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Blazar observation and extragalatic absorption

Blazar observation and extragalatic absorption. Denis Bastieri & Antonio Saggion. Blazars – Optical depth and flux calculation. with d F /dE = A × E – [ d F /dE ] = g cm –2 s –1 GeV –1 IR-photon dependence via a density table  easy update. E 0 : -energy ( z = 0).

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Blazar observation and extragalatic absorption

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  1. Blazar observation andextragalatic absorption Denis Bastieri & Antonio Saggion

  2. Blazars – Optical depth and flux calculation with dF/dE = A×E– [dF/dE] = g cm–2s–1GeV–1 IR-photon dependence via a density table easy update E0: -energy (z = 0). t(z): cosmic time: dt/dz = H0–1(1+z)–5/2. h0 = 0.75. ze: redshift of the source x = (1 – cosJ), J scattering angle n: bkg frequency at redshift z sgg: cross section gg  e+e– Numerical integration qgauss of Num. Recipes D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  3. Blazars – The photon density Data from the homepage of Tanja Kneiske http://www.astro.uni-wuerzburg.de/~kneiske/ D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  4. 10/3 Li & Ma 200 Blazars – Significativity calculation A α z Integration in log10(E[GeV]) log10(ΔEi) = [1, 1.1] … [3.9, 4] Flux Φ(Ei, θi) in γ/cm2 RA dec Aeff Sigma Novas Trigger Obs. time in ZA bins Δθi = [0, 5] … [65, 70] obs.time/night > 10 min γ detectable by Magic <F> (Hz) D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  5. Observability inset: hours/1year ZA bins. Source name & source flux cm–2s–1GeV–1 Unabsorbed flux Sensitivity data Flux interacting with IR EGRET – Markarian 421 D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  6. EGRET – 3c279 MAGIC should evidence the internal cutoff of FSRQ: fore- seen in many models around 100 GeV. Costamante & Ghisellini “TeV candidates BL Lac objects.” astro/ph0112201 D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  7. EGRET – Observation time: ΔTσ=5 List of EGRET sources. In the histogram on the left are shown the ΔTσ=5 for each source observable by MAGIC. There are 46 sources with an expected ΔTσ=5 less than 100 hours. Observation time to reach σ = 5 level for EGRET sources. X-bins are logarithmic. 25 13 8 5 3 D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  8. Catalogue of the best TeV candidates Ensembleof 246 different objects  33 TeV Candidates Selection criterium based on RADIO fluxesfor optical fluxes possible contamination from the host galaxy. D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  9. Costamante & Ghisellini: new lists Costamante-Ghisellini criterium Ghisellini model: Theoretical approach. SSC-model + fit on LC, Lsyn ratio. Data on A, α, z, RAand dec. 33 sources Fossati model: Phenomenology. SSC-model + LC ~ Lsyn 23 with data on z and with a total obs. time  0 Tables D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  10. Costamante: Ghisellini model 7 sources 12 sources 4 sources D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  11. Costamante: Fossati model 11 sources 9 sources 3 sources D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

  12. ??? different emission models dI/dE = A×E– “virtualAGN” engine Conclusions 46 + 23 Blazars are observable with σ ~ 5 in ~ 1 hour. Observation of “near”-FSRQs can provide a tool to measure internal cutoff and to verify emission models. D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

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