DEEP EXTRAGALACTIC X-RAY SURVEYS

By W. N. Brandt, G. Hasinger. 2005

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▪ Abstract Deep surveys of the cosmic X-ray background are reviewed in the context of observational progress enabled by the Chandra X-Ray Observatory and the X-Ray Multi-Mirror Mission-Newton. The sources found by deep surveys are described along with their redshift and luminosity distributions, and the effectiveness of such surveys at selecting active galactic nuclei (AGN) is assessed. Some key results from deep surveys are highlighted, including (a) measurements of AGN evolution and the growth of supermassive black holes, (b) constraints on the demography and physics of high-redshift AGN, (c) the X-ray AGN content of infrared and submillimeter galaxies, and (d) X-ray emission from distant starburst and normal galaxies. We also describe some outstanding problems and future prospects for deep extragalactic X-ray surveys.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/705f002b57c4483cb83ee004ef59992091a30ae0

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Citations in the corpus

A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, background): “…pe (for the most recent results see Churazov et al. 2007; Ajelloet al. 2008), coupled with the resolution of this radiation into individual sources (Brandt & Hasinger 2005), allow very sensitive tests of how the AGN luminosity and obscuration evolve with redshift(the so-called ’X-ray background…”
The Extended Chandra Deep Field-South Survey: Chandra Point-Source Catalogs (2005, background): “Deep and wide X-ray surveys indicate that the cosmic X-ray background is largely due to accretion onto supermassive black holes (SMBHs) integrated over cosmic time (e.g., see Brandt & Hasinger 2005 for a review).”
X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, background): “Recent ultradeep Chandra and multiwavelength surveys (e.g. Xue et al. 2011) have permitted robust observational tests of these correlations in distant galaxies (see also the review of Brandt & Hasinger 2005).”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, background): “X-ray surveys have been proved to be the most efficient way to compile nearly unbiased samples of Compton-thin AGNs (Brandt & Hasinger 2005), but they might miss Comptonthick AGNs (e.g. Comastri & Brusa 2008; La Massa et al. 2009).”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, background): “…that the self-termination process gives observable lifetim s ∼ 107yr for bright optical quasars, in good agreement with observations, and yields a large population of obscured sources as a natural stage of quasar evolution, as implied by observations (for a review, see Brandt & Hasinger 2005).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “X-ray surveys have played a critical role in defining the radiative-mode AGN population and delineating its evolution over cosmic time (see Brandt & Hasinger 2005 for a thorough review).”
DEEP U BAND AND R IMAGING OF GOODS-SOUTH: OBSERVATIONS, DATA REDUCTION AND FIRST RESULTS, (2009, background): “The contribution of LBG to the total stellar mass density of the universe, e.g., Grazian et al. (2007), and to the X-ray number counts (Brandt & Hasinger 2005) critically depends on a robust determination of their LF.”
Swift BAT Survey of AGNs (2007, background): “This effect seems to dominate the population seen in deep X-ray surveys (e.g., Barger et al. 2005; Brandt & Hasinger 2005), where a large fraction of the X-ray-selected objects do not have optical counterparts with classical AGN signatures.”
Multiwavelength Study of Massive Galaxies at z ~ 2. II. Widespread Compton-thick Active Galactic Nuclei and the Concurrent Growth of Black Holes and Bulges (2007, background): “Hard X-ray selection, the best means currently to find such sources at high redshift, is limited by telescope sensitivities and would al ow one to find only the brightest sources and with non-extreme column densities (e.g., Brandt & Hasinger 2005).”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “Maiolino et al. 1998; Risaliti, Maiolino & Salvati 1999; Fabian & Iwasawa 1999; Brandt & Hasinger 2005; Guainazzi, Matt & Perola 2005), thisstill seems unlikely to completely account for the three to four orders of magnitude scatter in Fig.”
The Hard X-Ray Spectrum as a Probe for Black Hole Growth in Radio-Quiet Active Galactic Nuclei (2008, methodology): “This method may allow tracing the history of BH growth in the Universe by utilizing large AGN datasets (see e.g., Brandt & Hasinger 2005) in which BH growth cannot be determined effectively using existing methods [i.e., reverberation-mapping based methods (aka singleepoch methods), e.g., K05, and…”
Infrared Power-Law Galaxies in the Chandra Deep Field-South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies (2006, background): “Active galactic nuclei (AGNs) are sources of luminous X-ray emission, and at cosmological distances AGNs are routinely selected from deepX-ray ( 10 keV,Chandra and XMM-Newton) exposures (for a recent review see Brandt & Hasinger 2005).”
The XMM-Newton Wide-Field Survey in the COSMOS Field. I. Survey Description (2006, background): “Moreover, because X–rays can both penetrate obscuring dust and are not sensitive to dilution by starlight in the host galaxy, the X–ray selection of AGN is not affected by some of the biases of the optical selection (see e.g. Brandt & Hasinger 2005).”
LSST: From Science Drivers to Reference Design and Anticipated Data Products (2008, background): “Similarly, deep optical data are required for identification of X-ray sources (Brandt & Hasinger 2005).”
The SRG/eROSITA all-sky survey (2024, neutral): “…of the supermassive black holes (SMBHs) that sit at the centres of galaxies and which may strongly influence their formation and subsequent evolution (Brandt & Hasinger 2005; Hopkins et al. 2008; Hickox et al. 2009; Fabian 2012; Alexander & Hickox 2012; Kormendy & Ho 2013; Brandt & Alexander 2015).”
The PalermoSwift-BAT hard X-ray catalogue: II. Results after 39 months of sky survey (2009, background): “…contribution: while the CXB at energies lower than 10 keV has been almost entirely resolved (80–90%, Moretti et al. 2003; Worsley et al. 2005, 2006; Brandt & Hasinger 2005), only a∼1.5% of the CXB at higher energies can be associated with resolved sources (Ajello et al. 2008b) Up to now, the…”