Simultaneous<i>XMM-Newton</i>and HST-COS observation of 1H 0419–577

Gesu, Laura Di; Costantini, E.; Piconcelli, E.; Ebrero, J.; Mehdipour, M.; Kaastra, J. S.

doi:10.1051/0004-6361/201322916

Cited by 20 publications

(25 citation statements)

References 72 publications

(79 reference statements)

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“…Parameters obtained when fitting spectra with ionized-reflection models are often extreme. A maximally rotating supermassive black hole and a very steep emissivity are required in most cases Crummy et al 2006), as well as fine-tuning of the ionization of the disk (Done & Nayakshin 2007). These parameters, which are similar to those obtained when modeling the broad component of the Fe Kα line , show that in this scenario most of the reprocessed radiation is produced very close to the event horizon.…”

Section: Introductionsupporting

confidence: 63%

“…The density structure assumed in a hydrostatic α disk (Shakura & Sunyaev 1973) is not always appropriate. In particular, it has been shown that the accretion disk cannot be in hydrostatic equilibrium if the soft excess is made via reflection (Done & Nayakshin 2007). In the relxilllp_ion model, the gas in the atmosphere of the accretion disk is assumed to be at a constant density .…”

Section: R Vs Q In Simulations Of Ionized Reflectionmentioning

confidence: 99%

“…This model has been successfully applied to NGC 5548 (Magdziarz et al 1998), RE J1034+396 (Middleton et al 2009), RX J0136.9−3510 (Jin et al 2009), Ark 120 , and 1H 0419−577 (Di Gesu et al 2014). This Comptonization model is supported by the existence of similarities between the spectral shape (Walter & Fink 1993) and the variability of the optical/UV and soft X-ray emission (Edelson et al 1996).…”

Section: Introductionmentioning

confidence: 99%

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A hard X-ray view of the soft excess in AGN

Boissay

Ricci

Paltani

2016

A&A

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An excess of X-ray emission below 1 keV, called soft excess, is detected in a large fraction of Seyfert 1-1.5s. The origin of this feature remains debated, as several models have been suggested to explain it, including warm Comptonization and blurred ionized reflection. In order to constrain the origin of this component, we exploit the different behaviors of these models above 10 keV. Ionized reflection covers a broad energy range, from the soft X-rays to the hard X-rays, while Comptonization drops very quickly in the soft X-rays. We present here the results of a study done on 102 Seyfert 1s (Sy 1.0, 1.2, 1.5 and NLSy1) from the Swift BAT 70-Month Hard X-ray Survey catalog. The joint spectral analysis of Swift/BAT and XMM-Newton data allows a hard X-ray view of the soft excess that is present in about 80% of the objects of our sample. We discuss how the soft-excess strength is linked to the reflection at high energy, to the photon index of the primary continuum and to the Eddington ratio. In particular, we find a positive dependence of the soft excess intensity on the Eddington ratio. We compare our results to simulations of blurred ionized-reflection models and show that they are in contradiction. By stacking both XMM-Newton and Swift/BAT spectra per soft-excess strength, we see that the shape of reflection at hard X-rays stays constant when the soft excess varies, showing an absence of link between reflection and soft excess. We conclude that the ionized-reflection model as the origin of the soft excess is disadvantaged in favor of the warm Comptonization model in our sample of Seyfert 1s.

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Section: Introductionsupporting

confidence: 63%

Section: R Vs Q In Simulations Of Ionized Reflectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A hard X-ray view of the soft excess in AGN

Boissay

Ricci

Paltani

2016

A&A

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“…The implied strong X-ray illumination should also give rise to reprocessed emission in the optical/UV bands. The UV/optical emission of this AGN are found variable (see e.g., Di Gesu et al 2014;Pounds et al 2004b) and their detailed relationship with the X-ray emission is explorable.…”

Section: Introductionmentioning

confidence: 99%

Complex optical/UV and X-ray variability of the Seyfert 1 galaxy 1H 0419–577

Pal

Dewangan

Kembhavi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present detailed broadband UV/optical to X-ray spectral variability of the Seyfert 1 galaxy 1H 0419-577 using six XMM-Newton observations performed during [2002][2003]. These observations covered a large amplitude variability event in which the soft X-ray (0.3-2 keV) count rate increased by a factor of ∼ 4 in six months. The X-ray spectra during the variability are well described by a model consisting of a primary power law, blurred and distant reflection. The 2-10 keV power-law flux varied by a factor ∼7 while the 0.3-2 keV soft X-ray excess flux derived from the blurred reflection component varied only by a factor of ∼ 2. The variability event was also observed in the optical and UV bands but the variability amplitudes were only at the 6-10% level. The variations in the optical and UV bands appear to follow the variations in the X-ray band. During the rising phase, the optical bands appear to lag behind the UV band but during the declining phase, the optical bands appear to lead the UV band. Such behavior is not expected in the reprocessing models where the optical/UV emission is the result of reprocessing of X-ray emission in the accretion disc. The delayed contribution of the broad emission lines in the UV band or the changes in the accretion disc/corona geometry combined with X-ray reprocessing may give rise to the observed behavior of the variations.

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“…By studying the correlations between the Suzaku light curves in different bands, Noda et al (2013) were able to extract the stable soft-excess component (Singh et al 1985) that may dominate the continuum emission at soft energies (i.e., below 2.0 keV). According to these authors, the most likely origin for the soft-excess in this source is thermal Comptonization of the disk photons in a warm plasma (see, e.g., Noda et al 2011;Done et al 2012;Jin et al 2012;Petrucci et al 2013;Di Gesu et al 2014;Giustini et al 2015;Boissay et al 2016). It was found, however, that the soft-excess underlies a heavy soft X-ray absorption.…”

Section: Introductionmentioning

confidence: 99%

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

Gesu

Costantini

2016

A&A

Self Cite

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Outflows of photoionized gas are commonly detected in the X-ray spectra of Seyfert 1 galaxies. However, the evidence for this phenomenon in broad line radio galaxies, which are analogous to Seyfert 1 galaxies in the radio-loud regime, has so far been scarce. Here, we present the analysis of the X-ray absorption in the radio-loud quasar 4C +74.26. With the aim of characterizing the kinetic and the ionization conditions of the absorbing material, we fitted jointly the XMM-Newton Reflection Grating Spectrometer (RGS) and the Chandra High Energy Transmission Grating Spectrometer (HETGS) spectra, which were taken 4 months apart. The intrinsic continuum flux did not vary significantly during this time lapse. The spectrum shows the absorption signatures (e.g., Fe-UTA, O vii, and Ne vii-Ne x) of a photoionized gas outflow ( N H ∼ 3.5 × 10 21 cm −2 , log ξ ∼ 2.6, v out ∼ 3600 km s −1 ) located at the redshift of source. We estimate that the gas is located outside the broad line region but within the boundaries of the putative torus. This ionized absorber is consistent with the X-ray counterpart of a polar scattering outflow reported in the optical band for this source. The kinetic luminosity carried by the outflow is insufficient to produce a significant feedback is this quasar. Finally, we show that the heavy soft X-ray absorption that was noticed in the past for this source arises mostly in the Galactic ISM.

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SimultaneousXMM-Newtonand HST-COS observation of 1H 0419–577

Cited by 20 publications

References 72 publications

A hard X-ray view of the soft excess in AGN

A hard X-ray view of the soft excess in AGN

Complex optical/UV and X-ray variability of the Seyfert 1 galaxy 1H 0419–577

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

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