The Progenitors and Lifetimes of Planetary Nebula

TL;DR

This study identifies two main progenitor populations for planetary nebulae in the Large Magellanic Cloud, linking their lifetimes and masses to distinct stellar evolution pathways and implications for nebula shaping mechanisms.

Contribution

It provides the first homogeneous observational evidence for two distinct progenitor populations of PNe, with specific lifetime and mass ranges, suggesting multiple formation channels.

Findings

Most PNe progenitors have lifetimes of 5-8 Gyr and masses 1.0-1.2 M$_{ ext{sun}}$.

A second progenitor population has lifetimes of 35-800 Myr and masses 2.1-8.2 M$_{ ext{sun}}$.

Average PN lifetime is approximately 26 kyr for the main population.

Abstract

Planetary Nebulae (PNe) are amongst the most spectacular objects produced by stellar evolution, but the exact identity of their progenitors has never been established for a large and homogeneous observational sample. We investigate the relationship between PNe and their stellar progenitors in the Large Magellanic Cloud (LMC) through the statistical comparison between a highly complete spectroscopic catalog of PNe and the spatially resolved age distribution of the underlying stellar populations. We find that most PN progenitors in the LMC have main-sequence lifetimes in a narrow range between 5 and 8 Gyr, which corresponds to masses between 1.2 and 1.0 M$_{\odot}$, and produce PNe that last $26^{+6}_{-7}$~kyr on average. We tentatively detect a second population of PN progenitors, with main-sequence lifetimes between 35 and 800~Myr, i.e., masses between 8.2 and 2.1 M$_{\odot}$, and average PN lifetimes of $11^{+6}_{-7}$ kyr. These two distinct and disjoint populations of progenitors strongly suggest the existence of at least two physically distinct formation channels for PNe. Our determination of PN lifetimes and progenitor masses has implications for the understanding of PNe in the context of stellar evolution models, and for the role that rotation, magnetic fields, and binarity can play in the shaping of PN morphologies.