This dataset and accompanying analysis examine how stellar population gradients vary across galaxy dynamical regimes using spatially resolved spectroscopy from the MaNGA DR17 survey. We analyse a sample of ~1900 galaxies with measured stellar kinematics and stellar population properties, focusing on the relationship between galaxy dynamical support (rotation versus dispersion) and radial gradients in stellar age and metallicity. Galaxies are classified using the ratio of ordered to random motion (v/σ), with rotation-dominated systems defined as v/σ > 1 and dispersion-dominated systems as v/σ < 1. Stellar population gradients are measured in units of dex per effective radius (dex / Rₑ), using both mass-weighted and light-weighted estimates. Key Findings Rotation-dominated galaxies exhibit systematically steeper stellar age gradients compared to dispersion-dominated systems Similar trends are observed in metallicity gradients, particularly in mass-weighted measurements These relationships persist after controlling for stellar mass using partial correlation analysis Matched-pair analysis confirms that the observed differences are not driven by mass or redshift selection effects Methods Overview Data source: MaNGA DR17 with FIREFLY stellar population outputs and NSA stellar masses Kinematic classification based on v/σ (vₒverₛigma) Gradient definition: linear slope of log (age) or metallicity versus radius normalised by effective radius Statistical methods: Median comparisons Kolmogorov–Smirnov tests Cohen’s d effect sizes Spearman and mass-controlled partial correlations Matched-pair construction with tight tolerances: Δlog (M*) ≤ 0. 015 dex Δz ≤ 0. 0010 Δ (v/σ) ≤ 0. 10 Files Included chiᵥ1ₛummary. json — Summary statistics for age gradients metallicityₛummary. json — Summary statistics for metallicity gradients mangaₜaugradientₛummary. csv — Full gradient dataset mangaₜaugradientₚartialcorrₘass. csv — Mass-controlled correlation results Reproducibility All results are derived using standard scientific Python libraries (NumPy, SciPy, Pandas). The analysis pipeline is fully reproducible using the provided data files and documented parameter thresholds. Scope and Use This dataset is intended for: Studies of galaxy formation and evolution Investigations of kinematic–stellar population coupling Benchmarking statistical methods on IFU survey data Comparative analysis with simulations and alternative surveys Notes This work focuses on empirical relationships and does not assume a specific physical model. The results provide constraints on how galaxy dynamical structure relates to internal stellar population distributions.
Lachlan McGill (Fri,) studied this question.