TeV gamma-rays from UHECR sources 22 radio log10(e /ev ) 16 photon horizon γγ e + e CMB 14 IR kpc 10kpc 100kpc M pc Virgo 10M pc 100M pc G
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- Clemence Martin
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1 Gamma-rays from CR sources Michael Kachelrieß NTNU, Trondheim []
2 TeV gamma-rays from UHECR sources 22 radio log10(e /ev ) 16 photon horizon γγ e + e CMB 14 IR kpc 10kpc 100kpc M pc Virgo 10M pc 100M pc G pc Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 2 / 34
3 TeV gamma-rays from UHECR sources during propagation: cosmogenic photons in sources: Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 3 / 34
4 TeV gamma-rays from UHECR sources during propagation: cosmogenic photons in sources: galactic CR sources GRB: large redshift time-delay UHECR photons makes direct correlation impossible for small EGMF: auto-correlation n GRB τṅ GRB <n AGN Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 3 / 34
5 TeV gamma-rays from UHECR sources during propagation: cosmogenic photons in sources: galactic CR sources GRB: large redshift time-delay UHECR photons makes direct correlation impossible for small EGMF: auto-correlation n GRB τṅ GRB <n AGN AGN: jets: small densities, B core: high B, large UV and IR densities, τ pγ 1 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 3 / 34
6 HESS observations of M87: A ) -1 s Feb March 2005 April 2005 May Φ(E>730GeV) (cm 4 2 B ) -1 s -2 Φ(E>730GeV) (cm /Feb -12 ) 10 16/Feb 09/Mar H.E.S.S. average H E G R A 16/Mar Chandra (HST-1) Chandra (nucleus) 30/Mar /Apr /May /May Date 12/ / / / /2006 Date s -2 f(0.2-6 kev) (erg cm Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 4 / 34
7 HESS observations of M87: A ) -1 s Feb March 2005 April 2005 May Φ(E>730GeV) (cm 4 2 B ) -1 s -2 Φ(E>730GeV) (cm /Feb -12 ) 10 16/Feb 09/Mar 16/Mar 30/Mar 06/Apr H.E.S.S fast average variability excludes acceleration along kpc jet H E G R A acceleration Chandra (HST-1) in hot 2003 spots marginally okay Chandra (nucleus) favors acceleration close to SMBH /May /May Date 12/ / / / /2006 Date s -2 f(0.2-6 kev) (erg cm Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 4 / 34
8 HESS & Veritas observations of M87: A ) -1 s Feb March 2005 April 2005 May Φ(E>730GeV) (cm 4 2 B ) -1 s -2 Φ(E>730GeV) (cm /Feb -12 ) 10 16/Feb 09/Mar 16/Mar 30/Mar 06/Apr H.E.S.S fast average variability excludes acceleration along kpc jet H E G R A acceleration Chandra (HST-1) in hot 2003 spots marginally okay Chandra (nucleus) favors acceleration close to SMBH /May /May Date 12/ / / / /2006 Date s -2 f(0.2-6 kev) (erg cm Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 4 / 34
9 Outline of the talk 1 Introduction 2 Gamma-rays produced in UHECR sources How do get multi TeV gamma-rays out off AGN cores: electromagnetic cascades in UHECR sources 3 Cosmogenic fluxes: Cosmogenic neutrino limits from Fermi-LAT Cosmogenic photons: diffuse flux Secondary photons from CR point sources 4 Lower limit on EGMF using gamma-rays 5 Summary Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 5 / 34
10 Outline of the talk 1 Introduction 2 Gamma-rays produced in UHECR sources How do get multi TeV gamma-rays out off AGN cores: electromagnetic cascades in UHECR sources 3 Cosmogenic fluxes: Cosmogenic neutrino limits from Fermi-LAT Cosmogenic photons: diffuse flux Secondary photons from CR point sources 4 Lower limit on EGMF using gamma-rays 5 Summary Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 5 / 34
11 Outline of the talk 1 Introduction 2 Gamma-rays produced in UHECR sources How do get multi TeV gamma-rays out off AGN cores: electromagnetic cascades in UHECR sources 3 Cosmogenic fluxes: Cosmogenic neutrino limits from Fermi-LAT Cosmogenic photons: diffuse flux Secondary photons from CR point sources 4 Lower limit on EGMF using gamma-rays 5 Summary Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 5 / 34
