High‐Resolution X‐Ray Spectroscopy and Modeling of the Absorbing and Emitting Outflow in NGC 3783

Kaspi, S.; Brandt, W. N.; Netzer, H.; George, I. M.; Chartas, G.; Behar, E.; Sambruna, R. M.; Garmire, G. P.; Nousek, J. A.

doi:10.1086/321333

Cited by 183 publications

(349 citation statements)

References 46 publications

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“…Level population ratio wrt. ground which has been pointed out in Kaspi et al (2001). Nonetheless, the density-sensitive line (13.420 Å) of O-like Fe xix is weaker than the ground level absorption lines (13.521 Å and 13.492 Å).…”

Section: Density Diagnostics For the Ionized Outflow In Ngc 5548mentioning

confidence: 75%

Density diagnostics of ionized outflows in active galactic nuclei

Mao

Kaastra

Mehdipour

et al. 2017

A&A

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Context. Ionized outflows in active galactic nuclei (AGNs) are thought to influence their nuclear and local galactic environment. However, the distance of the outflows with respect to the central engine is poorly constrained, which limits our understanding of their kinetic power as a cosmic feedback channel. Therefore, the impact of AGN outflows on their host galaxies is uncertain. However, when the density of the outflows is known, their distance can be immediately obtained from their modeled ionization parameters. Aims. We perform a theoretical study of density diagnostics of ionized outflows using absorption lines from metastable levels in Be-like to C-like cosmic abundant ions. Methods. With the new self-consistent PhotoIONization (PION) model in the SPEX code, we are able to calculate detailed level populations, including the ground and metastable levels. This enables us to determine under what physical conditions the metastable levels are significantly populated. We then identify characteristic lines from these metastable levels in the 1−2000 Å wavelength range. Results. In the broad density range of n H ∈ (10 6 , 10 20 ) m −3 , the metastable levels 2s2p ( 3 P 0−2 ) in Be-like ions can be significantly populated. For B-like ions, merely the first excited level 2s 2 2p ( 2 P 3/2 ) can be used as a density probe. For C-like ions, the first two excited levels 2s 2 2p 2 ( 3 P 1 and 3 P 2 ) are better density probes than the next two excited levels 2s 2 2p 2 ( 1 S 0 and 1 D 2 ). Different ions in the same isoelectronic sequence cover not only a wide range of ionization parameters, but also a wide range of density values. On the other hand, within the same isonuclear sequence, those less ionized ions probe lower density and smaller ionization parameters. Finally, we reanalyzed the high-resolution grating spectra of NGC 5548 observed with Chandra in January 2002 using a set of PION components to account for the ionized outflow. We derive lower (or upper) limits of plasma density in five out of six PION components based on the presence (or absence) of the metastable absorption lines. Once atomic data from N-like to F-like ions are available, combined with the next generation of spectrometers that cover both X-ray and UV wavelength ranges with higher spectral resolution and larger effective areas, tight constraints on the density and thus the location and kinetic power of AGN outflows can be obtained.

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Section: Density Diagnostics For the Ionized Outflow In Ngc 5548mentioning

confidence: 75%

Density diagnostics of ionized outflows in active galactic nuclei

Mao

Kaastra

Mehdipour

et al. 2017

A&A

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“…While the iron K emission line exists in almost all X-ray sources , K-line features from silicon have also been commonly observed (Kaspi et al 2001(Kaspi et al , 2002Kallman et al 2009). Young et al (2005) reported the detection of H-like Si absorption lines in MCG 6-30-15 and determined the outflow velocity by measuring the line blueshift.…”

