Black-hole masses of type 1 AGN in the<i>XMM-Newton</i>bright serendipitous survey

Caccianiga, A.; Fanali, R.; Severgnini, P.; Ceca, R. Della; Marchese, E.; Mateos, S.

doi:10.1051/0004-6361/201220343

Cited by 8 publications

(12 citation statements)

References 40 publications

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“…This is expected, as X-ray bright AGN samples are often dominated by broad-lined AGN (e.g. 70 per cent in the XXL-BOSS sample, Menzel et al 2016, and 88 per cent in the XBS sample, Della Ceca et al 2004;Caccianiga et al 2013). The average redshift of all our confirmed AGN is z = 0.28, average black hole mass is M BH = 5.5 × 10 8 M ⊙ and average Eddington ratio is L/L Edd = 0.2, all with large associated standard deviations.…”

Section: Discussionmentioning

confidence: 86%

“…Black hole mass estimates are not available for the full Slew/Veron sample, however we can compare our mass estimates with another XMM AGN sample which we describe in the following section. Caccianiga et al (2013) analyse a complete, flux-limited (S X > 7 × 10 −14 erg cm −2 s −1 at 0.5-4.5 keV and 4.5-7.5 keV) sample of Type I AGN from the XMM-Newton Bright Serendipitous Survey (XBS). They measure black hole masses from optical broad lines and UV continua for a subsample of 154 objects in a similar fashion to the method used here.…”

Section: The Full Slew Surveymentioning

confidence: 99%

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Characterization of AGN from the XMM–Newton Slew Survey

Starling

Wildy

Wiersema

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present optical spectroscopy of candidate AGN pinpointed by a Swift follow-up campaign on unidentified transients in the XMM-Newton Slew Survey, increasing the completeness of the identifications of AGN in the Survey. Our Swift follow-up campaign identified 17 XRTdetected candidate AGN, of which nine were selected for optical follow-up and a further two were confirmed as AGN elsewhere. Using data obtained at the William Herschel Telescope, Very Large Telescope and New Technology Telescope, we find AGN features in seven of the candidates. We classify six as Seyfert types 1.0 to 1.5, with broad-line region velocities spanning 2000-12000 km s −1 , and identify one as a possible Type II AGN, consistent with the lack of a soft band X-ray detection in the Slew Survey. The Virial black hole mass estimates for the sample lie between 1×10 8 M ⊙ and 3×10 9 M ⊙ , with one source likely emitting close to its Eddington rate, L Bol /L Edd ∼ 0.9. We find a wide redshift range of 0.08 < z < 0.9 for the nine now confirmed AGN drawn from the unidentified Slew Survey sample. One source remaining unclassified shows outbursts rarely seen before in AGN. We conclude that AGN discovered in this way are consistent with the largely non-varying, Slew-selected, known AGN population. We also find parallels with XMM-Newton Bright Serendipitous Survey AGN selected from pointed observations, and postulate that shallow X-ray surveys select AGN drawn from the same populations that have been characterised in deeper X-ray selected samples.

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Section: Discussionmentioning

confidence: 86%

Section: The Full Slew Surveymentioning

confidence: 99%

Characterization of AGN from the XMM–Newton Slew Survey

Starling

Wildy

Wiersema

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…For most of the type 1 sources in the XBS AGN sample, the optical/UV SED has been build, and the bolometric luminosity has been estimated by fitting a multicolour disk model (Marchese et al 2012). Caccianiga et al (2013) report their black hole masses, estimated using the "single epoch" spectral method (based on measuring the broad line widths and the continuum emission).…”

Section: The Xbs Sample Of X-ray Absorbed Qsosmentioning

confidence: 99%

The XMM-Newton Bright Survey sample of absorbed quasars: X-ray and accretion properties

Ballo,

Severgnini,

Della Ceca

et al. 2014

Preprint

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Although absorbed quasars are extremely important for our understanding of the energetics of the Universe, the main physical parameters of their central engines are still poorly known. In this work we present and study a complete sample of 14 quasars (QSOs) that are absorbed in the X-rays (column density N H > 4 × 10 21 cm −2 and X-ray luminosity L 2-10 keV > 10 44 ergs s −1 ; XQSO2) belonging to the XMM-Newton Bright Serendipitous Survey (XBS). From the analysis of their ultraviolet-to-mid-infrared spectral energy distribution we can separate the nuclear emission from the host galaxy contribution, obtaining a measurement of the fundamental nuclear parameters, like the mass of the central supermassive black hole and the value of Eddington ratio, λ Edd .Comparing the properties of XQSO2s with those previously obtained for the X-ray unabsorbed QSOs in the XBS, we do not find any evidence that the two samples are drawn from different populations. In particular, the two samples span the same range in Eddington ratios, up to λ Edd ∼ 0.5; this implies that our XQSO2s populate the "forbidden region" in the so-called "effective Eddington limit paradigm". A combination of low grain abundance, presence of stars inwards of the absorber, and/or anisotropy of the disk emission, can explain this result.

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“…• MBH and Eddington ratio λ: black hole masses of the XBS type 1 AGNs are computed in Caccianiga et al (2013) using the Single Epoch (SE) method (Peterson 2010 andSulentic 2012). This method assumes that the Broad Line Region (BLR) is gravitationally influenced by the SMBH, so the virial theorem can be applied.…”

Section: Parametersmentioning

confidence: 99%

“…In both relations, the line widths refer to the broad component, and it is assumed that a narrow component has been subtracted during the fitting procedure and that the iron emission has been taken into account. All the details on how the FWHM of the emission lines have been computed are given in Caccianiga et al (2013). The monochromatic luminosities at 5100 Å (L 5100 Å) and 3000 Å (L 3000 Å) respectively are derived from the SEDfitting presented in Marchese et al (2012).…”

Section: Parametersmentioning

confidence: 99%

Erratum: Studying the relationship between X-ray emission and accretion in AGNs using the XMM–Newton Bright Serendipitous Survey

Fanali¹,

Caccianiga²,

Severgnini³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We study the link between the X-ray emission in radio-quiet AGNs and the accretion rate on the central Supermassive Black Hole using a statistically well-defined and representative sample of 71 type 1 AGNs extracted from the XMM-Newton Bright Serendipitous Survey. We search and quantify the statistical correlations between some fundamental parameters that characterize the X-ray emission, i.e. the X-ray spectral slope, Γ, and the X-ray "loudness", and the accretion rate, both absolute (Ṁ ) and normalized to the Eddington luminosity (Eddington ratio, λ). We parametrize the Xray loudness using three different quantities: the bolometric correction, K bol , the twopoint spectral index α OX and the disk/corona luminosity ratio. We find that the X-ray spectral index depends on the normalized accretion rate while the "X-ray loudness" depends on both the normalized and the absolute accretion rate. The dependence on the Eddington ratio, in particular, is probably induced by the Γ − λ correlation. The two proxies usually adopted in the literature to quantify the X-ray loudness of an AGN, i.e. K bol and α OX , behave differently, with K bol being more sensitive to the Eddington ratio and α OX having a stronger dependence with the absolute accretion. The explanation of this result is likely related to the different sensitivity of the two parameters to the X-ray spectral index.

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Black-hole masses of type 1 AGN in theXMM-Newtonbright serendipitous survey

Cited by 8 publications

References 40 publications

Characterization of AGN from the XMM–Newton Slew Survey

Characterization of AGN from the XMM–Newton Slew Survey

The XMM-Newton Bright Survey sample of absorbed quasars: X-ray and accretion properties

Erratum: Studying the relationship between X-ray emission and accretion in AGNs using the XMM–Newton Bright Serendipitous Survey

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