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
IceCube detection of PeV events Events 20 and 14 ( Ernie and Bert, IceCube Collaboration, 2013, Science, 342) N 2 / 18
Atmospheric neutrinos Events per 662 Days 10 2 10 1 10 0 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 10-1 10 2 10 3 Deposited EM-Equivalent Energy in Detector (TeV) (IceCube Collaboration, 2013, Science, 342) 3 / 18
Atmospheric neutrinos Events per 662 Days 10 2 10 1 10 0 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 10-1 10 2 10 3 Deposited EM-Equivalent Energy in Detector (TeV) What are possible (astrophysical) sources of these events? 3 / 18
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
Active Galactic Nuclei ESO/M. Kornmesser 5 / 18
Blazar Spectral Energy Distribution 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18
Blazar Spectral Energy Distribution Synchrotron Emission 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18
Blazar Spectral Energy Distribution Big Blue Bump 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18
Blazar Spectral Energy Distribution Leptonic (SSC, EC)? Hadronic? 3C 273 (Türler et al., 1999, A&AS, 134, 89) 6 / 18
Active Galactic Nuclei - hadronic models p 7 / 18
Active Galactic Nuclei - hadronic models γ p 7 / 18
Active Galactic Nuclei - hadronic models n π` γ p 7 / 18
Active Galactic Nuclei - hadronic models e ν e p n ν µ ν µ νe µ` e` π` γ p 7 / 18
Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry VLBI monitoring at 8.4 & 22.3 GHz brightest γ-ray (GeV) and radio sources http://pulsar.sternwarte.uni-erlangen.de/tanami Ojha et al. 2010, A&A, 519, A45 8 / 18
TANAMI Blazars in the IceCube PeV Fields Bert Ernie Source α [ ] δ [ ] z Class. θ [ ] 0235 618 39.2218 61.6043 0.47 FSRQ 5.61 0302 623 45.9610 : 62.1904 : 1.35 FSRQ 5.98 0308 611 47.4838 : 60.9775 : 1.48 FSRQ 7.39 1653 329 254.0699 33.0369 2.40 FSRQ 11.18 1714 336 259.4001 33.7024? BL Lac 7.87 1759 396 270.6778 39.6689 1.32 FSRQ 12.50 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
VLBI Images Bert Ernie 80 0235-618 2011-11-13 10 70 0302-623 2010-05-07 0308-611 70 4 8 60 2010-05-07 1000 60 2 6 6 50 50 0 4-2 4 100 40 40 2-4 2 30-6 0 30 20-8 0-2 -10 10 5 0-5 -10-2 20 10-4 0-4 10 5 0-5 -10-6 0 1-20 -8-30 AT-PA-MP-HO-CD-HH-TI AT-PA-MP-HO-CD-TC -10 0 AT-PA-MP-HO-CD-TC -10 20 0-20 -40-60 -80 10 5 0-5 -10 40 20 0-20 20 1653-329 2008-02-07 20 1714-336 2011-11-13 1759-396 2010-05-07 1000 15 15 Relative DEC [mas] Relative DEC [mas] 10 5 0-5 -10-15 -20 20 10-15 AT-PA-MP-HO-CD -20 10 0-10 -20 20 Relative RA [mas] 5 0-5 -10 AT-PA-MP-HO- CD-TC-TD-HH-WW 10 0-10 -20 Relative RA [mas] 10 0-10 AT-PA-MP-HO-CD-TC-TI 15 10 5 0-5 -10-15 Relative RA [mas] 100 10 1 0 Flux Density [mjy/beam] Flux Density [mjy/beam] (Krauß et al., A&A, 2014, 556, L7) 10 / 18
Broadband coverage RADIO MICROWAVE IR OP UV soft hard X-rays γ-rays 1 0.01 10-4 10-6 10-8 10-10 10-12 10-14 10-16 10-18 10-20 λ [m] 10-6 10-4 0.01 1 100 10000 E [ev] 10 6 10 8 10 10 10 12 10 14 10 8 10 10 10 12 10 14 10 16 10 18 ν [Hz] 10 20 10 22 10 24 10 26 10 28 11 / 18
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 ] 10 1 0.1 10 46 10 45 10 44 10 47 10 46 10 45 10 47 10 46 10 45 νlν [erg s 1 ] 0.01 0235-618 E 20 10 43 0302-623 E 20 0308-611 E 20 100 TANAMI 2MASS WISE UVOT BAT INTEGRAL Fermi/LAT XRT 2FGL 10 48 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 ] 10 1 0.1 10 47 10 46 10 47 10 46 10 45 νlν [erg s 1 ] 0.01 1653-329 E 14 10 45 1714-336 E 14 1759-396 E 14 10 9 10 12 10 15 10 18 10 21 Frequency [Hz] 10 24 10 9 10 12 10 15 10 18 10 21 Frequency [Hz] 10 24 10 9 10 12 10 15 10 18 10 21 Frequency [Hz] 10 24 (Krauß et al., A&A, 2014, 556, L7) 12 / 18
Broadband spectra νfν [10 12 erg s 1 cm 2 ] 100 10 1 0.1 0.01 ATCA TANAMI Ced Planck 0302-623 2MASS WISE OM UVOT BAT XMM/pn XRT Fermi/LAT 2FGL E 20 10 47 10 46 10 45 νlν [erg s 1 ] 10 9 10 12 10 15 10 18 Frequency [Hz] 10 21 10 24 (Krauß et al., A&A, 2014, 556, L7) 13 / 18
Broadband spectra νfν [10 12 erg s 1 cm 2 ] 100 10 1 0.1 0.01 2MASS TANAMI WISE UVOT 1653-329 BAT INTEGRAL XRT Fermi/LAT 2FGL E 14 10 48 10 47 10 46 10 45 νlν [erg s 1 ] 10 9 10 12 10 15 10 18 Frequency [Hz] 10 21 10 24 (Krauß et al., A&A, 2014, 556, L7) 14 / 18
Neutrino fluence Bert Ernie source Fγperg cm 2 s 1 ) events 0235 618 `1.0`0.5 0.5 ˆ 10 10 0302 623 `3.4`0.7 0.7 ˆ 10 11 0308 611 `7.5`2.9 2.9 ˆ 10 11 1653 329 `4.5`0.5 0.5 ˆ 10 10 1714 336 `2.4`0.5 0.6 ˆ 10 10 1759 396 ˆ 10 10 `1.2`0.3 0.2 0.19`0.04 0.04 0.06`0.01 0.01 0.14`0.05 0.05 0.86`0.10 0.10 0.46`0.10 0.12 0.23`0.50 0.40 Total 1.9 0.4 estimate of maximum neutrino fluence using broadband spectra, based on Mannheim, 1993, A&A, 269, 67 Ñ 1.9 0.4 neutrinos in 662 days 15 / 18
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
Conclusions neutrinos would provide unambigious evidence of hadronic processes six TANAMI sources could explain the observed neutrinos 17 / 18