Section: Introductionmentioning

confidence: 99%

K-shell energy levels and radiative rates for transitions in Si ix

Wei

Shi

Wang

et al. 2014

A&A

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Context. Accurate atomic data are needed to analyze the Si ix K-shell features in astrophysical X-ray spectra. Relative large discrepancies in the existing atomic data have impeded this progress.Aims. We present the accurate Si ix K-shell transition data, including K-shell energy levels, wavelengths, radiative rates, and oscillator strengths. Methods. The flexible atomic code (FAC), which is a fully relativistic atomic code with configuration interaction (CI) included, was employed to calculate these data. To investigate the CI effects, calculations with different configurations included were carried out.Results. The K-shell atomic data of Si ix transitions between 1s 2 2s 2 2p 2 , 1s 2 2s2p 3 , 1s 2 2p 4 , 1s2s 2 2p 3 , 1s2s2p 4 , and 1s2p 5 are reported.The accuracy of our data is demonstrated by comparing them with the available experimental measurements and theoretical calculations. The energy levels are accurate to 3.5 eV, the wavelengths to within 15 mÅ. For most transitions, the radiative rates an accuracy of 20%. The effects of CI from high-energy configurations were investigated as well.

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“…Currently, the study of the warm absorber is being revolutionized with observations from the dispersion gratings onboard Chandra and XMM-Newton which have been able to resolve individual absorption lines from a myriad of metals and charge states in the warm gas (e.g., Kaastra et al 2000;Kaspi et al 2001;Collinge et al 2001;Lee et al 2001;Kaspi et al 2002). Photoionization modeling has then shown that, in many cases, more than one ionization parameter 1 is needed to describe the observed spectrum (e.g, Morales et al 2000;Kaspi et al 2001;Kaastra et al 2002).…”

Section: Introductionmentioning

confidence: 99%

“…Photoionization modeling has then shown that, in many cases, more than one ionization parameter 1 is needed to describe the observed spectrum (e.g, Morales et al 2000;Kaspi et al 2001;Kaastra et al 2002). Also, the positions of the lines point toward outflow velocities on the order of a few hundred to a few thousand km s −1 .…”

Section: Introductionmentioning

confidence: 99%

On the location and composition of the dust in the MCG–6-30-15 warm absorber

Ballantyne¹,

Weingartner²,

Murray³

2003

A&A

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Abstract. The warm absorber observed in the Seyfert 1 galaxy MCG-6-30-15 is known to consist of at least two zones and very likely contains dust. Hubble Space Telescope images of MCG-6-30-15 show a dust lane crossing the galaxy just below the nucleus. In this paper, we argue that this dust lane is responsible for the observed reddening of the nuclear emission and the Fe  edge hinted at in the Chandra spectrum of MCG-6-30-15. We further suggest that the gas within the dust lane can comprise much of the low ionization component (i.e., the one contributing the O  edge) of the observed warm absorber. Moreover, placing the warm absorbing material at such distances (hundreds of pc) can account for the small outflow velocities of the low ionization absorption lines as well as the constancy of the O  edge. Photoionization models of a dusty interstellar gas cloud (with a column appropriate for the reddening toward MCG-6-30-15) using a toy Seyfert 1 spectral energy distribution show that it is possible to obtain a significant O  edge (τ ∼ 0.2) if the material is ∼150 pc from the ionizing source. For MCG-6-30-15, such a distance is consistent with the observed dust lane. We emphasize the point first made by Kraemer et al.: dusty interstellar material will likely contribute to the warm absorber, and should be included in spectral modeling. The current data on MCG-6-30-15 is unable to constrain the dust composition within the warm absorber. Astronomical silicate is a viable candidate, but there are indications of a very low O abundance in the dust, which is inconsistent with a silicate origin. If true, this may indicate that there were repeated cycles of grain destruction and growth from shocks in the interstellar medium of MCG-6-30-15. Pure iron grains are an unlikely dust constituent due to the limit on their abundance in the Galaxy, yet they cannot be ruled out. The high column densities inferred from the highly ionized zone of the warm absorber implies that this gas is dust-free.

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High‐Resolution X‐Ray Spectroscopy and Modeling of the Absorbing and Emitting Outflow in NGC 3783

Cited by 183 publications

References 46 publications

Density diagnostics of ionized outflows in active galactic nuclei

Density diagnostics of ionized outflows in active galactic nuclei

K-shell energy levels and radiative rates for transitions in Si ix

On the location and composition of the dust in the MCG–6-30-15 warm absorber

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