<i>Chandra </i>imaging of the ~kpc extended outflow in 1H 0419-577

Gesu, Laura Di; Costantini, E.; Piconcelli, E.; Kaastra, J. S.; Mehdipour, M.; Paltani, S.

doi:10.1051/0004-6361/201731853

Cited by 5 publications

(3 citation statements)

References 64 publications

(71 reference statements)

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“…This suggests that the components with the same ionisation parameter in each epoch are the same plasma region. On the other hand, we do find the total equivalent column density increases from A degeneracy was found between N H and C cov by Di Gesu et al (2017) in their analysis of the Seyfert 1 AGN 1H 0419−577, using PION. This may explain the decrease in column density (∆N H = −17 × 10 25 m −2 ) between EM1 and EMA, where there is an increase in covering fraction (∆C cov = 0.13).…”

Section: Photoionised Plasma Componentsmentioning

confidence: 42%

Photoionisation modelling of the X-ray emission line regions within the Seyfert 2 AGN NGC 1068

Grafton-Waters

Branduardi‐Raymont

Mehdipour

et al. 2021

A&A

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Aims. We investigate the photoionised X-ray emission line regions (ELRs) within the Seyfert 2 galaxy NGC 1068 to determine if there are any characteristic changes between observations taken 14 years apart. Methods. We compared XMM-Newton observations collected in 2000 and 2014, simultaneously fitting the reflection grating spectrometer and EPIC-pn spectra of each epoch, for the first time, with the photoionisation model, PION, in SPEX. Results. We find that four PION components are required to fit the majority of the emission lines in the spectra of NGC 1068, with log ξ = 1−4, log NH > 26 m−2, and vout = −100 to −600 km s−1 for both epochs. Comparing the ionisation state of the components shows almost no difference between the two epochs, while there is an increase in the total equivalent column density. To estimate the locations of these plasma regions from the central black hole, we compare distance methods, excluding the variability arguments as there is no spectral change between observations. Although the methods are unable to constrain the distances for each plasma component, the locations are consistent with the narrow line region, with the possibility of the higher ionised component being part of the broad line region; we cannot conclude this for certain, but the photoionisation modelling does suggest this is possible. In addition, we find evidence for emission from collisionally ionised plasma, while previous analysis had suggested that collisional plasma emission was unlikely. However, although PION is unable to account for the Fe XVII emission lines at 15 and 17 Å, we do not rule out that photoexcitation is a valid processes to produce these lines as well. Conclusions. NGC 1068 has not changed, both in terms of the observed spectra or from our modelling, within the 14 year time period between observations. This suggests that the ELRs are fairly static relative to the 14 year time frame between observations, or there is no dramatic change in the spectral energy distribution, resulting from a lack of black hole variability.

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Section: Photoionised Plasma Componentsmentioning

confidence: 42%

Photoionisation modelling of the X-ray emission line regions within the Seyfert 2 AGN NGC 1068

Grafton-Waters

Branduardi‐Raymont

Mehdipour

et al. 2021

A&A

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“…Although increasing the covering fraction does decrease the column density, the resonance line is still not fitted by EM1, ruling out the possibility of resonant scattering being the cause. A degeneracy was found by Di Gesu et al (2017) between the column density and covering factor in their PION analysis of the Seyfert 1 galaxy 1H 0419-577. Further to this, we refit these two parameters (N H and C cov ), and the best fit is again obtained for the parameters in Table 3.…”

