X-ray colour-colour selection for heavily absorbed AGN

TL;DR

This paper introduces a simple X-ray colour-colour method using hardness ratios to identify heavily absorbed AGN at moderate redshift, improving obscuration estimates in low signal-to-noise data, with implications for future X-ray spectroscopy.

Contribution

The paper presents a novel, straightforward X-ray colour-colour technique using HR1 and HR2 to identify heavily absorbed AGN, addressing limitations of simple hardness ratio analysis.

Findings

61% of the sample have NH>10^23 cm^-2

Most sources do not match simple absorbed power-law spectra

Complex spectra are common, requiring advanced analysis

Abstract

We present a method for the identification of heavily absorbed AGN (NH>10^23 cm^-2) from X-ray photometric data. We do this using a set of XMM-Newton reference spectra of local galaxies for which we have accurate NH information, as described in Brightman & Nandra. The technique uses two rest-frame hardness ratios which are optimised for this task, which we designate HR1 (2-4/1-2 keV) and HR2 (4-16/2-4 keV). The selection method exploits the fact that while obscured AGN appear hard in HR2 due to absorption of the intrinsic source flux below ~4 keV, they appear soft in HR1 due to excess emission originating from scattered source light, thermal emission, or host galaxy emission. Such emission is ubiquitous in low redshift samples. The technique offers a very simple and straight forward way of estimating the fraction of obscured AGN in samples with relatively low signal-to-noise ratio in the X-ray band. We apply this technique to a moderate redshift (z~1) sample of AGN from the Chandra Deep Field North, finding that 61% of this sample has NH> 10^23 cm^-2. A clear and robust conclusion from our analysis, is that in deep surveys the vast majority of sources do not show hardness ratios consistent with a simple absorbed power-law. The ubiquity of complex spectra in turn shows that simple hardness ratio analysis will not yield reliable obscuration estimates, justifying the more complex colour-colour analysis described in this paper. While this method does very well at separating sources with NH> 10^23 cm^-2 from sources with lower NH, only X-ray spectroscopy can identify Compton thick sources, through the detection of the Fe Ka line. This will be made possible with the high throughput X-ray spectral capabilities of ATHENA.