12 Outline of the talk 1 Introduction 2 Gamma-rays produced in UHECR sources How do get multi TeV gamma-rays out off AGN cores: electromagnetic cascades in UHECR sources 3 Cosmogenic fluxes: Cosmogenic neutrino limits from Fermi-LAT Cosmogenic photons: diffuse flux Secondary photons from CR point sources 4 Lower limit on EGMF using gamma-rays 5 Summary Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 5 / 34
13 Astrophysical sources Centaurus A Multi-messenger astronomy with Cen A? + 2 events correlated with Cen A within more events close-by [Gorbunov et al. 07, Fargione 08, Rachen 08 ] + general correlation with AGN confusion with LSS? no confirmation by HiRes tension to PAO chemical composition E max for most AGN (incl. Cen A) high enough? correlations with AGN: independent/additional evidence? Cen A closest AGN good test case for multi-messenger astronomy: accompanying γ-ray and neutrino fluxes? Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 6 / 34
14 Astrophysical sources Centaurus A Results for acceleration close to the core: α =1.2 log 10 (E 2 Φ/eV km -2 yr -1 ) C G R O FERM I H E S S γ total ne utrinos initia l protons P AO fina l protons 14 γ log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 7 / 34
15 Astrophysical sources Centaurus A Results for acceleration close to the core: α =2 19 log 10 (E 2 Φ/eV km -2 yr -1 ) C G R O FERM I initia l protons fina l protons H E S S γ P AO total ne utrinos promising test case for HESS / FERMI γ γ-ray spectrum rather insensitive to α log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 7 / 34
16 Astrophysical sources HESS observations of Cen A Centaurus A no variability Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 8 / 34
17 Astrophysical sources HESS observations of Cen A Centaurus A no variability consistent with point source Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 8 / 34
18 Astrophysical sources HESS observations of Cen A Centaurus A no variability consistent with point source HE emission from central region (1 1.1 kpc) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 8 / 34
19 Astrophysical sources Centaurus A Comparison to recent HESS and FERMI observations log 10 (E 2 Φ/eV km -2 yr -1 ) broken Fermi initial protons final protons α=2 P AO H E S S α= γ γ log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 9 / 34
20 Astrophysical sources Centaurus A Comparison to recent HESS and FERMI observations log 10 (E 2 Φ/eV km -2 yr -1 ) broken Fermi shape and normalization okay TeV γ-ray and neutrino source initial protons final protons α=2 P AO H E S S α=1.2 γ γ log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics 10 9 / 34
21 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: a) (isotropic) source injection spectrum F γ (E) 1/E 2 E 2 F(E ) log10(e /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
22 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: a) (isotropic) source : thin above ev, ultra-rel. regime E 2 F(E ) E γε γ m 2 e log10(e /ev ) ultra-rel. regime Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
23 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: b) on EBL photons above ev cascade on EBL E 2 F(E ) log10(e /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
24 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: b) on EBL photons above ev cascade on EBL : fill up GeV TeV range E 2 F(E ) log10(e /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
25 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: b) on EBL photons above ev cascade on EBL : fill up GeV TeV range E 2 F(E ) main criteria: L UHE, not shape evidence for acceleration to UHECRs? however: anisotropic UV field complicates picture already in source log10(e /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
26 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: collinear regime log 10 τ γγ isotropic anisotropic log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
