OPTICAL MONITORING OF TWO BRIGHTEST NEARBY QUASARS, PHL 1811 AND 3C 273

被引：52
作者：
Fan, J. H. [1 ,2 ]
Kurtanidze, O. [3 ,4 ]
Liu, Y. [1 ,2 ]
Richter, G. M. [5 ]
Chanishvili, R. [3 ]
Yuan, Y. H. [1 ,2 ]
机构：
[1] Guangzhou Univ, Ctr Astrophys, Guangzhou 510006, Guangdong, Peoples R China
[2] Dept Educ Guangdong Prov, Astron Sci & Technol Res Lab, Guangzhou 510006, Guangdong, Peoples R China
[3] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Georgia
[4] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia
[5] Astrophys Inst Potsdam, D-14482 Potsdam, Germany
来源：
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2014年 / 213卷 / 02期
基金：
中国国家自然科学基金; 美国国家科学基金会;
关键词：
galaxies: active; galaxies: photometry; quasars:; individual; (PHL; 1811; 3C273); BL LACERTAE OBJECTS; EXTRAGALACTIC RADIO-SOURCES; HISTORICAL LIGHT-CURVE; GAMMA-RAY FLARE; BLACK-HOLE; MICROVARIABILITY OBSERVATIONS; MULTIWAVELENGTH OBSERVATIONS; VARIABILITY PROPERTIES; INTRADAY VARIABILITY; SPECTRAL VARIABILITY;
D O I：
10.1088/0067-0049/213/2/26
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Variability is one of the most observable characteristics of active galactic nuclei, and it is important when considering the emission mechanism. In this paper, we report optical photometry monitoring of two nearby brightest quasars, PHL 1811 and 3C 273, using the ST-6 camera attached to the Newtonian focus and the Ap6E CCD camera attached to the primary focus of the 70 cm meniscus telescope at the Abastumani Observatory, Georgia. PHL 1811 was monitored during the period from 2002 September to 2012 December, while 3C 273 was monitored during the period from 1998 February to 2008 May. During our monitoring period, the two sources did not show any significant intra-day variability. The largest detected variations are Delta R = 0.112 +/- 0.010 mag. for PHL 1811, Delta B = 0.595 +/- 0.099 mag, Delta V = 0.369 +/- 0.028 mag, Delta R = 0.495 +/- 0.076 mag, and Delta I = 0.355 +/- 0.009 mag for 3C 273. When the periodicity analysis methods are adopted for the observations of the sources, a period of p = 5.80 +/- 1.12 yr is obtained for PHL1811 in the R light curve in the present work, and periods of p = 21.10 +/- 0.14, 10.00 +/- 0.14, 7.30 +/- 0.09, 13.20 +/- 0.09, 2.10 +/- 0.06, and 0.68 +/- 0.05 yr are obtained for 3C 273 based on the data in the present work combined with historical works.
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