TOWARD THE STANDARD POPULATION SYNTHESIS MODEL OF THE X-RAY BACKGROUND: EVOLUTION OF X-RAY LUMINOSITY AND ABSORPTION FUNCTIONS OF ACTIVE GALACTIC NUCLEI INCLUDING COMPTON-THICK POPULATIONS

By Y. Ueda, M. Akiyama, G. Hasinger, T. Miyaji, Mike Watson. 2014

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We present the most up to date X-ray luminosity function (XLF) and absorption function of active galactic nuclei (AGNs) over the redshift range from 0 to 5, utilizing the largest, highly complete sample ever available obtained from surveys performed with Swift/BAT, MAXI, ASCA, XMM-Newton, Chandra, and ROSAT. The combined sample, including that of the Subaru/XMM-Newton Deep Survey, consists of 4039 detections in the soft (0.5–2 keV) and/or hard (>2 keV) band. We utilize a maximum likelihood method to reproduce the count rate versus redshift distribution for each survey, by taking into account the evolution of the absorbed fraction, the contribution from Compton-thick (CTK) AGNs, and broadband spectra of AGNs, including reflection components from tori based on the luminosity- and redshift-dependent unified scheme. We find that the shape of the XLF at z ∼ 1–3 is significantly different from that in the local universe, for which the luminosity-dependent density evolution model gives much better description than the luminosity and density evolution model. These results establish the standard population synthesis model of the X-ray background (XRB), which well reproduces the source counts, the observed fractions of CTK AGNs, and the spectrum of the hard XRB. The number ratio of CTK AGNs to the absorbed Compton-thin (CTN) AGNs is constrained to be ≈0.5–1.6 to produce the 20–50 keV XRB intensity within present uncertainties, by assuming that they follow the same evolution as CTN AGNs. The growth history of supermassive black holes is discussed based on the new AGN bolometric luminosity function.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2551451b71c7675c135d17bfde835e358869335e

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Citations in the corpus

Active galactic nuclei: what’s in a name? (2017, background): “L/LEdd > 0.01), which account for the majority of the BH growth in the Universe (e.g. Ueda et al. 2014; Aird et al. 2015).”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, background): “In Figure 4 we show in particular the comparison with a recent comprehensive study of the XLF by Ueda et al. (2014).”
The bolometric quasar luminosity function at z = 0–7 (2020, methodology): “…et al. 2005; Silverman et al. 2005), we include new observational data from Ebrero et al. (2009); Aird et al. (2008); Silverman et al. (2008); Yencho et al. (2009); Aird et al. (2010); Fiore et al. (2012); Ueda et al. (2014); Aird et al. (2015a,b); Miyaji et al. (2015); Khorunzhev et al. (2018).”
Consistent modelling of the meta-galactic UV background and the thermal/ionization history of the intergalactic medium (2018, methodology): “Finally, we update the HM12 prescription for the X-ray properties of AGN adopting the luminosity dependent density evolution of the [2- 10]keV luminosity function proposed by Ueda et al. (2014).”
Supermassive black holes and their feedback effects in the IllustrisTNG simulation (2017, background): “First, the luminosity function, which can be measured up to high redshift, gives insights about the mass growth via gas accretion over cosmic time (Hopkins et al. 2007; Shankar et al. 2009; Ueda et al. 2014; Lacy et al. 2015).”
BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics (2017, background): “…Kyoto 606-8502, Japan 15 Atmospheric and Environmental Research, 131 Hartwell Ave No. 4, Lexington, MA 02421, USA 16 Ambizione fellow 17 Zwicky fellow 18 Deceased cosmic X-ray background (CXB) spectrum (e.g., Comastri et al. 1995; Treister et al. 2009; Draper & Ballantyne 2010; Ueda et al. 2014).”
THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS (2015, background): “…exhibit a peak in star formation at z≃2 (Cimatti et al. 2006; Madau and Dickinson 2014), and SMBH growth peaks in the same redshift range (z=2-3), as the quasar luminosity function (Hasinger et al. 2005; Silverman et al. 2008; Hasinger 2008; Ueda et al. 2014; Aird et al. 2015; Miyaji et al. 2015).”
Blazar Flares as an Origin of High-energy Cosmic Neutrinos? (2018, background): “…the Hubble time and ξz represents the redshift evolution of the neutrino luminosity density of the sources: ξz ∼ 0.7 for the γ-ray luminosity density evolution of BL Lacs, ξz ∼ 8 for that of FSRQs, and ξz ∼ 3 for the X-ray luminosity density evolution of AGN (Ajello et al. 2014; Ueda et al. 2014).”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, methodology): “…function and black hole – galaxy scaling relations; iii) there are several lines of both theoretical and observational evidence (e.g. Mahadevan 1997; Ciotti et al. 2009; Ueda et al. 2014) indicating that radiative efficiencies might depend on black hole properties, such as their accretion rate.”
AGN wind scaling relations and the co-evolution of black holes and galaxies (2017, methodology): “BALs are from z = 2–3 QSOs.”
Blossoms from black hole seeds: properties and early growth regulated by supernova feedback (2016, background): “Such population is expected to account for 30-50% of the AGN population, based on lower redshift hard X-ray observations (Ueda et al. 2014, and references therein) and synthesis of the X-ray background (Gilli, Comastri & Hasinger 2007).”
The dust covering factor in active galactic nuclei (2016, methodology): “The decrease of the covering factor of the torus with increasing luminosity is systematically found in X-ray surveys (e.g. Ueda et al. 2003; Beckmann et al. 2009; Burlon et al. 2011; Ricci et al. 2013; Merloni et al. 2014; Ueda et al. 2014; Buchner et al. 2015).”
Universal bolometric corrections for active galactic nuclei over seven luminosity decades (2020, methodology): “For the X-ray selected LF, we adopted the Ueda et al. (2014) 2–10 keV LF, which was computed in various absorption ranges (i.e., at different NH).”
BAT AGN Spectroscopic Survey. V. X-Ray Properties of the Swift/BAT 70-month AGN Catalog (2017, background): “…of obscured and unobscured AGN (e.g., Della Ceca et al. 2008; Burlon et al. 2011; Aird et al. 2015), and is consistent with the observed decrease of the fraction of obscured sources with increasing luminosity (e.g., Ueda et al. 2003; Treister & Urry 2006; Burlon et al. 2011; Ueda et al. 2014).”
COMPTON-THICK ACCRETION IN THE LOCAL UNIVERSE (2015, methodology): “Ueda et al. (2014) consider reprocessed X-ray emission from the molecular torus by using an X-ray spectral model obtained from Monte Carlo simulations (Brightman & Nandra 2011), also taking into account disk reflection (using PEXRAV).”
Cosmic X-ray surveys of distant active galaxies (2015, methodology): “The current data generally suggest a decline in space density for moderate-luminosity AGNs at z > 3 (e.g., Fiore et al 2012a; Vito et al 2013, 2014a; Kalfountzou et al 2014; Ueda et al 2014).”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, methodology): “We compare the theoretical LF ( ) to the observational determination of the bolometric LF, of which different estimates exist (Hopkins et al. 2007; Shankar et al. 2009; Ueda et al. 2014).”