27 Astrophysical sources Electromagnetic cascades in the source Regenerating TeV photons: decaying muons log 10 (l/pc) R 1 l int, U V l int, IR no cutoff l dec,µ l int, IR cutoff log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
28 Astrophysical sources Regenerating TeV photons: log 10 (l/pc) R 1 l int, U V Electromagnetic cascades in the source adding IR l int, IR no cutoff l dec,µ l int, IR cutoff log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
29 Astrophysical sources adding IR from a compact source: Electromagnetic cascades in the source log 10 (E 2 Φ/eV km -2 yr -1 ) Fermi E max = ev E max = ev E max = ev H E S S 16 R IR = 1 pc log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
30 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos Photon and neutrino production relatively tight connected: protons: p + γ3k { p + π 0 p + 2γ n + π + p + 2e ± +4ν Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
31 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos Photon and neutrino production relatively tight connected: protons: p + γ3k { p + π 0 p +2γ n + π + p +2e ± +4ν nuclei: A + γ3k (A 1) + n (A 1) + p + e + ν e connection to UHECRs looser Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
32 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos Photon and neutrino production relatively tight connected: protons: p + γ3k { p + π 0 p +2γ n + π + p +2e ± +4ν nuclei: A + γ3k (A 1) + n (A 1) + p + e + ν e cascade limit: [Berezinsky, Smirnov 75 ] all energy in γ and e ± cascades below 100 GeV Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
33 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos Photon and neutrino production relatively tight connected: protons: p + γ3k { p + π 0 p +2γ n + π + p +2e ± +4ν nuclei: A + γ3k (A 1) + n (A 1) + p + e + ν e cascade limit: [Berezinsky, Smirnov 75 ] all energy in γ and e ± cascades below 100 GeV K(E/ε X ) 3/2 at E ε X J γ (E) = K(E/ε X ) 2 at ε X E 0 at E > ε a Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
34 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos Photon and neutrino production relatively tight connected: protons: p + γ3k { p + π 0 p +2γ n + π + p +2e ± +4ν nuclei: A + γ3k (A 1) + n (A 1) + p + e + ν e cascade limit: all energy in γ and e ± cascades below 100 GeV [Berezinsky, Smirnov 75 ] Fermi-LAT measurement of EGRB: ω cas > 4π de EI ν (E) 4π c E 0 c E 0I ν (>E 0 ) < ev/cm 3 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
35 Cosmogenic fluxes Neutrino limits from the EGRB Comparison of Monte Carlo and analytical estimate 1e M pc E -3/2 1e+14 E 2 *J(E ) 1e+13 1e+12 1e+11 1e+06 1e+07 1e+08 1e+09 1e+10 1e+11 1e+12 1e+13 1e+14 1e+15 E /ev Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
36 Cosmogenic fluxes Neutrino limits from the EGRB Comparison of Monte Carlo and analytical estimate 1e M pc 1000M pc E -3/2 E e+14 E 2 *J(E ) 1e+13 1e+12 1e+11 1e+06 1e+07 1e+08 1e+09 1e+10 1e+11 1e+12 1e+13 1e+14 1e+15 E /ev Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
37 Cosmogenic fluxes Neutrino limits from the EGRB Fermi-LAT vs. UHECR data: [Berezinsky et al. 10 ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
38 Cosmogenic fluxes Neutrino limits from the EGRB Fermi-LAT vs. UHECR data: [Berezinsky et al. 10 ] integrating EJ(E) gives bound ω cas < ev/cm 3 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
39 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos [Berezinsky et al. 10 ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
40 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos [Ahlers et al. 10 ] E min = ev HiRes (3 x ) RICE ( e,µ, ) BAIKAL ( e,µ, ) Auger (3 ) AMANDA (3 µ) AMANDA ( e,µ, ) ANITA ( e,µ, ) IceCube (5, 1yr) E [GeV] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
