Multi-wavelength campaign on NGC 7469

Abstract

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.

Reverberation Mapping Measurements of Black Hole Masses and Broad-Line Region Kinematics in Mrk 817 and NGC 7469

“…These researches found that (1) the ultraviolet emissions well correlate with Xray, this is different with Mrk 817; (2) Two absorbers in the ultraviolet band have outflow velocities of ∼ −600 km s −1 and ∼ −2000 km s −1 , and suggested that the low-velocity component located near the broad emission-line region was a highly ionized and high-density absorber, the high-velocity component likely resided farther from the central engine was a lowly ionized and low-density absorber. A parallel but more complicated emission-line region was observed by Grafton-Waters et al (2020).…”

Multiphase AGN winds from X-ray irradiated disk atmospheres

“…SED fitting calculations for NGC 5548 performed by different groups using photoionization modeling are in agreement that the corresponding S-curves have prominent TI zones (e.g., Arav et al 2015;Mehdipour et al 2015). The SED found by Mehdipour et al (2015), which has been implemented into CLOUDY (Ferland et al 2017), yields a Compton temperature of T C ≈ 10 8 K. The Compton radius for NGC 5548 is therefore about R IC = 0.2 pc, which is within the inferred distance of the warm absorbers observed in this system (Arav et al 2015;Ebrero et al 2016) and other similar systems like NGC 7469 (e.g., Grafton-Waters et al 2020). It is this correspondence that is suggestive of warm absorbers, which are found in more than half of all nearby AGN (Crenshaw et al 2003), being probes of the multiphase gas dynamics taking place within the thermally driven winds expected at these distances.…”

Density profile of ambient circumnuclear medium in Seyfert 1 galaxies

“…where f L is the fraction of the ionizing luminosity being absorbed or scattered by the WA cloud, which is about 2% according to Grafton-Waters et al (2020) and Wang et al (2022) and m p is the mass of proton. The average ionizing luminosity of the sources in our sample is 5 × 10 43 erg s −1 .…”