Origin of the Metallicity Distribution in the Thick Disc

TL;DR

This study uses cosmological simulations to explore how metallicity and kinematic gradients in thick galactic discs evolve with height and radius, revealing that feedback strength influences these gradients and that in-situ star formation shapes the metallicity distribution.

Contribution

It demonstrates how feedback processes affect metallicity gradients and provides a detailed explanation for the origin of the metallicity distribution in thick discs, aligning simulations with Milky Way observations.

Findings

Radial metallicity gradients flatten with height above the disc plane.

Stronger feedback can invert radial metallicity gradients at high altitudes.

Vertical metallicity gradients show no clear correlation with galactocentric radius.

Abstract

Aims. Using a suite of cosmological chemodynamical disc galaxy simulations, we assess how (a) radial metallicity gradients evolve with scaleheight; (b) the vertical metallicity gradients change through the thick disc; and (c) the vertical gradient of the stellar rotation velocity varies through the disc. We compare with the Milky Way to search for analogous trends. Methods. We analyse five simulated spiral galaxies with masses comparable to the Milky Way. The simulations span a range of star formation and energy feedback strengths and prescriptions, particle- and grid-based hydrodynamical implementations, as well as initial conditions/assembly history. Results. Consistently, we find that the steeper, negative, radial metallicity gradients seen in the mid-plane flatten with increasing height away from the plane. In simulations with stronger (and/or more spatially-extended) feedback, the negative radial gradients invert, becoming positive for heights in excess of 1 kpc. Such behaviour is consistent with that inferred from recent observations. Our measurements of the vertical metallicity gradients show no clear correlation with galactocentric radius, and are in good agreement with those observed in the Milky Way's thick disc (locally). Conclusions. Simulations employing stronger/more extended feedback prescriptions possess radial and vertical metallicity and kinematic gradients more in line with recent observations. The inverted, positive, radial metallicity gradients seen in the simulated thick stellar discs originate from a population of younger, more metal-rich, stars formed in-situ, superimposed upon a background population of older migrators from the inner disc; the contrast provided by the former increases radially, due to the inside-out growth of the disc. A similar behaviour may be responsible for the same flattening seen in the radial gradients with scaleheight in the Milky Way.