Invited_talk abstract details
PNe in the Magellanic Clouds and other Local Group galaxies
Abstract
A review of searches and research into planetary nebulae (PNe) within the Magellanic Clouds (MCs) and Local Group (LG) galaxies (within 1.3 Mpc of the Milky Way) over the past 5 years. Topics covered include surveys, imaging, population sizes, magnitude limits, a brief review of the science being conducted, results, instruments and telescopes being used.
We begin with the MCs, which provide an excellent laboratory in which to study extragalactic PNe. With known distances and low extinction, most PNe are bright enough to provide good spatial resolution and access to their central stars using today's modern telescopes. The astrophysical advantages of MC PNe include: a good sample size for statistical and kinematic studies, low to intermediate metallicity environments, PNe can be individually analysed and directly compared for size, shape, mass, metallicity, local environment and galactic location. With average diameters $<$4 arcsec on the sky, spectroscopy is able to cover the majority of the ionised shell, providing very accurate emission-line luminosities.
Turning our attention to the local group in general, advances over the last 5 years have seen increased research using HST imaging, SAGE-Spitzer multi-channel imaging and high-resolution ground-based spectroscopy using MOS and IFU instruments to measure an unprecedented number of parameters, including central stars, for nebula photoionisation models. Significantly, improved sensitivity on the Australia Telescope Compact Array (ATCA) has allowed the detection of radio emission from a number of bright PNe in the MCs. PNe in the MCs and M31 galaxies have become established as excellent distance calibrators for the PNLF, thanks to the consistent bright \OIII$\lambda$5007 cut-off.
We begin with the MCs, which provide an excellent laboratory in which to study extragalactic PNe. With known distances and low extinction, most PNe are bright enough to provide good spatial resolution and access to their central stars using today's modern telescopes. The astrophysical advantages of MC PNe include: a good sample size for statistical and kinematic studies, low to intermediate metallicity environments, PNe can be individually analysed and directly compared for size, shape, mass, metallicity, local environment and galactic location. With average diameters $<$4 arcsec on the sky, spectroscopy is able to cover the majority of the ionised shell, providing very accurate emission-line luminosities.
Turning our attention to the local group in general, advances over the last 5 years have seen increased research using HST imaging, SAGE-Spitzer multi-channel imaging and high-resolution ground-based spectroscopy using MOS and IFU instruments to measure an unprecedented number of parameters, including central stars, for nebula photoionisation models. Significantly, improved sensitivity on the Australia Telescope Compact Array (ATCA) has allowed the detection of radio emission from a number of bright PNe in the MCs. PNe in the MCs and M31 galaxies have become established as excellent distance calibrators for the PNLF, thanks to the consistent bright \OIII$\lambda$5007 cut-off.