ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O B-CelestialObject I-CelestialObject O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject B-CelestialObject I-CelestialObject O B-CelestialObject I-CelestialObject O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-URL O O O O O O O O O O O O O O O O O O O O O B-Software O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: of their central BH. It is therefore plausible that major merger events triggering the rapid growth phase of BHs could contribute to the formation of anomalously massive SMBHs. Based on hydrodynamical and cosmological simulations we thus expect the existence of observed M BH ( M ⋆ ) outliers with . Observed outliers with such large M BH are plausibly survivors of tidal stripping and it would be interesting to study their environment out to ∼1 Mpc. The positive correlation between the scatter in M BH (σ) and in [Mg/Fe](σ) indicates a strong relation between the M BH and the time-scale of the quenching process for massive galaxies. It would furthermore be interesting for future studies to investigate the relation between merger-driven rapid growth phases at high redshifts ( > 2) and anomalously high-mass SMBHs. APPENDIX A: BMG PROPERTIES In Table A1 , we list all of the relevant properties of the five BMGs and observed outliers. Additionally, we list information on some of the most notable observed M BH ( M ⋆ ) outliers. For NGC 1271 and NGC 1277, the [Mg/Fe] values are the best-fitting values derived by Martín-Navarro et al. ( 2016 ). In column 7, the ‘outlier ’ represents the lower limits of a 500 Myr time-step. Table A1. The five BMGs and their properties. Column 1 shows the BMG ID (for simulated galaxies) or name (for observations). From left to right: BH mass (column 2), stellar mass (column 3), half-mass radii for the simulated galaxies, or effective radius for observations (column 4), one-dimensional stellar velocity dispersion, which is computed from the average of the three-dimensional velocity dispersion (column 5), mass-weighted stellar age (column 6), and [Mg/Fe] abundance (column 7). Column 8 shows the redshift of the snapshot at which each galaxy crossed the a M BH / M ⋆ > 0.01 threshold. These redshifts have an uncertainty of 500 Myr. Column 9 is the distance to the nearest more massive neighbour of each BMG at = 0. The last two columns (10 and 11) show f strip and f age from equations ( 1 ) and ( 2 ), respectively. The last four rows show the observational values for NGC 1271, NGC 1277, and Mrk 1216 as determined by Walsh et al. ( 2015 , 2016 ), Ferré-Mateu et al. ( 2015 , 2017 ), and Martín-Navarro et al. ( 2016 ). In Fig. A1 , we have plotted the stellar mass density of outlier ID E and its surroundings at three different snapshots throughout the simulation. The remaining images are available at https://sites.google.com/view/vson-umbh-galaxies/homepage Figure A1. Stellar surface density distribution of BMG-ID E at three different snapshots. These images are created with the publicly available Py-SPHViewer, which uses the smoothed particle hydrodynamics interpolation scheme. The colours represent the projected density of stellar particles bound to BMG-ID E, with blue/pink corresponding to low density and yellow corresponding to high-mass density. BH particles are indicated with blue dots. The most relevant parameters of the