Section: The O VII Tripletmentioning

confidence: 96%

Multi-wavelength campaign on NGC 7469

Grafton-Waters

Branduardi‐Raymont

Mehdipour

et al. 2020

A&A

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Aims. We aim to investigate and characterise the photoionised X-ray emission line regions within the Seyfert 1 galaxy NGC 7469. Methods. We applied the photoionisation model, PION, within the spectral fitting code SPEX to analyse the 640 ks reflection grating spectrometer spectrum of NGC 7469 gathered during an XMM-Newton observing campaign in 2015. Results. We find the emission line region in NGC 7469 to be multiphased, consisting of two narrow components with ionisation parameters of log ξ = 0.4 and 1.6. A third, broad emission component, with a broadening velocity of vb ∼ 1400 km s−1 and an outflow velocity of vout ∼ −4500 km s−1 is required to fit the residuals in the O VII triplet at around 22 Å. Assuming a volume filling factor of 0.1, the lower distance limits of the narrow emission line region components are estimated for the first time at 2.6 and 2.5 pc from the central black hole, whereas the broad component has an estimated lower bound distance between 0.004 and 0.03 pc, depending on the assumed plasma parameters. The collisionally ionised plasma from the star burst region in NGC 7469 has a plasma temperature of 0.32 keV and an outflow velocity of −280 km s−1, which is consistent with previous results in this campaign. In addition, we model the photoionised plasma of the warm absorber (WA) in NGC 7469 and find that it consists of three photoionised phases with different values of ξ, NH and vout. The upper bound distances of these WA components are 1.9, 0.3, and 0.6 pc, respectively, consistent with archival results. Conclusion. The environment of NGC 7469 is a complex mix of plasma winds absorbing and emitting X-rays. We find the picture painted by our results can be attributed to line emitting plasma located at distances ranging from near the black hole to the torus and beyond the ionised outflows.

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Section: The O VII Tripletmentioning

confidence: 99%

Multi-wavelength Campaign on NGC 7469 VI. Photoionisation Modelling of the Emission Line Regions and the Warm Absorber

Grafton-Waters,

Branduardi-Raymont,

Mehdipour

et al. 2019

Preprint

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Aims. We aim to investigate and characterise the photoionised X-ray emission line regions within the Seyfert 1 galaxy NGC 7469. Methods. We applied the photoionisation model, PION, within the spectral fitting code SPEX to analyse the 640 ks reflection grating spectrometer (RGS) spectrum of NGC 7469 gathered during an XMM-Newton observing campaign in 2015. Results. We find the emission line region in NGC 7469 to be multiphased, consisting of two narrow components with ionisation parameters of log ξ = 0.4 and 1.6. A third, broad emission component, with a broadening velocity of v b ∼ 1400 km s -1 and an outflow velocity of v out ∼ −4500 km s -1 is required to fit the residuals in the O vii triplet at around 22 Å. Assuming a volume filling factor of 0.1, the lower distance limits of the narrow emission line region components are estimated for the first time at 2.6 and 2.5 pc from the central black hole, whereas the broad component has an estimated lower bound distance between 0.004 to 0.03 pc, depending on the assumed plasma parameters. The collisionally ionised plasma from the star burst region in NGC 7469 has a plasma temperature of 0.32 keV and an outflow velocity of -280 km s -1 , which is consistent with previous results in this campaign. In addition, we model the photoionised plasma of the warm absorber (WA) in NGC 7469 and find that it consists of three photoionised phases with different values of ξ, N H and v out . The upper bound distances of these WA components are 1.9, 0.3, and 0.6 pc, respectively, consistent with archival results. Conclusions. The environment of NGC 7469 is a complex mix of plasma winds absorbing and emitting X-rays. We find the picture painted by our results can be attributed to line emitting plasma located at distances ranging from near the black hole to the torus and beyond the ionised outflows.

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Chandra imaging of the ~kpc extended outflow in 1H 0419-577

Cited by 5 publications

References 64 publications

Photoionisation modelling of the X-ray emission line regions within the Seyfert 2 AGN NGC 1068

Photoionisation modelling of the X-ray emission line regions within the Seyfert 2 AGN NGC 1068

Multi-wavelength campaign on NGC 7469

Multi-wavelength Campaign on NGC 7469 VI. Photoionisation Modelling of the Emission Line Regions and the Warm Absorber

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