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Multiplicity functions of quasars: Predictions from the MassiveBlackII simulation
Astrophysics of Galaxies · Submitted 15 Feb 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that gravitationally bound multiple AGN systems tend to populate scales of $\lesssim0.7~\mathrm{cMpc}/h$; this corresponds to angular separations of $\lesssim100~\mathrm{arcsec}$ and a line of sight velocity difference $\lesssim200~\mathrm{km/sec}$.
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We examine multiple AGN systems (triples and quadruples, in particular) in the \texttt{MassiveBlackII} simulation over a redshift range of $0.06\lesssim z \lesssim 4$. We identify AGN systems (with bolometric luminosity $L_{\mathrm{bol}}>10^{42}~\mathrm{ergs/sec}$) at different scales~(defined by the maximum distance between member AGNs) to determine the AGN multiplicity functions. This is defined as the volume/ surface density of AGN systems per unit \textit{richness} $R$, the number of AGNs in a system. We find that gravitationally bound multiple AGN systems tend to populate scales of $\lesssim0.7~\mathrm{cMpc}/h$; this corresponds to angular separations of $\lesssim100~\mathrm{arcsec}$ and a line of sight velocity difference $\lesssim200~\mathrm{km/sec}$. The simulation contains $\sim 10$ and $\sim100$ triples/quadruples per $\mathrm{deg}^2$ up to depths of DESI ($g\lesssim24$) and LSST ($g\lesssim26$) imaging respectively; at least $20\%$ of these should be detectable in spectroscopic surveys. The simulated quasar ($L_{\mathrm{bol}}>10^{44}~\mathrm{ergs/sec}$) triples and quadruples predominantly exist at $1.5\lesssim z \lesssim 3$. Their members have black hole masses $10^{6.5}\lesssim M_{bh}\lesssim 10^{9}~M_{\odot}/h$ and live in separate (one central and multiple satellite) galaxies with stellar masses $10^{10}\lesssim M_{*}\lesssim 10^{12}~M_{\odot}/h$. They live in the most massive haloes (for e.g. $\sim 10^{13}~M_{\odot}/h$ at $z=2.5$; $\sim 10^{14}~M_{\odot}/h$ at $z=1$) in the simulation. Their detections provide an exciting prospect for understanding massive black hole growth and their merger rates in galaxies in the era of multi-messenger astronomy.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We examine multiple AGN systems (triples and quadruples, in particular) in the \texttt{MassiveBlackII} simulation over a redshift range of $0.06\lesssim z \lesssim 4$. | contribution 0.56 | 0.95 | 0.03 | asserted 0.93 |
| s1 | We identify AGN systems (with bolometric luminosity $L_{\mathrm{bol}}>10^{42}~\mathrm{ergs/sec}$) at different scales~(defined by the maximum distance between member AGNs) to determine the AGN multiplicity functions. | method 0.94 | 0.95 | 0.04 | asserted 0.97 |
| s2 | This is defined as the volume/ surface density of AGN systems per unit \textit{richness} $R$, the number of AGNs in a system. | method 0.95 | 0.44 | 0.03 | asserted 0.95 |
| s3 | We find that gravitationally bound multiple AGN systems tend to populate scales of $\lesssim0.7~\mathrm{cMpc}/h$; this corresponds to angular separations of $\lesssim100~\mathrm{arcsec}$ and a line of sight velocity difference $\lesssim200~\mathrm{km/sec}$. | result 1.00 | 0.93 | 0.22 | asserted 1.00 |
| s4 | The simulation contains $\sim 10$ and $\sim100$ triples/quadruples per $\mathrm{deg}^2$ up to depths of DESI ($g\lesssim24$) and LSST ($g\lesssim26$) imaging respectively; at least $20\%$ of these should be detectable in spectroscopic surveys. | result 1.00 | 0.91 | 0.14 | asserted 0.90 |
| s5 | The simulated quasar ($L_{\mathrm{bol}}>10^{44}~\mathrm{ergs/sec}$) triples and quadruples predominantly exist at $1.5\lesssim z \lesssim 3$. | result 1.00 | 0.92 | 0.18 | asserted 1.00 |
| s6 | Their members have black hole masses $10^{6.5}\lesssim M_{bh}\lesssim 10^{9}~M_{\odot}/h$ and live in separate (one central and multiple satellite) galaxies with stellar masses $10^{10}\lesssim M_{*}\lesssim 10^{12}~M_{\odot}/h$. | result 1.00 | 0.88 | 0.08 | asserted 1.00 |
| s7 | They live in the most massive haloes (for e.g. $\sim 10^{13}~M_{\odot}/h$ at $z=2.5$; $\sim 10^{14}~M_{\odot}/h$ at $z=1$) in the simulation. | result 1.00 | 0.87 | 0.11 | asserted 1.00 |
| s8 | Their detections provide an exciting prospect for understanding massive black hole growth and their merger rates in galaxies in the era of multi-messenger astronomy. | interpretation 0.97 | 0.11 | 0.15 | hedged possibility 0.74 |
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Original abstract
We examine multiple AGN systems (triples and quadruples, in particular) in the \texttt{MassiveBlackII} simulation over a redshift range of $0.06\lesssim z \lesssim 4$. We identify AGN systems (with bolometric luminosity $L_{\mathrm{bol}}>10^{42}~\mathrm{ergs/sec}$) at different scales~(defined by the maximum distance between member AGNs) to determine the AGN multiplicity functions. This is defined as the volume/ surface density of AGN systems per unit \textit{richness} $R$, the number of AGNs in a system. We find that gravitationally bound multiple AGN systems tend to populate scales of $\lesssim0.7~\mathrm{cMpc}/h$; this corresponds to angular separations of $\lesssim100~\mathrm{arcsec}$ and a line of sight velocity difference $\lesssim200~\mathrm{km/sec}$. The simulation contains $\sim 10$ and $\sim100$ triples/quadruples per $\mathrm{deg}^2$ up to depths of DESI ($g\lesssim24$) and LSST ($g\lesssim26$) imaging respectively; at least $20\%$ of these should be detectable in spectroscopic surveys. The simulated quasar ($L_{\mathrm{bol}}>10^{44}~\mathrm{ergs/sec}$) triples and quadruples predominantly exist at $1.5\lesssim z \lesssim 3$. Their members have black hole masses $10^{6.5}\lesssim M_{bh}\lesssim 10^{9}~M_{\odot}/h$ and live in separate (one central and multiple satellite) galaxies with stellar masses $10^{10}\lesssim M_{*}\lesssim 10^{12}~M_{\odot}/h$. They live in the most massive haloes (for e.g. $\sim 10^{13}~M_{\odot}/h$ at $z=2.5$; $\sim 10^{14}~M_{\odot}/h$ at $z=1$) in the simulation. Their detections provide an exciting prospect for understanding massive black hole growth and their merger rates in galaxies in the era of multi-messenger astronomy.
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