📝 SummarXiv

Abstract

The spatial distribution of chemical elements in the Galactic disk provides key constraints on models of galaxy evolution. However, studies using planetary nebulae (PNe) as tracers have been historically limited by large uncertainties in their distances. To overcome the long-standing distance uncertainties, we recalibrated the H$\alpha$ surface brightness-radius relation (Frew et al. 2016) with Gaia DR3 parallaxes, deriving statistical distances for 1,200 PNe and Bayesian distances for 419 objects with reliable parallaxes. Adopting Bayesian values preferentially, we determined the O/H radial gradient for 230 disk PNe. We tested three models: a single linear gradient, a segmented fit with one break, and a segmented fit with two breaks. Although model selection is statistically inconclusive, segmented fits indicate a change in slope near the solar radius ($R \sim 8$ kpc), with a flatter or slightly positive gradient inward and a steeper negative gradient outward. This feature may reflect changes in star formation efficiency driven by the Galactic bar or the corotation resonance of the spiral arms. Comparison with other tracers - Cepheids, red giants, and open clusters - shows qualitative consistency. The two-dimensional O/H distribution in the Galactic plane supports the adopted distances and reveals modest azimuthal asymmetry, with enhanced abundances near the bar at positive longitudes, and a bimodal abundance structure between the inner and outer solar regions. Our results provide new constraints on the chemical evolution of the Milky Way, the impact of non-axisymmetric structures, and the possible existence of distinct radial abundance regimes across the Galactic disk.