Constraints on the distribution of absorption in the X - ray selected AGN population found in the 13 H XMM - Newton / Chandra deep field

We present an analysis of the X-ray properties of sources detected in the 13H XMM-Newton deep (200ks) field. In order to constrain the absorbed AGN population, we use extensive Monte Carlo simulations to directly compare the X-ray colours of observed sources with those predicted by several model distributions. In particular, we have carried out our comparisons over the entire 0.2–10 keV energy range of the XMM-Newton cameras, making our analysis sensitive to a large range of absorbing column densities. We have tested the simplest form of the unified scheme, whereby the intrinsic luminosity function of absorbed AGN is set to be the same as that of their unabsorbed brethren, coupled with various model distributions of absorption. Of the tested distributions, the best fitting model has the fraction of AGN with absorbing column NH , proportional to (logNH). We have also tested two extensions to the unified scheme: an evolving absorption scenario, in which the fraction of absorbed sources is larger at higher redshifts, and a luminosity dependent model in which high luminosity AGN are less likely to be absorbed. Both of these models provide poorer matches to the observed X-ray colour distributions than the best fitting simple unified model. We find that a luminosity dependent density evolution luminosity function reproduces poorly the 0.5–2 keV source counts seen in the 13H field. Field to field variations could be the cause of this disparity. Computing the X-ray colours with a simple absorbed power-law spectral model is found to over-predict, by a factor of two, the fraction of hard sources that are completely absorbed below 0.5 keV, implying that an additional source of soft-band flux must be present in a number of the absorbed sources. The tested synthesis models predict that around 16% of the detections in the 13H field are due to AGN at z > 3. However, so far, only a single AGN with z > 3 has been identified in our approximately 50% complete optical spectroscopy follow up program. Finally, we use our simulations to demonstrate the efficacy of a hardness ratio selection scheme at selecting absorbed sources for further study. Using this selection scheme, we show that around 40% of the 13H sample are expected to be AGN with NH > 1022 cm−2.