41 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos MainEdifference: min = evexpected IceCube sensitivity end of exp. sensitivity for 1/E 2 flux: vs ev overall sensitivity of IceCube HiRes (3 x ) RICE ( e,µ, ) BAIKAL ( e,µ, ) Auger (3 ) AMANDA (3 µ) AMANDA ( e,µ, ) ANITA ( e,µ, ) IceCube (5, 1yr) E [GeV] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
42 Cosmogenic fluxes Neutrino limits from the EGRB Cascade limit for cosmogenic neutrinos MainEdifference: min = evexpected IceCube sensitivity end of exp. sensitivity for 1/E 2 flux: vs ev overall sensitivity of IceCube HiRes (3 x ) RICE ( e,µ, ) BAIKAL ( e,µ, ) Auger (3 ) AMANDA (3 µ) AMANDA ( e,µ, ) ANITA ( e,µ, ) All plots for proton primaries IceCube (5, 1yr) for nuclei reduced neutrino fluxes E [GeV] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
43 Cosmogenic fluxes Diffuse photons Cosmogenic photons [Hooper, Taylor, Sarkar 10 ] photon fra ction E max,z =(Z/26)x10 21 ev α=2.0 B<3 pg P rotons Iron log 10 E nergy [ev ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
44 Cosmogenic fluxes Diffuse photons Cosmogenic photons [Hooper, Taylor, Sarkar 10 ] photon fraction E max,z =(Z/26)x10 21 ev α=2.0 B<3 pg P rotons Iron log 10 E nergy [ev ] A>1: photons suppressed by factor 10 compared to protons even proton: requires sensitivity improved by 100 large E max and small α helps... Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
45 Cosmogenic fluxes Diffuse photons Cosmogenic photons [Hooper, Taylor, Sarkar 10 ] photon fra ction E max,z =(Z/26)x10 22 ev α=2.0 B<3 pg P rotons Iron log 10 E nergy [ev ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
46 Cosmogenic fluxes Diffuse photons Cosmogenic photons: dependence on α [Gelmini, Kalashev, Semikoz 05 ] j(e ) E 2 [ev cm -2 s -1 sr -1 ] e+19 1e+20 1e+21 E [ev ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
47 Cosmogenic fluxes Secondary photons from point sources Secondary photons from CR point sources for d<few 10 Mpc: UHE photons survive [Taylor et al. 09 ] protons E max =10 20 ev E max =10 21 ev Auger data (2007) R ate (>E ) [yr -1 ] photons S ource at 3.8 M pc α= log 10 E [ev ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
48 Cosmogenic fluxes Secondary photons from point sources Secondary photons from CR point sources for d<few 10 Mpc: UHE photons survive [Taylor et al. 09 ] non-observation is no constraint, but observation identifies close source Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
49 Cosmogenic fluxes Secondary photons from point sources Secondary photons from CR point sources for d<few 10 Mpc: UHE photons survive [Taylor et al. 09 ] larger distance: UHE photons cascade down in TeV range [Essey et al. 10 ] universal shape, depending only on EBL and z G ev G ev G ev 10 0 E 2 dn /de, ev cm -2 s E, G ev Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
50 Cosmogenic fluxes Secondary photons from point sources Secondary photons from CR point sources for d<few 10 Mpc: UHE photons survive [Taylor et al. 09 ] larger distance: UHE photons cascade down in TeV range [Essey et al. 10 ] universal shape, depending only on EBL and z G ev G ev G ev 10 0 E 2 dn /de, ev cm -2 s E, G ev large luminosities Leff erg/s in UHECR relatively small EGMFs in voids, B < G Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
51 Gamma-rays and the EGMF Gamma-rays and extragalactic magnetic fields (EGMF) Origin of seed for EGMF is mysterious Seed required as input for EGMF simulations Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
52 Gamma-rays and the EGMF Gamma-rays and extragalactic magnetic fields (EGMF) Origin of seed for EGMF is mysterious Seed required as input for EGMF simulations Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
53 Gamma-rays and the EGMF Gamma-rays and extragalactic magnetic fields (EGMF) Origin of seed for EGMF is mysterious Seed required as input for EGMF simulations Observations only in clusters, synchrotron halo: B (0.1 1) µg Faraday rotation: B (1 10) µg Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
