Anatomy of the AGN in NGC 5548

Mao, Junjie; Kaastra, J. S.; Mehdipour, M.; Gu, Liyi; Costantini, E.; Kriss, G. A.; Bianchi, S.; Branduardi‐Raymont, G.; Behar, E.; Gesu, Laura Di; Ponti, G.; Petrucci, Pierre-Olivier; Ebrero, J.

doi:10.1051/0004-6361/201732162

Cited by 29 publications

(53 citation statements)

References 73 publications

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“…The two narrow emission components have different emission measure, ionization parameter, turbulence velocity, and emission covering factor. This is similar to our previous analysis for NGC 4151 (Seyfert 1.5, Armentrout et al 2007), Mrk 335 (Seyfert 1, Longinotti et al 2008), NGC 4051 (Seyfert 1, Nucita et al 2010), NGC 424 (Seyfert 2, Marinucci et al 2011), and NGC 5548 (Seyfert 1.5, Mao et al 2018). On the other hand, Guainazzi et al (2009) andWhewell et al (2015) model the X-ray narrow emission features in NGC 1365 (Seyfert 1.8) and NGC 5548 (Seyfert 1.5), respectively, with only one photoionized component.…”

Section: Discussionsupporting

confidence: 91%

“…Similar to the previous analysis on NGC 5548 (Mao et al 2018), the narrow emission features in NGC 3783 can be reasonably fitted with two PION components (details in Section 4.3). Whether the soft X-ray continuum is obscured or not, four free parameters of each PION emission component are allowed to vary, namely N H , log ξ, v mic and C em .…”

Section: X-ray Photoionized Emittersupporting

confidence: 72%

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Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

Mao

Mehdipour

Kaastra

et al. 2019

A&A

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Our Swift monitoring program triggered two joint XMM-Newton, NuSTAR and HST observations on 11 and 21 December 2016 targeting NGC 3783, as its soft X-ray continuum was heavily obscured. Consequently, emission features, including the O vii radiative recombination continuum, stand out above the diminished continuum. We focus on the photoionized emission features in the December 2016 RGS spectra, and compare them to the time-averaged RGS spectrum obtained in 2000-2001 when the continuum was unobscured. A two-phase photoionized plasma is required to account for the narrow emission features. These narrow emission features are weakly varying between 2000-2001 and December 2016. We also find a statistically significant broad emission component in the time-averaged RGS spectrum in 2000-2001. This broad emission component is significantly weaker in December 2016, suggesting that the obscurer is farther away than the X-ray broad-line region. In addition, by analyzing the archival high-resolution X-ray spectra, we find that nine photoionized absorption components with different ionization parameters and kinematics are required for the warm absorber in X-rays.

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Section: Discussionsupporting

confidence: 91%

Section: X-ray Photoionized Emittersupporting

confidence: 72%

Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

Mao

Mehdipour

Kaastra

et al. 2019

A&A

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“…These spectra are similar to those found in NGC 5548 and NGC 3783 (Kaastra et al 2014;Mao et al 2018Mao et al , 2019, where major obscuration events caused by outflowing absorption cause large flux drops at low energies and reveal the soft X-ray emission lines. In this case, however, the flux drop is intrinsic to the source, and we see the effect of the outflow acting on the emission lines.…”

Section: Discussionsupporting

confidence: 82%

The nuclear environment of the NLS1 Mrk 335: Obscuration of the X-ray line emission by a variable outflow

Parker

Longinotti

Schartel

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present XMM-Newton, NuSTAR, Swift and Hubble Space Telescope observations of the Narrow-line Seyfert 1 galaxy Mrk 335 in a protracted low state in 2018 and 2019. The X-ray flux is at the lowest level so far observed, and the extremely low continuum flux reveals a host of soft X-ray emission lines from photoionised gas. The simultaneous UV flux drop suggests that the variability is intrinsic to the source, and we confirm this with broad-band X-ray spectroscopy. The dominance of the soft X-ray lines at low energies and distant reflection at high energies, is therefore due to the respective emission regions being located far enough from the X-ray source that they have not yet seen the flux drop. Between the two XMM-Newton spectra, taken 6 months apart, the emission line ratio in the Ovii triplet changes drastically. We attribute this change to a drop in the ionisation of intervening warm absorption, which means that the absorber must cover a large fraction of the line emitting region, and extend much further from the black hole than previously assumed. The HST spectrum, taken in 2018, shows that new absorption features have appeared on the blue wings of Ciii * , Lyα, Nv, Siiv and Civ, likely due to absorbing gas cooling in response to the low flux state.

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“…The 13 BLS1s that required warm absorbers were Ark 120 (Nardini et al 2011;Porquet et al 2018), H 0557-385 (Longinotti 2009), PG 0844+349 (Pounds & Page 2004), NGC 3516 (Huerta 2014;Costantini et al 2000;Mehdipour et al 2010), PG 1114+445 (Ashton et al 2004), NGC 3783 (Blustin et al 2002), Ark 374, IC 4329A (Steenbrugge K. C. et al 2005), NGC 5548 (Mao et al 2018), Mrk 1383, Mrk 876 (Porquet et al 2004), Mrk 304 (Piconcelli et al 2004;Brinkmann et al 2004), and Fairall 1146.…”

Section: Appendix A: Additional Spectral Resultsmentioning

confidence: 99%

The soft X-ray excess: NLS1s versus BLS1s

Gliozzi

Williams

2019

Monthly Notices of the Royal Astronomical Society

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The soft X-ray excess -the excess of X-rays below 2 keV with respect to the extrapolation of the hard X-ray spectral continuum model -is a very common feature among type 1 active galactic nuclei (AGN); yet the nature of the soft X-ray excess is still poorly understood and hotly debated. To shed some light on this issue, we have measured in a model-independent way the soft excess strength in a flux-limited sample of broad-line and narrow-line Seyfert 1 galaxies (BLS1s and NLS1s) that are matched in X-ray luminosity but different in terms of the black hole mass and the accretion rate values, with NLS1s being characterized by smaller M BH and larger m values. Our analysis, in agreement with previous studies carried out with different AGN samples, indicates that: 1) a soft excess is ubiquitously detected in both BLS1s and NLS1s; 2) the strength of the soft excess is significantly larger in the NLS1 sample, compared to the BLS1 sample; 3) combining the two samples, the strength of the soft excess appears to positively correlate with the photon index as well as with the accretion rate, whereas there is no correlation with the black hole mass. Importantly, our work also reveals the lack of an anticorrelation between the soft excess strength and the luminosity of the primary X-ray component, predicted by the absorption and reflection scenarios. Our findings suggest that the soft excess is consistent with being produced by a warm Comptonization component. Larger, more complete samples of NLS1s and BLS1s are needed to confirm these conclusions.

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Anatomy of the AGN in NGC 5548

Cited by 29 publications

References 73 publications

Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

The nuclear environment of the NLS1 Mrk 335: Obscuration of the X-ray line emission by a variable outflow

The soft X-ray excess: NLS1s versus BLS1s

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