Luminosity-dependent evolution of soft X-ray selected AGN : New Chandra and XMM-Newton surveys

By G. Hasinger, T. Miyaji, M. Schmidt. 2005

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We present new results on the cosmological evolution of unabsorbed (type-1) active galactic nuclei (AGN) selected in the soft (0.5-2 keV) X-ray band. From a variety of ROSAT , XMM-Newton and Chandra surveys we selected a total of ~1000 AGN with an unprecedented spectroscopic and photometric optical/NIR identification completeness. For the first time we are able to derive reliable space densities for low-luminosity (Seyfert-type) X-ray sources at cosmological redshifts. The evolutionary behaviour of AGN shows a strong dependence on X-ray luminosity: while the space density of high-luminosity AGN reaches a peak around $z\sim 2$, similar to that of optically selected QSO, the space density of low-luminosity AGNs peaks at redshifts below $z=1$. This confirms previous ROSAT findings of a luminosity-dependent density evolution. Using a rigorous treatment of the optical identification completeness we are able to show that the space density of AGN with X-ray luminosities $L_{\rm x} -1 declines significantly towards high redshifts.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b503fc3fa9a72a634bb0ea99a48fb45ecb21a7a9

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Citations in the corpus

OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, methodology): “This behaviour is most apparent at redshifts z ∼ 1− 2 and is only easy to parameterise using the Luminosity Dependent Density Evolution model (e.g. Ueda et al. (2003); Hasinger et al. (2005); Silverman et al. (2008)).”
THE LUMINOSITY FUNCTION OF FERMI-DETECTED FLAT-SPECTRUM RADIO QUASARS (2011, methodology): “The epoch of this “redshift peak” correlates with source luminosity (e.g., Ueda et al. 2003; Hasinger et al. 2005).”
CHASING HIGHLY OBSCURED QSOs IN THE COSMOS FIELD (2008, background): “…see Table 1 for a quantitative definition) peaks at z>∼ 2 and declines strongly afterwards, while lower luminosity AGN follow a much smoother behavior, peaking at lower redshifts, z=1-1.5 (Ueda et al. 2003, Cowie et al. 2003, Fiore et al. 2003, Hasinger et al. 2005, La Franca et al. 2005).”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, result): “This is in accord with recent results from studies of the hard X-ray luminosity function of quasars and AGNs, e.g., typical Seyfert-like objects with MBH 107Y108 M accreting at a few percent of the Eddington rate (e.g., Ueda et al. 2003; Hasinger et al. 2005).”
Cosmogenic neutrinos: parameter space and detectabilty from PeV to ZeV (2010, background): “Hasinger et al. (2005) argue that FRI type galaxies might follow a similar, though less steep trend.”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “The QSO luminosity function of the completed 2dF-SDSS opticallyselected QSO survey (Croom et al. 2009) agrees extremely well in both amplitude and shape with the X-ray selected QSO luminosity functions of Hasinger et al. (2005).”
HST WFC3/IR OBSERVATIONS OF ACTIVE GALACTIC NUCLEUS HOST GALAXIES AT z ∼ 2: SUPERMASSIVE BLACK HOLES GROW IN DISK GALAXIES (2010, background): “These AGN host galaxies are a significant fraction of the total AGN population by number density and in terms of light emitted by accretion (Ueda et al. 2003; Hasinger et al. 2005).”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, background): “One key consequence of this evolution is the observed “downsizing” of quasar activity: where by the spatial density of more luminous objects peaks at higher redshifts (Cowie et al. 2003; Ueda et al. 2003; Hasinger et al. 2005; Croom et al. 2009).”
THE XMM-NEWTON WIDE-FIELD SURVEY IN THE COSMOS FIELD (XMM-COSMOS): DEMOGRAPHY AND MULTIWAVELENGTH PROPERTIES OF OBSCURED AND UNOBSCURED LUMINOUS ACTIVE GALACTIC NUCLEI (2010, background): “…be luminosity dependent: the space density of bright QSOs (LX > 10 44 erg s−1) peaks at z∼ 2–3, to be compared with the z∼0.7–1 peak of lower luminosity Seyfert galaxies (Ueda et al. 2003; Hasinger et al. 2005; La Franca et al. 2005, Silverman et al. 2008; Ebrero et al. 2009, Yencho et al. 2009).”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “…Miyaji et al. 2000, 2001; La Franca et al. 2002; Cowie et al. 2003; Ueda et al. 2003; Fiore et al. 2003; Hunt et al. 2004; Cirasuolo et al. 2005; Hasinger et al. 2005) (although we still find 3 evidence for this evolution without these data), but independently these samples detect such…”
CONTRIBUTION OF GAMMA-RAY-LOUD RADIO GALAXIES’ CORE EMISSIONS TO THE COSMIC MeV AND GeV GAMMA-RAY BACKGROUND RADIATION (2011, background): “…for a long time in astrophysics, although it is well known that radio-quiet active galactic nuclei (AGNs) take into account the cosmic X-ray background (CXB) below several hundred keV (see, for reviews, Boldt 1987; Fabian & Barcons 1992; Ueda et al. 2003; Hasinger et al. 2005; Gilli et al. 2007).”
The bolometric quasar luminosity function at z = 0–7 (2020, background): “Apparently, the number density of faint quasars peaks at lower redshift than that of bright ones, consistent with the observed "cosmic downsizing" trend (e.g., Cowie et al. 1996; Barger et al. 2005; Hasinger et al. 2005) of AGN at z .”
THREE-YEAR SWIFT–BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING THEORY AND OBSERVATIONS? (2010, methodology): “We made a maximum likelihood fit to the two different data sets using a broken power law of the form (see, e.g., Ueda et al. 2003; Hasinger et al. 2005) Φ(LX, z = 0) = dN dLX = A ln(10)LX [( LX L∗ )γ1 + ( LX L∗ )γ2]−1 .”
The Mass Function of Active Black Holes in the Local Universe (2007, methodology): “On the other hand, low-luminosity, soft X-ray–selected sources,most likely closely linked to optically selected broad-line AGNs, also have a peak space density at low redshift (e.g., Hasinger et al. 2005).”
SELF-CONSISTENT MODELS OF THE AGN AND BLACK HOLE POPULATIONS: DUTY CYCLES, ACCRETION RATES, AND THE MEAN RADIATIVE EFFICIENCY (2007, background): “Hard X-ray selection is thus the least affected by obscuration, and deep X-ray surveys indeed reveal many faint AGNs that are missed by traditional optical selection criteria (e.g., Hasinger et al. 2005).”
A unified model for AGN feedback in cosmological simulations of structure formation (2007, background): “…with observational findings both from optical and X-rays surveys (e.g. Steffen et al., 2003; Ueda et al., 2003; Heckman et al., 2004; Barger et al., 2005; Hasinger et al., 2005) that indi- c© 0000 RAS, MNRAS 000, 000–000 cate that BHs are growing in a so-called ‘anti-hierarchical’ manner.”
The X-Ray-to-Optical Properties of Optically Selected Active Galaxies over Wide Luminosity and Redshift Ranges (2006, background): “…that low-luminosity (L2−8 keV <∼ 1044 erg s−1) AGNs do not agree with the PLE model, but instead appear to undergo luminosity-dependent density evolution (LDDE; e.g., Ueda et al. 2003; Steffen et al. 2003; Barger et al. 2005; Hasinger et al. 2005; La Franca et al. 2005; Silverman et al. 2005a).”