# Chemical abundances in Seyfert galaxies X. Sulphur abundance estimates

## TL;DR

This study measures sulphur abundances in Seyfert 2 galaxies using direct electron temperature estimates, revealing distinct chemical enrichment patterns compared to star-forming regions and analyzing the S/O ratio behavior across metallicities.

## Contribution

First direct sulphur abundance estimates in Seyfert 2 nuclei using electron temperature, highlighting differences from star-forming regions and analyzing S/O ratio trends.

## Key findings

- Sy 2s have similar temperatures to star-forming regions for S+ ions.
- Sy 2s show higher temperatures for S++ ions compared to star-forming regions.
- Sulphur abundances in Sy 2s are lower than in star-forming regions at similar metallicity.

## Abstract

For the first time, the sulphur abundance relative to hydrogen (S/H) in the Narrow Line Regions of a sample of Seyfert 2 nuclei (Sy 2s) has been derived via direct estimation of the electron temperature. Narrow emission line intensities from the SDSS DR17 [in the wavelength range 3000 < $\lambda$ < 9100] and from the literature for a sample of 45 nearby ($z$ < 0.08) Sy 2s were considered. Our direct estimates indicate that Sy 2s have similar temperatures in the gas region where most of the S+ ions are located in comparison with that of star-forming regions (SFs). However, Sy 2s present higher temperature values ($\sim$10000 K) in the region where most of the S++ ions are located relative to that of SFs. We derive the total sulphur abundance in the range of 6.2 < 12 + log(S/H) < 7.5, corresponding to 0.1-1.8 times the solar value. These sulphur abundance values are lower by $\sim$0.4 dex than those derived in SFs with similar metallicity, indicating a distinct chemical enrichment of the ISM for these object classes. The S/O values for our Sy 2 sample present an abrupt ($\sim$0.5 dex) decrease with increasing O/H for the high metallicity regime [12 + log(O/H) > 8.7)], what is not seen for the SFs. However, when our Sy 2 estimates are combined with those from a large sample of star-forming regions, we did not find any dependence between S/O and O/H.