosmic Ray Escape: total energy spectra E 2.5 F(E) [ev 2.5 /cm 2 /s/sr] Tibet KASCADE Grande Auger 2013 P He CNO Si Fe total E [ev] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
59 Knee explanations Transition to extragalactic CRs E 2.5 F(E) [ev 2.5 /cm 2 /s/sr] Tibet KASCADE Grande Auger 2013 P 2.7 He 2.57 CNO Si+Mg+Fe 25 pc Extra-Galactic total E [ev] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
60 Knee explanations Transition to extragalactic CRs E 2.5 F(E) [ev 2.5 /cm 2 /s/sr] Tibet KASCADE Grande Auger 2013 P 2.7 He 2.57 CNO Si+Mg+Fe 25 pc Extra-Galactic total E [ev] at E 2 17 ev: F gal (E) : F exgal (E) = 1 : 1 at E 2 18 ev: F gal (E) : F exgal (E) = 0 : 1 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
61 Knee explanations Knee from Cosmic Ray Escape: ln(a) ln(a) KASCADE-Grande KASCADE IceCube TUNKA Auger 0% exgal p p/fe exgal. mix 0 1e+15 1e+16 1e+17 1e+18 1e+19 1e+20 E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
62 Knee explanations Knee from Cosmic Ray Escape: ln(a) ln(a) KASCADE-Grande KASCADE IceCube TUNKA Auger 0% exgal p p/fe exgal. mix 0 1e+15 1e+16 1e+17 1e+18 1e+19 1e+20 E/eV exgal. mix: 60% p, 25% He, 15% N Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
63 Knee explanations Knee from Cosmic Ray Escape: dipole anisotropy dipole EAS-TOP IceCube PAO dipole E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
64 Knee explanations Knee from Cosmic Ray Escape: dipole anisotropy Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
![IceCube Neutrinos IceCube [ ] Michael Kachelrieß (NTNU Trondheim)](/docs-images/73/68107251/images/65-0.jpg "High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec.")
65 IceCube Neutrinos IceCube [ ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
66 IceCube Neutrinos Icecube: 2 events presented at Neutrino cascade events close to E min = 15 ev, bg = 0.14 Two events passed the selection criteria 2 events / days - background (atm. + conventional atm. ) expectation 0.14 events preliminary p-value: (2.36 Run Event Jan 3 rd 2012 NPE 9.628x 4 Number of Optical Sensors 312 CC/NC interactions in the detector MC Run Event August 9 th 2011 NPE x 4 Number of Optical Sensors 354 Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53 8
67 IceCube Neutrinos Icecube: prompt neutrino analysis [A. Schukraft, NOW2012 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
68 IceCube Neutrinos IceCube events: specifications for candidate sources 36 events with 14 bg: flukes are possible... Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
69 IceCube Neutrinos 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
70 IceCube Neutrinos IceCube events: 2 years 28 events Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
71 IceCube Neutrinos IceCube events: 3 years 36 events Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
72 IceCube Neutrinos Column density of gas [Evoli, Grasso, Maccione 07 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
73 IceCube Neutrinos Diffuse ν flux from Galactic plane [Evoli, Grasso, Maccione 07 ] averaged over 1,2,5 degrees Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
74 IceCube Neutrinos 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
75 IceCube Neutrinos 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 , conflict? Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
76 IceCube Neutrinos 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 , conflict? CR energies E p 20E ν up to few 16 ev, high for Galactic CRs lowish for cosmogenic, AGN, GRB Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
77 IceCube Neutrinos 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 , conflict? CR energies E p 20E ν up to few 16 ev, high for Galactic CRs lowish for cosmogenic, AGN, GRB initial flavor ratio consistent with 1:1:1? Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
78 IceCube Neutrinos Flavour ratio ratio R = N sh /N tr (N e + N τ )/N µ 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
79 IceCube Neutrinos Flavour ratio ratio R = N sh /N tr (N e + N τ )/N µ 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
80 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
81 Astrophysical sources Diffuse extragalactic flux Diffuse ν flux from normal and starburst galaxies 5 E 2 ν Φ ν [GeV/cm2 s sr] AMANDA(ν µ ); Baikal(ν e ) Star Bursts 0.1 km 2 WB Bound 9 Atmospheric 1 km 2 GZK E ν [GeV] [Loeb, Waxman 06 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
82 Astrophysical sources Diffuse extragalactic flux Diffuse ν flux from normal and starburst galaxies 5 E 2 ν Φ ν [GeV/cm2 s sr] 6 AMANDA(ν µ ); Baikal(ν e ) 7 Star Bursts km 2 WB Bound Atmospheric 1 km 2 GZK E ν [GeV] too optimistic? fraction of starbust galaxies? all calorimetric? [Loeb, Waxman 06 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
