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Markos Georganopoulos University of Maryland Baltimore County & NASA Goddard. Is the GeV emission of blazars really produced inside the broad line region?. External Compton scattering off the broad line ~10 eV photons. Sikora, Begelman, & Rees ‘94 >Spherical broad line region

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Markos Georganopoulos University of Maryland Baltimore County & NASA Goddard

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Markos georganopoulos university of maryland baltimore county nasa goddard

Markos GeorganopoulosUniversity of Maryland Baltimore County&NASA Goddard

Is the GeV emission of blazars really produced inside the broad line region?


External compton scattering off the broad line 10 ev photons

External Compton scattering off the broad line ~10 eV photons

Sikora, Begelman, & Rees ‘94

>Spherical broad line region

with R~1017-18 cm

Uo UBLRΓ2

oBLRΓ 2 10 -4 in mc2 units


Observed compton dominance up to 100 external compton losses dominate

Kubo et al ‘98

Observed Compton dominance up to ~100 =>External Compton losses dominate

photons of ~ few GeV 

electrons of at least the same energy (γ~104)

For seed photons o~10-4

oγ~1

GeV emission comes from scatterings in the gray area between the Thomson and Klein-Nishina regimes


The devil is in the details

The devil is in the details…

At GeV electron energies the cooling time is

~ energy independent!

Effect on n(γ) ?


The devil is in the details1

The devil is in the details…

At GeV electron energies the cooling time is

~ energy independent!

Effect on n(γ) ?


The electron distribution

The electron distribution


How ec dominated blazars should look

How EC dominated blazars should look

  • Unavoidable but unobserved marks:

  • The hump in the synchrotron component

  • 2. The flat/rising SED of the GeV component (rarely seen, typical GeV spectrum is steep)

  • 3. Achromatic variability for the synchrotron hump and the GeV regime.


How ec dominated blazars should look1

How EC dominated blazars should look

  • Unavoidable but unobserved marks:

  • The hump in the synchrotron component

  • 2. The flat/rising SED of the GeV component (rarely seen, typical GeV spectrum is steep)

  • 3. Achromatic variability for the synchrotron hump and the GeV regime.


Download the code at

Download the code at:

www.jca.umbc.edu/~markos/cs


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