Resolving the soft X-ray ultra fast outflow in PDS 456

dc.contributor.authorReeves, James
dc.contributor.authorBraito, Valentina
dc.contributor.authorChartas, George
dc.contributor.authorHamann, Fred
dc.contributor.authorLaha, Sibasish
dc.contributor.authorNardini, Emanuele
dc.date.accessioned2020-06-09T16:11:26Z
dc.date.available2020-06-09T16:11:26Z
dc.date.issued2020-04-26
dc.description.abstractPast X-ray observations of the nearby luminous quasar PDS 456 (at z=0.184) have revealed a wide angle accretion disk wind (Nardini et al. 2015), with an outflow velocity of ∼−0.25c, as observed through observations of its blue-shifted iron K-shell absorption line profile. Here we present three new XMM-Newton observations of PDS 456; one in September 2018 where the quasar was bright and featureless, and two in September 2019, 22 days apart, occurring when the quasar was five times fainter and where strong blue-shifted lines from the wind were present. During the second September 2019 observation, three broad (σ=3000 km s⁻¹) absorption lines were resolved in the high resolution RGS spectrum, which are identified with blue-shifted OVIII Lyα, NeIX Heα and NeX Lyα. The outflow velocity of this soft X-ray absorber was found to be v/c=−0.258±0.003, fully consistent with iron K absorber with v/c=−0.261±0.007. The ionization parameter and column density of the soft X-ray component (logξ=3.4, NH=2×10²¹ cm⁻²) outflow was lower by about two orders of magnitude, when compared to the high ionization wind at iron K (logξ=5, NH=7×10²³ cm⁻²). Substantial variability was seen in the soft X-ray absorber between the 2019 observations, declining from NH=10²³ cm⁻² to NH=10²¹ cm⁻² over 20 days, while the iron K component was remarkably stable. We conclude that the soft X-ray wind may originate from an inhomogeneous wind streamline passing across the line of sight and which due to its lower ionization, is located further from the black hole, on parsec scales, than the innermost disk wind.en_US
dc.description.sponsorshipJR acknowledges financial support through grants 80NSSC18K1603 and HST-GO-14477. VB acknowledges support from grant number GO7-18091X. VB and JR both acknowledge support from grant 80NSSC20K0793. EN acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0 and partial support from the EU Horizon 2020 Marie Skłodowska-Curie grant agreement no.664931 FH acknowledges support from the Hubble Space Telescope guest observer program HST-GO-15309. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.en_US
dc.description.urihttps://arxiv.org/abs/2004.12439en_US
dc.format.extent13 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m2ow02-y1um
dc.identifier.citationJames Reeves et al., Resolving the soft X-ray ultra fast outflow in PDS 456, Astrophysical Journal,10.3847/1538-4357/ab8cc4en_US
dc.identifier.uri10.3847/1538-4357/ab8cc4
dc.identifier.urihttp://hdl.handle.net/11603/18846
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology
dc.relation.ispartofUMBC Faculty Collection
dc.relation.ispartofUMBC Physics Department
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.titleResolving the soft X-ray ultra fast outflow in PDS 456en_US
dc.typeTexten_US

Files

Original bundle

Now showing 1 - 1 of 1
Loading...
Thumbnail Image
Name:
2004.12439.pdf
Size:
684.67 KB
Format:
Adobe Portable Document Format
Description:

License bundle

Now showing 1 - 1 of 1
Loading...
Thumbnail Image
Name:
license.txt
Size:
2.56 KB
Format:
Item-specific license agreed upon to submission
Description: