The forbidden high ionisation line region of the type 2 quasar Q1131+16: a clear view of the inner face of the torus?

TL;DR

This study investigates the physical conditions and location of forbidden high ionisation lines in a type 2 quasar, revealing they originate near the inner torus wall, providing insights into the AGN structure and viewing angle effects.

Contribution

It offers the first detailed analysis of FHIL regions in a type 2 quasar, suggesting their proximity to the AGN and the influence of viewing angle on observed line strengths.

Findings

FHIL region has high densities (10^5.5 to 10^8 cm^-3) and high ionisation parameters.

FHIL kinematics are similar to low ionisation lines, with no significant velocity shift.

FHILs are likely located close to the AGN, within 0.32 to 50 parsecs, on the inner torus wall.

Abstract

We present spectroscopic observations of the type 2 quasar SDSS J11311.05+162739.5 (Q1131+16 hereafter; z=0.1732), which has the richest spectrum of forbidden high ionisation lines (FHIL, e.g. [Fe \textsc{vii}], [Fe \textsc{x}], [Fe \textsc{xi}] and [Ne \textsc{v}]) yet reported for an AGN, as well as unusually strong [O \textsc{iii}]$\lambda$4363 emission. The study of this object provides a rare opportunity to investigate the physical conditions and kinematics of the region(s) emitting the FHILs. By comparison with photoionisation model results, we find that the FHIL region has high densities (10$^{5.5}$ $<$ $n_H$ $<10^{8.0}$ cm$\textsuperscript{-3}$) and ionisation parameters (-1.5 $<$ log[U] $<$ 0), yet its kinematics are similar to those of the low ionisation emission line region detected in the same object (FWHM $\sim$ 360$\pm$30 km/s), with no evidence for a significant shift between the velocity centroid of the FHILs and the rest frame of the host galaxy. The deduced physical conditions lie between those of the Broad-Line (n$_H$$>10^9$ cm$\textsuperscript{-3}$) and Narrow-Line Regions ($n_H$$<10^6$ cm$\textsuperscript{-3}$) of active galactic nuclei (AGN), and we demonstrate that the FHIL regions must be situated relatively close to the illuminating AGN (0.32 $<$ $r_{FHIL}$ $<$ 50pc). We suggest that the inner torus wall is the most likely location for the FHIL region, and that the unusual strength of the FHILs in this object is due to a specific viewing angle of the far wall of the torus, coupled with a lack of dust on larger scales that might otherwise obscure our view of the torus.