Multi-epoch properties of the warm absorber in the Seyfert 1 galaxy NGC 985

Abstract

Context. NGC 985 was observed by XMM-Newton twice in 2015, revealing that the source was coming out from a soft X-ray obscuration event that took place in 2013. These kinds of events are possibly recurrent since a previous XMM-Newton archival observation in 2003 also showed signatures of partial obscuration. Aims. We have analyzed the high-resolution X-ray spectra of NGC 985 obtained by the Reflection Grating Spectrometer onboard XMM-Newton in 2003, 2013, and 2015 in order to characterize the ionized absorbers superimposed to the continuum and to study their response as the ionizing flux varies. Methods. The spectra were analyzed with the SPEX fitting package and the photoionization code CLOUDY. Results. We found that up to four warm absorber (WA) components were present in the grating spectra of NGC 985, plus a mildy ionized (logξ ∼ 0.2−0.5) obscuring (NH ∼ 2 × 1022 cm−2) wind outflowing at ∼ − 6000 km s−1. The absorbers have a column density that ranges from ∼1021 to a few times 1022 cm−2, and ionization parameters ranging from logξ ∼ 1.6 to ∼2.9. The most ionized component is also the fastest, moving away at ∼ − 5100 km s−1, while the others outflow in two kinematic regimes, ∼ − 600 and ∼ − 350 km s−1. These components showed variability at different time scales in response to changes in the ionizing continuum. Assuming that these changes are due to photoionization and recombination mechanisms, we have obtained upper and lower limits on the density of the gas. We used these limits to pinpoint the location of the warm absorbers, finding that the closest two components are at parsec-scale distances, while the rest may extend up to tens of parsecs from the central source. With these constraints on the density and location, we found that the fastest, most ionized WA component accounts for the bulk of the kinetic luminosity injected back into the interstellar medium of the host galaxy, which is on the order of 0.8% of the bolometric luminosity of NGC 985. According to the models, this amount of kinetic energy per unit time would be sufficient to account for cosmic feedback. Conclusions. Observations of the onset and conclusion of transient obscuring events in active galactic nuclei are a key tool to understand both the dynamics and physics of the gas in their innermost regions, and also to study the response of the surrounding gas as the ionizing continuum varies.

TPHO: A Time-dependent Photoionization Model for AGN Outflows*

“…-, and column densities, N H = 10 21−23 cm −2 (Blustin et al 2005;McKernan et al 2007;Krongold et al 2009;Tombesi et al 2013;Laha et al 2014;Behar et al 2017). They are usually detected as absorption lines and edges from H-like and He-like ions of the most abundant elements, such as C, O, N, Ne, Mg, Si, Si, and Fe, in the soft spectra below 2 keV (Crenshaw et al 2003;Mehdipour et al 2010Mehdipour et al , 2018Ebrero et al 2021). Low-ionization absorbers (log 0 1.5 x = -…”

TPHO: a time-dependent photoionisation model for AGN outflows

“…Spectral studies of warm absorbers highlight their complex multiphase structure, which spans a wide range of ionisation parameters, log(ξ/erg cm s −1 ) = −1 to 3, and column densities, N H = 10 21−23 cm −2 (Blustin et al 2005;McKernan et al 2007;Krongold et al 2009;Tombesi et al 2013;Laha et al 2014;Behar et al 2017). They are usually detected as absorption lines and edges from H-like and He-like ions of the most abundant elements, such as C, O, N, Ne, Mg, Si, Si and Fe, in the soft spectra below 2 keV (Crenshaw et al 2003;Mehdipour et al 2010Mehdipour et al , 2018Ebrero et al 2021). Low ionisation absorbers (log ξ = 0 − 1.5) imprint deep spectral absorption troughs in the rest frame wavelength 15−17 Å due to the blended Fe M shell unresolved transitions array (UTA; Behar et al 2001).…”