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AGN emission models

What are the radiative processes in AGN, where are the main emission zones?

Once particles are accelerated, they produce non-thermal photons. These photons will then interact with the complex radiative environment of the AGN until they escape through the cosmos.

My work is focused on the modeling and interpretation of the spectral energy distribution of jetted AGN.
I
also developed tools for the scientific community, fully available on Github and Zenodo:

  • Bjet_MCMC

  • SED_Host_Galaxy_Correction

Code to remove the elliptical host galaxy emission in IR-to-UV SEDs of AGN. This code makes use of PEGASE 2 spectral templates of galaxies Fioc & Rocca-Volmerange 1999.

Github: https://github.com/Ohervet/SED_Host_Galaxy_Correction

Zenodo: https://zenodo.org/records/10800919

Relevant publications:

Bjet_MCMC_logo_v2.png

Bjet_MCMC is a MCMC python wrapper around the C++ code Bjet. It can be used to model multiwavelength spectral energy distributions of blazars, considering one-zone synchrotron-self-Compton (SSC) model with or without the addition of external inverse-Compton process from the thermal emission of the nucleus.

Github: https://github.com/Ohervet/Bjet_MCMC

Zenodo: https://zenodo.org/records/13129296

© 2024 by Olivier Hervet

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