📝 SummarXiv

Abstract

Distance measurements using the planetary nebula luminosity function (PNLF) rely on the bright-end power-law cut-off magnitude ($M^*$), which is defined by a number of the [OIII]$\lambda5007$-brightest planetary nebulae (PNe). In early-type galaxies (ETGs), the formation of these PNe is enigmatic; the population is typically too old to form the expected $M^*$ PNe from single star evolution. We aim to give a solution to this problem. We selected five ETGs with known MUSE-PNLF distances. The MUSE instrument allows us to calculate the PNLF and consistently investigate the underlying stellar populations. Using stellar population synthesis, we derive the population age, star formation history, metallicity, and alpha abundance. We compare these parameters to the PNLF variables: $M^*$ and luminosity-specific PN number at the top 0.5 mag of the PNLF ($\alpha_{0.5}$). We also compare our results with PNe In Cosmological Simulations (PICS) model applied to Magneticum Pathfinder analogue galaxies. The average mass-weighted ages and metallicities of our observations are typically old ($9 <\mathrm{Age}< 13.5$ Gyr) and rather metal-rich ($-0.4 <\mathrm{[M/H]}< +0.2$). We find $M^*$ to be independent of age and metallicity in these ages and metallicity intervals. We discover a positive correlation between $\alpha_{0.5}$ values and the mass fraction of stellar population ages of 2--10 Gyr, implying that most of the PNe originate from stars with intermediate ages. Similar trends are also found in the PICS analogue galaxies. We show that the presence of at least $\sim 2\%$ of stellar mass younger than 10 Gyr is, in principle, sufficient to form the $M^*$ PNe in ETGs. We also present observing requirements for an ideal PNLF distance determination in ETGs.