# Metallicity and ionization state of the gas in polar-ring galaxies

## TL;DR

This study investigates the ionization and metallicity distribution in 15 polar-ring galaxies using spectroscopic data, revealing dominant ionization by young stars in outer regions and shocks in inner regions, with implications for their formation history.

## Contribution

It provides the first detailed metallicity measurements for a significant sample of polar rings, challenging cold accretion formation scenarios.

## Key findings

- Ionization by young stars dominates in outer polar rings.
- Shocks significantly contribute to gas excitation in inner regions.
- Polar rings show shallow or no metallicity gradients, with no metal-poor gas detected.

## Abstract

The ionization state and oxygen abundance distribution in a sample of polar-ring galaxies (PRGs) were studied from the long-slit spectroscopic observations carried out with the SCORPIO-2 focal reducer at the Russian 6-m telescope. The sample consists of 15 PRGs classified as `the best candidates' in the SDSS-based Polar Ring Catalogue. The distributions of line-of-sight velocities of stellar and gaseous components have given kinematic confirmation of polar structures in 13 galaxies in the sample. We show that ionization by young stars dominates in the external parts of polar discs, while shocks have a significant contribution to gas excitation in the inner parts of polar structures. This picture was predicted earlier in a toy model implying the collision between gaseous clouds on polar orbits with the stellar disc gravitational potential well. The exception is a moderately inclined ring to the host galaxy NGC 5014: the accreted gas in the centre has already settled on the main plane and ionized by young stars, while the gas in the internal part of the ring is excited by shocks. The present study three times increases the number of polar structures with an available oxygen abundance estimation. The measured values of the gas metallicity almost do not depend on the galaxy luminosity. The radial [O/H] gradient in the considered polar rings is shallow or absent. No metal-poor gas was detected. We ruled out the scenario of the formation of polar rings due to cold accretion from cosmic filaments for the considered sample of PRGs.