基于结构函数方法的类星体证认

唐洁; 傅明星; 吴学兵

doi:10.7498/aps.61.219501

摘要

光变巡天是搜寻类星体的一个很有效的方法. 应用归一化结构函数对SDSS stripe 82中存在光变的1411个类星体和174个恒星进行分类, 选取幂函数模型拟合这些样本5个波段的结构函数. 综合幅值和幂指数两个物理量设置了合适的分类判据, 获得了比较理想的分类结果, 类星体和恒星最高分类正确率分别达到了92.2%和83.6%. 结果表明, 改正后的结构函数对类星体的证认有很好的效果, 能节约大型望远镜宝贵的观测时间, 让类星体巡天获得比较高的观测效率. 分析结论支持大部分类星体的光变缘于盘的不稳定性.

关键词:

结构函数 /
类星体 /
SDSS /
光变

Abstract

The variability sky survey is a very effective method of searching for quasars. In the paper, we present a novel method to discriminate quasars from variable stars based on their intrinsic variabilities. The power-law model is used to fit the light-curve structure function in five wavebands, but the value of the structure function is normalized. The developed method is applied to 1411 spectroscopically confirmed quasars and 174 stars in SDSS stripe 82. We set a suitable criterion, then obtain a reasonable classified result. The classification accuracies about quasars and stars reach 92.2% and 83.6% respectively. Compared with the structure function only based on one physical parameter, the normalized structure function with amplitude and power-law index has a good efficiency to deal with these data. The method for selecting quasar candidates ensures big sky survey telescope a high survey efficiency and saving valuable astronomical observation time. The results support that the optical variabilities of most of quasars originate from the instabilities of accretion disks.

Keywords:

作者及机构信息

1.
陕西理工学院物理与电信工程学院, 汉中 723001;

2.
北京大学物理学院天文系, 北京 100871

基金项目: 国家自然科学重点项目(批准号: 11033001)和国家重点基础研究发展计划(批准号: 2007CB815405)资助的课题.

Authors and contacts

1.
School of Physics and Telecommunication Engineering, Shaanxi University of Technology, Hanzhong 723001, China;

2.
Department of Astronomy, Peking University, Beijing 100871, China

Funds: Project supported by the Key Program of the National Natural Science Foundation of China (Grant No. 11033001) and the National Basic Research Program of China (Grant No. 2007CB815405).

参考文献

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施引文献

[1]	Fan J H, Zhang Y W, Qian B C, Tao J, Liu Y, Hua T X 2009 Astrophys. J. Suppl. Ser. 181 466
[2]	Fan J H, Liu Y, Qian B C, Tao J, Shen Z Q, Zhang J S, Huang Y, Wang J 2010 Res. Astron. Astrophys. 10 1100
[3]	Tang J, Zhang X 2010 Acta Phys. Sin. 59 7516 (in Chinese) [唐洁, 张雄 2010 59 7516]
[4]	Tang J, Wu X B 2011 Acta Phys. Sin. 60 119801 (in Chinese) [唐洁, 吴学兵 2011 60 119801]
[5]	Cao X W, Li F 2008 Mon. Not. R. Astron. Soc. 390 561
[6]	Li S L, Cao X W 2008 Mon. Not. R. Astron. Soc. 387 41
[7]	Cao X W, Bai J M 2008 Astrophys. J. 673 131
[8]	Huang K L 2005 Quasars and Active Galactic Nucleus (Beijing: Science Press) p33 (in Chinese) [黄克谅 2005 类星体与活动星系核 (北京: 科学出版社) 第33页]
[9]	Crisiani S, Trentini S, la France F 1996 Astron. Asrtophys. 306 395
[10]	MacLeod C L, ZIvezić C S, Kochanek S, Koztowski B, Kelly E, Bullock A, Kimball B, Sesar D, Westman K B 2010 Astrophys. J. 721 1014
[11]	Schmidt K B, Rix H W, Shields J C, Knecht M, Hogg D W, Maoz D, Bovy J 2012 Astrophys. J. 744 147
[12]	Palanque-Delabrouille N, Yeche C, Myers A D, Petitjean P, Nicholas P R, Sheldon E, Aubourg E 2011 Astron. Astrophys. 530 122
[13]	Wu X B, Jia Z D 2010 Mon. Not. R. Astron. Soc. 406 1583
[14]	Wu X B, Wang R, Schmidt K B, Bian F Y, Jiang L H, Fan X H 2011 Astron. J. 142 78
[15]	Hawkins M R S 1996 Mon. Not. R. Astron. Soc. 278 787
[16]	Hawkins M R S 1993 Nature 366 242
[17]	Zhang J S 2004 Chin. Phys. 13 1177
[18]	Deng J G, Huang R T 2008 Acta Phys. Sin. 57 1285 (in Chinese) [邓家干, 黄仁堂 2008 57 1285]
[19]	Meusinger H, Hinze A, Hoon A D 2011 Astron. Astrophys. 525 37
[20]	Wilhite B C, Brunner R J, Grier C J 2008 Mon. Not. R. Astron. Soc. 383 1232
[21]	Rengstorf A W, Brunner R J, Wilhite B C 2006 Astron. J. 131 1923

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