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Planetary nebulae as tracers of accreted stellar populations in massive galaxies in groups and clusters

Johanna Hartke

TL;DR

Planetary nebulae (PNe) are used as spatial and kinematic tracers to probe the assembly of halo and intra-cluster/intra-group light in massive galaxies within groups and clusters up to 100 Mpc. The review connects PN diagnostics such as the PN luminosity function (PNLF) and the luminosity-specific PN number $α$ to shifts between in-situ and ex-situ stellar populations and places results in the context of integral-field spectroscopy. It discusses advances in new observing techniques (e.g., IFU surveys, BlueMUSE, PHANGS-MUSE) and updated post-AGB stellar evolution models that address tensions between observed PNLFs and theory, and outlines expected gains from future facilities and simulations. The work argues that, with co-spatial PN and stellar population measurements and improved modelling (e.g., the PICS framework), PNe will become robust tracers of low-surface-brightness halo and intracluster components.

Abstract

Planetary nebulae (PNe) are valuable spatial and kinematic tracers of nearby galaxies. In this mini-review, I focus on their role in tracing the halo and intra-cluster/intra-group light assembly in groups and clusters of galaxies within 100~Mpc and, in particular, the link between characteristic PN metrics such as the $α$-parameter and the PN luminosity function and changes from the underlying in-situ to ex-situ stellar populations. These results from nearby groups and clusters are placed into context with integral-field spectroscopic surveys of galaxies, which allow the co-spatial measurement of PN and stellar population properties. I provide an outlook on upcoming instrumentation that will provide new opportunities for the study of extragalactic PN populations. I address the challenges of reconciling observations of extragalactic PN populations with predictions from stellar evolution models and how revised late-stellar-evolution models have alleviated some of the tensions between observations and theory.

Planetary nebulae as tracers of accreted stellar populations in massive galaxies in groups and clusters

TL;DR

Planetary nebulae (PNe) are used as spatial and kinematic tracers to probe the assembly of halo and intra-cluster/intra-group light in massive galaxies within groups and clusters up to 100 Mpc. The review connects PN diagnostics such as the PN luminosity function (PNLF) and the luminosity-specific PN number to shifts between in-situ and ex-situ stellar populations and places results in the context of integral-field spectroscopy. It discusses advances in new observing techniques (e.g., IFU surveys, BlueMUSE, PHANGS-MUSE) and updated post-AGB stellar evolution models that address tensions between observed PNLFs and theory, and outlines expected gains from future facilities and simulations. The work argues that, with co-spatial PN and stellar population measurements and improved modelling (e.g., the PICS framework), PNe will become robust tracers of low-surface-brightness halo and intracluster components.

Abstract

Planetary nebulae (PNe) are valuable spatial and kinematic tracers of nearby galaxies. In this mini-review, I focus on their role in tracing the halo and intra-cluster/intra-group light assembly in groups and clusters of galaxies within 100~Mpc and, in particular, the link between characteristic PN metrics such as the -parameter and the PN luminosity function and changes from the underlying in-situ to ex-situ stellar populations. These results from nearby groups and clusters are placed into context with integral-field spectroscopic surveys of galaxies, which allow the co-spatial measurement of PN and stellar population properties. I provide an outlook on upcoming instrumentation that will provide new opportunities for the study of extragalactic PN populations. I address the challenges of reconciling observations of extragalactic PN populations with predictions from stellar evolution models and how revised late-stellar-evolution models have alleviated some of the tensions between observations and theory.

Paper Structure

This paper contains 7 sections, 4 equations.

Table of Contents

  1. Introduction
  2. Characterisation of PN populations from observations
  3. Classical PN surveys
  4. New insights from integral-field spectroscopic surveys
  5. New facilities and opportunities
  6. Modelling PN populations and insights from stellar evolution models
  7. Conclusions and outlook