Luminous quasars do not live in the most overdense regions of galaxies at <i>z</i> ∼ 4

Uchiyama, Hisakazu; Toshikawa, Jun; Kashikawa, Nobunari; Overzier, Roderik; Chiang, Yi-Kuan; Marinello, Murilo; Tanaka, Masayuki; Niino, Yuu; Ishikawa, Shinya; Onoue, Masafusa; Ichikawa, Kohei; Akiyama, Masayuki; Coupon, J.; Harikane, Yuichi; Imanishi, Masatoshi; Kodama, Tadayuki; Komiyama, Yutaka; Lee, Chien‐Hsiu; Lin, Yen-Ting; Miyazaki, Satoshi; Nagao, Tohru; Nishizawa, A. J.; Ono, Yoshiyasu; Ouchi, Masami; Wang, Shiang‐Yu

doi:10.1093/pasj/psx112

Cited by 60 publications

(31 citation statements)

References 89 publications

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“…Consequently, it was expected that we should find galaxy overdensities in the vicinity of the most luminous quasars. However, no correlation has been found between luminous quasars and protocluster regions at z ∼ 3.8 (Uchiyama et al 2018). A similar negative result has been found for millimeter source overdensities at 6 < z < 7, albeit within ALMA's small field of view (Champagne et al 2018).…”

Section: Introductionmentioning

confidence: 55%

Tracing black hole and galaxy co-evolution in the Romulus simulations

Ricarte

Tremmel

Natarajan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the link between supermassive black hole growth and the stellar mass assembly of their host galaxies in the state-of-the-art Romulus suite of simulations. The cosmological simulations Romulus25 and RomulusC employ innovative recipes for the seeding, accretion, and dynamics of black holes in the field and cluster environments respectively. We find that the black hole accretion rate traces the star formation rate among star-forming galaxies. This result holds for stellar masses between 10 8 and 10 12 solar masses, with a very weak dependence on host halo mass or redshift. The inferred relation between accretion rate and star formation rate does not appear to depend on environment, as no difference is seen in the cluster/proto-cluster volume compared to the field. A model including the star formation rate, the black hole-to-stellar mass ratio, and the cold gas fraction can explain about 70 per cent of all variations in the black hole accretion rate among star forming galaxies. Finally, bearing in mind the limited volume and resolution of these cosmological simulations, we find no evidence for a connection between black hole growth and galaxy mergers, on any timescale and at any redshift. Black holes and their galaxies assemble in tandem in these simulations, regardless of the larger-scale intergalactic environment, suggesting that black hole growth simply follows star formation on galactic scales.

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Section: Introductionmentioning

confidence: 55%

Tracing black hole and galaxy co-evolution in the Romulus simulations

Ricarte

Tremmel

Natarajan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…According to recent results, high-redshift quasars are hosted in haloes with typical masses in the range 3×10 11 −×10 13 (Di Matteo et al 2017;Tenneti et al 2018b), they do not live in the most overdense regions of the Universe (Mazzucchelli et al 2017;Uchiyama et al 2018), and they are powered by BHs with masses above a few 10 8 M up to 10 10 M .…”

Section: Initial Conditionsmentioning

confidence: 99%

High-redshift quasars and their host galaxies – I. Kinematical and dynamical properties and their tracers

Lupi

Volonteri

Decarli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Observations of high-redshift quasars provide information on the massive black holes (MBHs) powering them and the galaxies hosting them. Current observations of z 6 hosts, at sub-mm wavelengths, trace the properties of cold gas, and these are used to compare with the correlations between MBHs and galaxies characterising the z = 0 population. The relations at z = 0, however, rely on stellar-based tracers of the galaxy properties. We perform a very-high resolution cosmological zoom-in simulation of a z = 7 quasar including state-of-the-art non-equilibrium chemistry, MBH formation, growth and feedback, to assess the evolution of the galaxy host and the central MBH, and compare the results with recent ALMA observations of high-redshift quasars. We measure both the stellar-based quantities used to establish the z = 0 correlations, as well as the gas-based quantities available in z 6 observations, adopting the same assumptions and techniques used in observational studies. The high-redshift studies argued that MBHs at high redshift deviate from the local MBH-galaxy correlations. In our analysis of the single galaxy we evolve, we find that the high-redshift population sits on the same correlations as the local one, when using the same tracers used at z = 0. When using the gas-based tracers, however, MBHs appear to be over-massive. The discrepancy between local and high-redshift MBHs seems caused by the different tracers employed, and necessary assumptions, and not by an intrinsic difference. Better calibration of the tracers, higher resolution data and availability of facilities that can probe the stellar population will be crucial to assess precisely and accurately highredshift quasar hosts.

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“…Conroy & White 2013), although observations have revealed no significant evidence for luminosity dependence (e.g. Chehade et al 2016;Uchiyama et al 2018;He et al 2018). The question regarding the mass of halos hosting the most luminous QSO at…”

Section: Secondary Parameters Dependent On Qso Luminositymentioning

confidence: 99%

Revealing the impact of quasar luminosity on giant Ly α nebulae

Mackenzie

Pezzulli

Cantalupo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which were selected to be much fainter (20 < iSDSS < 23) than in previous studies of Giant Lyα Nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect H I Lyα nebulae around 100% of our target quasars, with emission extending to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations between properties of the nebulae and their host quasars, with the goal of connecting variations in the properties of the illuminating QSO to the response in nebular emission. We show that the surface brightness profiles of the nebulae are similar to those of nebulae around bright quasars, but with a lower normalization. Our targeted quasars are on average 3.7 magnitudes (≃ 30 times) fainter in UV continuum than our bright reference sample, and yet the nebulae around them are only 4.3 times fainter in mean Lyα surface brightness, measured between 20 and 50 pkpc. We find significant correlations between the surface brightness of the nebula and the luminosity of the quasar in both UV continuum and Lyα. The latter can be interpreted as evidence for a substantial contribution from unresolved inner parts of the nebulae to the narrow components seen in the Lyα lines of some of our faint quasars, possibly from the inner CGM or from the host galaxy’s ISM.

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Luminous quasars do not live in the most overdense regions of galaxies at z ∼ 4

Cited by 60 publications

References 89 publications

Tracing black hole and galaxy co-evolution in the Romulus simulations

Tracing black hole and galaxy co-evolution in the Romulus simulations

High-redshift quasars and their host galaxies – I. Kinematical and dynamical properties and their tracers

Revealing the impact of quasar luminosity on giant Ly α nebulae

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