Differential Sensitivity to Extragalactic Point Sources
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Transcript of Differential Sensitivity to Extragalactic Point Sources
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Richard White 01
Differential Sensitivity to Extragalactic Point Sources
Richard WhiteUniversity of Leeds
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Richard White 02
Blazars - Reminder
Active Galactic Nuclei with the Jet oriented towards Earth.90 deg
60 deg
30 deg
0 deg
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Richard White 03
Target Blazars
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Target Blazars
z = 0.186
0.165
0.1170.071 0o 90o
-90o ~42o lat
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Richard White 05
Effective Area
Cos(Angle)
m2
Cos(0)Cos(-1)
Cos(1)
Neutrino Energy
(GeV)
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Richard White 06
Effective Area
PKS2155-304, 50% ERes
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Richard White 07
Angular Resolution
Assuming constant at the moment (1o – worst case).Using IceCube geometry doesn’t work well at all!
E (GeV)
Ang. R
es.
(deg)
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Richard White 08
Atm. Background
Use Volkova Soviet J. Nucl. Phys. 37, 784 (1980)
Function of Zenith angle
Calculate Daily Average.
Integrate over the search cone.
Rebinned to EResInside cone
Av. Source Zenith (over 2π)
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Richard White 09
ν Production Total Solution: pp, pγ, and leptonic contributions.
Upper (very upper) limit, just pp.
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Richard White 10
Measured γ-Ray spectrum.
Expected ν spectrum.
Kappes et al. (2006)
From γ-Rays to ν
Kelner et al. (2006)
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Richard White 11
Measured γ-Ray spectrum.
Expected ν spectrum.
Intrinsic γ-Ray spectrum.
From γ-Rays to ν
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Richard White 12
EBL
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Richard White 13
Measured γ-Ray spectrum.
Expected ν spectrum.
Intrinsic γ-Ray spectrum.
From γ-Rays to ν
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Richard White 14
Bringing it all together...
Input Eres, Emin, Emax
Input Aeff
Input Atm. Flux
Input ARes. Calc. El. vs. Time
Calc. fobs
Calc. E binsInput γ-Ray Spectrum
Apply EBL Model
Fit
Calc. Events >Ethres
Rebin to E bins
Rebin to E bins
Calc. ν Spectrum
Rebin to E bins
Calc. Source and Atm, ν in each E bin
Opt. Cone=1.585ARes
Integrate over Cone
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Richard White 15
Cone Size
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ν Upper Limits
Ns = 29Nb = 33
Differential Flux PKS2155-304, z=0.117
Spectral Index = -2.0
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ν Upper Limits
Ns = 1.36Nb = 33
Differential Flux PKS2155-304, z=0.117
Primack(SAM,05)
Spectral Index = -2.8
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ν Upper Limits
Ns = 651 !!Nb = 29
Differential Flux 1ES1101-232, z=0.186
Spectral Index Forced to -1.1
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ν Upper Limits
Ns = 135Nb = 29
Differential Flux 1ES1101-232, z=0.186
Spectral Index Forced to -1.5
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Richard White 17
ν Upper Limits
Ns = 26Nb = 29
Differential Flux 1ES1101-232, z=0.186
Spectral Index Forced to -2.0
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Richard White 18
Conclusions
UPPER LIMITS obtained for several southern hemisphere blazars.
Must extend to p-γ
WORK IN PROGRESS
Even with the lowest EBL model the most distant Blazars upper limits exceed the background... but differential detection seems unlikely.
Results heavily depend on EBL... γ horizon expanding to limit the EBL with more distant sources.