54 Gamma-rays and the EGMF Gamma-rays and extragalactic magnetic fields (EGMF) Origin of seed for EGMF is mysterious Seed required as input for EGMF simulations Observations only in clusters, synchrotron halo: B (0.1 1) µg Faraday rotation: B (1 10) µg Aharonian, Coppi, Völk 94: Pair halos around AGNs Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
55 Gamma-rays and the EGMF Gamma-rays and extragalactic magnetic fields (EGMF) Origin of seed for EGMF is mysterious Seed required as input for EGMF simulations Observations only in clusters, synchrotron halo: B (0.1 1) µg Faraday rotation: B (1 10) µg Aharonian, Coppi, Völk 94: Pair halos around AGNs Plaga 95: EGMFs deflect and delay cascade electrons search for delayed echoes of multi-tev AGN flares/grbs Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
56 Gamma-rays and the EGMF Observer misaligned with jet: [Neronov et al. 10 ] e + e e+ e O jet 0 obs O ext probability for misalignement p ϑ obs most blazars viewed with ϑ obs ϑ jet Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
57 Gamma-rays and the EGMF Observer misaligned with jet: [Neronov et al. 10 ] e + e e+ e O jet 0 obs O ext probability for misalignement p ϑ obs most blazars viewed with ϑ obs ϑ jet halos are not symmetric Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
58 Gamma-rays and the EGMF Observer misaligned with jet: [Neronov et al. 10 ] e + e e+ e O jet 0 obs O ext probability for misalignement p ϑ obs most blazars viewed with ϑ obs ϑ jet halos are not symmetric time-delay is function of ϑ, [ ][ ] T delay (ϑ) (ϑobs +Θ jet ) ϑ yr 5 5 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
59 Gamma-rays and the EGMF Asymmetric halos around TeV blazars ( GeV jets ): ϑ obs =0 ϑ obs =3 ϑ obs =6 ϑ obs =9 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
60 Gamma-rays and the EGMF GeV jets : B dependence G G G G 1 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
61 Gamma-rays and the EGMF GeV jets : time dependence of flares <T delay < 10 5 yr yr< T delay < 10 7 yr Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
62 Gamma-rays and the EGMF Lower limit on EGMF: choose blazar: large z, stationary, low GeV, high multi-tev emission Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
63 Gamma-rays and the EGMF Lower limit on EGMF: choose blazar: large z, stationary, low GeV, high multi-tev emission TeV photons cascade down: small EGMF: fill up GeV range large EGMF: deflected outside, isotropized Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
64 Gamma-rays and the EGMF Lower limit on EGMF: [F. Tavecchio et al. 10, A. Neronov, I. Vovk 10 ] Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
65 Gamma-rays and the EGMF Lower limit on EGMF: [F. Tavecchio et al. 10, A. Neronov, I. Vovk 10 ] B > G some dependence on ϑ jet Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
66 Gamma-rays and the EGMF Lower limit on EGMF: [F. Tavecchio et al. 10, A. Neronov, I. Vovk 10 ] B > G some dependence on ϑ jet no simulation of elmag. cascade with B what happens for structured B? Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
67 Gamma-rays and the EGMF Lower limit on EGMF: [MK, Ostapchenko, Tomàs ] log 10 (E 2 F/erg cm -2 s -1 ) Fermi G G G G G H E S S log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
68 Gamma-rays and the EGMF Lower limit on filling factor: [MK, Ostapchenko, Tomàs 10 ] model filaments by a top-hat: B = G B =0 10 Mpc Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
69 Gamma-rays and the EGMF Lower limit on filling factor: [MK, Ostapchenko, Tomàs 10 ] log 10 (E 2 F/erg cm -2 s -1 ) Fermi H E S S log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
70 Gamma-rays and the EGMF Lower limit on filling factor: [MK, Ostapchenko, Tomàs 10 ] log 10 (E 2 F/erg cm -2 s -1 ) linear filling factor > 50% Fermi H E S S mainly 3-step cascade: γ e ± γ 0.50 photon mean free path D γ (E) Mpc 0.90 electron mean free path D e (E) few kpc log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
