Absorption properties and evolution of active galactic nuclei

By G. Hasinger. 2008

275 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, methodology): “The number densities from the Fanidakis et al. (2012) model are calculated considering the entire population of AGN (both obscured and unobscured) and include the empirical obscuration prescription from Hasinger (2008).”
A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys (2013, background): “As the geometry of the torus is expected to change with X-ray luminosity and redshift (e.g. Lawrence 1991; Ueda et al. 2003; Hasinger 2008; Brightman & Ueda 2012), this component should not be neglected.”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, background): “This is an effect introduced by the well-known anticorrelation between obscured AGN fraction and luminosity (e.g. Hasinger 2008) in combination with the almost constant (X-ray) flux limit of the XMM–COSMOS survey, which implies that high-redshift sources are more luminous than low-redshift sources.”
The dust covering factor in active galactic nuclei (2016, result): “Note that the slope of the CXB model is much flatter than those found in X-ray surveys (e.g. Hasinger 2008) because of (a) the inclusion of Compton-thick AGNs, whose number is the same as that of Compton-thin absorbed AGNs in the Ueda et al. (2014) model, and of (b) the non-linear relation between…”
Revisiting the Unified Model of Active Galactic Nuclei (2015, background): “Earlier works like Hasinger (2008) claim an increase in the fraction of obscured sources with redshift.”
The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early-and late-type galaxies (2014, background): “The clustering of active galactic nuclei (AGN) host galaxies in the green valley further suggested a role for AGN feedback in particular (e.g. Nandra et al. 2007; Hasinger 2008; Silverman et al. 2008; Cimatti et al. 2013).”
What drives the growth of black holes (2011, background): “…evidence for an increase in the obscured AGN fraction with redshift (e.g., La Franca et al. 2005; Ballantyne et al. 2006; Treister & Urry 2006; Hasinger 2008; however, see also Akylas et al. 2006 and Dwelly & Page 2006), which would be expected if the nuclear regions of distant AGNs are…”
Cosmological simulations of black hole growth: AGN luminosities and downsizing (2013, background): “Some recent studies suggest that the obscured fraction is dependent on both luminosity and redshift (Hasinger 2008; Fiore MNRAS 442, 2304–2324 (2014) Downloaded from https://academic.oup.com/mnras/article-abstract/442/3/2304/1039443 by guest on 29 July 2018 et al. 2012), in contrast with the…”
Galaxy Interactions Trigger Rapid Black Hole Growth: an unprecedented view from the Hyper Suprime-Cam Survey (2017, background): “…UVJ may explain why many AGN have previously been believed to be an interesting population of transitioning ‘green-valley’ galaxies that lie between the blue cloud and red sequence (Bell et al. 2004; Faber et al. 2007; Nandra et al. 2007; Hasinger 2008; Silverman et al. 2008; Mendez et al. 2013).”
CHASING HIGHLY OBSCURED QSOs IN THE COSMOS FIELD (2008, background): “…population is large at low AGN luminosities and decreases at high luminosities, as it is indeed observed (Lawrence & Elvis 1982, Ueda et al. 2003, Steffen et al. 2003, La Franca et al. 2005, Treister & Urry 2005, 2006, Maiolino et al. 2007, Hasinger 2008, Trump et al. 2008, Della Ceca et al. 2008).”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, background): “• We find that in the Illustris AGN population there is evidence for cosmic downsizing (Barger et al. 2005; Hasinger 2008; Ueda et al. 2014).”
THE BULK OF THE BLACK HOLE GROWTH SINCE z ∼ 1 OCCURS IN A SECULAR UNIVERSE: NO MAJOR MERGER–AGN CONNECTION (2010, background): “At our redshift range, it is still safe to say that the HR values lower than –0.2 correspond to an unabsorbed, soft spectrum (Hasinger 2008).”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, background): “…the one hand, a slight evolution with redshift is suggested by some analyses (La Franca et al. 2005; Treister & Urry 2006; Ballantyne et al. 2006; Hasinger 2008; Della Ceca et al. 2008: Treister et al. 2009; Iwasawa et al. 2012); on the other hand, the space density of the obscured (log[NH/cm−2]…”
IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA (2012, background): “Because high luminosity AGN tend to be less obscured than their low luminosity counterparts, at least in X-ray selected samples, we might expect sources with redder IRAC colors to have a lower Type 2 fraction (e.g. Ueda et al. 2003; Gilli et al. 2007; Hasinger 2008).”
Faint AGNs at z > 4 in the CANDELS GOODS-S field: looking for contributors to the reionization of the Universe (2015, background): “44) shows that the fraction of obscured AGNs at high redshifts could be ∼ 50% (Hasinger (2008), Merloni et al. (2014)) although there is no tight correlation between X-ray absorption and the presence of broad emission lines since some X-ray absorbed AGNs show broad emission lines in their…”
The incidence of obscuration in active galactic nuclei (2013, background): “…to corroborate claims of positive evolution of the fraction of obscured AGN with increasing redshift (La Franca et al. 2005; Ballantyne et al. 2006; Treister et al. 2006; Hasinger 2008) as well as counterclaims of no significant evolution (Ueda et al. 2003; Tozzi et al. 2006; Gilli et al. 2007).”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, background): “In addition, the work of Hasinger (2008) shows similar results in the 2–10 keV energy band, even if just proxies of NH are used.”
The DEIMOS 10K Spectroscopic Survey Catalog of the COSMOS Field (2018, background): “This can be partially understood in terms of the difficulty of detecting broad lines of weak AGNs against the host galaxy light, but also due to a strong dependence of the obscured AGN fraction on X-ray luminosity (see, e.g., Hasinger 2008).”
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 (2014, methodology): “To maximize the completeness of redshift identification, sub-samples are defined from two off-axis intervals with different flux limits as detailed in Hasinger (2008) and H05.”
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).”