Abstract
We review results from cosmic X-ray surveys of active galactic nuclei (AGNs) over the past \(\approx 15\) years that have dramatically improved our understanding of growing supermassive black holes in the distant universe. First, we discuss the utility of such surveys for AGN investigations and the capabilities of the missions making these surveys, emphasizing Chandra, XMM-Newton, and NuSTAR. Second, we briefly describe the main cosmic X-ray surveys, the essential roles of complementary multiwavelength data, and how AGNs are selected from these surveys. We then review key results from these surveys on the AGN population and its evolution (“demographics”), the physical processes operating in AGNs (“physics”), and the interactions between AGNs and their environments (“ecology”). We conclude by describing some significant unresolved questions and prospects for advancing the field.
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Notes
For purposes of basic comparison, the column density through your hand is \(N_\mathrm{H}\sim 10^{23}~\hbox {cm}^{-2}\), while that through your chest is \(N_\mathrm{H}\sim 10^{24}~\hbox {cm}^{-2}\) (with significant variation depending upon the amount of bone intercepted).
Note that many X-ray detectors, including those used on Chandra and XMM-Newton to perform cosmic surveys, simultaneously obtain imaging, spectral, and timing data for the collected photons (e.g., Strüder et al. 2001; Turner et al. 2001; Garmire et al. 2003). Such X-ray observations are qualitatively different from those generally taken in the optical/infrared where, e.g., imaging and spectroscopy are largely distinct.
Additional (likely smaller) relevant factors to consider include (1) XLF incompleteness due to uncertainties in the masses and growth processes of the high-redshift “seeds” of SMBHs (see Sect. 3.2), and (2) the ejection of SMBHs from galactic nuclei due to gravitational-wave production in SMBH merger events. Volonteri et al. (2013) and Gilfanov and Merloni (2014) provide further discussion of these factors.
In this review we use the term host-galaxy environment to describe the properties of the host galaxy (e.g., mass, color, morphology, SFR) rather than the large-scale environment in which the galaxy resides.
Given the evident mass dependence on the colors of galaxies, color-mass diagrams are now often used in preference to color-magnitude diagrams for host-galaxy analyses.
Here it is assumed that higher-mass galaxies have more massive SMBHs than lower-mass galaxies, which is reasonable since (1) there is a broad relationship between host-galaxy mass and SMBH mass and (2) any evolution in the stellar-SMBH mass relationship with redshift appears to be modest (e.g., Jahnke et al. 2009; Bennert et al. 2011; Schramm and Silverman 2013).
Ideally the bolometric luminosity would be directly measured from the primary AGN continuum over the optical-X-ray waveband. However, it is expected to peak at far-UV wavelengths, which is unobservable due to absorption from the Galaxy. See, for example, Vasudevan and Fabian (2009) and Jin et al. (2012b) for some observational approaches to estimating the primary AGN continuum of nearby AGNs.
In stacking analyses, the images of a selected source population are combined (i.e., stacked) and the flux is measured from the combined image, providing a constraint on the average flux of the source population. An advantage of stacking is that individually undetected sources can be included in the analysis and average constraints can even be placed on the fluxes of source populations when none of the sources are individually detected.
The X-ray source density predictions are based on the Gilli et al. (2007) model for AGNs with \(N_\mathrm{H}=10^{20}{-}10^{24}~\hbox {cm}^{-2}\); see http://www.bo.astro.it/~gilli/counts.html.
For further details of JWST; see http://www.jwst.nasa.gov.
For further details of the ELTs; see http://www.eso.org/public/teles-instr/e-elt/,http://www.gmto.org/, and http://www.tmt.org/.
For example, see the list of proposed X-ray observatory concepts solicited by NASA in 2012: http://pcos.gsfc.nasa.gov/studies/xray/x-ray-mission-rfis.php.
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Acknowledgments
We thank J.A. Aird, F.E. Bauer, P.N. Best, J.N. Bregman, M. Brightman, M. Brusa, A. Comastri, J.L. Donley, P. Gandhi, R. Gilli, C.M. Harrison, R.C. Hickox, L.C. Ho, D.D. Kocevski, J.H. Krolik, B.D. Lehmer, B. Luo, E. Lusso, A. Merloni, J.R. Mullaney, R.P. Norris, D.J. Rosario, A.E. Scott, O. Shemmer, Y. Shen, F. Stanley, M. Sun, E. Treister, J.R. Trump, Y. Ueda, C. Vignali, M. Volonteri, and Y.Q. Xue for feedback, helpful discussions, and sharing information. We gratefully acknowledge financial support from NASA ADP grant NNX10AC99G (WNB), Chandra X-ray Center grants AR3-14015X and G04-15130A (WNB), the Leverhulme Trust (DMA), and the Science and Technology Facilities Council (ST/I001573/1; DMA).
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Brandt, W.N., Alexander, D.M. Cosmic X-ray surveys of distant active galaxies. Astron Astrophys Rev 23, 1 (2015). https://doi.org/10.1007/s00159-014-0081-z
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DOI: https://doi.org/10.1007/s00159-014-0081-z