<i>XMM‐Newton</i>Reflection Grating Spectrometer Observations of Discrete Soft X‐Ray Emission Features from NGC 1068

Kinkhabwala, Ali; Šako, M.; Behar, E.; Kahn, S. M.; Paerels, F.; Brinkman, A. C.; Kaastra, J. S.; Gu, M. F.; Liedahl, D. A.

doi:10.1086/341482

Cited by 315 publications

(543 citation statements)

References 43 publications

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“…However, it is not consistent with the soft X-ray photoionised gas being the same responsible for the highly ionised, outflowing iron absorption lines discovered by XMM-Newton (Risaliti et al 2005a), and probably associated to a disk outflow. The width of the oxygen RRC features constrains the gas temperature to be ∼10 5 K, of the same order of magnitude as the temperature measured in NGC 1068 (Kinkhabwala et al 2002) or other CIELO AGN (GB07). The only He-like ion, for whose He-α triplet meaningful constraints on the diagnostic parameters G and R (Porquet & Dubau 2000) can be derived is Ovii.…”

Section: Properties Of the Photoionised Plasma In Ngc 1365mentioning

confidence: 53%

“…In NGC 1068, by far the brightest obscured AGN of the soft X-ray sky, the contribution from an optically thin collisionally ionised plasma can be constrained to be ∼ < 10% of integrated soft X-ray flux (Brinkman et al 2002). Resonant scattering plays also an important role in the overall ionisation balance (Kinkhabwala et al 2002); this constrains the gas column density to N H ∼ 10 17−18 /Z O cm −2 (GB07), where Z O is the oxygen abundance.…”

Section: Ionising the Nlrs: The X-ray Viewmentioning

confidence: 99%

“…Such a continuum component cannot be associated to transmission of the nuclear emission through a Compton-thin state, because the column density in these states is always higher than 1.5 × 10 23 cm −2 (Risaliti et al 2007(Risaliti et al , 2009a. This component represents a first remarkable difference with respect to the archetypal Seyfert 2 galaxy NGC 1068 (Kinkhabwala et al 2002). We compared the intensities of the eight brightest emission lines in the spectra accumulated during each individual observation.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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AGN/starburst connection in action: the half million second RGS spectrum of NGC 1365

Guainazzi¹,

Risaliti

Nucita³

et al. 2009

A&A

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Context. High-resolution X-ray observations in the imaging and spectral domain have recently opened a new window on active galactic nuclei (AGN) feedback onto the circumnuclear gas. Spectral diagnostics, as well as the remarkable morphological coincidence between [O iii] and X-rays, point to AGN photoionisation as the dominant ionisation mechanism on scales as large as a few kpc.Aims. In this paper we extend these studies to the nearby Seyfert 2 galaxy NGC 1365, known to host a circumnuclear ring of intense star formation at 1.3 kpc from the nucleus. The main scope of this investigation is to study the connection between nuclear activity and star formation in nearby AGN. Methods. We present a deep ( 5.8 days) 0.3-2 keV high-resolution spectrum of NGC 1365, collected with the reflection grating spectrometer (RGS) on board XMM-Newton. Results. The spectrum is dominated by strong recombination lines of He-and H-like transitions from carbon to silicon, as well as by L transitions from Fexvii. The continuum is strong, especially in the 10 to 20 Å range. Formal fits require two optically thin, collisionally ionised plasma components, with temperatures 300 and 640 eV. However, they leave the bulk of the forbidden components of the He-α Ovii and Nvi triplets unaccounted for. These features can be explained as being produced by photoionised gas. NGC 1365 is therefore the first obscured AGN, whose high-resolution X-ray spectrum requires both collisional ionisation and photoionisation. Conclusions. The relative weakness of photoionisation does not stem from the intrinsic weakness of its AGN, whose X-ray luminosity is ∼ > 10 42 erg s −1 . We suggest that it may instead come from the line-of-sight from the active nucleus to the NLR being blocked by optically thick matter in the broad line region, at the same time responsible for the large observed variation of the column density obscuring the X-ray active nucleus. Alternatively, NGC 1365 could host a remarkably luminous nuclear starburst when compared to the AGN accretion power.

