BAT AGN Spectroscopic Survey. VIII. Type 1 AGN with Massive Absorbing Columns

Abstract

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe explore the relationship between X-ray absorption and optical obscuration within the BAT AGN Spectroscopic Survey (BASS), which has been collecting and analyzing the optical and X-ray spectra for 641 hard X-ray selected (E>14keV) active galactic nuclei (AGNs). We use the deviation from a linear broad Hα-to-X-ray relationship as an estimate of the maximum optical obscuration toward the broad line region (BLR) and compare the A V to the hydrogen column densities (N H ) found through systematic modeling of their X-ray spectra. We find that the inferred columns implied by A V toward the BLR are often orders of magnitude less than the columns measured toward the X-ray emitting region, indicating a small-scale origin for the X-ray absorbing gas. After removing 30% of Sy 1.9s that potentially have been misclassified due to outflows, we find that 86% (164/190) of the Type 1 population (Sy 1-1.9) are X-ray unabsorbed as expected based on a single obscuring structure. However, 14% (26/190), of which 70% (18/26) are classified as Sy 1.9, are X-ray absorbed, suggesting that the BLR itself is providing extra obscuration toward the X-ray corona. The fraction of X-ray absorbed Type 1 AGNs remains relatively constant with AGN luminosity and Eddington ratio, indicating a stable BLR covering fraction.

The multiphase gas structure and kinematics in the circumnuclear region of NGC 5728

“…To determine the necessary kinematic components to model the doublets, we first fit the [OIII]λλ4959,5007 emis-sion lines to use as a robust template for the presence, location, and width of the existing kinematic components comprising the ionized gas as we recently did for this same galaxy in Shimizu et al (2018). In fitting the [OIII] doublet, we fixed the velocity and dispersion of the components to be the same between each of the lines and fixed the intensity ratio (5007/4959) to 3, the theoretical value.…”

BAT AGN Spectroscopic Survey – XIX. Type 1 versus type 2 AGN dichotomy from the point of view of ionized outflows

“…Koss et al (2017) presented an overview of the optical spectroscopic data. Additional extended multi-wavelength campaigns from near-IR (NIR) to soft X-ray wavelengths (Berney et al 2015;Lamperti et al 2017;Oh et al 2017;Ricci et al 2017b;Trakhtenbrot et al 2017;Ricci et al 2017a;Oh et al 2018;Powell et al 2018;Ricci et al 2018;Shimizu et al 2018) have allowed us to further characterize the BASS sample, studying for example the connection between X-ray and optical obscuration, NIR lines, X-ray photon index, absorption and coronal properties.…”

“…We have also considered the opposite view, i.e. that type 1.9 behave as type 2 Seyfert AGN, where the BLR is mimicked in long-slit spectra by an outflow that broadens the emission lines (Shimizu et al (2018); hereafter S18). Of the 57 type 1.9 sources analyzed in S18, 16 (28%) are found to possibly be type 2 AGN with the BLR simulated by an outflow that is detected in [O iii].…”

X-Ray Observations of a [C ii]-bright, z = 6.59 Quasar/Companion System

“…If a significant screen of dust existed, we would expect it to drive the hardness ratio to much harder values. Likewise, the broad Mg II emission (FWHM ∼ 4700 km s −1 ) reported by Mazzucchelli et al (2017, see also Figure 1) indicates that PJ231−20 is a Type 1 AGN; Type 1 AGN have long been seen to have minimal amounts of dust (N H 10 22 cm −2 ; e.g., Shimizu et al 2018). Due to the extreme redshift of PJ231−20, such column densities would have no impact on our observed spectrum.…”