The evolution of the hard X-ray luminosity function of AGN

By J. Aird, K. Nandra, E. Laird, A. Georgakakis, M. Ashby, Pauline Barmby, A. Coil, J.-S. Huang, A. Koekemoer, C. Steidel and 1 more. 2009

294 citations recorded by the source corpus.

We present new observational determinations of the evolution of the 2–10 keV X-ray luminosity function (XLF) of active galactic nuclei (AGN). We utilize data from a number of surveys including both the 2 Ms Chandra Deep Fields and the AEGIS-X 200 ks survey, enabling accurate measurements of the evolution of the faint end of the XLF. We combine direct, hard X-ray selection and spectroscopic follow-up or photometric redshift estimates at z 50 per cent of black hole growth takes place at z > 1 , with around half in L_X < 10^(44) erg s^(−1) AGN.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/aeed8eccf8655426c38e5712d420906519c06a67

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Citations in the corpus

A remarkably flat relationship between the average star formation rate and AGN luminosity for distant X-ray AGN. (2015, background): “…that the volume average of the SMBH mass accretion rate tracks that of the star formation rate (SFR), within ∼3–4 orders of magnitude, up to redshifts of z ∼ 2 (e.g. Heckman et al. 2004; Merloni, Rudnick & Di Matteo 2004; Aird et al. 2010) suggesting a co-evolution of AGN and star-forming activity.”
BLACK HOLE VARIABILITY AND THE STAR FORMATION–ACTIVE GALACTIC NUCLEUS CONNECTION: DO ALL STAR-FORMING GALAXIES HOST AN ACTIVE GALACTIC NUCLEUS? (2013, background): “…et al. 2009), the remarkable similarity between the global histories of SF and BH accretion (e.g., Boyle & Terlevich 1998; Silverman et al. 2008; Aird et al. 2010; Merloni & Heinz 2013), and the observed tendency of luminous active galactic nuclei (AGNs) to reside in star-forming hosts (e.g.,…”
CANDELS: CONSTRAINING THE AGN–MERGER CONNECTION WITH HOST MORPHOLOGIES AT z ∼ 2 (2011, background): “In the hard X-ray band this knee occurs at a luminosity of roughly LX ∼ 1044 erg s−1 (Aird et al. 2010).”
The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “The flattening of the faint-end slope with redshift from X-ray luminosity functions (Silverman et al. 2008; Aird et al. 2010)supports the latter explanation.”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, background): “We find that the positive evolution continues up to z ∼ 3 (as in Aird et al. 2010) above which the population starts to decline.”
Narrow-line region gas kinematics of 24 264 optically selected AGN: the radio connection (2013, background): “…that the redshift range of our sample does not span the epoch of peak star formation and AGN activity (i.e. z ∼ 1–3; Merloni, Rudnick & Di Matteo 2004; Hopkins & Beacom 2006; Aird et al. 2010) when quasar-mode AGN-driven outflows are thought to have had their greatest impact on galaxy growth.”
Evolution of the AGN UV luminosity function from redshift 7.5 (2018, background): “Figure 7 also shows the familiar downsizing feature in which the number density of faint AGN peaks at lower redshifts than that of the bright AGN (Hunt et al. 2004; Nandra et al. 2005; Richards et al. 2006; Matute et al. 2006; Ebrero et al. 2009; Kolodzig et al. 2013; Aird et al. 2010, 2015).”
DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USING XMM- AND CHANDRA-COSMOS SAMPLES (2011, background): “…the key physical parameters such as the QSO duty cycle, the black hole seed mass function, and the accretion rates, reliable observations of the QSO luminosity function and its evolution at high redshift are required (Civano et al 2011, Brusa et al. 2010; Aird et al. 2010; Fontanot et al. 2007).”
The bolometric quasar luminosity function at z = 0–7 (2020, unknown): “…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).”
Faint high-redshift AGN in the Chandra deep field south: the evolution of the AGN luminosity function and black hole demography (2011, methodology): “We chose to describe the evolution of the high-z AGN luminosity function with the LADE (luminosity and density evolution) model, introduced by Aird et al. (2010).”
THE HIDDEN “AGN MAIN SEQUENCE”: EVIDENCE FOR A UNIVERSAL BLACK HOLE ACCRETION TO STAR FORMATION RATE RATIO SINCE z ∼ 2 PRODUCING AN MBH–M* RELATION (2012, unknown): “Integrating the “LADE” AGN X-ray luminosity function of Aird et al. 2010, we estimate that ∼20–30% of all SMBH accretion at 0.5 < z < 2.5 takes place in AGNs that are rare enough such that ≤ 3 would be expected to be found in our survey (i.e., rarer than three per 2 × 105 Mpc3 at z ∼ 1 and three…”
THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “…correspond to the peak epoch in the black hole accretion history of the Universe and the knee of the X-ray luminosity function (e.g., Ueda et al. 2003; La Franca et al. 2005; Aird et al. 2010); thus, NuSTAR should detect the AGN source population that dominates the cosmic growth of black holes.”
THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES (2012, methodology): “…method has become common recently and has been applied first to radio surveys (Ciliegi et al. 2005) and to several medium and faintChandra and XMM-Newtonsurveys (Cardamone et al. 2008, Laird et al. 2009, Aird et al. 2010, Luo et al. 2010, Brusa et al. 2010, Xue et al. 2011, Rovilos et al. 2011).”
THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, background): “One caveat here is that the hard X-ray samples used in Aird et al. (2010) are most secure at z < 1.2.”
xCOLD GASS: The Complete IRAM 30 m Legacy Survey of Molecular Gas for Galaxy Evolution Studies (2017, background): “…link between black hole and galaxy growth includes the remarkable similarity between the redshift evolution of star formation activity (i.e the LillyMadau diagram) and that of the rate of accretion onto supermassive black holes (e.g. Boyle & Terlevich 1998; Aird et al. 2010; Merloni & Heinz 2013).”
Defining the intrinsic AGN infrared spectral energy distribution and measuring its contribution to the infrared output of composite galaxies (2011, background): “…the intrinsic quasar SED can be applied to the much larger, less luminous (i.e.,L2−10keV < 1044 ergs s−1) population of AGNs which represents the majority of the integrated accretion output of AGNs in the Universe (e.g., Ueda et al. 2003; Barger et al. 2005; Hasinger et al. 2005; Aird et al. 2010).”
Cosmological simulations of black hole growth: AGN luminosities and downsizing (2013, background): “…uncertainties, we additionally attempt in this subsection to correct our model predictions for obscuration and to directly compare them with recent soft (0.5–2 keV) and hard (2–10 keV) X-ray measurements of the AGN luminosity function (Hasinger et al. 2005; Ebrero et al. 2009; Aird et al. 2010).”
Cosmic X-ray surveys of distant active galaxies (2015, background): “7; e.g., Barger et al 2005; Hasinger et al 2005; La Franca et al 2005; Silverman et al 2008a; Ebrero et al 2009; Yencho et al 2009; Aird et al 2010; Ueda et al 2014).”
X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue (2014, background): “The typical SMBH grows through active accretion at redshift 0.5 − 3 (see e.g. Aird et al. 2010).”