Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey

By E. Lusso, A. Comastri, B. Simmons, M. Mignoli, G. Zamorani, C. Vignali, M. Brusa, F. Shankar, D. Lutz, J. Trump and 18 more. 2012

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Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) active galactic nuclei (AGN) from the XMM–Newton survey in the Cosmic Evolution Survey field are presented. The sample is composed of 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65 per cent of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83 and 52 per cent, respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high-quality multiwavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 and 160 μm) to the optical–ultraviolet allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol- Lbol relations derived in this work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. and Hopkins et al. Black hole (BH) masses and Eddington ratios are available for 170 Type-1 AGN, while BH masses for Type-2 AGN are computed for 481 objects using the BH mass–stellar mass relation and the morphological information. We confirm a trend between kbol and λEdd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, the Eddington ratio increases with redshift for all types of AGN at any given MBH, while no clear evolution with redshift is seen at any given Lbol.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/493f0776d620abd91d3720dd37f7e8f92e81f1c9

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Citations in the corpus

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects (2014, methodology): “We estimated the total AGN bolometric luminosities (Lbol) for our sources following the methods presented in Lusso et al. (2012) and Lusso et al. (2013) for the XMMCOSMOS sample.”
Universal bolometric corrections for active galactic nuclei over seven luminosity decades (2020, methodology): “Moreover, all of them, except for Lusso et al. (2012), focused on luminous, unobscured (type 1) sources, where the bolometric luminosity is much more easily measured because the SED is less strongly affected by obscuration and galaxy contamination than in type 2 sources.”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, background): “A more complex analysis, including multiple dust emission components, has been carried out by Lusso et al. (2012).”
Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “…but simply randomly picked from a grid of values, the torus is effectively fit to the data in a simultane- ous 3-component model (see also Fritz et al. 2006; Berta et al. 2007; Noll et al. 2009; Santini et al. 2012; Lusso et al. 2012; Bongiorno et al. 2012, for alternative implementations).”
A physical model of the broad-band continuum of AGN and its implications for the UV/X relation and optical variability (2018, background): “This already MNRAS 000, 1–14 (2018) limits the black hole mass to > 107.5M⊙ for objects with a standard disc below Eddington, and the masses reported in (Lusso et al. 2012, Fig.6) are clustered around (1 − 10) × 108 M⊙ .”
Cosmic X-ray surveys of distant active galaxies (2015, background): “Optical spectroscopic selection based on high-ionization emission lines (e.g., Steidel et al 2002; Hunt et al 2004; Alexander et al 2008; Trump et al 2011b; Juneau et al 2013, 2014; Vignali et al 2014).”
x-cigale: fitting AGN/galaxy SEDs from X-ray to infrared (2020, background): “However, recent observations indicate that a non-negligible amount of extinction exists for some type 1 AGNs (e.g. Bongiorno et al. 2012; Elvis et al. 2012; Lusso et al. 2012), which can be attributed to the dust existing along polar directions (e.g. Stalevski et al. 2017, 2019; Lyu & Rieke 2018).”
THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS (2015, background): “…survey (LX >10 44 erg s−1) has been already explored in a series of publication from XMM-COSMOS (e.g. Brusa et al. 2009, 2010, hereafter B10; Allevato et al. 2011; Mainieri et al. 2011; Bongiorno et al. 2012; Lusso et al. 2012, 2013; Merloni et al. 2014; Miyaji et al. 2015 among others).”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, background): “…functions large uncertainties remain due to poorly constrained bolometric corrections (Hopkins et al. 2007; Vasudevan & Fabian 2007, 2009; Lusso et al. 2012) and the c© 0000 RAS, MNRAS 000, 000–000 uncertain fraction of Compton-thick sources for z & 0 (e.g. see recent papers by Ueda et…”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, background): “…(2012) and Bongiorno et al. (2012), and the Schechter function proposed by Schulze et al. (2015): we do predict a turnover, but at lower values than found by Schulze et al. (2015) and Lusso et al. (2012), keeping in mind that the latter two papers have estimated fEdd, rather than the specific BHAR.”
THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG (2016, background): “These observations have been crucial for characterizing the most luminous Active Galactic Nuclei (AGN) in COSMOS (e.g. Brusa et al. 2010, Mainieri et al. 2011, Allevato et al. 2011, Lusso et al. 2012, among others).”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, background): “Such an assumption relies on the fact that large kbol values have been found in hard X-rays, of the order of 20−30 (Risaliti & Elvis 2004; Marconi et al. 2004; Hopkins et al. 2007; Pozzi et al. 2007; Vasudevan & Fabian 2009; Lusso et al. 2012), increasing as a function of Lbol,AGN.7 In Fig.”