Space Telescope and Optical Reverberation Mapping Project. XI. Disk-wind Characteristics and Contributions to the Very Broad Emission Lines of NGC 5548

被引：13
|
作者：
Dehghanian, M. [1 ]
Ferland, G. J. [1 ]
Kriss, G. A. [2 ]
Peterson, B. M. [2 ,3 ,4 ]
Korista, K. T. [5 ]
Goad, M. R. [6 ]
Chatzikos, M. [1 ]
Guzman, F. [1 ]
de Rosa, G. [2 ]
Mehdipour, M. [7 ]
Kaastra, J. [7 ,8 ]
Mathur, S. [3 ,4 ]
Vestergaard, M. [9 ,10 ]
Proga, D. [11 ]
Waters, T. [11 ]
Bentz, M. C. [12 ]
Bisogni, S. [13 ]
Brandt, W. N. [14 ,15 ,16 ]
Dalla Bonta, E. [17 ,18 ]
Fausnaugh, M. M. [19 ,20 ]
Gelbord, J. M. [21 ]
Horne, Keith [22 ]
McHardy, I. M. [23 ]
Pogge, R. W. [3 ,4 ]
Starkey, D. A. [22 ]
机构：
[1] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA
[2] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[3] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA
[4] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[5] Western Michigan Univ, Dept Phys, 1120 Everett Tower, Kalamazoo, MI 49008 USA
[6] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England
[7] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands
[8] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands
[9] Univ Copenhagen, Niels Bohr Inst, DARK, Lyngbyvej 2, DK-2100 Copenhagen O, Denmark
[10] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA
[11] Univ Arizona, Steward Observ, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA
[12] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA
[13] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, Via Corti 12, I-20133 Milan, Italy
[14] Penn State Univ, Eberly Coll Sci, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA
[15] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA
[16] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA
[17] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy
[18] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
[19] MIT, Dept Phys, Cambridge, MA 02139 USA
[20] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA
[21] Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA
[22] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland
[23] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
来源：
ASTROPHYSICAL JOURNAL | 2020年 / 898卷 / 02期
基金：
美国国家科学基金会;
关键词：
Seyfert galaxies; Active galaxies; Active galactic nuclei; ACTIVE GALACTIC NUCLEI; BLACK-HOLE; SPECTRA; CLOUDS;
D O I：
10.3847/1538-4357/ab9cb2
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
In 2014 the NGC 5548 Space Telescope and Optical Reverberation Mapping campaign discovered a two-month anomaly when variations in the absorption and emission lines decorrelated from continuum variations. During this time the soft X-ray part of the intrinsic spectrum had been strongly absorbed by a line-of-sight (LOS) obscurer, which was interpreted as the upper part of a disk wind. Our first paper showed that changes in the LOS obscurer produces the decorrelation between the absorption lines and the continuum. A second study showed that the base of the wind shields the broad emission-line region (BLR), leading to the emission-line decorrelation. In that study, we proposed the wind is normally transparent with no effect on the spectrum. Changes in the wind properties alter its shielding and affect the spectral energy distribution (SED) striking the BLR, producing the observed decorrelations. In this work we investigate the impact of a translucent wind on the emission lines. We simulate the obscuration using XMM-Newton, NuSTAR, and Hubble Space Telescope observations to determine the physical characteristics of the wind. We find that a translucent wind can contribute a part of the Heiiand Fe K alpha emission. It has a modest optical depth to electron scattering, which explains the fainter far-side emission in the observed velocity-delay maps. The wind produces the very broad base seen in the UV emission lines and may also be present in the Fe K alpha line. Our results highlight the importance of accounting for the effects of such winds in the analysis of the physics of the central engine.
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页数：8
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