Kinematics of the Broad-line Region of 3C 273 from a 10 yr Reverberation Mapping Campaign
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Author
Zhang, Zhi-XiangDu, Pu
Smith, Paul S.
Zhao, Yulin
Hu, Chen
Xiao, Ming
Li, Yan-Rong
Huang, Ying-Ke
Wang, Kai
Bai, Jin-Ming
Ho, Luis C.

Wang, Jian-Min
Affiliation
Univ Arizona, Steward ObservIssue Date
2019-05-01
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Zhi-Xiang Zhang et al 2019 ApJ 876 49Journal
ASTROPHYSICAL JOURNALRights
Copyright © 2019. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
Despite many decades of study, the kinematics of the broad-line region of 3C 273 are still poorly understood. We report a new, high signal-to-noise, reverberation mapping campaign carried out from 2008 November to 2018 March that allows the determination of time lags between emission lines and the variable continuum with high precision. The time lag of variations in H beta relative to those of the 5100 angstrom continuum is 146.8(-1)(2.1)(+8.3) days in the rest frame, which agrees very well with the Paschen-alpha region measured by the GRAVITY at The Very Large Telescope Interferometer. The time lag of the H gamma emission line is found to be nearly the same as that for H beta. The lag of the Fe II emission is 322.0(-57)(.9)(+55.5) days, longer by a factor of similar to 2 than that of the Balmer lines. The velocity-resolved lag measurements of the H beta line show a complex structure that can be possibly explained by a rotation-dominated disk with some inflowing radial velocity in the H beta-emitting region. Taking the virial factor of f(BLR) = 1.3, we derive a BH mass of M. = 4.1(-0.4)(+0.3) x 10(8) M-circle dot and an accretion rate of 9.3 L-Edd C-2 from the H beta line. The decomposition of its Hubble Space Telescope images yields a host stellar mass of M-* = 10(11.)(3 +/- 0.7) M-circle dot, and a ratio of M./M-* approximate to 2.0 x 10(-3) in agreement with the Magorrian relation. In the near future, it is expected to compare the geometrically thick BLR discovered by the GRAVITY in 3C 273 with its spatially resolved torus in order to understand the potential connection between the BLR and the torus.Note
Open access journalISSN
0004-637XVersion
Final published versionSponsors
National Key R&D Program of China [2016YFA0400701, 2016YFA0400702]; NSFC [NSFC-11873048, NSFC-11833008, NSFC-11473002, NSFC-11721303, NSFC-11690024]; Key Research Program of Frontier Sciences, CAS [QYZDJ-SSW-SLH007]; Strategic Priority Research Program of the Chinese Academy of Sciences [XDB23010400]; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G, NNX12AO93G, NNX15AU81G]; CAS; People's Government of Yunnan Provinceae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ab1099
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Except where otherwise noted, this item's license is described as Copyright © 2019. The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence.