Suzaku Discovery of a Hard Component Varying Independently of the Power-Law Emission in MCG −6–30–15

Noda, Hirofumi; Makishima, Kazuo; Uehara, Yuuichi; Yamada, S.; Nakazawa, K.

doi:10.1093/pasj/63.2.449

Cited by 30 publications

(33 citation statements)

References 24 publications

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“…Similarly, the middle vs. hard CCP, shown in figure 2(b), represents generally positive correlations, but the data scatter is too large for a linear fit. The scatter suggests the presence of a variable hard component independent of the dominant power-law, as reported in MCG-6-30-15 (Noda et al 2011). This issue will be studied elsewhere.…”

Section: Timing Analysismentioning

confidence: 55%

“…Because of its genuine broad-band sensitivity, Suzaku (Mitsuda et al 2007) obviously provides the best available mean to search AGN spectra for the expected MZC effects. Given these, we studied the archival Suzaku data of the Seyfert galaxy MCG-6-30-15, and successfully detected a hard X-ray component that varies independently of the dominant PL continuum (Noda et al 2011). This new component can be interpreted as a thermal Compton emission with a relatively high optical depth.…”

Section: Introductionmentioning

confidence: 99%

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Suzaku Studies of Wide-Band Spectral Variability of the Bright Type I Seyfert Galaxy Markarian 509

Noda

Makishima

Yamada

et al. 2011

Publications of the Astronomical Society of Japan

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The Type I Seyfert galaxy Markarian 509 was observed with Suzaku in 2010 November, for a gross time span of 2.2 days. Timing and spectral properties of the 0.5-45 keV X-rays, detected with the XIS and HXD, consistently revealed the presence of a soft spectral component that remained constant while the total Xray intensity varied by ±10%. This stable soft component, found in the 0.5-3.0 keV range, was interpreted as a result of thermal Comptonization in a corona with a temperature of ∼ 0.5 keV and an optical depth of ∼ 18. The time-avearged 0.5-45 keV Suzaku spectrum was reproduced successfully, as a combination of this thermal Comptonization component, a harder power-law of photon index ∼ 1.8, moderate reflection, and an iron K-emission line. By analyzing four archival Suzaku datasets of the same object obtained in 2006, the thermal Comptonization component, which was stable during the 2.2 day pointing in 2010, was found to vary on time scales of a few weeks, independently of the power-law component. Implications of these results are discussed in terms of the "multi-zone Comptonization" view, obtained with Suzaku from the black hole binary Cygnus X-1.

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Section: Timing Analysismentioning

confidence: 55%

Section: Introductionmentioning

confidence: 99%

Suzaku Studies of Wide-Band Spectral Variability of the Bright Type I Seyfert Galaxy Markarian 509

Noda

Makishima

Yamada

et al. 2011

Publications of the Astronomical Society of Japan

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“…Moreover, we require that the intensity of the Kβ has to be 0. Cerruti et al (2011), andNoda et al (2011) suggest that the inner accretion disc in Mrk 509 might be highly ionised, and thus the ionised emission of the Fe K complex might be associated to a relativistic ionised reflection component produced in the inner disc. To test this hypothesis, we substitute the two narrow lines (Fe xxv and Fe xxvi) with one broad ionised line (model 4 in Table 1) with a relativistic profile (disc line profile for a Schwarzschild black hole; diskline model in Xspec).…”

Section: The Mean Spectrummentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Ponti

