Galactic Neutrinos. Michael Kachelrieß. NTNU, Trondheim
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1 Galactic Neutrinos Michael Kachelrieß NTNU, Trondheim []
2 Introduction Outline of the talk 1 Introduction Observations Cascade limit and implications 2 Neutrinos from the Galactic CR sea Galactic plane 3 Neutrinos from Galactic CR sources 4 Neutrinos from extended sources TeV γ-ray excess in Fermi-LAT Interpretations 5 Conclusions Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 2 / 30
3 Introduction IceCube events: Soft low-energy spectrum? Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 3 / 30
4 Introduction IceCube events: power-law fit of energy spectrum Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 4 / 30
5 Introduction IceCube events: power-law fit of energy spectrum Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 4 / 30
6 Introduction Cascade limit The photon horizon 22 radio log(e/ev) 16 photon horizon γγ e + e CMB 14 IR 12 kpc kpc 0kpc Mpc Mpc 0Mpc Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 5 / 30 Gpc
7 Introduction Cascade limit Cascade limit: α = 21 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) Galactic neutrinos VLVNT, 2 October 18 6 / 30
8 Introduction Cascade limit Cascade limit: α = 23 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) Galactic neutrinos VLVNT, 2 October 18 6 / 30
9 Introduction Cascade limit Cascade limit: α = 25 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) Galactic neutrinos VLVNT, 2 October 18 6 / 30
10 Introduction Cascade limit Cascade limit: 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 Slope α > 22 E/eV requires hidden sources or Galactic origin Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 6 / 30
11 Introduction Cascade limit (Isotropic) photon limits [Ahlers, Murase 13 ] GRAPES-3 UMC HEGRA EAS-TOP IC-40 (γ) KASCADE GAMMA CASA-MIA 4 E 2 Jγ [GeV cm 2 s 1 sr 1 ] kpc 20kpc 30kpc E γ [TeV] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 7 / 30
12 Introduction Cascade limit (Isotropic) photon limits [Ahlers, Murase 13 ] GRAPES-3 HEGRA IC-40 (γ) GAMMA UMC EAS-TOP KASCADE CASA-MIA 4 E 2 Jγ [GeV cm 2 s 1 sr 1 ] kpc 20kpc 30kpc Eγ [TeV] KASCADE limits reanalysed 17 and increased Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 7 / 30
13 Neutrinos from the Galactic CR sea Galactic plane Hints for a Galactic plane contribution? [Neronov, Semikoz 14, 15 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 8 / 30
14 Neutrinos from the Galactic CR sea Galactic plane Hints for a Galactic plane contribution? [Neronov, Semikoz 14, 15 ] Neronov & Semikoz 15: Galactic latitude distribution of 4yr IceCube data with > 0 TeV inconsistent at 3σ with isotropy Palladino & Vissani 15: Two component fit, soft Galactic E 24 25% Galactic contribution Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 8 / 30
15 Neutrinos from the Galactic CR sea Galactic plane Expectation: CR interactions with gas in Galactic plane give guaranteed ν flux [Berezinsky, Smirnov 75 ] [Gaggero et al 15, Pagliaroli, Evoli, Villante 17, ] agreement: -20% Galactic contribution at 0 TeV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 9 / 30
16 Neutrinos from the Galactic CR sea Galactic plane Expectation: CR interactions with gas in Galactic plane give guaranteed ν flux [Berezinsky, Smirnov 75 ] [Gaggero et al 15, Pagliaroli, Evoli, Villante 17, ] agreement: -20% Galactic contribution at 0 TeV However, uncertainties are very large: elemental composition unclear, but Z ν A 1 γ CRs locally measured close to knee diffusion may be unreliable gas density Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 9 / 30
17 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition Kascade-Grande: dependenc on interaction model Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 / 30
18 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition Kascade-Grande: dependenc on interaction model Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October 18 / 30
