PROBING THE $\mathcal M_{\rm BH}$-σ_*RELATION IN THE NON-LOCAL UNIVERSE USING RED QSOs

Abstract

We describe a method to measure the M BH -σ * relation in the non-local universe using dustobscured QSOs. We present results from a pilot sample of nine 2MASS red QSOs with redshifts 0.14 < z < 0.37. We find that there is an offset (0.8 dex, on average) between the position of our objects and the local relation for AGN, in the sense that the majority of red QSO hosts have lower velocity dispersions and/or more massive BHs than local galaxies. These results are in agreement with recent studies of AGN at similar and higher redshifts. This could indicate an unusually rapid growth in the host galaxies since z ∼ 0.2, if these objects were to land in the local relation at present time. However, the z > 0.1 AGN (including our sample and those of previous studies) have significantly higher M BH than those of local AGN, so a direct comparison is not straightforward. Further, using several samples of local and higher-z AGN, we find a striking trend of an increasing offset with respect to the local M BH -σ * relation as a function of AGN luminosity, with virtually all objects with log(L 5100 /erg s −1 ) > 43.6 falling above the relation. Given the relatively small number of AGN at z > 0.1 for which there are direct measurements of stellar velocity dispersions, it is impossible at present to determine whether there truly is evolution in M BH -σ * with redshift. Larger, carefully selected samples of AGN are necessary to disentangle the dependence of M BH -σ * on mass, luminosity, accretion rates, and redshift.supermassive BHs and galaxies co-evolve.The most important observational tools for studying the co-evolution of BHs and galaxies are the empirical scaling relations between BH mass and global galaxy properties, such as the M BH -σ * relation (Ferrarese and Merritt 2000; Gebhardt et al. 2000a), a particularly tight relation between BH mass, M BH , and the central, stellar velocity dispersion, σ * . The M BHσ * relation suggests a causal connection between the BH and the bulge (although see e.g., Jahnke and Macciò 2011, for a counter argument), and is believed to hold clues to understanding the galaxy formation process. By studying how the BH mass relates to the mass of the bulge (as measured by σ * ), the galaxy evolution process can be examined across different redshift ranges and for different galaxy types.Active galactic nuclei (AGN) have become in-

Stronger Constraints on the Evolution of the MBH− Relation up to z ∼ 0.6

“…They pointed out that the limited dynamic range and higher average AGN luminosities in Woo et al (2006Woo et al ( , 2008 are responsible for the observed offset compared to local objects with considerably lower average luminosities. This trend, which is observed here and in other studies of the non-local M BH −σ * relation (Shen et al 2008;Canalizo et al 2012;Hiner et al 2012;Park et al 2015;Shen et al 2015), makes it clear that significant statistical biases are at work in luminosity threshold samples. However, as we have shown here, these biases can be overcome by probing lower luminosities and lower BH masses at higher redshifts.…”

“…This is problematic since it means that bulges must undergo significant stellar mass assembly in a relatively short amount of time, and the possible mechanisms for doing so without significantly growing their BHs remain largely speculative. Similar studies by Canalizo et al (2012) using dust-reddened 2MASS quasi-stellar objects (QSOs) at 0.14 < z < 0.37, and Hiner et al (2012) using poststarburst QSOs at z ∼ 0.3, found a similar significant positive offset from the local relation, which further exacerbated the problem.…”

The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies

“…Marconi & Hunt 2003;Häring & Rix 2004). More recently, several groups (Treu et al 2004(Treu et al , 2007Walter et al 2004;Peng et al 2006a,b;Shields et al 2006;Woo et al 2006Woo et al , 2008Ho 2007;Decarli et al 2010;Merloni et al 2010;Wang et al 2010;Bennert et al 2011;Canalizo et al 2012;Targett et al 2012;Bongiorno et al 2014) have attempted to sample this relation beyond the local Universe showing that there are indications for a possible evolution with redshift. In particular these works suggested a parameterisation of the ratio Γ = M BH /M gal as a function of redshift, Γ ∝ (1 + z) β .…”

THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: NO EVIDENCE FOR EVOLUTION IN THE ${{M}_{\bullet }}-{{\sigma }_{*}}$ RELATION TO $z\sim 1$

“…Given the importance of these BH scaling relations in our understanding of galaxy formation and evolution, there have been extensive observational efforts in the past decade both to refine the measurements of the local relations (e.g., Ferrarese & Merritt 2000;Gebhardt et al 2000a;Graham et al 2001Graham et al , 2011Tremaine et al 2002;Marconi & Hunt 2003;Häring and Rix 2004;Aller & Richstone 2007;Bentz et al 2009;Gültekin et al 2009;Kormendy & Ho 2013;McConnell & Ma 2013, and references therein) and to probe their possible redshift evolution (e.g., Treu et al 2004Treu et al , 2007Peng et al 2006aPeng et al , 2006bWoo et al 2006Woo et al , 2008Salviander et al 2007;Shen et al 2008b;Jahnke et al 2009;McLeod & Bechtold 2009;Bennert et al 2010;Decarli et al 2010;Merloni et al 2010;Cisternas et al 2011;Canalizo et al 2012;Hiner et al 2012;Targett et al 2012;Salviander & Shields 2013;Bongiorno et al 2014;Matsuoka et al 2014). Given the small angular size of the sphere of influence of the BH, so far all measurements beyond the local universe are based on broad-line quasar samples, where the BH mass can be estimated using the properties of the broad lines, instead of spatially resolved gas or stellar kinematics.…”