A New Population of Planetary Nebulae Discovered in the Large Magellanic Cloud (III): The Luminosity Function

TL;DR

This study presents an extensive analysis of the Large Magellanic Cloud's planetary nebula luminosity function, providing a new distance estimate and insights into its shape, metallicity effects, and comparison with other galaxies.

Contribution

It offers the first detailed shape analysis of the LMC PNLF over a 10 magnitude range, including a new distance measurement and comparison with other galaxy samples.

Findings

The bright cutoff (M*) of the PNLF is estimated at 18.46 distance modulus.

The shape of the PNLF is now characterized in greater detail due to increased sample size.

Comparison reveals effects of metallicity on the [OIII]5007 line fluxes.

Abstract

Our previous identification and spectroscopic confirmation of 431 faint, new planetary nebulae in the central 25 deg^2 region of the LMC permits us to now examine the shape of the LMC Planetary Nebula Luminosity Function (PNLF) through an unprecedented 10 magnitude range. The majority of our newly discovered and previously known PNe were observed using the 2dF, multi-object fibre spectroscopy system on the 3.9-m Anglo-Australian Telescope and the FLAMES multi-object spectrograph on the 8-m VLT. We present reliable [OIII]5007 and H-beta flux estimates based on calibrations to well established PN fluxes from previous surveys and spectroscopic standard stars. The bright cutoff (M*) of the PNLF is found by fitting a truncated exponential curve to the bright end of the PNLF over a 3.4 magnitude range. This cutoff is used to estimate a new distance modulus of 18.46 to the LMC, in close agreement with previous PNLF studies and the best estimates by other indicators. The bright end cutoff is robust to small samples of bright PNe since significantly increased PN samples do not change this fiducial. We then fit a truncated exponential curve directly to the bright end of the function over a 6 magnitude range and test the curve's ability to indicate the position of M*. Because of the significant increase in the number of LMC PN, the shape of the PNLF is now examined in greater detail than has previously been possible. Through cumulative functions, the new LMC PNLF is compared to those from the SMC and a new deep local Galactic sample revealing the effects of incompleteness. The new [OIII]5007 LMC PNLF is then compared to our new H-beta LMC PNLF using calibrated and measured fluxes for the same objects, revealing the effects of metallicity on the [OIII]5007 line.