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Title: On the small-scale clustering of quasars: constraints from the MassiveBlack II simulation

Abstract

Here, we explore recent high-precision measurements of small-scale quasar clustering (at z ~ 0.5–2 on scales of |$${\sim }25~\mathrm{kpc}\, h^{-1}$$|) from the SDSS in the context of the MassiveBlack II (MBII) cosmological hydrodynamic simulation and conditional luminosity function (CLF) modelling. At these high luminosities (g < 20.85 quasars), the MBII simulation volume (|$$100~\mathrm{cMpc}\, h^{-1}$$| comoving boxsize) has only three quasar pairs at distances of 1–4 Mpc. The black hole masses for the pairs range between |$$M_{\rm bh}\sim 1{\, \rm and\, }3\times 10^{9}~\mathrm{M}_{\odot }\, h^{-1}$$| and the quasar hosts are haloes of |$$M_{\rm h}\sim 1\hbox{--}3\times 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$$|. Such pairs show signs of recent major mergers in the MBII simulation. By modelling the central and satellite AGN CLFs as lognormal and Schechter distributions, respectively (as seen in MBII AGNs), we arrive at CLF models which fit the simulation predictions and observed luminosity function and the small-scale clustering measured for the SDSS sample. Furthermore, the small-scale clustering of our mock quasars is well-explained by central--satellite quasar pairs that reside in |$$M_{\rm h}\gt 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$$| dark matter haloes. For these pairs, satellite quasar luminosity is similar to that of central quasars. Our CLF models imply a relatively steep increase in the maximum satellite luminosity, |$$L^*_{\mathrm{sat}}$$|, in haloes of |$$M_{\rm h}\gt 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$$| with associated larger values of |$$L^*_{\mathrm{sat}}$$| at higher redshift. This leads to increase in the satellite fraction that manifests itself in an enhanced clustering signal at ≲1 Mpch-1. For the ongoing eBOSS-CORE sample, we predict ~200–500 quasar pairs at z ~ 1.5 (with |$$M_{\rm h} \gtrsim 10^{13}~\mathrm{M}_{\odot }\, h^{-1}$$| and |$$M_{\rm bh} \gtrsim 10^{8}~\mathrm{M}_{\odot }\, h^{-1}$$|) at ~25 kpc scales. Such a sample would be ≳ 10 times larger than current pair samples.

Authors:
ORCiD logo [1];  [1];  [2];  [3]
  1. McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh PA 15213, USA
  2. Department of Physics, Southern Methodist University, 3215 Daniel Ave., Dallas, TX 75225, USA, Department of Physics & Astronomy, University of Utah, Salt Lake City, UT 84112, USA
  3. Department of Physics & Astronomy, University of Wyoming, 1000 University Ave., Laramie, WY 82071, USA
Publication Date:
Research Org.:
Univ. of Wyoming, Laramie, WY (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP); National Science Foundation (NSF)
OSTI Identifier:
1498191
Alternate Identifier(s):
OSTI ID: 1595835
Grant/Contract Number:  
SC0019022; ACI-1614853; AST-1517593
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 485 Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Small-scale clustering; halo occupation; quasars: general; close pairs

Citation Formats

Bhowmick, Aklant K., DiMatteo, Tiziana, Eftekharzadeh, Sarah, and Myers, Adam D. On the small-scale clustering of quasars: constraints from the MassiveBlack II simulation. United Kingdom: N. p., 2019. Web. doi:10.1093/mnras/stz519.
Bhowmick, Aklant K., DiMatteo, Tiziana, Eftekharzadeh, Sarah, & Myers, Adam D. On the small-scale clustering of quasars: constraints from the MassiveBlack II simulation. United Kingdom. doi:10.1093/mnras/stz519.
Bhowmick, Aklant K., DiMatteo, Tiziana, Eftekharzadeh, Sarah, and Myers, Adam D. Wed . "On the small-scale clustering of quasars: constraints from the MassiveBlack II simulation". United Kingdom. doi:10.1093/mnras/stz519.
@article{osti_1498191,
title = {On the small-scale clustering of quasars: constraints from the MassiveBlack II simulation},
author = {Bhowmick, Aklant K. and DiMatteo, Tiziana and Eftekharzadeh, Sarah and Myers, Adam D.},
abstractNote = {Here, we explore recent high-precision measurements of small-scale quasar clustering (at z ~ 0.5–2 on scales of |${\sim }25~\mathrm{kpc}\, h^{-1}$|) from the SDSS in the context of the MassiveBlack II (MBII) cosmological hydrodynamic simulation and conditional luminosity function (CLF) modelling. At these high luminosities (g < 20.85 quasars), the MBII simulation volume (|$100~\mathrm{cMpc}\, h^{-1}$| comoving boxsize) has only three quasar pairs at distances of 1–4 Mpc. The black hole masses for the pairs range between |$M_{\rm bh}\sim 1{\, \rm and\, }3\times 10^{9}~\mathrm{M}_{\odot }\, h^{-1}$| and the quasar hosts are haloes of |$M_{\rm h}\sim 1\hbox{--}3\times 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$|. Such pairs show signs of recent major mergers in the MBII simulation. By modelling the central and satellite AGN CLFs as lognormal and Schechter distributions, respectively (as seen in MBII AGNs), we arrive at CLF models which fit the simulation predictions and observed luminosity function and the small-scale clustering measured for the SDSS sample. Furthermore, the small-scale clustering of our mock quasars is well-explained by central--satellite quasar pairs that reside in |$M_{\rm h}\gt 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$| dark matter haloes. For these pairs, satellite quasar luminosity is similar to that of central quasars. Our CLF models imply a relatively steep increase in the maximum satellite luminosity, |$L^*_{\mathrm{sat}}$|, in haloes of |$M_{\rm h}\gt 10^{14}~\mathrm{M}_{\odot }\, h^{-1}$| with associated larger values of |$L^*_{\mathrm{sat}}$| at higher redshift. This leads to increase in the satellite fraction that manifests itself in an enhanced clustering signal at ≲1 Mpch-1. For the ongoing eBOSS-CORE sample, we predict ~200–500 quasar pairs at z ~ 1.5 (with |$M_{\rm h} \gtrsim 10^{13}~\mathrm{M}_{\odot }\, h^{-1}$| and |$M_{\rm bh} \gtrsim 10^{8}~\mathrm{M}_{\odot }\, h^{-1}$|) at ~25 kpc scales. Such a sample would be ≳ 10 times larger than current pair samples.},
doi = {10.1093/mnras/stz519},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 485,
place = {United Kingdom},
year = {2019},
month = {2}
}

Journal Article:
Free Publicly Available Full Text
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DOI: 10.1093/mnras/stz519

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Cited by: 4 works
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