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Section: Properties Of the Photoionised Plasma In Ngc 1365mentioning

confidence: 53%

Section: Ionising the Nlrs: The X-ray Viewmentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

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AGN/starburst connection in action: the half million second RGS spectrum of NGC 1365

Guainazzi¹,

Risaliti

Nucita³

et al. 2009

A&A

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“…Matt et al 1999;Sambruna et al 2001;Molendi et al 2003), NGC 1068 (e.g. Kinkhabwala et al 2002;Matt et al 2004) and Mrk 3 (e.g. Sako et al 2000;Bianchi et al 2005;Pounds & Page 2005).…”

Section: Introductionmentioning

confidence: 99%

The X-ray spectral signatures from the complex circumnuclear regions in the Compton thick AGN NGC 424

Marinucci

Bianchi

Matt

et al. 2010

A&A

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Aims. Most of our knowledge of the circumnuclear matter in Seyfert galaxies is based on the X-ray spectra of the brightest Compton-thick Seyfert 2 galaxies. The complete obscuration of the nuclear radiation in these sources allows us to study all the components arising from reprocessing of the primary continuum in the circumnuclear matter in detail, while they are heavily diluted in unobscured sources, often down to invisibility. Methods. We present the XMM-Newton RGS and EPIC pn spectra of a long ( 100 ks) observation of one of the soft X-ray brightest Compton-thick Seyfert 2 galaxies, NGC 424. As a first step, we performed a phenomenological analysis of the data to derive the properties of all the spectral components. On the basis of these results, we fitted the spectra with self-consistent photoionisation models, produced with cloudy.Results. The high-energy part of the spectrum is dominated by a pure neutral Compton reflection component and a neutral iron Kα line, together with Kα emission from neutral Ni, suggesting a significant Ni/Fe overabundance. The soft X-ray RGS spectrum comes mostly from line emission from H-like and He-like C, N, O, and Ne, as well as from the Fe L-shell. The presence of narrow RRC from O viii, O vii, and C vi, the last two with resolved widths corresponding to temperatures around 5-10 eV, is a strong indication of a gas in photoionisation equilibrium, as confirmed by the prevalence of the forbidden component in the O vii triplet. Two gas phases with different ionisation parameters are needed to reproduce the spectrum with a self-consistent photoionisation model, any contribution from a gas in collisional equilibrium being no more than 10% of the total flux in the 0.35-1.55 keV band. When this self-consistent model is applied to the 0.5-10 keV band of the EPIC pn spectrum, a third photoionised phase is needed to account for emission lines with higher ionisation potential, although Kα emission from S xv and Fe xxvi remains under-predicted.

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“…The heavy obscuration of the pri-⋆ E-mail: marinucci@fis.uniroma3.it (AM) mary radiation from the nucleus, at least up to 10 keV, permits a clear view of these components, which are strongly diluted in unobscured sources. Indeed, most of our knowledge about the circumnuclear reprocessing matter, at least as far as their X-ray properties are concerned, is based on the brightest Compton-thick sources, like NGC 1068 (Kinkhabwala et al 2002;Matt et al 2004;Bauer et al 2015;Marinucci et al 2016), Circinus (e.g. Molendi, Bianchi & Matt 2003;Arévalo et al 2014) and Mrk 3 (e.g.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved Fe K spectroscopy of NGC 4945

Marinucci

Bianchi

Fabbiano

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the imaging and spectroscopic analysis of the combined Chandra ACIS-S observations of the Compton-thick Seyfert 2 galaxy NGC 4945. We performed a spatially-resolved spectroscopy of the circumnuclear environment of the source, picturing the innermost 200 parsecs around the highly absorbed nucleus. The additional 200 ks ACIS-S data with respect to the previous campaign allowed us to map with even greater detail the central structure of this source and to discover an enhanced iron emission in the innermost nuclear region, with respect to the associated Compton reflection continuum. We revealed that the Equivalent Width of the iron Kα line is spatially variable (ranging from 0.5 to 3 keV), on scales of tens of parsecs, likely due to the ionization state and orientation effects of the reprocessing material, with respect to the central X-ray illuminating source. A clump of highly ionized Fe xxv He-α is also detected, 40 parsecs east to the nucleus. When observations taken years apart are considered, the central unresolved reflected emission is found to remain constant.

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XMM‐NewtonReflection Grating Spectrometer Observations of Discrete Soft X‐Ray Emission Features from NGC 1068

Cited by 315 publications

References 43 publications

AGN/starburst connection in action: the half million second RGS spectrum of NGC 1365

AGN/starburst connection in action: the half million second RGS spectrum of NGC 1365

The X-ray spectral signatures from the complex circumnuclear regions in the Compton thick AGN NGC 424

Spatially resolved Fe K spectroscopy of NGC 4945

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