# Self-consistent predictions for LIER-like emission lines from post-AGB stars

## TL;DR

This paper presents self-consistent models showing that post-AGB stars can produce LIER-like emission lines in early type galaxies, matching observations and explaining UV-excess phenomena.

## Contribution

It introduces the first predictive models linking post-AGB stars to LIER emission, incorporating stellar evolution and photoionization processes.

## Key findings

- Post-AGB stars can reproduce observed LIER emission line ratios.
- Line strengths are insensitive to post-AGB timescale variations.
- Models can explain UV colors and UV-excess in old ETGs.

## Abstract

Early type galaxies (ETGs) frequently show emission from warm ionized gas. These Low Ionization Emission Regions (LIERs) were originally attributed to a central, low-luminosity active galactic nuclei. However, the recent discovery of spatially-extended LIER emission suggests ionization by both a central source and an extended component that follows a stellar-like radial distribution. For passively-evolving galaxies with old stellar populations, hot post-Asymptotic Giant Branch (AGB) stars are the only viable extended source of ionizing photons. In this work, we present the first prediction of LIER-like emission from post-AGB stars that is based on fully self-consistent stellar evolution and photoionization models. We show that models where post-AGB stars are the dominant source of ionizing photons reproduce the nebular emission signatures observed in ETGs, including LIER-like emission line ratios in standard optical diagnostic diagrams and H$\alpha$ equivalent widths of order 0.1-3 angstroms. We test the sensitivity of LIER-like emission to the details of post-AGB models, including the mass loss efficiency and convective mixing efficiency, and show that line strengths are relatively insensitive to post-AGB timescale variations. Finally, we examine the UV-optical colors of the models and the stellar populations responsible for the UV-excess observed in some ETGs. We find that allowing as little as 3% of the HB population to be uniformly distributed to very hot temperatures (30,000 K) produces realistic UV colors for old, quiescent ETGs.