19 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition [Gaisser, Stanev & Tilav 13 ] E 26 I(E) [GeV 16 m -2 sr -1 s -1 ] p He C O Fe total E/eV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
20 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition [Hörandel 0? ] τ E 26 I(E) [GeV 16 m -2 sr -1 s -1 ] p He Li-Fl Ne-Cr Mn-Co total E/eV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
21 Neutrinos from the Galactic CR sea Galactic plane Resulting ν fluxes (τ = 1 at PeV) [MK, Ostapchenko 14 ] E 26 I(E) [GeV 16 m -2 sr -1 s -1 ] Hillas Polygonato Escape E/eV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
22 act Neutrinos from the Galactic CR sea Galactic plane power-law spectrum corresponds to a deficit with a del statistical significance of 42 standard deviations To see vy Uncertainties: if any artificial CRfeature composition could have been produced in our in ARGO-YBJ: position of p+he knee 700 TeV ing we ent: 6% 6% 1% 1% ev ev 7% 2% 165 (GeV) -1 ssr) 2 (m 265 Flux E 4 3 H+He This work ARGO/WFCTA-02 ARGO-YBJ CREAM KASCADE SIBYLL KASCADE QGSJET-II 02 Tibet-Phase II QGSJET Tibet-Phase II SIBYLL 4 5 Energy (GeV) FIG (color online) H&He spectrum obtained by the hybrid Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October /
23 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition ARGO-YBJ: position of p+he knee 700 TeV ] 16 s -1 sr -1 GeV -2 [m 26 Flux E ARGO-YBJ all-particle (unfolding) ARGO-YBJ P+He (unfolding) ARGO-YBJ P+He (Hybrid) ARGO-YBJ all-particle (NP8Max) ARGO-YBJ P+He (NP8Max) ARGO-YBJ P+He (Digital) Horandel ALL Gaisser-Stanev-Tilav ALL Horandel P+He Gaisser-Stanev-Tilav P+He 4 5 Energy [GeV] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October /
24 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: CR composition ARGO-YBJ: position of p+he knee 700 TeV ] 16 s -1 sr -1 GeV 4-2 [m 26 E Flux 3 2 ARGO-YBJ all-particle (unfolding) ARGO-YBJ P+He (unfolding) ARGO-YBJ P+He (Hybrid) ARGO-YBJ all-particle (NP8Max) ARGO-YBJ P+He (NP8Max) ARGO-YBJ P+He (Digital) Horandel ALL Gaisser-Stanev-Tilav ALL Horandel P+He Gaisser-Stanev-Tilav P+He 4 5 neutrino knee at TeV 6 Energy [GeV] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October /
25 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: diffusion approach diffusion picture requires R L (E ) L coh /(2π) for L coh 50 pc and B fewµg: E 16 ev Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
26 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: diffusion approach diffusion picture requires R L (E ) L coh /(2π) for L coh 50 pc and B fewµg: E 16 ev LOFAR: l coh < pc in disc diffusion has to be anisotropic [Giacinti, MK, Semikoz 18 ] grammage X(E) in the escape model [Giacinti, MK, Semikoz 14, 15 ] X(E) in g/cm β=1, L=pc β=01, L=pc 001 β=1/8, L=25pc δ=1/3 AMS-02 (a) AMS-02 (b) 0001 Jones E/Z in ev Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
27 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: diffusion approach diffusion picture requires R L (E ) L coh /(2π) for L coh 50 pc and B fewµg: E 16 ev LOFAR: l coh < pc in disc diffusion has to be anisotropic [Giacinti, MK, Semikoz 18 ] grammage X(E) in the escape model [Giacinti, MK, Semikoz 14, 15 ] X(E) in g/cm β=1, L=pc β=01, L=pc 001 β=1/8, L=25pc δ=1/3 AMS-02 (a) AMS-02 (b) Jones E/Z in ev reduced τ above few 15 ev Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
28 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: deviations from local spectrum CR slope from molecular clouds: α 24 [Neronov, Malyshev, Semikoz 17 ] 26 χ 2 /NDF=20/ i Galactic LMC Cygnus RCrA Rho Oph Chameleon Cepheus Mon R2 Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30 Orion A Orion B Perseus Taurus
29 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: deviations from local spectrum CR slope from molecular clouds: α 24 [Neronov, Malyshev, Semikoz 17 ] 26 χ 2 /NDF=20/ RCrA Rho Oph Chameleon Cepheus Mon R2 Orion A Orion B Perseus i1 Galactic LMC Taurus Cygnus agrees with local slope of nuclei (and δ = 1/3) deviation of α p 27 vs α nuc 25 local effect? Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