83 Astrophysical sources Diffuse extragalactic flux Reminder: The photon horizon 22 radio log(e/ev) 16 photon horizon γγ e + e CMB 14 IR 12 kpc kpc 0kpc Mpc Mpc 0Mpc Gpc Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
84 Astrophysical sources Cascade spectrum Development of the elmag. cascade: Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
85 Astrophysical sources Cascade spectrum Development of the elmag. cascade: analytical estimate: [Strong 74, Berezinsky, Smirnov 75 ] K(E/ε X ) 3/2 at E ε X J γ (E) = K(E/ε X ) 2 at ε X E ε a 0 at E > ε a three regimes: Thomson cooling: E γ = 4 ε bb Ee 2 3 m 2 e 0 MeV ( ) 2 Ee 1TeV plateau region: ICS Eγ E e above pair-creation threshold smin = 4E γ ε bb = 4m 2 e : flux exponentially suppressed Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
86 Astrophysical sources Cascade spectrum Cascade limit: for pp interactions, α = 2.1 E 2 J(E) [ev/cm 2 s sr] gamma nu Fermi EGRB 1 1e+ 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
87 Astrophysical sources Cascade spectrum Cascade limit: for pp interactions, α = 2.3 E 2 J(E) [ev/cm 2 s sr] gamma nu Fermi EGRB 1 1e+ 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
88 Astrophysical sources Cascade spectrum Cascade limit: for pp interactions, α = 2.5 E 2 J(E) [ev/cm 2 s sr] gamma nu Fermi EGRB 1 1e+ 1e+11 1e+12 1e+13 1e+14 1e+15 1e+16 1e+17 E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
89 Astrophysical sources Cascade spectrum Cascade limit: pp vs. pγ interactions pp interactions: no way to reduce low-energy secondaries for α ν > 2.3 problems with EGRB Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
90 Astrophysical sources Cascade spectrum Cascade limit: pp vs. pγ interactions pp interactions: no way to reduce low-energy secondaries for α ν > 2.3 problems with EGRB pγ interactions: slope below Eth differs can be modified by max. energy & redshift evolution cascades in source can be modified Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
91 Astrophysical sources Cascade spectrum Cascade limit: pp vs. pγ interactions pp interactions: no way to reduce low-energy secondaries for α ν > 2.3 problems with EGRB pγ interactions: slope below Eth differs can be modified by max. energy & redshift evolution cascades in source can be modified successful paradigm: Stecker model Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
92 Astrophysical sources CR sea interactions in bulge and plane Neutrinos from Galactic Sea CRs: X = 30g/cm 2 E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] Hillas Polygonato Escape E/eV [MK, S.Ostapchenko 14 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
93 Astrophysical sources CR sea interactions in bulge and plane Neutrinos from Galactic Sea CRs: X = 30g/cm 2 E 2.6 I(E) [GeV 1.6 m -2 sr -1 s -1 ] Hillas Polygonato Escape 0.1 model dependence impacts background in IceCube E/eV Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
94 Astrophysical sources CR sea interactions in bulge and plane Neutrinos from Galactic Sea CRs gives negligible contribution to IceCube signal τ pp is too small even towards GC gas is concentrated as n(z) n 0 exp[ (z /z 12 ) 2 ] with z kpc results apply also to other normal galaxies as starburst galaxies: Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
95 Astrophysical sources CR sea interactions in bulge and plane Neutrinos from Galactic Sea CRs gives negligible contribution to IceCube signal τ pp is too small even towards GC gas is concentrated as n(z) n 0 exp[ (z /z 12 ) 2 ] with z kpc results apply also to other normal galaxies as starburst galaxies: magnetic fields factor 0 higher: Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
96 Astrophysical sources CR sea interactions in bulge and plane Neutrinos from Galactic Sea CRs gives negligible contribution to IceCube signal τ pp is too small even towards GC gas is concentrated as n(z) n 0 exp[ (z /z 12 ) 2 ] with z kpc results apply also to other normal galaxies as starburst galaxies: magnetic fields factor 0 higher: if knee is caused by diffusion: Ecr B, neutrino knee at few 16 ev source: Emax B CR, neutrino knee at few 14 ev Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
97 Astrophysical sources Galactic point sources Galactic sources at low energies: many sources, large confinement times Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
98 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
99 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
100 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
![Astrophysical sources Galactic point sources Point source in gamma-ray source HESS J1825-137 [Neronov, Semikoz, Tchernin 13 ] 0.00600 90.000 60.000 0.00550 Cygnus region 0.00500 30.000 Crab 0.00450 0.](/docs-images/73/68107251/images/101-0.jpg "00400 315.000 HESS J1825 270.000region 225.000 180.000 135.000 90.000 45.000 0.000 0.000 0.00350 0.00300 Galactic Center HESS J1632 region Kookaburra region Vela region -30.000 0.00250 0.00200-60.")
