Systematic X-ray study of GeV gamma-ray emitting radio galaxies

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  • uploaded June 25, 2021

Discussion timeslot (ZOOM-Meeting): 16. July 2021 - 18:00
ZOOM-Meeting URL: https://icrc2021.desy.de/pf_access_abstracts
Corresponding Session: https://icrc2021-venue.desy.de/channel/Presenter-Forum-1-Evening-All-Categories/48
Abstract:
Black Holes (BHs) at the center of galaxies have a 10^6 - 10^9 rnsolar mass and thus are called Supermassive Black hole (SMBH). When a large amount of matter accretes onto SMBH, the accreting matter shines brightly, and this phenomenon is called active galactic nuclei (AGN). Only 10% of AGNs have a powerful radio jet, and these objects are roughly classified either radio galaxy or blazar. Blazar is bright but its radiation almost comes from the core jet because of strong beaming effect, while radio galaxy whose beaming effect is weak show various emission components from outer-layer jet, outer jet, and disk/corona. Therefore, radio galaxies are considered to be important objects to understand jet structure. To study the relation between jet and disk is considered to be an important point to understand jet ejection mechanism X-ray emission from radio galaxies contain both jet and disk/corona radiation. Thus, we have to investigate contributions from jet and disk/corona to the X-ray band.rnIn this work, we investigate X-ray and Gamma-ray properties of GeV emitting radio galaxies listed in the 4FGL-DR2 catalog. We use X-ray data of Swift/XRT. We studied time variability, the relation between X-ray and gamma-ray photon index, together with accretion rate, and found they are classified into 3 groups, X-ray emission in the first group is dominated by jet emission, X-ray of the second group is dominated by disk/corona emission, and for the third group both jet and disk/corona contribute to the X-ray band.'

Authors: Hiroto Matake
Co-Authors: Yasushi Fukazawa
Indico-ID: 937
Proceeding URL: https://pos.sissa.it/395/635

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Presenter: Hiroto Matake

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