A Hubble Space Telescope Imaging Survey of Low-Redshift Swift-BAT Active Galaxies

TL;DR

This study uses Hubble Space Telescope imaging to analyze the host galaxies of low-redshift Swift-BAT AGN, revealing insights into galaxy types, merging features, and their relation to AGN luminosity and type.

Contribution

First high-resolution imaging survey of Swift-BAT AGN hosts, providing detailed analysis of galaxy morphology and merging features in a hard X-ray selected sample.

Findings

Nearly half of the hosts are early-type galaxies.

Merging features are present in 18-25% of hosts.

Merging fraction increases with AGN luminosity.

Abstract

We present initial results from a Hubble Space Telescope snapshot imaging survey of the host galaxies of Swift-BAT active galactic nuclei (AGN) at z<0.1. The hard X-ray selection makes this sample sample relatively unbiased in terms of obscuration compared to optical AGN selection methods. The high-resolution images of 154 target AGN enable us to investigate the detailed photometric structure of the host galaxies, such as the Hubble type and merging features. We find that 48% and 44% of the sample is hosted by early-type and late-type galaxies, respectively. The host galaxies of the remaining 8% of the sample are classified as peculiar galaxies because they are heavily disturbed. Only a minor fraction of host galaxies (18%-25%) exhibit merging features (e.g., tidal tails, shells, or major disturbance). The merging fraction increases strongly as a function of bolometric AGN luminosity, revealing that merging plays an important role in triggering luminous AGN in this sample. However, the merging fraction is weakly correlated with the Eddington ratio, suggesting that merging does not necessarily lead to an enhanced Eddington ratio. Type 1 and type 2 AGN are almost indistinguishable in terms of their Hubble type distribution and merging fraction. However, the merging fraction of type 2 AGN peaks at a lower bolometric luminosity compared with those of type 1 AGN. This result may imply that the triggering mechanism and evolutionary stages of type 1 and type 2 AGN are not identical.