A Detection Of An X-ray Wind And An Ionized Disk In The Chandra HETGS Observation Of The Seyfert 2 Galaxy IRAS 18325-5926
Name
canizares1.pdf
Size
611.24 KB
Format
Adobe PDF
Checksum (MD5)
56f183ce098d2db132b39d1ef620c7d2
Author(s)
Mocz, Philip
Lee, Julia C.
Iwasawa, Kazushi
Canizares, Claude R.
Date Issued
February 2011
Journal
Astrophysical Journal
Publisher
IOP Publishing
Citation
Mocz, Philip et al. “A DETECTION OF AN X-RAY WIND AND AN IONIZED DISK IN THE
CHANDRA
HETGS OBSERVATION OF THE SEYFERT 2 GALAXY IRAS 18325-5926.” The Astrophysical Journal 729.1 (2011): 30.
Version
Author's final manuscript
Abstract
We analyze the Chandra High Energy Transmission Grating Spectrometer observation of the Seyfert 2 AGN IRAS 18325-5926. We detect a v = –360[superscript +41] [subscript –66] km s[superscript –1] blueshifted ionized absorber in the X-ray spectrum, with photoionization parameter log ξ = 2.0[superscript +0.1] [subscript –0.1] and hydrogen column density N H = 1.55[superscript +0.75] [subscript –0.38] × 10[superscript 21] cm[superscript –2]. The absorber may be a photoionized wind originating in the obscuring torus/global covering around the black hole or outer edge of the accretion disk. The estimated mass outflow rate suggests that the supermassive black hole in IRAS 18325-5926 may significantly affect the large-scale environment of the host galaxy, unless the solid angle subtended by the outflow or the gas filling factor is small. A second warm absorber may be needed to explain the absorption features in the vicinity of the iron K edge, although insufficient counts in the data beyond 7.0 keV make it difficult to assess the nature of the second absorber. Most plausible is a high ionization (log ξ ~ 2.3 to 2.6), high column density (N H ~ 1023 cm–2) absorber with v ~ –3000 to 0 km s–1, although these parameters are not well constrained. We also examine the broad Fe K emission line in the spectrum, which is likely due to Fe XXV in a highly ionized accretion disk inclined at 25°, consistent with the XMM-Newton EPIC observations of the emission line. Because we are able to view both the obscuring gas and the accretion disk of IRAS 18325-5926, the surrounding gas of IRAS 18325-5926 may be patchy or we are viewing the system at an angle just grazing the obscuring torus.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike 3.0
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1088/0004-637x/729/1/30
