On The Role of Supermassive Black Holes in Quenching Star Formation in Local Central Galaxies. (arXiv:1908.04813v1 [astro-ph.GA])

<a href="http://arxiv.org/find/astro-ph/1/au:+Arora_N/0/1/0/all/0/1">Nikhil Arora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_M/0/1/0/all/0/1">Matteo Fossati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fontanot_F/0/1/0/all/0/1">Fabio Fontanot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirschmann_M/0/1/0/all/0/1">Michaela Hirschmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilman_D/0/1/0/all/0/1">David J. Wilman</a>

In this work, we analyze the role of AGN feedback in quenching star formation

for massive, central galaxies in the local Universe. In particular, we compare

the prediction of two semi-analytic models (L-GALAXIES and SAGE) featuring

different schemes for AGN feedback, with the SDSS DR7 taking advantage of a

novel technique for identifying central galaxies in an observational dataset.

This enables us to study the correlation between the model passive fractions,

which is predicted to be suppressed by feedback from an AGN, and the observed

passive fractions in an observationally motivated parameter space. While the

passive fractions for observed central galaxies show a good correlation with

stellar mass and bulge mass, passive fractions in L-GALAXIES correlate with the

halo and black hole mass. For SAGE, the passive fraction correlate with the

bulge mass as well. Among the two models, SAGE has a smaller scatter in the

black hole – bulge mass (M_BH – M_Bulge) relation and a slope that agrees

better with the most recent observations at z sim 0. Despite the more

realistic prescription of radio mode feedback in SAGE, there are still tensions

left with the observed passive fractions and the distribution of quenched

galaxies. These tensions may be due to the treatment of galaxies living in

non-resolved substructures and the resulting higher merger rates that could

bring cold gas which is available for star formation.

In this work, we analyze the role of AGN feedback in quenching star formation

for massive, central galaxies in the local Universe. In particular, we compare

the prediction of two semi-analytic models (L-GALAXIES and SAGE) featuring

different schemes for AGN feedback, with the SDSS DR7 taking advantage of a

novel technique for identifying central galaxies in an observational dataset.

This enables us to study the correlation between the model passive fractions,

which is predicted to be suppressed by feedback from an AGN, and the observed

passive fractions in an observationally motivated parameter space. While the

passive fractions for observed central galaxies show a good correlation with

stellar mass and bulge mass, passive fractions in L-GALAXIES correlate with the

halo and black hole mass. For SAGE, the passive fraction correlate with the

bulge mass as well. Among the two models, SAGE has a smaller scatter in the

black hole – bulge mass (M_BH – M_Bulge) relation and a slope that agrees

better with the most recent observations at z sim 0. Despite the more

realistic prescription of radio mode feedback in SAGE, there are still tensions

left with the observed passive fractions and the distribution of quenched

galaxies. These tensions may be due to the treatment of galaxies living in

non-resolved substructures and the resulting higher merger rates that could

bring cold gas which is available for star formation.

http://arxiv.org/icons/sfx.gif