Origin of simulation–observation discrepancies in element-pair correlation measurements

Ascertain whether the observed discrepancies between element-pair abundance correlations measured in Milky Way stellar surveys and the correlations predicted by the Ripples of Stellar Enrichment (RoSE) simulations are caused by deficiencies or missing physics in the RoSE simulations, or instead by systematic uncertainties in the observational abundance measurements and age estimates.

Background

The paper compares element-pair cross-correlations predicted by the RoSE star-by-star chemical enrichment simulations with measurements from two Milky Way stellar datasets and finds generally encouraging qualitative agreement, but with quantitative tensions for some element pairs.

The authors note that the inter-dataset scatter between independent observational surveys is substantial and can be comparable to the simulation–observation differences, raising the possibility that remaining discrepancies are due to observational systematics rather than simulation shortcomings.

This uncertainty motivates determining whether the residual differences trace missing physical processes in the simulations (e.g., additional mixing or migration physics) or instead reflect limitations in current observational abundance and age determinations.