http://arxiv.org/abs/2305.03762
From a purely photometric perspective galaxies are generally decomposed into a bulge+disc system, with bulges being dispersion-dominated and discs rotationally-supported. However, recent observations have demonstrated that such framework oversimplifies complexity, especially if one considers galaxy kinematic.To address this issue we introduced with the GPU-based code \textsc{bang} a novel approach that employs analytical potential-density pairs as galactic components, allowing for a computationally fast, still reliable fit of the morphological and kinematical properties of galaxies. Here we apply \textsc{bang} to the SDSS-MaNGA survey, estimating key parameters such as mass, radial extensions, dynamics, for both bulges and discs of +10,000 objects. We test our methodology against a smaller subsample of galaxies independently analysed with an orbit-based algorithm, finding agreement in the recovered total stellar mass. We also manage to reproduce well-established scaling relations, demonstrating how a proper dynamical modelling can result in tighter correlations and provide corrections to standard approaches. Finally, we propose a more general way of decomposing galaxies into “hot” and “cold” components, showing a correlation with orbit-based approaches and visually determined morphological type. Unexpected tails in the “hot-to-total” mass-ratio distribution are present for galaxies of all morphologies, possibly due to visual morphology misclassifications.
F. Rigamonti, M. Dotti, S. Covino, et. al.
Tue, 9 May 23
9/88
Comments: 13 pages, 10 figures