Blazar observation andextragalatic absorption

Denis Bastieri& Antonio

Saggion

2D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Blazars – Optical depth and flux calculation

E0: -energy (z = 0).t(z): cosmic time: dt/dz = H0

–1(1+z)–5/2. h0 = 0.75.ze: redshift of the sourcex = (1 – cos), scattering angle: bkg frequency at redshift z: cross section e+e–

E0: -energy (z = 0).t(z): cosmic time: dt/dz = H0

–1(1+z)–5/2. h0 = 0.75.ze: redshift of the sourcex = (1 – cos), scattering angle: bkg frequency at redshift z: cross section e+e–

Numerical integrationqgauss of Num. Recipes

Numerical integrationqgauss of Num. Recipes

with d/dE = A×E–

[d/dE] = cm–2s–1GeV–1

IR-photon dependence viaa density table easy update

with d/dE = A×E–

[d/dE] = cm–2s–1GeV–1

IR-photon dependence viaa density table easy update

0

03

2

00

0 1212

, zxhEsh

zuzd

xdx

dzdt

dzczEez

e

E

EedEd

dEE

3D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Blazars – The photon density

Data from the homepageof Tanja Kneiske

Data from the homepageof Tanja Kneiske

http://www.astro.uni-wuerzburg.de/~kneiske/

4D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Blazars – Significativity calculation

FluxFlux

αA z

NovasNovas

Φ(Ei, θi) in γ/cm2Φ(Ei, θi) in γ/cm2

decRA

TriggerTriggerAeff SigmaSigma

γ detectableby Magic<> (Hz)

γ detectableby Magic<> (Hz)

Integration in log10(E[GeV])

log10(ΔEi) = [1, 1.1] … [3.9, 4]

Obs. time in ZA binsΔθi = [0, 5] … [65, 70]

obs.time/night > 10 min

TS

TNSQF

61

2200

Li & Ma10/3

25

s900

T

5D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

EGRET – Markarian 421

Source name& source fluxcm–2s–1GeV–1

Sensitivitydata

Unabsorbedflux

Fluxinteracting

with IR

Observabilityinset:

hours/1yearZA bins.

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

EGRET – 3c279

MAGIC shouldevidence theinternal cutoffof FSRQ: fore-seen in manymodels around100 GeV.

Costamante & Ghisellini“TeV candidatesBL Lac objects.”astro/ph0112201

7D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

EGRET – Observation time: ΔTσ=5

Observation time to reach σ = 5 level forEGRET sources. X-bins are logarithmic.

25

13

85 3

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.

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.

9D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Costamante & Ghisellini: new lists

Costamante-Ghisellinicriterium

Costamante-Ghisellinicriterium

33 sources33 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 onLC, Lsyn ratio.

Ghisellini model:

Theoretical approach.SSC-model + fit onLC, Lsyn ratio.

Fossati model:

Phenomenology.SSC-model + LC ~ Lsyn

Fossati model:

Phenomenology.SSC-model + LC ~ Lsyn

Data onA, α, z, RA and dec.

Data onA, α, z, RA and dec.

TablesTables

10D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Costamante: Ghisellini modelSource z A (Hz) T>5

2200+428 0.069 3.74 1.06×10–5 16. 3.5 s 1553+113 0.360 2.97 3.21×10–7 2.9 1.8 min 1114+202 0.139 3.21 2.91×10–7 1.6 6.4 min 1136+673 0.135 2.98 8.02×10–8 0.82 23 min 1417+257 0.237 2.73 4.09×10–8 0.68 34 min 1218+304 0.182 2.78 4.19×10–8 0.62 40 min 1101-232 0.186 2.19 8.18×10–9 0.52 57 min 0414+009 0.287 2.93 4.23×10–8 0.44 1.3 hr 1133+704 0.045 3.12 5.36×10–8 0.42 1.5 hr 1959+650 0.047 3.10 4.88×10–8 0.38 1.8 hr 0556-384 0.034 2.28 6.13×10–9 0.32 2.6 hr 0120+340 0.272 2.39 8.15×10–9 0.29 3 hr 1727+502 0.055 2.80 2.03×10–8 0.28 3.2 hr 0323+022 0.147 3.37 7.33×10–8 0.28 3.4 hr 2356-309 0.165 2.42 6.14×10–9 0.25 4.1 hr 1011+496 0.200 2.57 1.08×10–8 0.25 4.1 hr 1741+196 0.084 2.34 6.03×10–9 0.24 4.3 hr 0229+200 0.139 2.25 3.76×10–9 0.18 7.5 hr 1722+119 0.018 3.11 2.58×10–8 0.17 8.7 hr 0033+595 0.086 2.22 2.65×10–9 0.14 13 hr 1440+122 0.162 2.51 4.98×10–9 0.13 15 hr 0214+517 0.049 2.55 4.84×10–9 0.12 18 hr 0548-322 0.069 2.36 2.39×10–9 0.12 19 hr

7 sources

12 sources

4 sources

11D. Bastieri: Flux extrapolation – GLAST s/w meeting – Udine, Jan. 31st 2003.

Costamante: Fossati modelSource z A (Hz) T>5

2200+428 0.069 2.50 1.69×10–7 4.6 43 s 1133+704 0.045 1.99 2.44×10–8 2.3 2.9 min 1722+119 0.018 1.89 2.03×10–8 2.2 3.1 min 1959+650 0.047 2.01 2.32×10–8 2. 3.8 min 0214+517 0.049 1.99 1.66×10–8 1.4 7.3 min 0548-322 0.069 2.01 1.34×10–8 1.4 8.3 min 1727+502 0.055 2.00 1.53×10–8 1.3 8.8 min 0556-384 0.034 1.93 1.15×10–8 1.2 9.8 min 1741+196 0.084 2.08 1.69×10–8 1.2 10 min 1553+113 0.360 2.88 9.33×10–8 1. 14 min 0033+595 0.086 1.99 5.79×10–9 0.52 57 min 1114+202 0.139 2.07 5.23×10–9 0.39 1.7 hr 2356-309 0.165 2.10 4.35×10–9 0.35 2.1 hr 1101-232 0.186 2.14 4.48×10–9 0.32 2.6 hr 0229+200 0.139 2.03 3.44×10–9 0.28 3.3 hr 1136+673 0.135 2.03 3.24×10–9 0.27 3.6 hr 1218+304 0.182 2.12 3.92×10–9 0.26 3.7 hr 0323+022 0.147 2.03 2.94×10–9 0.23 4.8 hr 1440+122 0.162 2.02 2.65×10–9 0.21 5.6 hr 1417+257 0.237 2.14 2.50×10–9 0.16 10 hr 0120+340 0.272 2.20 2.69×10–9 0.15 11 hr 0414+009 0.287 2.26 3.03×10–9 0.14 13 hr 1011+496 0.200 2.31 2.07×10–9 0.086 35 hr

11 sources

9 sources

3 sources

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 measureinternal cutoff and to verify emission models.

dI/dE = A×E–dI/dE = A×E– differentemission models

differentemission models

“virtualAGN” engine

“virtualAGN” engine

???