1. Blazar observation and extragalatic absorption Denis Bastieri & Antonio Saggion

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

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

4. 4D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003. Blazars – Significativity calculation Flux αAz Novas Φ(E i, θ i ) in γ/cm 2 decRA Trigger A eff Sigma γ detectable by Magic (Hz) γ detectable by Magic (Hz) Integration in log 10 (E[GeV]) log 10 (ΔE i ) = [1, 1.1] … [3.9, 4] Obs. time in ZA bins Δθ i = [0, 5] … [65, 70] obs.time/night > 10 min 200 Li & Ma 10/3

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

6. 6D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003. 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

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

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

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

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

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

12. 12D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003. 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. dI/dE = A×E –  different emission models different emission models “virtualAGN” engine “virtualAGN” engine ???