Suzaku Observations of Moderately Obscured (Compton-Thin) Active Galactic Nuclei Selected by Swift/Bat Hard X-Ray Survey

Kawamuro, T.; Ueda, Yoshihiro; Tazaki, Fumie; Ricci, Cláudio; Terashima, Yuichi

doi:10.3847/0067-0049/225/1/14

Cited by 62 publications

(74 citation statements)

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“…The Suzaku data of 3 objects are published here for the first time. We fit the Suzaku and Swift spectra with models utilizing an analytic reflection code and those utilizing (Kawamuro et al 2016a) suggests that the properties of these CTAGNs can be understood as a smooth extension from Compton-thin AGNs with heavier obscuration; we find no evidence that the bulk of the population of hard X-ray selected CTAGN is different from less obscured objects. …”

mentioning

confidence: 88%

“…First, we apply two analytic models (Baseline1 and Baseline2) often adopted to represent the broadband spectra of obscured AGNs (e.g., Schurch et al 2002;Matt et al 2004;Bianchi et al 2005;Piconcelli et al 2007;Ueda et al 2007;Comastri et al 2010;Kawamuro et al 2016a;Tanimoto et al 2016). The models are basically composed of an absorbed direct component, an unabsorbed scattered component, a reflection component and narrow Fe K emission lines.…”

Section: Baseline Modelsmentioning

confidence: 99%

“…The intrinsic continuum is modeled by a power law (zpowerlw) with an exponential cutoff (zhighect). In the Baseline1, we only consider photoelectric absorption (zphabs) as is the case in Kawamuro et al (2016a) for Compton thin AGNs. In the Baseline2 model, we also consider Compton scattering out of the line of sight (cabs) whose hydrogen column density (N Dir H ) is linked to that of zphabs.…”

Section: Baseline Modelsmentioning

confidence: 99%

“…The combination of Suzaku and Swift is proved to be very powerful for studying the broadband spectra of local AGNs (Ueda et al 2007;Eguchi et al 2009Eguchi et al , 2011Winter et al 2009b;Tazaki et al 2011Tazaki et al , 2013Gandhi et al 2013Gandhi et al , 2015Kawamuro et al 2013Kawamuro et al , 2016a. Recently, NuSTAR have started to observe nearby CTAGNs (e.g., Puccetti et al 2014;Koss et al 2015;Rivers et al 2015;Guainazzi et al 2016) covering the 4-80 keV.…”

Section: Introductionmentioning

confidence: 99%

“…This paper presents a summary of uniform spectral analyses of local CTAGNs observed with Suzaku and Swift, following Kawamuro et al (2016a) for Comptonthin (22 ≤ log N H /cm −2 < 24) AGNs. Section 2 describes the sample selection and data reduction of the Suzaku data.…”

Section: Introductionmentioning

confidence: 99%

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Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Tanimoto

Ueda

Kawamuro

et al. 2018

ApJ

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We present a uniform broadband X-ray (0.5-100.0 keV) spectral analysis of 12 Swift/Burst Alert Telescope (BAT) selected Compton-thick (log N H /cm −2 ≥ 24) Active Galactic Nuclei (CTAGNs) observed with Suzaku. The Suzaku data of 3 objects are published here for the first time. We fit the Suzaku and Swift spectra with models utilizing an analytic reflection code and those utilizing (Kawamuro et al. 2016a) suggests that the properties of these CTAGNs can be understood as a smooth extension from Compton-thin AGNs with heavier obscuration; we find no evidence that the bulk of the population of hard X-ray selected CTAGN is different from less obscured objects.

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confidence: 88%

Section: Baseline Modelsmentioning

confidence: 99%

Section: Baseline Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Tanimoto

Ueda

Kawamuro

et al. 2018

ApJ

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Structure of an Absorbing Medium in the Nucleus of the Galaxy Mrk 417 Based on NuSTAR and Swift/Bat Data

Kompaniiets

Vasylenko

2020

Astrophysics

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The close environments of accreting massive black holes are shaped by radiative feedback

Ricci

Trakhtenbrot

Koss

et al. 2017

Nature

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309

375

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The large majority of the accreting supermassive black holes in the Universe are obscured by large columns of gas and dust [1][2][3] . The location and evolution of this obscuring material have been the subject of intense research in the past decades 4,5 , and are still highly debated. A decrease in the covering factor of the circumnuclear material with increasing accretion rates has been found by studies carried out across the electromagnetic spectrum 1,[6][7][8] . The origin of this trend has been suggested to be driven either by the increase in the inner radius of the obscuring material with incident luminosity due to the sublimation of dust 9 ; by the gravitational potential of the black hole 10 ; by radiative feedback [11][12][13][14] ; or by the interplay between outflows and inflows 15 . However, the lack of a large, unbiased and complete sample of accreting black holes, with reliable information on gas column density, luminosity and mass, has left the main physical mechanism regulating obscuration unclear. Using a systematic multi-wavelength survey of hard X-ray-selected black holes, here we show that radiation pressure on dusty gas is indeed the main physical mechanism regulating the distribution of the circumnuclear material. Our results imply that the bulk of the obscuring dust and gas in these objects is located within the sphere of influence of the black hole (i.e., a few to tens of parsecs), and that it can be swept away even at low radiative output rates. The main physical driver of the differences between obscured and unobscured accreting black holes is therefore their mass-normalized accretion rate.Our group has carried out a large multi-wavelength study of the 836 accreting supermassive black holes (i.e., active galactic nuclei or AGN) detected by the all-sky hard X-ray (14-195 keV) Swift Burst Alert Telescope survey 16, 17 (see §1 of the Methods). The energy range covered by Swift/BAT makes it ideal for studying the characteristics and evolu- Figure 1: Relation between the fraction of obscured AGN and the Eddington ratio. The fraction of obscured Compton-thin [10 22 ≤ (NH/cm −2 ) < 10 24 ] sources shown as a function of the Eddington ratio λ Edd (i.e. the AGN luminosity normalized by the maximum value for solar-metalicity, fully-ionized, dust-free gas in a spherical geometry) for our hard X-ray selected sample in the 10 −5.6 ≤ λ Edd < 1 range. The values are normalized to unity in the 10 20 ≤ (NH/cm −2 ) < 10 24 interval. The shaded area represents the 16th and 84th quantiles of a binomial distribution 20 . The vertical red dashed line represents the effective Eddington limit for a dusty gas 14 with NH = 10 22 cm −2 (see §2). The figure shows that the covering factor of the obscuring material with 10 22 ≤ (NH/cm −2 ) < 10 24 decreases sharply around the Eddington limit for dusty gas, highlighting the fact that radiation pressure strongly affects obscuration in AGN.tion of the absorbing material surrounding the AGN, being unaffected by obscuration up to column densities NH ≃ 10 24 cm −2 . More...

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Suzaku Observations of Moderately Obscured (Compton-Thin) Active Galactic Nuclei Selected by Swift/Bat Hard X-Ray Survey

Cited by 62 publications

References 119 publications

Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Structure of an Absorbing Medium in the Nucleus of the Galaxy Mrk 417 Based on NuSTAR and Swift/Bat Data

The close environments of accreting massive black holes are shaped by radiative feedback

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