Metal Abundances of Intermediate-Redshift AGN: Evidence for a Population of Lower-Metallicty Seyfert 2 Galaxies at z = 0.3-0.4

TL;DR

This study measures oxygen abundances in Seyfert 2 galaxies at different redshifts to investigate metallicity evolution over 3-4 billion years, revealing some intermediate-redshift galaxies have lower metallicities than local ones.

Contribution

It introduces a photoionization modeling approach to derive metallicities of Seyfert 2 galaxies and compares their chemical evolution across redshifts.

Findings

Intermediate-redshift Seyfert 2 galaxies show lower metallicities than local counterparts.

Modest chemical evolution of about 0.18 dex over 3-4 Gyrs.

Evidence for lower metallicity Seyfert 2 galaxies at z=0.3-0.4.

Abstract

We derive oxygen abundances for two samples of Seyfert 2 (Sy2) active galactic nuclei (AGN) selected from the KPNO International Spectroscopic Survey (KISS). The two samples from KISS include 17 intermediate-redshift (0.29 < z < 0.42) Sy2s detected via their [O III] lines, and 35 low-redshift (z < 0.1), Halpha-detected Sy2s. The primary goal of this work is to explore whether the metallicity distribution of these two samples changes with redshift. To determine the oxygen abundances of the KISS galaxies, we use Cloudy to create a large number of photoionization model grids by varying the temperature of the accretion disk, the ratio of X-ray to UV continuum light, the ionization parameter, the hydrogen density, and the metallicity of the narrow-line region clouds. We link the results of these models to the observed [O III]/H-beta and [N II]/H-alpha emission-line ratios of the KISS sample on the BPT diagram, interpolating across the model grids to derive metallicity. The two redshift samples overlap substantially in terms of derived metal abundances, but we find that some of the intermediate-redshift Sy2 galaxies possess lower abundances than their local universe counterparts. Our analysis provides evidence for modest levels of chemical evolution (0.18 +/- 0.06 dex) over 3-4 Gyrs of look-back time. We compare our results to other AGN abundance derivation methods from the literature.