Supermassive Black Holes in the Distant Universe

By A. Barger. 2004

226 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/00b47f06374720d6e1165a3227c33b802e0faea3

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Citations in the corpus

Cosmic X-ray surveys of distant active galaxies (2015, background): “When AGNs have been reliably identified using optical, infrared, and/or radio techniques, they almost always also show X-ray AGN signatures (e.g., see Fig. 1; e.g., Avni and Tananbaum 1986; Brandt et al 2000; Mushotzky 2004; Gibson et al 2008).”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “Comastri 2004; Nandra & Iwasawa 2007; Alexander et al. 2008).”
The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei (2004, background): “…region of the CDF-N shown for three X-ray luminosity intervals (triangles, LX > 10 44 ergs s 1; diamonds, LX ¼ 1043 1044 ergs s 1; squares, LX ¼ 1042 1043 ergs s 1). narrow AGNs were being swamped by the host galaxy light, thereby washing out the broad-line signal (Moran et al. 2002; Moran 2004).”
Spin, Accretion, and the Cosmological Growth of Supermassive Black Holes (2004, background): “Excellent overviews of the input physics have appeared elsewhere (see, e.g. Haiman & Quataert 2004, and references to earlier work).”
Chandra and XMM-Newton Observations of a Sample of Low-Redshift FR I and FR II Radio Galaxy Nuclei (2005, methodology): “…and Chiaberge et al. (2000) interpret these sources as being oriented to the observer such that significant optical emission from an accretion disk is observed, consistent with predictions from active galactic nucleus (AGN) unification schemes (e.g., Antonucci 1993; Urry & Padovani 1995).”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, background): “Nonetheless, a large fraction of Compton-thick (NH 1.5 × 1024 H-atoms cm−2; for a review see Comastri 2004) AGNs still escapes detection.”