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Differential Sensitivity to Extragalactic Point Sources

Differential Sensitivity to Extragalactic Point Sources. Richard White. University of Leeds. 01. Active Galactic Nuclei with the Jet oriented towards Earth. 90 deg. 60 deg. 30 deg. 0 deg. Blazars - Reminder. 02. Target Blazars. 03. z = 0.186. 0.165. 0.117. 0 o. 90 o. 0.071.

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Differential Sensitivity to Extragalactic Point Sources

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  1. Differential Sensitivity to Extragalactic Point Sources Richard White University of Leeds 01

  2. Active Galactic Nuclei with the Jet oriented towards Earth. 90 deg 60 deg 30 deg 0 deg Blazars - Reminder 02

  3. Target Blazars 03

  4. z = 0.186 0.165 0.117 0o 90o 0.071 -90o ~42o lat Target Blazars 04

  5. Effective Area Cos(0) Cos(-1) m2 Cos(1) Neutrino Energy (GeV) Cos(Angle) 05

  6. PKS2155-304, 50% ERes Effective Area 06

  7. Angular Resolution Assuming constant at the moment (1o – worst case). Ang. Res. (deg) Using IceCube geometry doesn’t work well at all! E (GeV) 07

  8. Atm. Background Use Volkova Soviet J. Nucl. Phys. 37, 784 (1980) Function of Zenith angle Calculate Daily Average. Rebinned to ERes Integrate over the search cone. Inside cone Av. Source Zenith (over 2π) 08

  9. ν Production Total Solution: pp, pγ, and leptonic contributions. Upper (very upper) limit, just pp. 09

  10. Expected ν spectrum. Fromγ-Rays toν Measured γ-Rayspectrum. Kappes et al. (2006) Kelner et al. (2006) 10

  11. Expected ν spectrum. Intrinsic γ-Ray spectrum. Fromγ-Rays toν Measured γ-Rayspectrum. 11

  12. EBL 12

  13. Expected ν spectrum. Intrinsic γ-Ray spectrum. Fromγ-Rays toν Measured γ-Rayspectrum. 13

  14. Opt. Cone=1.585ARes Rebin to E bins Rebin to E bins Integrate over Cone Rebin to E bins Calc. Events >Ethres Calc. Source and Atm, ν in each E bin Bringing it all together... Calc. El. vs. Time Input ARes. Input Aeff Input Eres, Emin, Emax Calc. fobs Calc. E bins Input γ-Ray Spectrum Apply EBL Model Input Atm. Flux Fit Calc. ν Spectrum 14

  15. Cone Size 15

  16. ν Upper Limits Differential Flux PKS2155-304, z=0.117 Spectral Index = -2.0 Ns = 29 Nb = 33 16

  17. ν Upper Limits Differential Flux PKS2155-304, z=0.117 Primack(SAM,05) Spectral Index = -2.8 Ns = 1.36 Nb = 33 16

  18. ν Upper Limits Differential Flux 1ES1101-232, z=0.186 Spectral Index Forced to -1.1 Ns = 651 !! Nb = 29 17

  19. ν Upper Limits Differential Flux 1ES1101-232, z=0.186 Spectral Index Forced to -1.5 Ns = 135 Nb = 29 17

  20. ν Upper Limits Differential Flux 1ES1101-232, z=0.186 Spectral Index Forced to -2.0 Ns = 26 Nb = 29 17

  21. Conclusions UPPER LIMITS obtained for several southern hemisphere blazars. Results heavily depend on EBL... γ horizon expanding to limit the EBL with more distant sources. Even with the lowest EBL model the most distant Blazars upper limits exceed the background... but differential detection seems unlikely. WORK IN PROGRESS Must extend to p-γ 18

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