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Published October 10, 2020 | Accepted Version + Published
Journal Article Open

Space Telescope and Optical Reverberation Mapping Project. XII. Broad-Line Region Modeling of NGC 5548

Williams, P. R. ORCID icon
Pancoast, A. ORCID icon
Treu, T. ORCID icon
Brewer, B. J.
Peterson, B. M. ORCID icon
Barth, A. J. ORCID icon
Malkan, M. A. ORCID icon
De Rosa, G.
Horne, Keith ORCID icon
Kriss, G. A. ORCID icon
Arav, N.
Bentz, M. C. ORCID icon
Cackett, E. M. ORCID icon
Dalla Bontà, E.
Dehghanian, M. ORCID icon
Done, C.
Ferland, G. J. ORCID icon
Grier, C. J. ORCID icon
Kaastra, J. ORCID icon
Kara, E. ORCID icon
Kochanek, C. S. ORCID icon
Mathur, S. ORCID icon
Mehdipour, M.
Pogge, R. W. ORCID icon
Proga, D. ORCID icon
Vestergaard, M. ORCID icon
Waters, T.
Adams, S. M. ORCID icon
Anderson, M. D.
Arévalo, P. ORCID icon
Beatty, T. G. ORCID icon
Bennert, V. N. ORCID icon
Bigley, A.
Bisogni, S. ORCID icon
Borman, G. A.
Boroson, T. A. ORCID icon
Bottorff, M. C.
Brandt, W. N. ORCID icon
Breeveld, A. A. ORCID icon
Brotherton, M. ORCID icon
Brown, J. E.
Brown, J. S. ORCID icon
Canalizo, G. ORCID icon
Carini, M. T. ORCID icon
Clubb, K. I.
Comerford, J. M.
Corsini, E. M.
Crenshaw, D. M. ORCID icon
Croft, S. ORCID icon
Croxall, K. V. ORCID icon
Deason, A. J. ORCID icon
De Lorenzo-Cáceres, A.
Denney, K. D.
Dietrich, M.
Edelson, R. ORCID icon
Efimova, N. V.
Ely, J. ORCID icon
Evans, P. A. ORCID icon
Fausnaugh, M. M. ORCID icon
Filippenko, A. V. ORCID icon
Flatland, K.
Fox, O. D. ORCID icon
Gardner, E.
Gates, E. L.
Gehrels, N.
Geier, S. ORCID icon
Gelbord, J. M. ORCID icon
Gonzalez, L.
Gorjian, V. ORCID icon
Greene, J. E.
Grupe, D. ORCID icon
Gupta, A.
Hall, P. B. ORCID icon
Henderson, C. B. ORCID icon
Hicks, S.
Holmbeck, E. ORCID icon
Holoien, T. W.-S. ORCID icon
Hutchison, T.
Im, M. ORCID icon
Jensen, J. J.
Johnson, C. A.
Joner, M. D.
Jones, J.
Kaspi, S.
Kelly, P. L. ORCID icon
Kennea, J. A. ORCID icon
Kim, M.
Kim, S.
Kim, S. C.
King, A.
Klimanov, S. A.
Knigge, C.
Krongold, Y.
Lau, M. W. ORCID icon
Lee, J. C. ORCID icon
Leonard, D. C.
Li, Miao ORCID icon
Lira, P.
Lochhaas, C.
Ma, Zhiyuan ORCID icon
MacInnis, F.
Manne-Nicholas, E. R.
Mauerhan, J. C. ORCID icon
McGurk, R. ORCID icon
McHardy, I. M.
Montuori, C.
Morelli, L.
Mosquera, A.
Mudd, D.
Müller-Sánchez, F. ORCID icon
Nazarov, S. V.
Norris, R. P. ORCID icon
Nousek, J. A.
Nguyen, M. L.
Ochner, P.
Okhmat, D. N.
Papadakis, I.
Parks, J. R.
Pei, L.
Penny, M. T. ORCID icon
Pizzella, A. ORCID icon
Poleski, R. ORCID icon
Pott, J.-U. ORCID icon
Rafter, S. E.
Rix, H.-W. ORCID icon
Runnoe, J. ORCID icon
Saylor, D. A. ORCID icon
Schimoia, J. S. ORCID icon
Scott, B.
Sergeev, S. G.
Shappee, B. J. ORCID icon
Shivvers, I. ORCID icon
Siegel, M.
Simonian, G. V. ORCID icon
Siviero, A.
Skielboe, A. ORCID icon
Somers, G. ORCID icon
Spencer, M.
Starkey, D.
Stevens, D. J. ORCID icon
Sung, H.-I.
Tayar, J. ORCID icon
Tejos, N. ORCID icon
Turner, C. S. ORCID icon
Uttley, P. ORCID icon
Van Saders, J.
Vaughan, S. A.
Vican, L.
Villanueva, S. ORCID icon
Villforth, C. ORCID icon
Weiss, Y.
Woo, J.-H.
Yan, H.
Young, S.
Yuk, H.
Zheng, W.
Zhu, W.
Zu, Y.

Abstract

We present geometric and dynamical modeling of the broad line region (BLR) for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The data set includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the Hβ, C iv, and Lyα broad emission lines. We find an extended disk-like Hβ BLR with a mixture of near-circular and outflowing gas trajectories, while the C iv and Lyα BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with C iv and Lyα emission arising at smaller radii than the Hβ emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of log₁₀(M_(BH)/M_⊙) = 7.64_(-0.18)^(+0.21). We examine the effect of using the V band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV–optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that the V band is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the Hβ results to similar models of data obtained in 2008 when the active galactic nucleus was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remained unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole.

Additional Information

© 2020. The American Astronomical Society. Received 2020 July 3; revised 2020 September 16; accepted 2020 September 21; published 2020 October 14. Support for HST program No. GO-13330 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Research by P.R.W. and T.T. is supported by NSF grants AST-1412315 and AST-1907208. T.T. and P.R.W. acknowledge support from the Packard Foundation through a Packard Fellowship to T.T. Research by AJB was supported by NSF grant AST-1907290. G.F. and M.D. acknowledge support by NSF (1816537, 1910687), NASA (17-ATP17-0141, 19-ATP19-0188), and STScI (HST-AR-15018, HST-AR-14556). M.I. acknowledges the support form the NRF grant, No. 2020R1A2C3011091, funded by the Korea government (MSIT). M.V. gratefully acknowledges support from the Independent Research Fund Denmark via grant No. DFF 8021-00130. C.S.K. is supported by NSF grants AST-1908952 and AST-1814440. V.N.B. acknowledges assistance from a NASA grant associated with HST proposal GO 15215, a NASA ADAP grant (grant # 80NSSC19K1016) and a National Science Foundation (NSF) Research at Undergraduate Institutions (RUI) grant (AST-1909297). Note that findings and conclusions do not necessarily represent views of the NSF. D.J.S. acknowledges funding support from the Eberly Research Fellowship from The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. A.V.F.'s group at U.C. Berkeley is grateful for the financial support of NSF grant AST-1211916, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). Research at Lick Observatory is partially supported by a generous gift from Google.

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Accepted Version - 2010.00594.pdf

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Additional details

Created:
August 22, 2023
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