71 Gamma-rays and the EGMF Lower limit on filling factor: [MK, Ostapchenko, Tomàs 10 ] log 10 (E 2 F/erg cm -2 s -1 ) linear filling factor > 50% Fermi H E S S mainly 3-step cascade: γ e ± γ 0.50 photon mean free path D γ (E) Mpc 0.90 electron mean free path D e (E) few kpc -14 electrons are created everywhere and feel B only close to interaction point log 10 (E /ev ) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
72 Gamma-rays and the EGMF EGMF in voids already observed? [Ando, Kusenko 10 ] stack 170 brightest AGN Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
73 Gamma-rays and the EGMF EGMF in voids already observed? [Ando, Kusenko 10 ] stack 170 brightest AGN search for excess over PSF Rel. DEC (deg) C ounts M ap (3-10 G ev ) Rel DEC (deg) M odel M ap (3-10 G ev ) Rel. RA (deg) R el R A (deg) (counts) (counts) Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
74 Gamma-rays and the EGMF EGMF in voids already observed? [Ando, Kusenko 10 ] stack 170 brightest AGN search for excess over PSF Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
75 Gamma-rays and the EGMF EGMF in voids already observed? [Ando, Kusenko 10 ] stack 170 brightest AGN search for excess over PSF Rel. DEC (deg) Counts Map (3-10 GeV ) Rel DEC (deg) M odel M ap (3-10 G ev ) Rel. RA (deg) R el R A (deg) (counts) (counts) explained by B G(λ B /1 kpc) 1/2 and λ B < kpc Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
76 Gamma-rays and the EGMF EGMF in voids already observed? [Ando, Kusenko 10 ] stack 170 brightest AGN search for excess over PSF Rel. DEC (deg) Counts Map (3-10 GeV ) Rel DEC (deg) M odel M ap (3-10 G ev ) Rel. RA (deg) R el R A (deg) (counts) (counts) lower limit B > G requires λ B < 0.1 kpc Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
77 Gamma-rays and the EGMF EGMF already observed? Probably not... [Neronov et al. 10 ] point source Crab shows the same halo as stacked AGN: Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
78 Gamma-rays and the EGMF EGMF already observed? Probably not... [Neronov et al. 10 ] point source Crab shows the same halo as stacked AGN: tail of PSF wrong (?), difference between front and back photons Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
79 Summary Gamma-rays and the EGMF multi-tev photons from AGN cores require photons in KN regime HE muons hadronic models Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
80 Summary Gamma-rays and the EGMF multi-tev photons from AGN cores require photons in KN regime HE muons hadronic models secondary photons: chemical composition TeV sources?? Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
81 Summary Gamma-rays and the EGMF multi-tev photons from AGN cores require photons in KN regime HE muons hadronic models secondary photons: chemical composition TeV sources?? cascade limit from Fermi data reduced by factor 7 Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
82 Summary Gamma-rays and the EGMF multi-tev photons from AGN cores require photons in KN regime HE muons hadronic models secondary photons: chemical composition TeV sources?? cascade limit from Fermi data reduced by factor 7 lower limit on EGMF in voids B > G Michael Kachelrieß (NTNU Trondheim) Gamma-rays from CR sources TeV Particle Astrophysics / 34
Lower bound on the extragalactic magnetic field
Lower bound on the extragalactic magnetic field Michael Kachelrieß NTNU, Trondheim [] Dolag, MK, Ostapchenko, Tomàs 10 Neronov, Semikoz, MK, Ostapchenko, Elyiv 10 Introduction Mean free path of photons
Multi-Messenger Astonomy with Cen A?
Multi-Messenger Astonomy with Cen A? Michael Kachelrieß NTNU, Trondheim [] Outline of the talk 1 Introduction 2 Dawn of charged particle astronomy? Expectations vs. Auger data Effects of cluster fields
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