Estimation of neutrino spectra from AGNs using measured VHE -ray spectra Garabed HALLADJIAN December 9 th, 2008 -cr-ν workshop, PARIS 9 December 2008 G. Halladjian 1
Presentation plan Hypotheses & Aim Extra-Galactic Background Light (EBL) Definition & characteristics Interaction with VHE -rays Optical depth Definition & Analyses Conversion of -ray energy spectrum to ν energy spectrum ν energy spectra for 1ES1101-232 ν energy spectra index for different AGNs Questions 9 December 2008 G. Halladjian 2
Hypotheses AGN Intergalactic Space Earth 9 December 2008 G. Halladjian 3
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) ν e 9 December 2008 G. Halladjian 4
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena ν e ν e ν τ 9 December 2008 G. Halladjian 5
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena 3. -rays absorption while they travel through space ν e ν e ν τ 9 December 2008 G. Halladjian 6
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena 3. -rays absorption while they travel through space ν e ν e ν τ 9 December 2008 G. Halladjian 7
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena 3. -rays absorption while they travel through space ν e ν e ν τ 9 December 2008 G. Halladjian 8
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena 3. -rays absorption while they travel through space ν e ν e ν τ 9 December 2008 G. Halladjian 9
Hypotheses 1. -rays & ν emitted by π 0 decay (p-p interaction) 2. ν oscillation phenomena 3. -rays absorption while they travel through space ν e ν e ν τ 9 December 2008 G. Halladjian 10
Extra-Galactic Background Light (EBL) EBL is the light emitted from all objects in the Universe during its entire history It forms a diffused sea of photons that permeates intergalactic space 9 December 2008 G. Halladjian 11
-ray attenuation by EBL (E) + (ε) e + + e 9 December 2008 G. Halladjian 12
EBL (different experiments) 9 December 2008 G. Halladjian 13
EBL spectra (Upper & lower limits) On Gamma Ray Burst and Blazar AGN Origins of the Ultra-High Energy Cosmic Rays in Light of First Results from Auger Charles D. Dermer 9 December 2008 G. Halladjian 14
EBL spectra 9 December 2008 G. Halladjian 15
Optical depth τ The optical depth expresses the quantity of light removed from a beam by scattering or absorption during its path through a medium. If I 0 is the intensity of radiation at the source and I is the observed intensity after a given path, then optical depth τ is defined by the following equation: I = I 0 e τ 9 December 2008 G. Halladjian 16
Optical depth τ τ E, z = 0 z d z ' 1 1 dµ ' ' εth d ε [ dl 1 µ d z ' 2 n ε ε ', z ' σ ' E dl dz = R H 1 z { 1 z 2 m z 1 z 2 z [ 1 z 2 r Λ ]} 1/2, ε ', µ ] σ E,ε, µ = 3σ T 16 1 β2 [ 2β β 2 2 3 β 4 ln 1 β 1 β ] β= 1 ε th ε ε th E, µ = 2m 2 e E 1 µ ' ε th =ε th E ', µ E ' =E 1 z ' Simultaneous constraints on the spectrum of the extragalactic background light and the intrinsic TeV spectra of Mrk 421, Mrk 501, and H1426+428 Eli Dwek & Frank Krennrich 9 December 2008 G. Halladjian 17
1ES1101-232 z = 0.186 Dec = -23 o 29 31 Vis = 0.632017 9 December 2008 G. Halladjian 18
Optical Depth τ 9 December 2008 G. Halladjian 19
Optical Depth τ On Gamma Ray Burst and Blazar AGN Origins of the Ultra-High Energy Cosmic Rays in Light of First Results from Auger Charles D. Dermer 9 December 2008 G. Halladjian 20
Optical Depth τ 9 December 2008 G. Halladjian 21
Optical Depth τ 9 December 2008 G. Halladjian 22
-ray spectra (Hess) 9 December 2008 G. Halladjian 23
Conversion from -ray to ν spectra Hypothesis: TeV ray emission is dominated by the decay of π 0 produced in p-p interactions The following parameterization is for galactic sources dn p de p =k p E p 1 TeV dn k E de 1TeV dn ν de ν k ν E ν 1 TeV Γ p Γ exp E p ε p exp E ε Γ ν exp E ν ε ν k ν 0.71 0.16 Γ p Γ ν Γ Γ p 0.1 ε ν 0. 59 ε ε p /40 ε p ε ε ν k Potential Neutrino Signals from Galactic -Ray Sources (Aharonian & al.) 9 December 2008 G. Halladjian 24
ν spectrum (Hess) Neutrino spectrum 9 December 2008 G. Halladjian 25
-ray & ν spectra 9 December 2008 G. Halladjian 26
1ES1101-232 (-ray) -ray spectra at Earth -ray spectra at source (HESS) -ray spectra at source (example) -ray spectra at source (upper limit) -ray spectra at source (lower limit) F =5.49541 10 13 E 2. 76 TeV 1 cm 2 s 1 1 TeV F =5.88844 10 12 E 1. 5 TeV 1 cm 2 s 1 1 TeV F =7.24436 10 12 E 1. 41 TeV 1 cm 2 s 1 1 TeV F =1.58489 10 11 E 0. 86 TeV 1 cm 2 s 1 1 TeV F =3.98107 10 12 E 1.81 TeV 1 cm 2 s 1 1 TeV 9 December 2008 G. Halladjian 27
1ES1101-232 (ν) -ray spectra at Earth ν spectra at source (HESS) ν spectra at source (example) ν spectra at source (upper limit) ν spectra at source (lower limit) F =5.49541 10 13 E 2. 76 TeV 1 cm 2 s 1 1 TeV F =2. 67335 10 12 E 1.5 TeV 1 cm 2 s 1 1 TeV F =3.39326 10 12 E 1.41 TeV 1 cm 2 s 1 1 TeV F =8.81835 10 12 E 0.86 TeV 1 cm 2 s 1 1 TeV F =1.60995 10 12 E 1. 81 TeV 1 cm 2 s 1 1 TeV 9 December 2008 G. Halladjian 28
Spectrum index AGN z Dec. Γ Earth Γ min Γ max 1ES1101-232 0.186-23 o 29 31-2.76-1.81-0.86 1ES0347-121 0.188-11 o 59 27-2.82-1.85-0.87 PG1553+113 (0.35) +11 o 11 24-4.41-2.79-1.37 1ES0229+200 0.14 +20 o 17 16-2.59-1.88-1.22 H2356-309 0.165-30 o 37 22-3.08-2.25-1.55 PKS2155-304 0.116-30 o 13 18-3.27-2.65-2.05 PKS2005-489 0.071-48 o 49 19-3.59-3.19-2.81 9 December 2008 G. Halladjian 29
Questions EBL correction: Γ < 1.6 is physical? Other models for EBL? Internal absorption model? (is going on the good way for us) Conversion -ray flux to ν flux: Need model of p- may be use model developed for GRB in any case, what X-ray data will be used? Thanks! 9 December 2008 G. Halladjian 30