blazar observation and extragalatic absorption
DESCRIPTION
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). - PowerPoint PPT PresentationTRANSCRIPT
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
???