The Tully-Fisher relation from SDSS-MaNGA: Physical causes of scatter and variation at different radii

• DOI: 10.48550/arxiv.2311.13251
• Publication Date: 2023-01-01
• Authors: Andrei Ristea; L. Cortese; Amelia Fraser-McK...; Barbara Catinella; Jesse van de Sande; S. M. Croom; A. M. Swinbank
• Keywords: Effective radius; Stellar mass; Tully–Fisher relation

The stellar mass Tully-Fisher relation (STFR) and its scatter encode valuable information about the processes shaping galaxy evolution across cosmic time. However, we are still missing a proper quantification of STFR slope dependence on baryonic tracer used to quantify rotational velocity, velocity measurement radius integrated properties. We present catalogue ionised gas (traced by H$\alpha$ emission) kinematic measurements for sample galaxies drawn from MaNGA Galaxy Survey, providing an ideal tool formation model calibration comparison with high-redshift studies. compute STFRs rotation at 1, 1.3 2 effective radii ($R_e$). relations both components become shallower 2$R_e$ compared 1$R_e$ 1.3$R_e$. report steeper stars in inner parts ($\leq R_e$) gas. At 2$R_e$, two consistent. When accounting covariances v/$\sigma$, shows no strong correlation with: optical morphology, star rate surface density, tidal interaction strength or accretion signatures. Our results suggest that is driven increase stellar/gas dispersional support, either external (mergers) internal (feedback) processes. No between environment found. Nearby Universe have their statistically different states dynamical equilibrium R_e$), while 2$R_{e}$ dynamically coupled.