scholarly journals X-ray analysis of the accreting supermassive black hole in the radio galaxy PKS 2251+11

2019 ◽  
Vol 625 ◽  
pp. A26
Author(s):  
S. Ronchini ◽  
F. Tombesi ◽  
F. Vagnetti ◽  
F. Panessa ◽  
G. Bruni
Keyword(s):  
Black Hole ◽  
Power Law ◽  
Radio Galaxy ◽  
Timing Analysis ◽  
Seyfert Galaxies ◽  
Radio Galaxies ◽  
Broad Line ◽  
X Ray ◽  
Supermassive Black Hole ◽  
Link Type

Context. We have investigated the dichotomy between jetted and non-jetted active galactic nuclei (AGNs), focusing on the fundamental differences of these two classes in the accretion physics onto the central supermassive black hole (SMBH). We tested the validity of the unification model of AGNs through the characterization of the mutual interaction between accreting and outflowing matter in radio galaxies. Aims. Our aim is to study and constrain the structure, kinematics and physical state of the nuclear environment in the broad line radio galaxy (BLRG) PKS 2251+11. The high X-ray luminosity and the relative proximity make such AGN an ideal candidate for a detailed analysis of the accretion regions in radio galaxies. The investigation will help to shed light on the analogies and differences between the BLRGs and the larger class of radio-quiet Seyfert galaxies and hence on the processes that trigger the launch of a relativistic jet. Methods. We performed a spectral and timing analysis of a ∼64 ks observation of PKS 2251+11 in the X-ray band with XMM-Newton. We modeled the spectrum considering an absorbed power law superimposed to a reflection component. We performed a time-resolved spectral analysis to search for variability of the X-ray flux and of the individual spectral components. Results. We find that the power law has a photon index Γ = 1.8 ± 0.1, absorbed by an ionized partial covering medium with a column density NH = (10.1 ± 0.8) × 1023 cm−2, a ionization parameter log ξ = 1.3 ± 0.1 erg s−1 cm and a covering factor f ≃ 90%. Considering a density of the absorber typical of the broad line region (BLR), its distance from the central SMBH is of the order of r ∼ 0.1 pc. An Fe Kα emission line is found at 6.4 keV, whose intensity shows variability on timescales of hours. We derive that the reflecting material is located at a distance r ≳ 600rs, where rs is the Schwarzschild radius. Conclusions. Concerning the X-ray properties, we found that PKS 2251+11 does not differ significantly from the non-jetted AGNs, confirming the validity of the unified model in describing the inner regions around the central SMBH, but the lack of information regarding the state of the very innermost disk and SMBH spin still leaves unconstrained the origin of the jet.

scholarly journals Measuring the supermassive black hole parameters with space missions

2006 ◽  
Vol 2 (S238) ◽  
pp. 475-476
Author(s):  
Alexander F. Zakharov
Keyword(s):  
Black Hole ◽  
Spectral Line ◽  
Accretion Disks ◽  
Seyfert Galaxies ◽  
Emission Lines ◽  
X Ray ◽  
Line Shapes ◽  
Supermassive Black Hole ◽  
Broad Emission ◽  
Different Types

AbstractRecent X-ray observations of microquasars and Seyfert galaxies reveal broad emission lines in their spectra, which can arise in the innermost parts of accretion disks. Recently Müller & Camenzind (2004) classified different types of spectral line shapes and described their origin. Zakharov (2006b) clarified their conclusions about an origin of doubled peaked and double horned line shapes in the framework of a radiating annulus model and discussed s possibility to evaluate black hole parameters analyzing spectral line shapes.

scholarly journals Incoherent fast variability of X-ray obscurers

2020 ◽  
Vol 634 ◽  
pp. A65 ◽  
Author(s):  
B. De Marco ◽  
T. P. Adhikari ◽  
G. Ponti ◽  
S. Bianchi ◽  
G. A. Kriss ◽  
...  
Keyword(s):  
Column Density ◽  
Timing Analysis ◽  
Seyfert Galaxies ◽  
Fast Response ◽  
Broad Line ◽  
X Ray ◽  
Line Region ◽  
Timing Properties ◽  
The Impact ◽  
High Column

Context. Obscuration events caused by outflowing clumps or streams of high column density and low ionised gas, shown to absorb the X-ray continuum heavily, have been witnessed across a number of Seyfert galaxies. Aims. We report on the X-ray spectral-timing analysis of the December 2016 obscuration event in NGC 3783, which was aimed at probing variability of the X-ray obscurer on the shortest possible timescales. The main goals of this study are to obtain independent constraints on the density and, ultimately on the distance of the obscuring gas, as well as to characterise the impact of variable obscuration on the observed X-ray spectral-timing characteristics of Seyfert galaxies. Methods. We carried out a comparative analysis of NGC 3783 during unobscured (using archival 2000–2001 XMM-Newton data) and obscured states (using XMM-Newton and NuSTAR data from the 2016 observational campaign). The analysed timescales range between ten hours and about one hour. This study was then generalised to discuss the signatures of variable obscuration in the X-ray spectral-timing characteristics of Seyfert galaxies as a function of the physical properties of the obscuring gas. Results. The X-ray obscurer in NGC 3783 is found to vary on timescales between about one hour to ten hours. This variability is incoherent with respect to the variations of the X-ray continuum. A fast response (on timescales shorter than about 1.5 ks) of the ionisation state of the obscuring gas to the short timescale variability of the primary X-ray continuum provides a satisfactory interpretation of all the observed X-ray spectral-timing properties. This study enabled us to put independent constraints on the density and location of the obscuring gas. We found the gas to have a density of ne >  7.1 × 107 cm−3, which is consistent with a location in the broad line region.

