Simultaneous<i>XMM-Newton</i>and HST-COS observation of 1H0419-577

Gesu, Laura Di; Costantini, E.; Arav, Nahum; Borguet, B.; Detmers, R. G.; Ebrero, J.; Edmonds, Doug; Kaastra, J. S.; Piconcelli, E.; Verbunt, F.

doi:10.1051/0004-6361/201321416

Cited by 17 publications

(34 citation statements)

References 61 publications

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“…We can conclude that no warm absorber or at least an even smaller column (N H ≈ 10 20 cm −2 ) is required for the MF state. The result matches the RGS spectral analysis of the MF observations (N H ≈ 10 19.9 cm −2 ) in Di Gesu et al (2013). The warm absorber in the HF state can account for the spectral difference between the MF and HF spectra at the 0.6-0.8 keV band, in addition to the continuum variability.…”

Section: Multi-epoch Spectral Analysissupporting

confidence: 85%

“…Also a variable power-law continuum emission in the high energy band was noticed in later XMM-Newton observations (Pounds et al 2004a,b;Pounds 2005). A long XMM-Newton observation in 2010 shows a thin, lowly ionized warm absorber in its high resolution grating spectrum (Di Gesu et al 2013). By fitting the XMM-Newton spectrum at an extreme low flux state with the relativistic reflection model, Fabian et al (2005) obtained a disc inner radius of r in < 2r g , indicating a black hole spin of a * > 0.95.…”

Section: Introductionmentioning

confidence: 99%

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A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis withXMM–NewtonandNuSTAR

Jiang

Walton

Fabian

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of the spectral properties of the Seyfert 1 galaxy 1H0419−577, based on the archival XMM-Newton, NuSTAR and simultaneous Swift observations taken between 2002-2015. All the observations show a broad emission line feature at the iron band. We demonstrate that the broad band spectral variability at different levels can be explained by the combination of light-bending effects in the vicinity of the central black hole plus a thin warm absorber. We obtain a black hole spin of a > 0.98 by fitting the multi-epoch spectra with the relativistic disc reflection model. 1H0419−577 is accreting at 40% of its Eddington limit and its X-ray band shows the hardest powerlaw continuum in the highest flux state, which was previously more commonly seen in AGNs with a low accretion rate (e.g. L x /L Edd < 10 −2 ). The NuSTAR observation shows a cool coronal temperature of kT = 30 +22 −7 keV in the high flux state.

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Section: Multi-epoch Spectral Analysissupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis withXMM–NewtonandNuSTAR

Jiang

Walton

Fabian

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…1). In the Reflection Grating Spectrometer (RGS) spectrum of this dataset (already presented in Di Gesu et al 2013, hereafter Paper I) we detected a lowly ionized absorbing gas (also observed in Suzaku, Winter et al 2012). We found that the X-ray and the UV absorbing gas (Edmonds et al 2011) are consistent to be one and the same.…”

Section: H 0419-577: a Variable Seyfert Galaxysupporting

confidence: 53%

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

Gesu

Costantini

Piconcelli

et al. 2014

A&A

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In this paper, we present the longest exposed (97 ks) XMM-Newton EPIC-pn spectrum ever obtained for the Seyfert 1.5 galaxy 1H 0419-577. With the aim of explaining the broadband emission of this source, we took advantage of the simultaneous coverage in the optical/UV that was provided in the present case by the XMM-Newton Optical Monitor and by a HST-COS observation. Archival FUSE flux measurements in the far-ultraviolet were also used for the present analysis. We successfully modeled the X-ray spectrum and the optical/UV fluxes data points using a Comptonization model. We found that a blackbody temperature of T ∼ 56 eV accounts for the optical/UV emission originating in the accretion disk. This temperature serves as an input for the Comptonized components that model the X-ray continuum. Both a warm (T wc ∼ 0.7 keV, τ wc ∼ 7) and a hot corona (T hc ∼ 160 keV, τ hc ∼ 0.5) intervene to upscatter the disk photons to X-ray wavelengths. With the addition of a partially covering (C v ∼ 50%) cold absorber with a variable opacity ( N H ∼ [10 19 −10 22 ] cm −2 ), this model can also explain the historical spectral variability of this source, with the present dataset presenting the lowest one ( N H ∼ 10 19 cm −2 ). We discuss a scenario where the variable absorber becomes less opaque in the highest flux states because it gets ionized in response to the variations of the X-ray continuum. The lower limit for the absorber density derived in this scenario is typical for the broad line region clouds. We infer that 1H 0419-577 may be viewed from an intermediate inclination angle i ≥ 54 • , and, on this basis, we speculate that the X-ray obscuration may be associated with the innermost dust-free region of the obscuring torus. Finally, we critically compare this scenario with all the different models (e.g., disk reflection) that have been used in the past to explain the variability of this source.

