@article{
 title = {Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ESO 362-G18},
 type = {article},
 year = {2014},
 keywords = {Galaxies: active,Galaxies: seyfert,X-rays: galaxies},
 volume = {443},
 id = {da9ddcd8-b4ba-356d-8307-d3f4d7a7f322},
 created = {2023-02-13T08:14:03.441Z},
 file_attached = {false},
 profile_id = {e942ccc1-42d0-35f9-8d4a-089f3df6b085},
 last_modified = {2023-02-13T08:14:03.441Z},
 read = {false},
 starred = {false},
 authored = {true},
 confirmed = {false},
 hidden = {false},
 private_publication = {true},
 abstract = {We report results from multi-epoch X-ray observations of the Seyfert 1.5 galaxyESO362-G18 performed between 2005 November and 2010 June. ESO 362-G18 generally exhibits the typical X-ray spectrum of type 1 active galactic nuclei. A disc-reflection component accounts for broad residuals in the iron K band and above 10 keV, as well as for a significant soft excess. From our best-fitting reflection model, we measure a black hole spin a ≥ 0.92 at the 99.99 per cent confidence level. ESO 362-G18 is also (typically) mildly absorbed by a column of neutral gas. The absorber is variable and one observation, performed ~2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of ~3-4 × 1023 cm-2, nearly two orders of magnitude higher than that during any other observation. UV variability between the heavily absorbed observation and the others suggests that the absorber can be identified with a dusty, clumpy torus. The absorption variability time-scale enables us to locate the X-ray-emitting region within the innermost ~50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.},
 bibtype = {article},
 author = {Agís-González, B. and Miniutti, G. and Kara, E. and Fabian, A.C. and Sanfrutos, M. and Risaliti, G. and Bianchi, S. and Strotjohann, N.L. and Saxton, R.D. and Parker, M.L.},
 doi = {10.1093/mnras/stu1358},
 journal = {Monthly Notices of the Royal Astronomical Society},
 number = {4}
}

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ESO 362-G18 generally exhibits the typical X-ray spectrum of type 1 active galactic nuclei. A disc-reflection component accounts for broad residuals in the iron K band and above 10 keV, as well as for a significant soft excess. From our best-fitting reflection model, we measure a black hole spin a ≥ 0.92 at the 99.99 per cent confidence level. ESO 362-G18 is also (typically) mildly absorbed by a column of neutral gas. The absorber is variable and one observation, performed ~2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of ~3-4 × 1023 cm-2, nearly two orders of magnitude higher than that during any other observation. UV variability between the heavily absorbed observation and the others suggests that the absorber can be identified with a dusty, clumpy torus. The absorption variability time-scale enables us to locate the X-ray-emitting region within the innermost ~50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.","bibtype":"article","author":"Agís-González, B. and Miniutti, G. and Kara, E. and Fabian, A.C. and Sanfrutos, M. and Risaliti, G. and Bianchi, S. and Strotjohann, N.L. and Saxton, R.D. and Parker, M.L.","doi":"10.1093/mnras/stu1358","journal":"Monthly Notices of the Royal Astronomical Society","number":"4","bibtex":"@article{\n title = {Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ESO 362-G18},\n type = {article},\n year = {2014},\n keywords = {Galaxies: active,Galaxies: seyfert,X-rays: galaxies},\n volume = {443},\n id = {da9ddcd8-b4ba-356d-8307-d3f4d7a7f322},\n created = {2023-02-13T08:14:03.441Z},\n file_attached = {false},\n profile_id = {e942ccc1-42d0-35f9-8d4a-089f3df6b085},\n last_modified = {2023-02-13T08:14:03.441Z},\n read = {false},\n starred = {false},\n authored = {true},\n confirmed = {false},\n hidden = {false},\n private_publication = {true},\n abstract = {We report results from multi-epoch X-ray observations of the Seyfert 1.5 galaxyESO362-G18 performed between 2005 November and 2010 June. ESO 362-G18 generally exhibits the typical X-ray spectrum of type 1 active galactic nuclei. A disc-reflection component accounts for broad residuals in the iron K band and above 10 keV, as well as for a significant soft excess. From our best-fitting reflection model, we measure a black hole spin a ≥ 0.92 at the 99.99 per cent confidence level. ESO 362-G18 is also (typically) mildly absorbed by a column of neutral gas. The absorber is variable and one observation, performed ~2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of ~3-4 × 1023 cm-2, nearly two orders of magnitude higher than that during any other observation. UV variability between the heavily absorbed observation and the others suggests that the absorber can be identified with a dusty, clumpy torus. The absorption variability time-scale enables us to locate the X-ray-emitting region within the innermost ~50 gravitational radii. 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