Evidence for a radiatively driven disc-wind in PDS 456?

Matzeu, G. A.; Reeves, J. N.; Braito, V.; Nardini, E.; McLaughlin, Dean E.; Lobban, A.; Tombesi, Francesco; Costa, M.

doi:10.1093/mnrasl/slx129

Cited by 96 publications

(131 citation statements)

References 37 publications

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“…Moreover, a positive correlation between the outflow velocity of the UFOs and the X-ray luminosity (e.g. Matzeu et al 2017;Pinto et al 2018) has been observed, and this is expected in a radiatively driven wind scenario. These disc winds are observed at sub-parsec scales from the central SMBH and seem to be powerful enough to affect the host galaxy environment (e.g.…”

Section: Introductionmentioning

confidence: 80%

A broadband X-ray view of the NLSy1 1E 0754.6+3928

Middei

Tombesi

Vagnetti

et al. 2020

A&A

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Context. The soft X-ray band of many active galactic nuclei (AGN) is affected by obscuration due to partially ionised matter crossing our line of sight. In this context, two past XMM-Newton observations (6 months apart) and a simultaneous NuSTAR-Swift (∼8 years later) exposure of the Narrow Line Seyfert 1 galaxy 1E 0754.6+392.8 revealed an intense and variable WA and hints of additional absorbers in the Fe Kα band. Aims. We aim at providing the first X-ray characterisation of this AGN discussing its broadband (0.3-79 keV) spectrum and temporal properties. Methods. We conduct a temporal and spectroscopic analysis on two ∼10 ks (net exposure) XMM-Newton snapshots performed in April and October 2006. We also study the high energy behaviour of 1E 0754.6+392.8 modelling its broadband spectrum using simultaneous Swift-NuSTAR data. Both phenomenological and physically motivated models are tested. Results. We find the presence of flux variability (∼150% and 30% for 0.3-2 and 2-10 keV bands, respectively) and spectral changes at months timescales (∆Γ ∼0.4). A reflection component that is consistent with being constant over years and arising from relatively cold material far from the central super massive black hole is detected. The main spectral feature shaping the 1E 0754.6+392.8 spectrum is a warm absorber. Such a component is persistent over the years and variability of its ionisation and column density is observed down on months in the ranges 3×10 22 cm −2 N H 7.2 × 10 22 cm −2 and 1.5 log(ξ/erg s −1 cm) 2.1. Despite the short exposures, we find possible evidence of two additional high-ionisation and high-velocity outflow components in absorption. Conclusions. Our analysis suggests the existence of a complex system of absorbers in 1E 0754.6+392.8. Longer exposures are mandatory in order to characterise, on more solid grounds, the absorbers in this AGN.

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Section: Introductionmentioning

confidence: 80%

A broadband X-ray view of the NLSy1 1E 0754.6+3928

Middei

Tombesi

Vagnetti

et al. 2020

A&A

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“…The wind energetics are similar for both AGN, with the mass outflow rate and kinetic power typically of 10% Eddington (see Section 6.1). Overall, I Zw 1 may represent a lower mass analogue of the powerful disk wind in PDS 456. larger in PDS 456, where v/c = 0.29 ± 0.01 from the absorption line centroid, although we note that the outflow velocity in PDS 456 has been observed to vary from 0.25 − 0.35c over all the X-ray observations (2001)(2002)(2003)(2004)(2005)(2006)(2007)(2008)(2009)(2010)(2011)(2012)(2013)(2014)(2015)(2016)(2017) to date (Matzeu et al 2017).…”

Section: Comparison With the Wind In Pds 456mentioning

confidence: 86%

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

Reeves

Braito

2019

ApJ

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I Zw 1 is the prototype optical narrow line Seyfert 1 galaxy. It is also a nearby (z = 0.0611), luminous QSO, accreting close to the Eddington limit. XMM-Newton observations of I Zw 1 in 2015 reveal the presence of a broad and blueshifted P-Cygni iron K profile, as observed through a blue-shifted absorption trough at 9 keV and a broad excess of emission at 7 keV in the X-ray spectra. The profile can be well fitted with a wide angle accretion disk wind, with an outflow velocity of at least −0.25c. In this respect, I Zw 1 may be an analogous to the prototype fast wind detected in the QSO, PDS 456, while its overall mass outflow rate is scaled down by a factor ×50 due to its lower black hole mass. The mechanical power of the fast wind in I Zw 1 is constrained to within 5 − 15% of Eddington, while its momentum rate is of the order unity. Upper-limits placed on the energetics of any molecular outflow, from its CO profile measured by IRAM, appear to rule out the presence of a powerful, large scale, energy conserving wind in this AGN. We consider whether I Zw 1 may be similar to a number of other AGN, such as PDS 456, where the large scale galactic outflow is much weaker than what is anticipated from models of energy conserving feedback.

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“…Analysis of the RGS data was performed by Reeves et al (2016), who found Broad Absorption Line (BAL) profiles around 1 keV, identified as He-and H-like Neon and L-shell Iron lines blueshifted by a velocity of v out = −0.1-−0.2c, which could be the signature of a lower ionization and clumpy phase of the accretion disk wind responsible for the absorption trough around 9 keV. The emission lines detected by Nardini et al (2015), Reeves et al (2016) and Matzeu et al (2017a) in Suzaku data are likely associated with the re-emission from the outflow in PDS 456. Reflection on ionized material has also been considered in several studies, but the scenario of an ultrafast outflow absorbing the hot corona emission was often preferred (Reeves et al 2009;Behar et al 2010;Reeves et al 2014;Nardini et al 2015;Chiang et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Relativistic Components of the Ultra-fast Outflow in the Quasar PDS 456 from Chandra/HETGS, NuSTAR, and XMM-Newton Observations

Boissay-Malaquin

Danehkar

Marshall

et al. 2019

ApJ

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We present the spectral analysis of Chandra/HETGS and NuSTAR observations of the quasar PDS 456 from 2015, and XMM-Newton and NuSTAR archival data from 2013-2014, together with Chandra/HETGS data from 2003. We analyzed these three different epochs in a consistent way, looking for absorption features corresponding to highly ionized blueshifted absorption lines from H-like and He-like ions of iron (and nickel), as well as of other elements (O, Ne, Si, and S) in the soft band. We confirm the presence of a persistent ultrafast outflow (UFO) with a velocity of v out = −0.24-−0.29c, previously detected. We also report the detection of an additional faster component of the UFO with a relativistic velocity of v out = −0.48c. We implemented photoionization modeling, using XSTAR analytic model warmabs, to characterize the physical properties of the different kinematic components of the ultra-fast outflow and of the partial covering absorber detected in PDS 456. These two relativistic components of the ultra-fast outflow observed in the three epochs analyzed in this paper are powerful enough to impact the host galaxy of PDS 456 through AGN feedback.

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Evidence for a radiatively driven disc-wind in PDS 456?

Cited by 96 publications

References 37 publications

A broadband X-ray view of the NLSy1 1E 0754.6+3928

A broadband X-ray view of the NLSy1 1E 0754.6+3928

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

Relativistic Components of the Ultra-fast Outflow in the Quasar PDS 456 from Chandra/HETGS, NuSTAR, and XMM-Newton Observations

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