scholarly journals UV and X-Ray Variability of 3C 390.3

1997 ◽  
Vol 159 ◽  
pp. 155-158
Author(s):  
Ting-gui Wang ◽  
Willem Wamsteker ◽  
Fu.-Zhen Cheng
Keyword(s):  
Power Law ◽  
Radio Galaxy ◽  
Line Strength ◽  
Broad Line ◽  
X Ray ◽  
Blue Wing ◽  
Highly Correlated ◽  
Single Power ◽  
The Continuum ◽  
Red Wing

AbstractWe present the results of an analysis of the UV and X-ray variability of the broad-line radio galaxy 3C 390.3 over 15 years. The UV continuum of 3C 390.3 showed large variations with amplitudes of up to a factor of 10. The variations of C IV and Lyα are highly correlated with the UV continuum, and are delayed with respect to the continuum variations by 65-120 days with the red wing of both C IV and Lyα leading the blue wing, implying that the C IV and Lyα-emitting gas is infalling towards the center. The C IV/Lyα ratio is positively correlated with both the continuum flux and UV line strength. The overall UV/optical to X-ray spectrum can be described by a single power law with αuvx = 0.90. The behavior of C IV/Lyα variations might be related to this hard ionizing continuum in 3C 390.3.

scholarly journals Multi-Zone Warm and Cold Clumpy Absorbers in Three Seyfert Galaxies

2009 ◽  
Vol 5 (S267) ◽  
pp. 404-404
Author(s):  
Claudio Ricci ◽  
Volker Beckmann ◽  
Marc Audard ◽  
T. J.-L. Courvoisier
Keyword(s):  
Black Hole ◽  
Power Law ◽  
Thermal Emission ◽  
Accretion Rate ◽  
Seyfert Galaxies ◽  
High Energy ◽  
X Ray ◽  
The Past ◽  
High Energy Tail ◽  
Open Issue

A soft (E≲2 keV) excess over the power-law component dominant at higher energies has been found in the X-ray spectra of many Seyfert galaxies. The origin of the soft excess is still an open issue. In the past it was often associated with the high-energy tail of the thermal emission of the accretion disk, but it has been shown recently that the temperature of the disk should be constant (0.1–0.2 keV), regardless of the mass and luminosity of the AGN (Gierlinski & Done 2004). This result implies that some other mechanism is at work, as the temperature of the disk should depend on both the mass of the black hole and the accretion rate.

scholarly journals A bright off-nuclear X-ray source: a type IIn supernova, a bright ULX or a recoiling supermassive black hole in CXO J122518.6+144545

2010 ◽  
Vol 407 (1) ◽  
pp. 645-650 ◽  
Author(s):  
P. G. Jonker ◽  
M. A. P. Torres ◽  
A. C. Fabian ◽  
M. Heida ◽  
G. Miniutti ◽  
...  
Keyword(s):  
Black Hole ◽  
X Ray ◽  
Supermassive Black Hole

scholarly journals Broadband X-Ray Observation of Broad-line Radio Galaxy 3C 109

2020 ◽  
Vol 897 (1) ◽  
pp. 47
Author(s):  
Sulov Chalise ◽  
Anne M. Lohfink ◽  
Erin Kara ◽  
Andrew C. Fabian
Keyword(s):  
Radio Galaxy ◽  
Broad Line ◽  
X Ray

A Photoionization Method for Estimating Black Hole Masses in Quasars

2018 ◽  
Vol 14 (S342) ◽  
pp. 270-271
Author(s):  
C. Alenka Negrete ◽  
Deborah Dultzin ◽  
Paola Marziani ◽  
Jack W. Sulentic ◽  
M. L. Martínez-Aldama
Keyword(s):  
Black Hole ◽  
High Redshift ◽  
Broad Line ◽  
Reverberation Mapping ◽  
Physical Conditions ◽  
Broad Line Region ◽  
Supermassive Black Hole ◽  
Line Region ◽  
Black Hole Masses

AbstractWe present a method that uses photoionization codes (CLOUDY) to estimate the supermassive black hole masses (MBH) for quasars at low and high redshift. This method is based on the determination of the physical conditions of the broad line region (BLR) using observational diagnostic diagrams from line ratios in the UV. We also considered that the density and metallicity of the BLR in quasars at high z could be different from those at the nearby Universe. The computed black hole masses obtained using this method are in agreement with those derived from the method of reverberation mapping.

scholarly journals Discovery of a New X-ray Transient in Scorpius GRO J1655-40 ≡ X-ray Nova Scorpii 1994

1996 ◽  
Vol 165 ◽  
pp. 363-367
Author(s):  
W.S. Paciesas ◽  
S.N. Zhang ◽  
B.C. Rubin ◽  
B.A. Harmon ◽  
C.A. Wilson ◽  
...  
Keyword(s):  
Black Hole ◽  
High Resolution ◽  
Power Law ◽  
Radio Observations ◽  
X Ray ◽  
Black Hole Candidate ◽  
Radio Jets ◽  
Transient Source ◽  
Galactic Source ◽  
Photon Index

A bright transient X-ray source, GRO J1655-40 (X-ray Nova Scorpii 1994) was discovered with BATSE (the Burst and Transient Source Experiment) in late July 1994. More recently, the source also became a strong radio emitter, its rise in the radio being approximately anti-correlated with a decline in the hard X-ray intensity. High-resolution radio observations subsequent to this symposium showed evidence for superluminally expanding jets. Since the hard X-ray emission extends to at least 200 keV and we find no evidence of pulsations, we tentatively classify the source as a black-hole candidate. However, its hard X-ray spectrum is unusually steep (power-law photon index α ≃ −3) relative to most other black-hole candidates. In this regard, it resembles GRS 1915+105, the first galactic source to show superluminal radio jets.

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