Ernie and Bert in the radio. TANAMI blazars in the IceCube neutrino fields

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1 TANAMI blazars in the IceCube neutrino fields Felicia Krauß (Remeis-Observatory & ECAP/FAU, Würzburg University) M. Kadler, K. Mannheim, J. Wilms, R. Ojha, A. Kreikenbohm, M. Langejahn, C. Müller, R. Schulz, J. Trüstedt on behalf of the TANAMI and the Fermi-LAT collaborations ASTRO WÜRZBURG

2 IceCube detection of PeV events Events 20 and 14 ( Ernie and Bert, IceCube Collaboration, 2013, Science, 342) N 2 / 18

3 Atmospheric neutrinos Events per 662 Days Background Atmospheric Muon Flux Bkg. Atmospheric Neutrinos (π/k) Background Stat. and Syst. Uncertainties Atmospheric Neutrinos (Benchmark Charm Flux) Atmospheric Neutrinos (90% CL Charm Limit) Signal+Bkg. Best-Fit Astrophysical E 2 Spectrum Data Deposited EM-Equivalent Energy in Detector (TeV) (IceCube Collaboration, 2013, Science, 342) 3 / 18

4 Atmospheric neutrinos Events per 662 Days Background Atmospheric Muon Flux Bkg. Atmospheric Neutrinos (π/k) Background Stat. and Syst. Uncertainties Atmospheric Neutrinos (Benchmark Charm Flux) Atmospheric Neutrinos (90% CL Charm Limit) Signal+Bkg. Best-Fit Astrophysical E 2 Spectrum Data Deposited EM-Equivalent Energy in Detector (TeV) What are possible (astrophysical) sources of these events? 3 / 18

5 IceCube detection of PeV events Single source in Galactic center excluded (Adrián-Martínez et al., 2014, ApJL 786, L5) homogenous distribution Gamma-ray Burst (GRB) origin unlikely Ñ candidate: active galaxies (Mannheim K., 1995, Astroparticle Physics 3, 295) 4 / 18

6 Active Galactic Nuclei ESO/M. Kornmesser 5 / 18

7 Blazar Spectral Energy Distribution 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18

8 Blazar Spectral Energy Distribution Synchrotron Emission 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18

9 Blazar Spectral Energy Distribution Big Blue Bump 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18

10 Blazar Spectral Energy Distribution Leptonic (SSC, EC)? Hadronic? 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18

11 Active Galactic Nuclei - hadronic models p 7 / 18

12 Active Galactic Nuclei - hadronic models γ p 7 / 18

13 Active Galactic Nuclei - hadronic models n π` γ p 7 / 18

14 Active Galactic Nuclei - hadronic models e ν e p n ν µ ν µ νe µ` e` π` γ p 7 / 18

15 Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry VLBI monitoring at 8.4 & 22.3 GHz brightest γ-ray (GeV) and radio sources Ojha et al. 2010, A&A, 519, A45 8 / 18

16 TANAMI Blazars in the IceCube PeV Fields Bert Ernie Source α [ ] δ [ ] z Class. θ [ ] FSRQ : : 1.35 FSRQ : : 1.48 FSRQ FSRQ ? BL Lac FSRQ Healey et al. (2008) Cutri et al. (2003) : Lambert&Gontier (2009) Immer et al. (2011) Fomalont et al. (2003) Véron-Cetty&Véron (2006) Massaro et al. (2009) Masetti et al. (2008) 9 / 18

17 VLBI Images Bert Ernie AT-PA-MP-HO-CD-HH-TI AT-PA-MP-HO-CD-TC AT-PA-MP-HO-CD-TC Relative DEC [mas] Relative DEC [mas] AT-PA-MP-HO-CD Relative RA [mas] AT-PA-MP-HO- CD-TC-TD-HH-WW Relative RA [mas] AT-PA-MP-HO-CD-TC-TI Relative RA [mas] Flux Density [mjy/beam] Flux Density [mjy/beam] (Krauß et al., A&A, 2014, 556, L7) 10 / 18

18 Broadband coverage RADIO MICROWAVE IR OP UV soft hard X-rays γ-rays λ [m] E [ev] ν [Hz] / 18

19 Broadband spectra 100 ATCA 2MASS BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL ATCA 2MASS BAT TANAMI WISE OM XMM/pn Ced Planck UVOT XRT Fermi/LAT 2FGL ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νfν [10 12 erg s 1 cm 2 ] νlν [erg s 1 ] E E E TANAMI 2MASS WISE UVOT BAT INTEGRAL Fermi/LAT XRT 2FGL ATCA 2MASS TANAMI WISE Planck UVOT BAT XRT Fermi/LAT 2FGL ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νfν [10 12 erg s 1 cm 2 ] νlν [erg s 1 ] E E E Frequency [Hz] Frequency [Hz] Frequency [Hz] (Krauß et al., A&A, 2014, 556, L7) 12 / 18

20 Broadband spectra νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Ced Planck MASS WISE OM UVOT BAT XMM/pn XRT Fermi/LAT 2FGL E νlν [erg s 1 ] Frequency [Hz] (Krauß et al., A&A, 2014, 556, L7) 13 / 18

21 Broadband spectra νfν [10 12 erg s 1 cm 2 ] MASS TANAMI WISE UVOT BAT INTEGRAL XRT Fermi/LAT 2FGL E νlν [erg s 1 ] Frequency [Hz] (Krauß et al., A&A, 2014, 556, L7) 14 / 18

22 Neutrino fluence Bert Ernie source Fγperg cm 2 s 1 ) events `1.0` ˆ `3.4` ˆ `7.5` ˆ `4.5` ˆ `2.4` ˆ ˆ `1.2` ` ` ` ` ` ` Total estimate of maximum neutrino fluence using broadband spectra, based on Mannheim, 1993, A&A, 269, 67 Ñ neutrinos in 662 days 15 / 18

23 Neutrino fluence - caveats more realistic neutrino spectrum Ñ lower number of neutrinos additional contributions from faint sources ÝÑ AGN/blazars are able to explain the observed number of PeV neutrinos! 16 / 18

24 Conclusions neutrinos would provide unambigious evidence of hadronic processes six TANAMI sources could explain the observed neutrinos 17 / 18

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