The survey of planetary nebulae in Andromeda (M 31) V. Chemical enrichment of the thin and thicker discs of Andromeda. Oxygen to argon abundance ratios for planetary nebulae and H II regions

Abstract

We use oxygen and argon abundances for planetary nebulae (PNe) with low internal extinction (progenitor ages of (>4.5 Gyr) and high extinction (progenitor ages <2.5 Gyr), as well as those of the H II regions, to constrain the chemical enrichment and star formation efficiency in the thin and thicker discs of M31. The argon element is produced in larger fraction by Type Ia supernovae (SNe) than oxygen. We find that the mean log(O/Ar) values of PNe as a function of their argon abundances, 12 + log(Ar/H), trace the inter-stellar matter (ISM) conditions at the time of birth of the M 31 disc PN progenitors. Thus the chemical enrichment and star formation efficiency information encoded in the [alpha/Fe] vs. [Fe/H] distribution of stars is also imprinted in the oxygen-to-argon abundance ratio log(O/Ar) vs. argon abundance for the nebular emissions of the different stellar evolution phases. We propose to use the log(O/Ar) vs. (12 + log(Ar/H)) distribution of PNe with different ages to constrain the star-formation histories of the parent stellar populations in the thin and thicker M31 discs. For the inner M31 disc (R_{GC} < 14 kpc), the chemical evolution model that reproduces the mean log(O/Ar) values as function of argon abundance for the high- and low-extinction PNe requires a second infall of metal poorer gas during a gas-rich (wet) satellite merger. In M31, the thin disc is younger and less radially extended, formed stars at a higher star formation efficiency, and had a faster chemical enrichment timescale than the more extended, thicker disc. Both the thin and thicker disc in M31 reach similar high argon abundances ( 12 + log(Ar/H) ) ~ 6.7. The chemical and structural properties of the thin/thicker discs in M31 are thus remarkably different from those determined for the Milky Way thin and thick discs.

13 pages, 12 figures. Accepted for publication on 16.07.2022 in Section 4. Extragalactic astronomy of Astronomy and Astrophysics

References in corpus (17)

• The KMOS^3D Survey: design, first results, and the evolution of galaxy kinematics from 0.7<z<2.7
• Keck HIRES Spectroscopy of Extragalactic HII Regions: C and O Abundances from Recombination Lines
• Stellar Absorption Line Analysis of Local Star-Forming Galaxies: The Relation Between Stellar Mass, Metallicity, Dust Attenuation and Star Formation Rate
• The AMBRE Project: chemical evolution models for the Milky Way thick and thin discs
• The Radical Consequences of Realistic Satellite Orbits for the Heating and Implied Merger Histories of Galactic Disks
• APOGEE DR16: a multi-zone chemical evolution model for the Galactic disc based on MCMC methods
• A clear age-velocity dispersion correlation in Andromeda's stellar disk
• The Nature and Origin of Substructure in the Outskirts of M31 -- II. Detailed Star Formation Histories
• Lick Indices in the Thin and Thick Disks of Edge-On Disk Galaxies
• Oxygen enrichment in carbon-rich planetary nebulae
• An Ultraviolet Study of Star-Forming Regions in M31
• The Planetary Nebula Spectrograph survey of S0 galaxy kinematics. Data and Overview
• Chemical abundances in Galactic planetary nebulae with Spitzer spectra
• The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields
• The kinematics of local thick discs do not support an accretion origin
• An [$\alpha$/Fe]-enhanced thick disk in a Milky Way Analogue
• Gas fractions and depletion times in galaxies with different degrees of interaction

Cited by in corpus (1)

• The survey of planetary nebulae in Andromeda (M31) VI. Kinematics of M31 inner-halo substructures and comparison with major-merger simulation predictions