The Illustris Simulation: Supermassive Black Hole − Galaxy Connection Beyond the Bulge

Abstract

We study the spiral arm morphology of a sample of the local spiral galaxies in the Illustris simulation and explore the supermassive black hole−galaxy connection beyond the bulge (e.g., spiral arm pitch angle, total stellar mass, dark matter mass, and total halo mass), finding good agreement with other theoretical studies and observational constraints. It is important to study the properties of supermassive black holes and their host galaxies through both observations and simulations and compare their results in order to understand their physics and formative histories. We find that Illustris prediction for supermassive black hole mass relative to pitch angle is in rather good agreement with observations and that barred and non-barred galaxies follow similar scaling relations. Our work shows that Illustris presents very tight correlations between supermassive black hole mass and large-scale properties of the host galaxy, not only for early-type galaxies but also low-mass, blue and star-forming galaxies. These tight relations beyond the bulge suggest that halo properties determine those of a disc galaxy and its supermassive black hole.

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (vmax, MoM)–(σ0, MBH, ϕ) Relations

“…which is consistent with the slope from Equation (11) at the level of 0.17 σ. This slope for spiral galaxies is notably steeper than reported in past studies (e.g., Haehnelt et al 1998;Silk & Rees 1998;Ferrarese 2002;Baes et al 2003;Bandara et al 2009;Booth & Schaye 2010;Bogdán & Goulding 2015;Mutlu-Pakdil et al 2018).…”

“…The M * ,tot -M DM relation is traditionally fit with a double power law, exhibiting a steep low-mass slope and a shallow high-mass slope (Yang et al 2012;Moster 29 From inspection of Figures 7 and 8 from Mutlu-Pakdil et al (2018), we point out an apparent bend in the respective scaling relations with black hole mass. There is a noticeable dichotomy between low-and high-mass black holes, such that it warrants a steeper slope for spiral galaxies hosting low-mass black holes and a shallow slope for early-type galaxies hosting high-mass black holes, rather than their single regression fit to the combined sample.…”

“…The ability of φ to predict dark matter halo masses in late-type galaxies with such a small slope and level of scatter is remarkable given that no other parameter in this paper is as simple to measure or has such minimal observational requirements. Mutlu-Pakdil et al (2018) also presented an M DM -φ relation by measuring the pitch angles of spiral galaxies produced from the Illustris simulation (Vogelsberger et al 2014). They found from 95 simulated spiral galaxies that M DM ∝ (−0.029 ± 0.001)|φ|.…”

Black Hole Mass Scaling Relations for Spiral Galaxies. II. MBH–M*,tot and MBH–M*,disk

“…To date, its limited publication history has not been without dramatic disagreement. The very existence of an M BH -M * ,tot relation (or its proxy relation with bulge luminosity) has improved infinitely from a state of nonexistence (Kormendy & Gebhardt 2001) to existing, but not being as strong a tracer of supermassive black hole mass as the bulge (Beifiori et al 2012;, to being elevated to a stature equal with that of the bulge arXiv:1810.04888v3 [astro-ph.GA] 11 Mar 2019 (Läsker et al 2014;Mutlu-Pakdil et al 2018). The latter claim would bring the M BH -M * ,tot relation in line with suggestions that SMBH growth is a derivative of the overall potential of its host galaxy (Ferrarese 2002;Volonteri et al 2011).…”

Outflows in the Disks of Active Galaxies

“…For each luminosity bin, the input quantities for the model, i.e., the total mass M (or the circular velocity V c ) and the gas mass M gas of the host galaxy, are related to L AGN through available average scaling relations. The total mass M, we adopt the central value of the relation log(M BH /M ) = (1.55 ± 0.02) log(M/M ) -(11.26 ± 0.20) found from analysis of the Illustris N-body simulations by Mutlu-Pakdil et al (2018) such a relation is consistent with a wide set of observational data (see references in the above paper). An average M − L AGN relation is then derived after converting the black hole mass in bolometric luminosity assuming Eddington emission; assuming an Eddington ratio peaked at 0.3 (as indicated by some observations, see, e.g., Kauffmann & Heckman 2009;Shankar, Weinberg, Miralda-Escudé 2013) does not change appreciably our results.…”