The Halo Occupation Distribution of SDSS Quasars

Richardson, Jonathan; Zheng, Zheng; Chatterjee, Suchetana; Nagai, Daisuke; Shen, Yue

doi:10.1088/0004-637x/755/1/30

Cited by 81 publications

(187 citation statements)

References 132 publications

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“…The shape of these distributions is roughly consistent with predictions from halo occupation distribution (HOD) analyses of unobscured quasars, which find that quasar hosts have a log-normal mass distribution (e.g. Richardson et al 2012;Chatterjee et al 2013). Figure 6 also shows that this model predicts that the stellar masses of the obscured population will be higher, and that this is a driver for the difference in halo mass.…”

Section: Comparison With Observationssupporting

confidence: 80%

A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

DiPompeo

Hickox

Myers

2016

Mon. Not. R. Astron. Soc.

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Recent measurements of the dark matter halo masses of infrared-selected obscured quasars are in tension -some indicate that obscured quasars have higher halo mass compared to their unobscured counterparts, while others find no difference. The former result is inconsistent with the simplest models of quasar unification that rely solely on viewing angle, while the latter may support such models. Here, using empirical relationships between dark matter halo and supermassive black hole masses, we provide a simple evolutionary picture that naturally explains these findings and is motivated by more sophisticated merger-driven quasar fueling models. The model tracks the growth rate of haloes, with the black hole growing in spurts of quasar activity in order to "catch-up" with the M bh -M stellar -M halo relationship. The first part of the quasar phase is obscured and is followed by an unobscured phase. Depending on the luminosity limit of the sample, driven by observational selection effects, a difference in halo masses may or may not be significant. For high luminosity samples, the difference can be large (a few to 10 times higher masses in obscured quasars), while for lower luminosity samples the halo mass difference is very small, much smaller than current observational constraints. Such a simple model provides a qualitative explanation for the higher mass haloes of obscured quasars, as well as rough quantitative agreement with seemingly disparate results.

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Section: Comparison With Observationssupporting

confidence: 80%

A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

DiPompeo

Hickox

Myers

2016

Mon. Not. R. Astron. Soc.

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“…Hopkins et al (2007) argued instead that strong quasar clustering on small scales is simply indicative of quasars occupying group-scale or "merger-prone" environments. More recently, the small-scale clustering of quasars has been modeled using the "onehalo" term in the HOD (e.g., Kayo & Oguri 2012;Richardson et al 2012Richardson et al , 2013). As we argue in §4.1, this "excess" is, in fact, probably close-to-consistent with the amplitude of clustering found for some types of galaxies on small scales.…”

Section: Redshift Dependence Ofwpmentioning

confidence: 99%

Clustering on very small scales from a large sample of confirmed quasar pairs: does quasar clustering track from Mpc to kpc scales?

Eftekharzadeh

Myers

Djorgovski

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the most precise estimate to date of the clustering of quasars on very small scales, based on a sample of 47 binary quasars with magnitudes of g < 20.85 and proper transverse separations of ∼ 25 h −1 kpc. Our sample of binary quasars, which is about 6 times larger than any previous spectroscopically confirmed sample on these scales, is targeted using a Kernel Density Estimation technique (KDE) applied to Sloan Digital Sky Survey (SDSS) imaging over most of the SDSS area. Our sample is "complete" in that all of the KDE target pairs with 17.0 R 36.2 h −1 kpc in our area of interest have been spectroscopically confirmed from a combination of previous surveys and our own long-slit observational campaign. We catalogue 230 candidate quasar pairs with angular separations of < 8 ′′ , from which our binary quasars were identified. We determine the projected correlation function of quasars (W p ) in four bins of proper transverse scale over the range 17.0 R 36.2 h −1 kpc. The implied small-scale quasar clustering amplitude from the projected correlation function, integrated across our entire redshift range, is A = 24.1±3.6 at ∼ 26.6 h −1 kpc. Our sample is the first spectroscopically confirmed sample of quasar pairs that is sufficiently large to study how quasar clustering evolves with redshift at ∼ 25 h −1 kpc. We find that empirical descriptions of how quasar clustering evolves with redshift at ∼ 25 h −1 Mpc also adequately describe the evolution of quasar clustering at ∼ 25 h −1 kpc.

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“…This is inferred from halo occupation distribution (HOD) modeling of the quasar-galaxy two-point cross-correlation and when normalized, gives the probability distribution of quasar host halo masses. Different quasar HOD models are often known to be degenerate with clustering measurements (Richardson et al 2012;Kayo & Oguri 2012;Chatterjee et al 2013), and the uncertainties on the bestfit occupation functions are often large. Nevertheless, they provide a useful check of our high-redshift feedback results, and so we utilize the quasar M halo distribution inferred in Shen et al (2013) using both a 5-parameter and 6-parameter HOD model (see their Figures 14 e and f).…”

Section: Separating Quasar Feedbackmentioning

confidence: 99%

DETECTION OF QUASAR FEEDBACK FROM THE THERMAL SUNYAEV–ZEL’DOVICH EFFECT INPLANCK

Ruan

McQuinn

Anderson

2015

ApJ

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Poorly understood feedback processes associated with highly-luminous black hole accretion in quasars may dramatically affect the properties of their host galaxies. We search for the effect of quasar feedback on surrounding gas using Planck maps of the thermal Sunyaev-Zel'dovich effect (tSZ). By stacking tSZ Compton-y maps centered on the locations of 26,686 spectroscopic quasars from the Sloan Digital Sky Survey, we detect a strong but unresolved tSZ Compton-y signal at >5σ significance that likely originates from a combination of virialized halo atmosphere gas and quasar feedback effects. We show that the feedback contribution to our detected quasar tSZ signal is likely to dominate over virialized halo gas by isolating the feedback tSZ component for high-and low-redshift quasars. We find that this quasar tSZ signal also scales with black hole mass and bolometric luminosity, all consistent with general expectations of quasar feedback. We estimate the mean angularly-integrated Compton-y of quasars at z 1.5 to be 3.5×10 −6 Mpc 2 , corresponding to mean total thermal energies in feedback and virialized halo gas of 1.1 (±0.2) × 10 62 erg, and discuss the implications for quasar feedback. If confirmed, the large total thermal feedback energetics we estimate of 5% (±1% statistical uncertainty) of the black hole mass will have important implications for the effects of quasar feedback on the host galaxy, as well as the surrounding intergalactic medium.

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The Halo Occupation Distribution of SDSS Quasars

Cited by 81 publications

References 132 publications

A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

A unifying evolutionary framework for infrared-selected obscured and unobscured quasar host haloes

Clustering on very small scales from a large sample of confirmed quasar pairs: does quasar clustering track from Mpc to kpc scales?

DETECTION OF QUASAR FEEDBACK FROM THE THERMAL SUNYAEV–ZEL’DOVICH EFFECT INPLANCK

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