Mass–Velocity Dispersion Relation in MaNGA Brightest Cluster Galaxies

We investigate a kinematic scaling relation between the baryonic mass and flat velocity dispersion, i.e. mass-velocity dispersion (MVDR), from brightest cluster galaxies (BCGs) to galaxy clusters. In our studies, of BCGs is mainly estimated by photometry. The profiles are explored with integrated field unit (IFU) Mapping Nearby Galaxies at Apache Point Observatory (MaNGA). For first time, we reveal two significant results 54 MaNGA BCGs: (1) profiles; (2) tight empirical on BCG-cluster scale together samples, i.e., MVDR, $\log(M_\mathrm{bar}/M_\odot)=4.1^{+0.1}_{-0.1}\log(\sigma_{\mathrm{los}}/\mathrm{km}\,\mathrm{s}^{-1})+1.6^{+0.3}_{-0.3}$, tiny lognormal intrinsic scatter $10^{+2}_{-1}\%$. This slope identical acceleration in clusters, which reminiscent spiral galaxies, albeit larger characteristic scale. residuals MVDR represent Gaussian distribution, displaying no correlations four properties: mass, length, surface density, redshift. Notably, provides strict test, disfavors general prediction three dark matter model.