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THE VARIABILITY OF OPTICAL Fe II EMISSION IN PG QSO 1700+518
Bian, WH; Huang, K; Hu C(胡晨); Wang JM(王建民); Hu, C; Zhang, L; Yuan, QR; Huang, KL; Wang, JM
2010
发表期刊ASTROPHYSICAL JOURNAL
卷号718期号:1页码:460-466
通讯作者[Bian, Wei-Hao ; Huang, Kai ; Zhang, Li ; Yuan, Qi-Rong ; Huang, Ke-Liang] Nanjing Normal Univ, Dept Phys, Nanjing 210097, Peoples R China ; [Bian, Wei-Hao ; Huang, Kai ; Zhang, Li ; Yuan, Qi-Rong ; Huang, Ke-Liang] Nanjing Normal Univ, Inst Theoret Phys, Nanjing 210097, Peoples R China ; [Hu, Chen ; Wang, Jian-Min] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100039, Peoples R China
文章类型Article
摘要It is found that Fe II emission contributes significantly to the optical and ultraviolet spectra of most active galactic nuclei. The origin of the optical/UV Fe II emission is still open to debate. The variability of Fe II would give clues to this origin. Using 7.5 yr spectroscopic monitoring data of one Palomar-Green (PG) quasi-stellar object (QSO), PG 1700+518, with strong optical Fe II emission, we obtain the light curves of the continuum f(lambda)(5100 angstrom), Fe II, the broad component of H beta, and the narrow component of H beta by spectral decomposition. Through the interpolation cross-correlation method, we calculate the time lags for the light curves of Fe II, the total H beta, the broad component of H beta, and the narrow component of H beta with respect to the continuum light curve. We find that the Fe II time lag in PG 1700+518 is 209(-147)(+100) days, while the H beta time lag cannot be determined. Assuming that the Fe II and H beta emission regions follow the virial relation between the time lag and the FWHM for the H beta and Fe II emission lines, we can derive the H beta time lag to be 148(-104)(+72) days. The H beta time lag calculated from the empirical luminosity-size relation is 222 days, which is consistent with our measured Fe II time lag. Considering the optical Fe II contribution, PG 1700+518 shares the same spectral slope variability characteristic, i.e., harder spectrum during brighter phase, as the other 15 PG QSOs in our previous work.
关键词black hole physics galaxies: nuclei quasars: emission lines
学科领域Astronomy & Astrophysics
研究领域[WOS]Astronomy & Astrophysics ; Astronomy & Astrophysics
DOI10.1088/0004-637X/718/1/460
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语种英语
研究领域[WOS]Astronomy & Astrophysics ; Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
WOS记录号WOS:000280340800039
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被引频次:12[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ihep.ac.cn/handle/311005/237570
专题粒子天体物理中心
作者单位中国科学院高能物理研究所
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Bian, WH,Huang, K,Hu C,et al. THE VARIABILITY OF OPTICAL Fe II EMISSION IN PG QSO 1700+518[J]. ASTROPHYSICAL JOURNAL,2010,718(1):460-466.
APA Bian, WH.,Huang, K.,胡晨.,王建民.,Hu, C.,...&Wang, JM.(2010).THE VARIABILITY OF OPTICAL Fe II EMISSION IN PG QSO 1700+518.ASTROPHYSICAL JOURNAL,718(1),460-466.
MLA Bian, WH,et al."THE VARIABILITY OF OPTICAL Fe II EMISSION IN PG QSO 1700+518".ASTROPHYSICAL JOURNAL 718.1(2010):460-466.
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