The morphology of the 3-6 keV continuum and Fe-K emission of NGC 3393
Abstract
Galaxies with a luminous centre are likely to have an active galactic nucleus (AGN). Within the AGN X-Rays are emitted from the accretion disk corona and also in the collimated jets undergoing Inverse Compton scattering. However, the details of this AGN feedback and especially how it interacts with the AGN's host galaxy, is poorly understood. It has been suggested that the interaction between the AGN feedback and the interstellar gas of the host galaxy could initiate star formation, a vital component to the mechanism of galaxy formation. Recent papers based on the Chandra data of ESO 428-G014 have shown the presence of kpc size 3-6 keV continuum and Fe-K emission. We explore how common this extended emission is by revisiting the Chandra data of Compton thick AGN NGC 3393. The observations, taken on the ACIS-S chip, have a combined exposure time of 334ks in the energy range 0.3 keV to 7 keV. We present a morphological analysis of this hard X-ray emission.
- Publication:
-
American Astronomical Society Meeting Abstracts #233
- Pub Date:
- January 2019
- Bibcode:
- 2019AAS...23324218P