Cappi

Costantini

et al. 2012

A&A

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Context. We report on a detailed study of the Fe K emission/absorption complex in the nearby, bright Seyfert 1 galaxy Mrk 509. The study is part of an extensive XMM-Newton monitoring consisting of 10 pointings (∼60 ks each) about once every 4 days, and includes a reanalysis of previous XMM-Newton and Chandra observations. Aims. We aim at understanding the origin and location of the Fe K emission and absorption regions. Methods. We combine the results of time-resolved spectral analysis on both short and long time-scales including model-independent rms spectra. Results. Mrk 509 shows a clear (EW = 58±4 eV) neutral Fe Kα emission line that can be decomposed into a narrow (σ = 0.027 keV) component (found in the Chandra HETG data) plus a resolved (σ = 0.22 keV) component. We find the first successful measurement of a linear correlation between the intensity of the resolved line component and the 3-10 keV flux variations on time scales of years down to a few days. The Fe Kα reverberates the hard X-ray continuum without any measurable lag, suggesting that the region producing the resolved Fe Kα component is located within a few light days to a week (r < ∼ 10 3 r g ) from the black hole (BH). The lack of a redshifted wing in the line poses a lower limit of ≥40 r g for its distance from the BH. The Fe Kα could thus be emitted from the inner regions of the BLR, i.e. within the ∼80 light days indicated by the Hβ line measurements. In addition to these two neutral Fe Kα components, we confirm the detection of weak (EW ∼ 8-20 eV) ionised Fe K emission. This ionised line can be modelled with either a blend of two narrow Fe xxv and Fe xxvi emission lines (possibly produced by scattering from distant material) or with a single relativistic line produced, in an ionised disc, down to a few r g from the BH. In the latter interpretation, the presence of an ionised standard α-disc, down to a few r g , is consistent with the source high Eddington ratio. Finally, we observe a weakening/disappearing of the mediumand high-velocity high-ionisation Fe K wind features found in previous XMM-Newton observations. Conclusions. This campaign has made the first reverberation measurement of the resolved component of the Fe Kα line possible, from which we can infer a location for the bulk of its emission at a distance of r ∼ 40-1000 r g from the BH.

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“…On the other hand, a steep primary continuum, which can be explained by a PL model with Γ  2.3, is dominant in X-rays from highly accreting AGNs such as narrow-line type 1 Seyferts (e.g., Laor et al 1994;Boller et al 1996). Recently, Noda et al (2011aNoda et al ( , 2013aNoda et al ( , 2014 revealed that these primary continua,both flat and steep, are simultaneously present in the X-ray emission from multiple Seyfert galaxies. The presence of these different primary X-rays may represent the presence of several distinct types of coronae with different electron temperatures and optical depths.…”

Section: Introductionmentioning

confidence: 99%

X-Ray and Optical Correlation of Type I Seyfert NGC 3516 Studied With Suzaku and Japanese Ground-Based Telescopes

Noda

Minezaki

Watanabe

et al. 2016

ApJ

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From 2013 April to 2014 April, we performed X-ray and optical simultaneous monitoring of the type 1.5 Seyfert galaxy NGC3516. We employed Suzaku and five Japanese ground-based telescopes-the Pirka, Kiso Schmidt, Nayuta, MITSuME, and the Kanata telescopes. The Suzaku observations were conducted seven times with various intervals ranging from days or weeks to months, with an exposure of ∼50 ks each. The optical B-band observations not only covered those of Suzaku almost simultaneously, but also followed the source as frequently as possible. As a result, NGC3516 was found in its faint phase with a 2-10 keV flux of 0.21-2.70×10 −11 erg s. The 2-45 keV X-ray spectra were composed of a dominant variable hard power-law (PL) continuum with a photon index of ∼1.7 and a nonrelativistic reflection component with a prominent Fe-Kα emission line. Producing the B-band light curve by differential image photometry, we found that the B-band flux changed by ∼2.7×10 −11 erg s, which is comparable to the X-ray variation, and we detected a significant flux correlation between the hard PL component in X-rays and the B-band radiation, for the first time in NGC3516. By examining their correlation, we found that the X-ray flux preceded that in the B band by -+ 2.0 0.6 0.7 days (1σ error). Although this result supports the X-ray reprocessing model, the derived lag is too large to be explained by the standard view, which assumes a "lamppost"-type X-ray illuminator located near a standard accretion disk. Our results are better explained by assuming a hot accretion flow and a truncated disk.

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Suzaku Discovery of a Hard Component Varying Independently of the Power-Law Emission in MCG −6–30–15

Cited by 30 publications

References 24 publications

Suzaku Studies of Wide-Band Spectral Variability of the Bright Type I Seyfert Galaxy Markarian 509

Suzaku Studies of Wide-Band Spectral Variability of the Bright Type I Seyfert Galaxy Markarian 509

Multiwavelength campaign on Mrk 509

X-Ray and Optical Correlation of Type I Seyfert NGC 3516 Studied With Suzaku and Japanese Ground-Based Telescopes

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