Discovery of Hard X-Ray Delays in the X-Ray Emission of the Seyfert 1 Galaxy Markarian 110: Possible Evidence of Comptonization

Dasgupta, Surajit; Rao, A. R.

doi:10.1086/509117

Cited by 22 publications

(22 citation statements)

References 33 publications

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“…This result is in very good agreement with the work of Dasgupta & Rao (2006), who did a detailed analysis of the variability during the same XMM-Newton observation. They reported the discovery of X-ray delays ranging from a few minutes to an hour between the light curves in seven selected spectral intervals (0.2-0.3, 0.3-0.42, 0.42-0.58, 0.58-0.8, 0.8-1.2, 1.2-2, and 2-12 keV).…”

Section: Variabilitysupporting

confidence: 91%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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Aims. We seek a comprehensive analysis of all the information provided by the XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810, CTS A08.12, and Mrk 110, including the UV range, to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra by taking advantage of the spectral range of these cameras. The high-resolution RGS spectra were analyzed to characterize the absorbing and emission line features that arise in the spectra of the sources. All these data, complemented by information in the UV, are analyzed jointly in order to achieve a consistent characterization of the observed features in each object. Results. The continuum emission of the sources can be characterized either by a combination of a power law and a black body for the weakest objects or by two power law components for the brightest ones. The continuum is not absorbed by neutral or ionized material in the line of sight to any of these sources. In all of them we have identified a narrow Fe-Kα line at 6.4 keV. In ESO 359-G19 we also find an Fexxvi line at about 7 keV. In the soft X-rays band, we identify only one Ovii line in the spectra of HE 1143-1810 and CTS A08.12, and two Ovii-Heα triplets and a narrow Oviii-Lyα emission line in Mrk 110. Conclusions. Not detecting warm material in the line of sight to the low state objects is due to intrinsically weaker or absent absorption in the line of sight and not to a low signal-to-noise ratio in the data. Besides this, the absence of clear emission lines cannot be fully attributed to dilution of those lines by a strong continuum.

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Section: Variabilitysupporting

confidence: 91%

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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“…Our results suggests that the time lag increases with the mean energy of observed photons. A similar dependence of lag on energy has been seen in other AGNs as well and the observed lag is interpreted as Compton scattering time scale (Dasgupta & Rao 2006). If this lag is due to the process of Comptonization, we can get some useful constraints on the geometry of the inner accretion disk.…”

Section: Energy Dependent Lag From Comptonizationsupporting

confidence: 72%

“…2. A Gaussian model was used to evaluate the time lags and errors are estimated using the criteria ∆χ 2 =4 (see Dasgupta & Rao 2006) (see Table 1). The mean energy is given in Table 1 is the weighted mean for all the photons in each energy band.…”

Section: Energy Dependent Lagmentioning

confidence: 99%

Energy-Dependent Time Lags in the Seyfert 1 Galaxy NGC 4593

Sriram

Agrawal

Rao

2009

ApJ

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We investigate the energy-time lag dependence of the source NGC 4593 using XMM-Newton/EPIC-pn data. We found that the time lag dependency is linear in nature with respect to the logarithm of different energy bands. We also investigate the frequency dependent time lags and identify that at some frequency range (5 × 10 −5 Hz -2 × 10 −4 Hz) the X-ray emission is highly coherent, mildly frequency dependent and very strongly energy dependent. These observations can be explained in the frame work of the thermal Comptonization process and they indicate a truncated accretion disk very close to the black hole. We discuss the plausible spectral state to explain the phenomenon and conclude that the observed properties bear a close resemblance to the intermediate state or the steep power-law state, found in galactic black hole sources.

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“…XMM-Newton Seyfert sample. Column (1): common name of object; Columns (2)-(4): position and redshift from NED; Column (5): Galactic absorption column from Elvis, Wilkes & Lockman (1989), Stark et al (1992) or Dickey & Lockman (1990); Column (6): references for previously published XMM-Newton spectra: (1) ; (2) Matt et al (2006); (3) Immler et al (2003) (4) Schurch et al (2006); (5) Dasgupta & Rao (2006); (6) Dewangan, Griffiths & Schurch (2003); (7) Balestra, ; (8) Awaki et al (2006); (9) Braito et al (2007); (10) Turner et al (2002); (11) Bianchi et al (2004); (12) Iwasawa et al (2004); (13) Turner et al (2005); (14) Blustin et al (2002); (15) Reeves et al (2004); (16) Uttley et al (2004); (17) Ogle et al (2004); (18) Pounds et al (2004); (19) Ponti et al (2006); (20) Schurch et al (2003); (21) Schurch et al (2004) (22) Mason et al (2003); (23) Pounds et al (2003c); (24) Turner et al (2006); (25) Miller et al (2006); (26) Vaughan et al (2005); (27) Steenbrugge et al (2003); (28) Reynolds et al (2004a); (29) Wilms et al (2001); (30) Fabian et al (2002); (31) ; (32) Gondoin et al (2001); (33) Matt et al (2001); (34) Dewangan & Griffiths (2005); (35) Pounds et al (2003b); (36) Pounds et al (2001); (37) Dadina...…”

Section: Sample Selectionmentioning

confidence: 99%

An XMM-Newton survey of broad iron lines in Seyfert galaxies

Nandra

O’Neill

George

et al. 2007

Monthly Notices of the Royal Astronomical Society

595

747

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We present an analysis of the X-ray spectra of a sample of 37 observations of 26 Seyfert galaxies observed by XMM-Newton in order to characterize their iron K emission. All objects show evidence for iron line emission in the 6-7 keV band. A narrow core at 6.4 keV is seen almost universally in the spectra, and we model this using a neutral Compton reflection component, assumed to be associated with distant, optically thick material such as the molecular torus. Once this, and absorption by a zone of ionized gas in the line-of-sight is accounted for, less than half of the sample observations show an acceptable fit. Approximately 2/3 of the sample shows evidence for further, broadened emission in the iron K-band. When modeled with a Gaussian, the inferred energy is close to that expected for neutral iron, with a slight redshift, with an average velocity width of ~0.1c. The mean parameters are consistent with previous ASCA results and support the idea that the broad components can be associated with the accretion disk. Before proceeding to that conclusion, we test an alternative model comprising a blend of 3-4 narrow, unshifted emission lines (including the 6.4 keV core), together with 1-2 zones of highly ionized gas in the line-of-sight. Around 1/3 of the objects are not adequately fit by this model, and in general better fits are obtained with a relativistic disk line model, which has fewer free parameters. Nonetheless we find that absorption by ionized gas affects the spectrum above 2.5 keV in approximately half the sample. There is evidence for multiple ionized zones in at least 3 objects, but in all those cases a blurred reflector is required in addition to the complex absorption. (truncated)Comment: 36 pages, 13 figures, accepted for publication in MNRA

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Discovery of Hard X-Ray Delays in the X-Ray Emission of the Seyfert 1 Galaxy Markarian 110: Possible Evidence of Comptonization

Cited by 22 publications

References 33 publications

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Energy-Dependent Time Lags in the Seyfert 1 Galaxy NGC 4593

An XMM-Newton survey of broad iron lines in Seyfert galaxies

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