101 Astrophysical sources Galactic point sources Point source in gamma-ray source HESS J [Neronov, Semikoz, Tchernin 13 ] Cygnus region Crab HESS J region Galactic Center HESS J1632 region Kookaburra region Vela region Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
102 Astrophysical sources Galactic point sources Gamma-ray point sources flux from HESS J , GC and GP Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
103 Astrophysical sources Galactic point sources (Isotropic) photon limits GRAPES-3 UMC HEGRA EAS-TOP IC-40 (γ) GAMMA KASCADE CASA-MIA 4 E 2 Jγ [GeV cm 2 s 1 sr 1 ] kpc 20kpc 30kpc E γ [TeV] [Ahlers, Murase 13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
104 PeV dark matter PeV dark matter re-incarnation of SHDM idea for AGASA excess: non-thermal 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
105 PeV dark matter PeV dark matter re-incarnation of SHDM idea for AGASA excess: non-thermal 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
106 PeV dark matter PeV dark matter re-incarnation of SHDM idea for AGASA excess: non-thermal 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 Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
107 PeV dark matter PeV dark matter E Ν 2 dj de Ν TeV cm 2 s 1 sr 1 11 DM Ν e Ν e 15, bb 85 DM Ν e Ν e 12, cc 88 DM e e 40, qq E Ν TeV [Esmaili, Serpico 13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
108 PeV dark matter PeV dark matter events bin data E 2 spec. DM ΝΝ, qq 2 3 E Ν TeV [Esmaili, Serpico 13 ] Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
109 Summary Summary Knee due to CR escape characteristic feature: recovery of p/he as suggested by KASCADE-Grande probes GMF: suggests small Brms and small l coh transition to light-medium extragalactic CRs completed at 3 17 ev propagation feature is unavoidable, only possible to shift to higher energies source effects may be on top, but seem not necessary Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
110 Summary Summary Knee due to CR escape characteristic feature: recovery of p/he as suggested by KASCADE-Grande probes GMF: suggests small Brms and small l coh transition to light-medium extragalactic CRs completed at 3 17 ev propagation feature is unavoidable, only possible to shift to higher energies source effects may be on top, but seem not necessary Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
111 Summary Summary Knee due to CR escape characteristic feature: recovery of p/he as suggested by KASCADE-Grande probes GMF: suggests small Brms and small l coh transition to light-medium extragalactic CRs completed at 3 17 ev propagation feature is unavoidable, only possible to shift to higher energies source effects may be on top, but seem not necessary Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
112 Summary Summary Knee due to CR escape characteristic feature: recovery of p/he as suggested by KASCADE-Grande probes GMF: suggests small Brms and small l coh transition to light-medium extragalactic CRs completed at 3 17 ev propagation feature is unavoidable, only possible to shift to higher energies source effects may be on top, but seem not necessary Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
113 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
114 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
115 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
116 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
117 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
118 Summary Summary IceCube neutrinos: 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? favours pγ? 5 PeV dark matter: angular distibution follows DM profile Michael Kachelrieß (NTNU Trondheim) High-Energy Cosmic Rays and Neutrinos APC Paris, 9. Dec / 53
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