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“…Multi-waveband campaigns A&A 589, A76 (2016) provided the detailed broad-band spectrum and the timedependent behavior of X-ray outflows in a number of bright Seyfert-1 galaxies: NGC 7469 , NGC 5548 Kaastra et al 2004;Steenbrugge et al 2005), Mrk 509 Steenbrugge et al 2011;Kaastra et al 2011Kaastra et al , 2012Ebrero et al 2011;Arav et al 2012), IRAS 13449+2438 (Lee et al 2013;Di Gesu et al 2013, NGC 3783 (Kaspi et al 2002;Gabel et al 2003;Netzer et al 2003).…”

Section: Introductionmentioning

confidence: 99%

The thermal instability of the warm absorber in NGC 3783

Goosmann

Holczer

Mouchet

et al. 2016

A&A

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Context. The X-ray absorption spectra of active galactic nuclei frequently show evidence of winds with velocities in the order of 10 3 km s −1 extending up to 10 4 km s −1 in the case of ultra-fast outflows. At moderate velocities, these winds are often spectroscopically explained by assuming a number of absorbing clouds along the line of sight. In some cases it was shown that the absorbing clouds are in pressure equilibrium with each other. Aims. We assume a photo-ionized medium with a uniform total (gas+radiation) pressure. The irradiation causes the wind to be radiation pressure compressed (RPC). We attempt to reproduce the observed spectral continuum shape, ionic column densities, and X-ray absorption measure distribution (AMD) of the extensively observed warm absorber in the Seyfert galaxy NGC 3783. Methods. We compare the observational characteristics derived from the 900 ks Chandra observation to radiative transfer computations in pressure equilibrium using the radiative transfer code titan. We explore different values of the ionization parameter ξ of the incident flux and adjust the hydrogen-equivalent column density, N 0 H , of the warm absorber to match the observed soft X-ray continuum. From the resulting models we derive the column densities for a broad range of ionic species of iron and neon and a theoretical AMD that we compare to the observations. Results. We find an extension of the degeneracy between ξ and N 0 H for the constant pressure models previously discussed for NGC 3783. Including the ionic column densities of iron and neon in the comparison between observations and data we conclude that a range of ionization parameters between 4000 and 8000 erg cm s −1 is preferred. For the first time, we present theoretical AMDs for a constant pressure wind in NGC 3783 that correctly reproduces the observed level and is in approximate agreement with the observational appearance of an instability region. Conclusions. Using a variety of observational indicators, we confirm that the X-ray outflow of NGC 3783 can be described as an RPC medium in pressure equilibrium. The observed AMD agrees with a uniformly hot or a uniformly cold thermal state. The measured ionic column densities suggest that the wind tends to the uniformly cold thermal state. The occurrence of thermal instability in the warm absorber model may depend on the computational method and the spatial scale on which the radiative transfer is solved.

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SimultaneousXMM-Newtonand HST-COS observation of 1H0419-577

Cited by 17 publications

References 61 publications

A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis withXMM–NewtonandNuSTAR

A relativistic disc reflection model for 1H0419–577: Multi-epoch spectral analysis withXMM–NewtonandNuSTAR

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

The thermal instability of the warm absorber in NGC 3783

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