30 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: deviation from local spectrum explanations: local source [MK, Neronov, Semikoz 15 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
31 Neutrinos from the Galactic CR sea Galactic plane Uncertainties: deviation from local spectrum explanations: local source [MK, Neronov, Semikoz 15 ] diffusion depends on ρ, D = D(ρ) [Yang, Aharonian, Evoli 16 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
32 Neutrinos from the Galactic CR sea Galactic plane Detection prospects: [Pagliaroli, Evoli, Villante 16 ] φν( ) ( ) b = 0 C B A Isotropic ( ) A: local; B: n sources,c: E δ(r) Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
33 Neutrinos from the Galactic CR sea Galactic plane Detection prospects: [Pagliaroli, Evoli, Villante 16 ] φν( ) ( ) l = 0 C B A Isotropic ( ) Close to GC: always an excess rel extragal detectability requires good angular resolution Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
34 Neutrinos from Galactic CR sources Galactic sources at low energies: many sources, large confinement times average CR sea plus few recent sources Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
35 Neutrinos from Galactic CR 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) Galactic neutrinos VLVNT, 2 October / 30
36 Neutrinos from Galactic CR 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 connection to γ rays: sources transparent: φγ (E) φ ν (E) but requires extrapolation above TeV young SNRs, Cygnus region, Fermi bubbles, Galactic center Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
37 Neutrinos from Galactic CR sources Galactic center E 2 dφ/deγ/dω [GeVcm 2 s 1 sr 1 ] Galactic ridge Conventional diffusion Base model Gamma model Fermi Data PASS8 HESS Data 2006 Best Fit Fermi + HESS data Hard diffusion E [T ev ] [Gaggero et al 17 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
38 Neutrinos from Galactic CR sources Galactic center E 2 dφ/deγ/dω [GeVcm 2 s 1 sr 1 ] Pacman region Conventional diffusion Base model Gamma model Fermi Data PASS8 HESS Data 2016 Best Fit HESS+Fermi Hard diffusion E [T ev ] [Gaggero et al 17 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
39 Neutrinos from Galactic CR sources Antares IceCube limit 7 E 2 dφ/dedω [GeV cm 2 s 1 sr 1 ] 8 KRAγ model Combined UL KRAγ 5 Combined UL KRAγ 50 ANTARES UL KRAγ 5 IceCube UL KRAγ 50 IceCube starting events IceCube up-going ν µ 5 PeV CR cutoff 50 PeV CR cutoff E [TeV] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
40 Neutrinos from Galactic CR sources Slow diffusion around sources: Geminga D(0 TeV) [cm 2 /s] 28 HAWC (3 µg) B rms = 3 µg 2 µg 4 µg 5 µg L c [pc] possible explanations: weak regular field, smallish Lcoh [López-Coto, Giacinti 17 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
41 Neutrinos from Galactic CR sources Slow diffusion around sources: Geminga D(0 TeV) [cm 2 /s] 28 HAWC (3 µg) B rms = 3 µg 2 µg 4 µg 5 µg L c [pc] possible explanations: weak regular field, smallish Lcoh [López-Coto, Giacinti 17 ] self-generated turbulence by CRs [ Evoli, Linden, Morlino 18 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
42 Neutrinos from extended sources Sources in Local & Loop I superbubble [Andersen, MK, Semikoz 17 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
43 Neutrinos from extended sources Sources in Local & Loop I superbubble [Andersen, MK, Semikoz 17 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
44 Neutrinos from extended sources Sources in Local & Loop I superbubble [Andersen, MK, Semikoz 17 ] 2 IceCube all flavors IceCube muon*3 local flux EG 1/E 21 total E 2 F(E) [ev/cm 2 /s/sr] E [ev] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
45 Neutrinos from extended sources Sources in Local & Loop I superbubble [Andersen, MK, Semikoz 17 ] KASCADE I(>E)/(cm 2 s sr) E/eV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
