Relativistic O<scp>viii</scp>Emission and Ionized Outflow in NGC 4051 Measured with<i>XMM‐Newton</i>

Ogle, Patrick; Mason, K. O.; Page, M. J.; Salvi, N. J.; Córdova, F. A.; McHardy, I. M.; Priedhorsky, W. C.

doi:10.1086/382744

Cited by 72 publications

(136 citation statements)

References 65 publications

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“…Considering the large error bars, this velocity is consistent with the optical Hβ FWHM of 5500 km s −1 reported by Boroson & Green (1992). Broad emission features in the soft X-ray spectra of Seyfert 1 Galaxies has been reported in the Chandra-LETG of Mrk 279 (Costantini et al 2007), NGC 5548 (Steenbrugge et al 2005), NGC 4051 (Steenbrugge et al 2009), and in the XMM-Newton-RGS spectra of NGC 4051 (Ogle et al 2004;Ponti et al 2006). In most of these cases, the line profiles were consistent with Gaussians, and in the first two sources, the velocity width of the emission lines was in agreement with measurements of UV lines in the BLR.…”

Section: The Broad Ovii Line In the Rgs Datasupporting

confidence: 89%

High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

Longinotti

Costantini

Petrucci

et al. 2010

A&A

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Context. The Seyfert 1 galaxy Mrk 841 was observed five times between 2001 and 2005 by the XMM-Newton X-ray observatory. The source is well known for showing spectral complexity in the variable iron line and in the soft X-ray excess. Aims. The availability of multiple exposures obtained by the reflection grating spectrometer (RGS) cameras allows thorough study of the complex absorption and emission spectral features in the soft X-ray band. This paper reports on the first study of Mrk 841 soft X-ray spectrum at high spectral resolution. Methods. The three combined exposures obtained in January 2001 and the two obtained in January and July 2005 were analysed with the SPEX software. Results. We detect a two-phase warm absorber. A medium ionisation component (log ξ ∼ 1.5−2.2 erg s cm −1 ) is responsible for a deep absorption feature in the unresolved transition array of the Fe M-shell and for several absorption lines in the OVI-VIII band, and a higher ionisation phase with log ξ ∼ 3 erg s cm −1 is required to fit absorption in the NeIX-X band. The ionisation state and the column density of the gas present moderate variation from 2001 to 2005 for both phases. The high ionisation component of the warm absorber has no effect on the Fe K band. No significant velocity shift of the absorption lines is measured in the RGS data. Remarkably, the 2005 spectra show emission features consistent with photoionisation in a high-density (n e ≥ 10 11 cm −3 ) gas. A prominent OVII line triplet was clearly observed in January 2005 and narrow radiative recombination continua (RRC) of OVII and CVI were observed in both 2005 data sets. A broad Gaussian line around 21.7 Å was also required to fit all the data sets. The derived radial distance for the emission lines seems to suggest that the photoionisation takes place within the optical broad line region of the source.

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Section: The Broad Ovii Line In the Rgs Datasupporting

confidence: 89%

High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

Longinotti

Costantini

Petrucci

et al. 2010

A&A

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“…As reported by Ogle et al (2004), the high state X-ray spectrum of NGC 4051 in the soft band is a combination of continuum and emission line components. Curvature in the spectrum cannot be explained with simple models, i.e.…”

Section: Introductionsupporting

confidence: 55%

A characterization of the NGC 4051 soft X-ray spectrum as observed byXMM-Newton

Nucita¹,

Guainazzi²,

Longinotti³

et al. 2010

A&A

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Context. Soft X-ray high resolution spectroscopy of obscured AGNs shows a complex soft X-ray spectrum dominated by emission lines of He and H-like transitions of elements from carbon to neon, as well as L-shell transitions due to iron ions. Aims. In this paper we characterize the XMM-Newton RGS spectrum of the Seyfert 1 galaxy NGC 4051 observed during a low flux state and infer the physical properties of the emitting and absorbing gas in the soft X-ray regime. Methods. X-ray high-resolution spectroscopy offers a powerful diagnostic tool because the observed spectral features strongly depend on the physical properties of matter (ionization parameter U, electron density n e , hydrogen column density N H ), which in turn are tightly related to the location and size of the X-ray emitting clouds. We carried out a phenomenological study to identify the atomic transitions detected in the spectra. This study suggests that the spectrum is dominated by emission from a photoionized plasma. Then we used the photoionization code Cloudy to produce synthetic models for the emission line component and the warm absorber observed during phases of high intrinsic luminosity. Results. The low state spectrum cannot be described by a single photoionization component. A multi-ionization phase gas with an ionization parameter in the range of log U ∼ 0.63−1.90 and a column density log N H = 22.10−22.72 cm −2 is required, while the electron density n e remains unconstrained. A warm absorber medium is required by the fit with the parameters log U ∼ 0.85, log N H = 23.40 and log n e < ∼ 5. The model is consistent with an X-ray emitting region at a distance > ∼ 5 × 10 −2 pc from the central engine.

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“…An analysis of a 130 ks grating observation with XMM-Newton of Mrk 766 [232] led to the conclusion that a relativistic line interpretation provides a better fit to the data than the warm absorber model. A similar conclusion was found for the Seyfert 1 galaxy NGC 4051 [233]. If correct, these spectral features, formed by radiative recombinaton onto bare nuclei, could provide additional "handles" that would allow tighter constraints to be placed on models of the accretion disk structure in the relativistic regime.…”

Section: Alternative X-ray Signatures Of Relativistic Effectssupporting

confidence: 70%

Atomic X-ray spectroscopy of accreting black holes

Liedahl¹,

Torres²

2005

Can. J. Phys.

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Current astrophysical research suggests that the most persistently luminous objects in the Universe are powered by the flow of matter through accretion disks onto black holes. Accretion disk systems are observed to emit copious radiation across the electromagnetic spectrum, each energy band providing access to rather distinct regimes of physical conditions and geometric scale. X-ray emission probes the innermost regions of the accretion disk, where relativistic effects prevail. While this has been known for decades, it also has been acknowledged that inferring physical conditions in the relativistic regime from the behavior of the X-ray continuum is problematic and not satisfactorily constraining. With the discovery in the 1990s of iron X-ray lines bearing signatures of relativistic distortion came the hope that such emission would more firmly constrain models of disk accretion near black holes, as well as provide observational criteria by which to test general relativity in the strong field limit. Here we provide an introduction to this phenomenon. While the presentation is intended to be primarily tutorial in nature, we aim also to acquaint the reader with trends in current research. To achieve these ends, we present the basic applications of general relativity that pertain to X-ray spectroscopic observations of black hole accretion disk systems, focusing on the Schwarzschild and Kerr solutions to the Einstein field equations. To this we add treatments of the fundamental concepts associated with the theoretical and modeling aspects of accretion disks, as well as relevant topics from observational and theoretical X-ray spectroscopy. PACS Nos.: 32.30. Rj, 32.80.Hd, 95.30.Dr, 95.30.Sf, 95.85.Nv, 97.10.Gz. 97.80.Jp, 98.35.Mp, 98.62.Mw

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Relativistic OviiiEmission and Ionized Outflow in NGC 4051 Measured withXMM‐Newton

Cited by 72 publications

References 65 publications

High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

High-resolution X-ray spectroscopy of the Seyfert 1 Mrk 841: insights into the warm absorber and warm emitter

A characterization of the NGC 4051 soft X-ray spectrum as observed byXMM-Newton

Atomic X-ray spectroscopy of accreting black holes

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