Ionization of the diffuse gas in galaxies: Hot low-mass evolved stars at work -- proceedings IAUS284

TL;DR

This study models the ionization of diffuse gas in galaxy NGC 891, highlighting the roles of OB stars and HOLMES, and finds that metallicity and N/O ratios vary with distance from the galactic plane.

Contribution

It introduces a detailed photoionization model combining OB stars and HOLMES to explain ionization patterns in galaxy halos, emphasizing metallicity effects.

Findings

Electron density decreases with height above the galactic plane.

Models suggest HOLMES dominate ionization at higher altitudes with near-solar metallicity.

N/O ratio increases with distance from the galactic plane.

Abstract

We revisit the question of the ionization of the diffuse medium in late type galaxies, by studying NGC 891. The most important challenge for the models considered so far was the observed increase of [OIII]/Hb, [OII]/Hb, and [NII]/Ha with increasing distance to the galactic plane. We propose a scenario based on the expected population of massive OB stars and hot low-mass evolved stars (HOLMES) in this galaxy to explain this observational fact. In the framework of this scenario we construct a finely meshed grid of photoionization models. For each value of the galactic latitude z we look for the models which simultaneously fit the observed values of the [OIII]/Hb, [OII]/Hb, and [NII]/Ha ratios. For each value of z we find a range of solutions which depends on the value of the oxygen abundance. The models which fit the observations indicate a systematic decrease of the electron density with increasing z. They become dominated by the HOLMES with increasing z only when restricting to solar oxygen abundance models, which argues that the metallicity above the galactic plane should be close to solar. They also indicate that N/O increases with increasing z.