46 Neutrinos from extended sources TeV γ-ray excess Are multi-tev photons in the Fermi data? [Neronov, MK, Semikoz 18 ] Caveats Analyzing LAT Pass 8 Data: because the validation process was hampered by lack of statistics, using data below 30 MeV or above 1 TeV is discouraged gtlike tool has limit 850 GeV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
47 Neutrinos from extended sources TeV γ-ray excess Are multi-tev photons in the Fermi data? [Neronov, MK, Semikoz 18 ] Caveats Analyzing LAT Pass 8 Data: because the validation process was hampered by lack of statistics, using data below 30 MeV or above 1 TeV is discouraged gtlike tool has limit 850 GeV eff area & energy resolution up to 32 TeV: 15% at 1 TeV & 25% at 3 TeV aperture photometry possible Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
48 Neutrinos from extended sources TeV γ-ray excess Cross calibration test: Galactic plane Galactic plane ( b < 5 and 40 < l < 0 ) spectrum from ARGO-YBJ and Milagro 40 < l < 0 5 < b < 5 E 2 dn/de, GeV/(cm 2 s sr) 5 6 Fermi/LAT Argo-YBJ MILAGRO E, GeV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
49 Neutrinos from extended sources TeV γ-ray excess Extension to 3 TeV for b > 20 : 6 residual CR IGRB b > 20, total counts b > 20, PS, IGRB & CR subtracted E 2 dn/de, GeV/(cm 2 s sr) E, GeV Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
50 Neutrinos from extended sources TeV γ-ray excess Extension to 3 TeV for b > 20 : 6 residual CR IGRB b > 20, total counts b > 20, PS, IGRB & CR subtracted E 2 dn/de, GeV/(cm 2 s sr) E, GeV bin 1 17 TeV: expected 14 (185) for nominal (renormalised) exposure observed (after subtr CR): 47 bin 17 3 TeV: expected 24 (355), observed 17 Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
51 Neutrinos from extended sources TeV γ-ray excess Adding neutrinos: IGRB LAT 0 decay model Fermi/LAT all sky IceCube HESE, 6 yr IceCube HESE, 4 yr 7 ) 8 4 ANTARES IceCube Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
52 Neutrinos from extended sources Intepretation Possible explanations: interface Loop I/local superbubble: strong dipole? Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
53 Neutrinos from extended sources Intepretation Possible explanations: interface Loop I/local superbubble: strong dipole? extended CR halo [Taylor, Gabici, Aharonian 14 ] [Dolag 02 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
54 Neutrinos from extended sources Intepretation Possible explanations: interface Loop I/local superbubble: strong dipole? extended CR halo for B 001µ G and L coh 0 pc: CR with E = 0 TeV is in large-angle scattering regime D(E ) 29 cm 2 /s escape time τ = H 2 /2D t 0 [Dolag 02 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
55 Neutrinos from extended sources Intepretation Possible explanations: interface Loop I/local superbubble: strong dipole? extended CR halo PeV dark matter: re-incarnation of SHDM idea for AGASA excess: non-hermal DM avoids cascacde limit Galactic anisotropy Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
56 Neutrinos from extended sources Intepretation 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 [Kusenko et al 13, Esmaili, Serpico 13 ] Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
57 Neutrinos from extended sources Intepretation Possible explanations: heavy dark matter nu tot gam gal gam gal ICS gam ex casc gam tot IceCube Fermi x 1x 11 1x 12 1x 13 1x 14 1x 15 1x 16 Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
58 Summary Summary 1 EGRB constrains stronly neutrino sources: slope of extragal neutrino α < 22 neutrino sources are not main source class of EGRB 2 Standard Galactic neutrinos: northern km 3 telescope very useful important info on propagation and acceleration 3 Soft neutrino signal in IceCube: isotropy: extragalactic or large Galactic halo TeV γ-ray excess consistent with neutrino flux Michael Kachelrieß (NTNU Trondheim) Galactic neutrinos VLVNT, 2 October / 30
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