# Semi-empirical metallicity calibrations based on ultraviolet emission lines of type-2 AGNs

## TL;DR

This paper develops semi-empirical UV emission-line calibrations to estimate metallicity in the Narrow Line Regions of type-2 AGNs, revealing lower metallicities than in Broad Line Regions and confirming a host galaxy mass-metallicity relation at high redshift.

## Contribution

It introduces new UV emission-line calibrations for NLR metallicity and compares them with photoionization models, enhancing understanding of AGN and galaxy evolution at high redshift.

## Key findings

- NLR metallicities are 2-3 times lower than BLR metallicities.
- Confirmed the mass-metallicity relation in high-redshift AGN host galaxies.
- Derived a M-Z relation consistent with star-forming galaxies at similar redshifts.

## Abstract

We derived two semi-empirical calibrations between the metallicity of the Narrow Line Region (NLR) of type-2 Active Galactic Nuclei and the rest-frame of the N V$\lambda$1240/He II$\lambda1640$, C43=log[(C IV$\lambda1549$+C III]$\lambda1909$)/HeII$\lambda1640$] and C III]$\lambda1909$/C IV$\lambda1549$ emission-line intensity ratios. A metallicity-independent calibration between the ionization parameter and the C III]$\lambda1909$/C IV$\lambda1549$ emission-lines ratio was also derived. These calibrations were obtained comparing ratios of measured UV emission-line intensities, compiled from the literature, for a sample of 77 objects (redshift $0 \: < \: z \: < \: 3.8$) with those predicted by a grid of photoionization models built with the Cloudy code. Using the derived calibrations, it was possible to show that the metallicity estimations for NLRs are lower by a factor of about 2-3 than those for Broad Line Regions (BLRs). Besides we confirmed the recent result of the existence of a relation between the stellar mass of the host galaxy and its NLR metallicity. We also derived a $M-Z$ relation for the objects in our sample at $1.6 \: < \: z \: < \: 3.8$. This relation seems to follow the same trend as the ones estimated for Star Forming galaxies of similar high redshifts but for higher masses.

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Source: https://tomesphere.com/paper/1905.00691