Radiative feedback from quasars and the growth of massive black holes in stellar spheroids

By S. Sazonov, Jeremiah P. Ostriker, Luca Ciotti, R. Sunyaev. 2004

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We discuss the importance of feedback via photoionization and Compton heating on the co-evolution of massive black holes (MBHs) at the centre of spheroidal galaxies, and their stellar and gaseous components. We first assess the energetics of the radiative feedback from a typical quasar on the ambient interstellar medium (ISM). We then demonstrate that the observed M BH -σ relation could be established following the conversion of most of the gas of an elliptical progenitor into stars, specifically when the gas-to-stars mass ratio in the central regions has dropped to a low level ∼0.01 or less, so that gas cooling is no longer able to keep up with the radiative heating by the growing central massive black hole (MBH). A considerable amount of the remaining gas will be expelled and both MBH accretion and star formation will proceed at significantly reduced rates thereafter, in agreement with observations of present-day ellipticals. We find further support for this scenario by evolving over an equivalent Hubble time a simple, physically based toy model that additionally takes into account the mass and energy return for the spheroid evolving stellar population, a physical ingredient often neglected in similar approaches.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7c178417e849564acfeba814116d1fb3a63f31b4

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The physics of galactic winds driven by active galactic nuclei (2012, background): “…addition to radiation pressure on electrons and on dust, radiation pressure on UV lines (e.g., Murray et al. 1995; Proga et al. 2000), hydromagnetic processes (e.g., Emmering et al. 1992; Konigl & Kartje 1994), and Compton heating (e.g., Sazonov et al. 2005) may contribute to accelerating outflows.”
Stellar and Quasar Feedback in Concert: Effects on AGN Accretion, Obscuration, and Outflows (2015, background): “As discussed in Sazonov et al. (2004, 2005), this effect is nearly independent of obscuration: Compton heating is entirely dominated by photons with energies 10keV (for which we can usually safely ignore obscuration) and Compton cooling by the bolometric luminosity in lower-energy photons…”
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A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, methodology): “However, such models have made progress in estimating the duty cycles of quasars and showing that the objects left behind have characteristics similar to those observed, with quasar feedback being a critical element in reproducing these features (e.g. Sazonov et al. 2005; Kawata & Gibson 2005).”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “…and their energetic output are of vital importance when it comes to studying how the interplay between the accretion and ejection flows at small radii can affect the host galaxy on larger scales (e.g. Ferrarese & Merritt 2000; King & Pounds 2003; Sazonov et al. 2005; Ciotti, Ostriker & Proga 2009).”
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The Evolution of the MBH-σ Relation (2005, background): “…& van Albada 2001; Nipoti et al. 2003), unregulated gas accretion (Archibald et al. 2002; Kazantzidis et al. 2005), and the self-regulated growth of black holes by momentum- or pressure-driven winds (Silk & Rees 1998; King 2003; Murray et al. 2005; Di Matteo et al. 2005; Sazonov et al. 2005).”
Theoretical Challenges in Galaxy Formation (2016, background): “One dimensional and two dimensional high resolution simulations of the effect of AGN feedback (Binney & Tabor 1995; Ciotti & Ostriker 2001; Novak, Ostriker & Ciotti 2011; Sazonov et al. 2005) indicated that AGN feedback alleviates this problem.”
MOMENTUM DRIVING: WHICH PHYSICAL PROCESSES DOMINATE ACTIVE GALACTIC NUCLEUS FEEDBACK? (2010, methodology): “Sazonov et al. (2005) present a simple analytical exploration of the effects and Paper I presents a more detailed one-dimensional treatment.”
Black Holes in Galaxy Mergers: Evolution of Quasars (2005, background): “…of the remaining gas is heated to very high temperatures; e.g. Cox et al. 2005), and the hydrodynamical modeling of Ciotti & Ostriker (1997, 2001); Sazonov et al. (2005) demonstrates that residual accretion from stellar feedback and “cooling flows” is dramatically suppressed by even relatively…”
First Measurement of the Clustering Evolution of Photometrically Classified Quasars (2005, background): “An obvious explanation is a natural limit to quasar fuel reserves, or a central engine that grows to a point where it produces sufficient radiation pressure to expel its fuel source (e.g., Silk & Rees 1998; Fabian 1999; Sazonov et al. 2005; Di Matteo et al. 2005).”
Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas (2007, methodology): “In particular, Sazonov et al. (2005) provide a fitting formula for the Compton plus photoionization and line heating/cooling that we implemented into our numerical code, together with additional physics that was missing in CO97 and CO01; a very preliminary exploration of the new models can be found…”
A Log-Quadratic Relation for Predicting Supermassive Black Hole Masses from the Host Bulge Sérsic Index (2006, background): “5 level6 (Wyithe 2006b; see also E. Noyola et al. 2007, in preparation) or may curve down at low SMBH masses and up at high SMBH masses (Sazonov et al. 2005).”
Hot Accretion Flows Around Black Holes (2014, background): “Usually TC ∼ 10 7 K is adopted, as appropriate for typical spectra of quasars (Sazonov et al. 2005, Ciotti et al. 2010, Novak et al. 2011).”