The warm absorber in the radio-loud quasar 4C +74.26

Gesu, Laura Di; Costantini, E.

doi:10.1051/0004-6361/201628670

Cited by 9 publications

(13 citation statements)

References 67 publications

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“…The spectral emission components are attenuated by Galactic absorption, excess neutral absorption above the Galactic value, and a warm absorber (Ballantyne 2005;Di Gesu & Costantini 2016). Tombesi et al (2014) also detected signs of a highly ionized ultra-fast outflow in the XMM-Newton data of the source.…”

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confidence: 87%

The X-Ray Reflection Spectrum of the Radio-loud Quasar 4C 74.26

Lohfink

Fabian

Ballantyne

et al. 2017

ApJ

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The relativistic jets created by some active galactic nuclei are important agents of AGN feedback. In spite of this, our understanding of what produces these jets is still incomplete. X-ray observations, which can probe the processes operating in the central regions in the immediate vicinity of the supermassive black hole, the presumed jet launching point, are potentially particularly valuable in illuminating the jet formation process. Here, we present the hard X-ray NuSTAR observations of the radio-loud quasar 4C 74.26 in a joint analysis with quasi-simultaneous, soft X-ray Swift observations. Our spectral analysis reveals a high-energy cutoff of -+ 3551 keV and confirms the presence of ionized reflection in the source. From the average spectrum we detect that the accretion disk is mildly recessed, with an inner radius of R in =4-180 R g . However, no significant evolution of the inner radius is seen during the three months covered by our NuSTAR campaign. This lack of variation could mean that the jet formation in this radio-loud quasar differs from what is observed in broad-line radio galaxies.

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confidence: 87%

The X-Ray Reflection Spectrum of the Radio-loud Quasar 4C 74.26

Lohfink

Fabian

Ballantyne

et al. 2017

ApJ

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“…An in-depth analysis of the rich X-ray dataset for 4C +74.26, using the most recent observations with XMM-Newton, Chandra, and NuSTAR, has been reported by Di Gesu & Costantini (2016) and Lohfink et al (2017). Here we re-analyze the NuSTAR data for the target in the hard X-ray regime, focusing predominantly on the characterization of the main parameters of the underlying accretion disk, in particular its inner radius, in the context of the multi-wavelength correlation studies reported in the previous Section 3.2.…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

“…In addition, in order to account for the presence of a warm absorber in the source (e.g. Di Gesu & Costantini 2016), as well as the Galactic absorption, we combined RELXILL with the TBABS (Wilms et al 2000) and WARMABS models.…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

“…Guided by the previous studies reported in the literature, in the modelling we fixed the Galactic column density at N H, Gal = 2.31 × 10 21 cm −2 (see Di Gesu & Costantini 2016). For the single-zone warm absorber with the outflow velocity of 3600 km s −1 , we assumed the column density N H, wa = 3.5 × 10 21 cm −2 , the ionization parameter log ξ wa = 2.6, and the turbulent velocity v turb = 100 km s −1 (Di Gesu & Costantini 2016).…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

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Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

Bhatta

Stawarz

Markowitz

et al. 2018

ApJ

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Here we explore the disk-jet connection in the broad-line radio quasar 4C+74.26, utilizing the results of the multiwavelength monitoring of the source. The target is unique in that its radiative output at radio wavelengths is dominated by a moderately-beamed nuclear jet, at optical frequencies by the accretion disk, and in the hard X-ray range by the disk corona. Our analysis reveals a correlation (local and global significance of 96% and 98%, respectively) between the optical and radio bands, with the disk lagging behind the jet by 250 ± 42 days. We discuss the possible explanation for this, speculating that the observed disk and the jet flux changes are generated by magnetic fluctuations originating within the innermost parts of a truncated disk, and that the lag is related to a delayed radiative response of the disk when compared with the propagation timescale of magnetic perturbations along relativistic outflow. This scenario is supported by the re-analysis of the NuSTAR data, modelled in terms of a relativistic reflection from the disk illuminated by the coronal emission, which returns the inner disk radius R in /R ISCO = 35 +40 −16 . We discuss the global energetics in the system, arguing that while the accretion proceeds at the Eddington rate, with the accretion-related bolometric luminosity L bol ∼ 9 × 10 46 erg s −1 ∼ 0.2L Edd , the jet total kinetic energy L j ∼ 4 × 10 44 erg s −1 , inferred from the dynamical modelling of the giant radio lobes in the source, constitutes only a small fraction of the available accretion power.

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“…The intrinsic cold absorption is low and poorly constrained, and is fixed at N H = 0.19 × 10 22 cm −2 which is the averaged best-fit value from four observations. A warm absorber (with parameters fixed at the values derived by Di Gesu & Costantini 2016) are included. For relxill, we fix a = 0 , r in = 6 R g , r out = 400 R g , and we leave emissivity profile index, ξ and the iron abundance A F e free to vary, and the cosine Figure 11.…”

Section: The Usefulness Of Spectra Ratiosmentioning

confidence: 99%

On Measuring the Variation of High-energy Cutoff in Active Galactic Nuclei

Zhang

Wang

Zhu

2018

ApJ

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The variation in the high energy cut-off E c in active galactic nuclei uniquely probes the corona physics. In this work we show that the ratio of two NuSTAR spectra (in analogy to difference imaging technique widely used in astronomy) is uniquely useful in studying E c variations. The spectra ratio could directly illustrate potential E c variation between two spectra. By comparing with the ratio of two spectral fitting models, it also examines the reliability of the spectral-fitting measured E c variation. Assisted with this technique, we revisit the 5 AGNs in literature 3C 382, NGC 4593, NGC 5548 and Mrk 335) for which E c (kT e ) variations have been claimed with NuSTAR observations. We show the claimed E c variations appear inconsistent with the spectra ratios in three of them, thus need to be revised, demonstrating the striking usefulness of spectra ratio. We present thereby improved spectral fitting results and E c variations. We also report a new source with E c variations based on NuSTAR observations (radio galaxy 4C +74.26). We find the corona tends to be hotter when it brightens NGC 5548, Mrk 335 and 4C +74.27, show no evidence of significant E c variations. Meanwhile all 6 sources in this small sample appear softer-when-brighter. Changes in corona geometry are required to explain the observed hotter-when-brighter trends.

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The warm absorber in the radio-loud quasar 4C +74.26

Cited by 9 publications

References 67 publications

The X-Ray Reflection Spectrum of the Radio-loud Quasar 4C 74.26

The X-Ray Reflection Spectrum of the Radio-loud Quasar 4C 74.26

Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

On Measuring the Variation of High-energy Cutoff in Active Galactic Nuclei

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