neutrinos, agn and auger data
DESCRIPTION
ANTARES Meeting December 5th, 2007. Neutrinos, AGN and Auger data. Nicolas Busca, APC. Scope. Auger found a correlation of CR with nearby AGN The UHECR flux at Earth is ~ 1 event/yr/1000km 2 Use this flux to normalize the - PowerPoint PPT PresentationTRANSCRIPT
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Neutrinos, AGN and Auger data
ANTARES Meeting
December 5th, 2007
Nicolas Busca, APC
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Scope
• Auger found a correlation of CR with nearby AGN
• The UHECR flux at Earth is ~ 1 event/yr/1000km2
• Use this flux to normalize the
• Will only consider interactions of CR with the AGN photon background
• Results will refer to point source fluxes (diffuse flux study in progress…)
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Review of Auger results
Analysis:
• Before May 26th 2006 - explorationFound 12/15 events in correlation with a VC AGN by scanning for the best combination of angle, energy and redshift
(3.10, Emin = 56EeV, zmax=0.018)
• Prescription
• After May 26th 2006 - confirmationFound 8/13 events in correlation with a VC AGN with parameters fixed a priori
Results:After rescanning, the parameters were found to be ~ 60,
Emin~60 EeV, zmax~0.024 (100 Mpc)
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Review of Auger results
AGN correlation
• 21 events of E>57EeV (outside the galactic plane)
• 19 within 3.20 of a VC AGN with z<0.018 (75 Mpc)
Super galactic plane
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Review of Auger results
AGN correlation
• 21 events of E>57EeV
• 19 within 3.20 of a VC AGN with z<0.018 (75 Mpc)
Virgo clusterSuper galactic plane
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Review of Auger results
AGN correlation
• 21 events of E>57EeV
• 19 within 3.20 of a VC AGN with z<0.018 (75 Mpc)
2 events (ESO 139 G12, 73 Mpc)
Super galactic plane
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Review of Auger results
AGN correlation
• 21 events of E>57EeV
• 19 within 3.20 of a VC AGN with z<0.018 (75 Mpc)
2 events (Cen A, 4 Mpc)Super galactic plane
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Review of Auger results
What does this mean?
• CRs are anisotropic
• CRs come preferentially from the direction of some VC AGN
But…
• are AGN really the sources?
• do CR sources have the same distribution as VC AGNs?
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Review of Auger results
What does this mean?
• CRs are anisotropic
• CRs come preferentially from the direction of some VC AGN
But…
• are AGN really the sources?
• do CR sources have the same distribution as VC AGNs?
CRs traverse the environment of an AGN before reaching us!!
(and produce neutrinos…)
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Implications for ’s
nucleus
CR
Production modes:
• foreign (to the AGN)
foreign
• CRs are accelerated away from the nucleus
• AGN need not be the source
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Implications for ’s
nucleus
CR
Production modes:
• foreign (to the AGN)
• local
nucleus
CR
foreign local
• CRs are accelerated away from the nucleus
• AGN need not be the source
• CRs are accelerated near the core of the AGN
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Implications for ’s
nucleus
CR
Production modes:
• foreign (to the AGN)
• local
nucleus
CR
foreign local
• CRs are accelerated away from the nucleus
• AGN need not be the source
• CRs are accelerated near the core of the AGN
€
p+ γ → π 0 + p
p+ γ → π + + n+ isospin symmetric interactions
Interactions:
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CR propagation in AGNs
R ~ 30 Rs ~ 6x1012 cm ~ 2x10-12 Mpc
R
Foreign:
• CR traverse Leff = R
• is a free parameter
Local:
• CRs traverse exactly R
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Photon background (Cen A)
AGN photon background
Steinle (2006)
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AGN photon background
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Proton interaction length
Cen A model
Stecker (1991)
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Proton interaction length
Cen A model
Stecker (1991)
thick
thick
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Spectrum normalization
Cen A
ESO 139 G12
• same exposure to both sources
• same flux at Earth
• but very different luminosity since DCenA ~ 4Mpc and DESO ~ 75 Mpc
• ’s normalized together with the spectrum
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Results: local mode
• source optically thick above the photopion threshold
• no UHECRs would be observed from the source
• model is excluded
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Results: foreign mode, = 1e-3
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Results: foreign mode, = 6e-4
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Results: foreign mode, = 3e-4
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Results: foreign mode, = 1e-4
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Results: foreign mode, = 1e-4
Evolution with spectral index ~ 10x each 0.2
(2.0 is 105 x less than 2.7)