# Obscured AGN at 1.5 < z < 3.0 from the zCOSMOS-deep Survey I. Properties of the emitting gas in the Narrow Line Region

## TL;DR

This study investigates the properties of obscured AGN at high redshift, focusing on their narrow line regions, and introduces new photo-ionization model ingredients to explain observed UV emission line ratios and metallicity evolution.

## Contribution

The paper presents a novel analysis of high-z obscured AGN, incorporating micro-turbulence and small NLR radii into photo-ionization models, revealing metallicity evolution without strong host galaxy mass dependence.

## Key findings

- Successful reproduction of UV line ratios requires micro-turbulence and small NLR radii.
- Detected significant evolution of NLR metallicity with redshift.
- No strong correlation between NLR metallicity and host galaxy stellar mass.

## Abstract

We select a sample of 90 obscured (type2) AGN with 1.45<z<3.05 from the zCOSMOS-deep galaxy sample by 5 sigma-detection of the high-ionization CIV {\lambda}1549 narrow emission line. The presence of this feature in a galaxy spectrum is often associated with nuclear activity, and the selection effectiveness has been also confirmed by ultraviolet (UV) emission line ratio diagnostic diagrams. Applying the same selection technique, a sample of 102 unobscured (type 1) AGN was collected. Taking advantage of the large amount of multi-band data available in the COSMOS field, we investigate the properties of the CIV-selected type 2 AGN, focusing on their host galaxies, X-ray emission and UV emission lines. Finally, we investigate the physical properties of the ionized gas in the Narrow Line Region (NLR) of this type 2 AGN sample, combining the analysis of strong UV emission lines with predictions from photo-ionization models. We find that, in order to successfully reproduce the relative intensity of UV emission lines of the selected high-z type 2 AGN, two new ingredients in the photo-ionization models are fundamental,i.e. small inner radii of the NLR (~90pc for LAGN = 10^45erg/s) and the internal dissipative micro-turbulence of the gas emitting clouds (with vmicr~100km/s). With these modified models, we compute the gas-phase metallicity of the NLR, and our measurements indicate a statistically significant evolution of the metal content with redshift. Finally, we do not observe, in our CIV-selected type 2 AGN sample, a strong relationship between the NLR gas metallicity and the stellar mass of the host galaxy.