The mass-energy budget of the ionised outflow in NGC 7469

Blustin, A. J.; Kriss, G. A.; Holczer, Tomer; Behar, E.; Kaastra, J. S.; Page, M. J.; Kaspi, S.; Branduardi‐Raymont, G.; Steenbrugge, K. C.

doi:10.1051/0004-6361:20066883

Cited by 67 publications

(96 citation statements)

References 44 publications

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“…For the 40 ks RGS spectrum of NGC 3783, Blustin et al (2002) measured the abundances to be consistent with solar, with the exception of Fe. Similar abundances were measured by Steenbrugge et al (2003) for NGC 5548 using a 137 ks RGS spectrum, as well as by Blustin et al (2007) for a 160 ks RGS spectrum of NGC 7469. Holczer et al (2007) determined the abundances for IRAS 13349+2438 and NGC 3783 using the updated dielectronic recombination rates and determined abundances relative to Fe consistent with proto-solar ratios for O, Ne, Mg, Si, and S (NGC 3783 only).…”

Section: Abundances From Narrow Absorption Linessupporting

confidence: 76%

Multiwavelength campaign on Mrk 509

Steenbrugge

Kaastra

Detmers

et al. 2011

A&A

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Context. The study of abundances in the nucleus of active galaxies allows us to investigate the evolution of the abundance by comparing local and higher redshift galaxies. However, the methods used so far have substantial drawbacks or rather large uncertainties. Some of the measurements are at odds with the initial mass function derived from the older stellar population of local elliptical galaxies. Aims. We determine accurate and reliable abundances of C, N, Ne, and Fe relative to O from the narrow absorption lines observed in the X-ray spectra of Mrk 509. Methods. We use the stacked 600 ks XMM-Newton RGS and 180 ks Chandra LETGS spectra. Thanks to simultaneous observations with INTEGRAL and the optical monitor on-board XMM-Newton for the RGS observations and HST-COS and Swift for the LETGS observations, we have an individual spectral energy distribution for each dataset. Owing to the excellent quality of the RGS spectrum, the ionisation structure of the absorbing gas is well constrained, allowing for a reliable abundance determination using ions over the whole observed range of ionisation parameters. Results. We find that the relative abundances are consistent with the proto-solar abundance ratios: C/O = 1.19 ± 0.08, N/O = 0.98 ± 0.08, Ne/O = 1.11 ± 0.10, Mg/O = 0.68 ± 0.16, Si/O = 1.3 ± 0.6, Ca/O = 0.89 ± 0.25, and Fe/O = 0.85 ± 0.06, with the exception of S, which is slightly under-abundant, S/O = 0.57 ± 0.14. Our results, and their implications, are discussed and compared to the results obtained using other techniques to derive abundances in galaxies.

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Section: Abundances From Narrow Absorption Linessupporting

confidence: 76%

Multiwavelength campaign on Mrk 509

Steenbrugge

Kaastra

Detmers

et al. 2011

A&A

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“…This suggests that the warm absorbing gas covers a wide range of ionization, as has been observed in other Seyfert 1 galaxies, e.g. NGC 3783: (Kaspi et al 2000(Kaspi et al , 2001Krongold et al 2003), NGC 5548: (Kaastra et al 2002;Andrade-Velázquez et al 2010), Mrk 509: (Yaqoob et al 2003Smith et al 2007), NGC 7469: (Blustin et al 2007), IC 4329A: (Steenbrugge et al 2005a), NGC 3516: (Holczer & Behar 2012), MCG-6-30-15: (Lee et al 2001;Turner et al 2004), Mrk 279: (Costantini et al 2007). …”

Section: Chandra Observations and Data Reductionsupporting

confidence: 62%

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

Reeves

Braito

Behar

et al. 2017

ApJ

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High resolution X-ray spectroscopy of the warm absorber in the nearby X-ray bright Seyfert 1 galaxy, Mrk 1040 is presented. The observations were carried out in the 2013-2014 timeframe using the Chandra High Energy Transmission Grating with a total exposure of 200 ks. A multitude of absorption lines from Ne, Mg and Si are detected from a wide variety of ionization states. In particular, the detection of inner K-shell absorption lines from Ne, Mg and Si, from charge states ranging from F-like to Li-like ions, suggests the presence of a substantial amount of low ionization absorbing gas, illuminated by a steep soft X-ray continuum. The observations reveal at least 3 warm absorbing components ranging in ionization parameter from log(ξ/erg cm s −1 ) = 0 − 2 and with column densities of N H = 1.5 − 4.0 × 10 21 cm −2 . The velocity profiles imply that the outflow velocities of the absorbing gas are low and within ±100 km s −1 of the systemic velocity of Mrk 1040, which suggests any outflowing gas may have stalled in this AGN on large enough scales. The warm absorber is likely located far from the black hole, within 300 pc of the nucleus and is spatially coincident with emission from an extended Narrow Line Region as seen in the HST images. The iron K band spectrum reveals only narrow emission lines, with Fe Kα at 6.4 keV consistent with originating from reflection off Compton thick pc-scale reprocessing gas.

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“…Nevertheless, our combined observational and modeling work excludes for NGC 3783 a so-called "continuous AMD" that corresponds to a homogeneous flow and is observed in, e.g., NGC 5548 (Steenbrugge et al 2005). In Behar (2009) (Blustin et al 2007), MCG-6-30-15 (Holczer et al 2010) and NGC 3516 (Holczer & Behar 2012). Again, in almost all cases a gap is detected, which is consistent with a multi-zone absorber.…”

Section: Reproducing the Observed Amd With An Isobaric Rpc Modelmentioning

confidence: 56%

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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The mass-energy budget of the ionised outflow in NGC 7469

Cited by 67 publications

References 44 publications

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

The thermal instability of the warm absorber in NGC 3783

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