Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data

被引:18
|
作者
Guo, Wei-Jian [1 ]
Zou, Hu [1 ]
Fawcett, Victoria A. [2 ]
Canning, Rebecca [3 ]
Juneau, Stephanie [4 ]
Davis, Tamara M. [5 ]
Alexander, David M. [6 ]
Jiang, Linhua [7 ]
Aguilar, Jessica Nicole [8 ]
Ahlen, Steven [9 ]
Brooks, David [10 ]
Claybaugh, Todd [8 ]
de la Macorra, Axel [11 ]
Doel, Peter [10 ]
Fanning, Kevin [12 ]
Forero-Romero, Jaime E. [13 ,14 ]
Gontcho, Satya Gontcho A. [8 ]
Honscheid, Klaus [12 ,15 ,16 ]
Kisner, Theodore [8 ]
Kremin, Anthony [8 ]
Landriau, Martin [8 ]
Meisner, Aaron [17 ]
Miquel, Ramon [18 ,19 ]
Moustakas, John [20 ]
Nie, Jundan [1 ]
Pan, Zhiwei [7 ,21 ]
Poppett, Claire [8 ,22 ,23 ]
Prada, Francisco [24 ]
Rezaie, Mehdi [25 ]
Rossi, Graziano [26 ]
Siudek, Malgorzata [27 ]
Sanchez, Eusebio [28 ]
Schubnell, Michael [29 ,30 ]
Seo, Hee-Jong [31 ]
Sui, Jipeng [1 ,32 ]
Tarle, Gregory [30 ]
Zhou, Zhimin [1 ]
机构
[1] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China
[2] Newcastle Univ, Sch Math Stat & Phys, Newcastle NE1 7RU, England
[3] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, England
[4] NSFs NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA
[5] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia
[6] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England
[7] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
[8] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
[9] Boston Univ, Phys Dept, 590 Commonwealth Ave, Boston, MA 02215 USA
[10] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England
[11] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, Mexico
[12] Ohio State Univ, Chillicothe, OH 43210 USA
[13] Univ Andes, Dept Fis, Cra 1 18A-10,Edificio Ip, Bogota 111711, Colombia
[14] Univ Andes, Observ Astron, Cra 1 18A-10,Edificio H, Bogota 111711, Colombia
[15] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[16] Ohio State Univ, Dept Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[17] NSFs NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA
[18] Passeig Lluis Co 23, E-08010 Barcelona, Spain
[19] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Barcelona, Spain
[20] Siena Coll, Dept Phys & Astron, 515 Loudon Rd, Loudonville, NY 12211 USA
[21] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China
[22] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA
[23] Univ Calif Berkeley, 110 Sproul Hall 5800, Berkeley, CA 94720 USA
[24] CSIC, Inst Astrofis Andaluci, Glorieta Astron S-N, E-18008 Granada, Spain
[25] Kansas State Univ, Dept Phys, 116 Cardwell Hall, Manhattan, KS 66506 USA
[26] Sejong Univ, Dept Phys & Astron, Seoul 143747, South Korea
[27] Inst Space Sci ICE, CSIC, Campus UAB,Carrerde Can Magrans S-N, E-08193 Barcelona, Spain
[28] CIEMAT, Ave Complutense 40, E-28040 Madrid, Spain
[29] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[30] Univ Michigan, Ann Arbor, MI 48109 USA
[31] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA
[32] Univ Chinese Acad Sci, Sch Astron & Space Sci, 19 A Yuquan Rd, Beijing 100049, Peoples R China
来源
基金
国家重点研发计划; 中国国家自然科学基金;
关键词
BROAD-LINE REGION; DIGITAL SKY SURVEY; BLACK-HOLE MASSES; RAPID TURN-ON; TARGET-SELECTION; SEYFERT-GALAXIES; DATA RELEASE; QUASAR CANDIDATES; VISUAL INSPECTION; MONITORING AGNS;
D O I
10.3847/1538-4365/ad118a
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Changing-look active galactic nuclei (CL AGNs) can be generally confirmed by the emergence (turn-on) or disappearance (turn-off) of broad emission lines (BELs), associated with a transient timescale (about 100 similar to 5000 days) that is much shorter than predicted by traditional accretion disk models. We carry out a systematic CL AGN search by crossmatching the spectra coming from the Dark Energy Spectroscopic Instrument and the Sloan Digital Sky Survey. Following previous studies, we identify CL AGNs based on H alpha, H beta, and Mg ii at z <= 0.75 and Mg ii, C iii], and C iv at z > 0.75. We present 56 CL AGNs based on visual inspection and three selection criteria, including 2 H alpha, 34 H beta, 9 Mg ii, 18 C iii], and 1 C iv CL AGN. Eight cases show simultaneous appearances/disappearances of two BELs. We also present 44 CL AGN candidates with significant flux variation of BELs, but remaining strong broad components. In the confirmed CL AGNs, 10 cases show additional CL candidate features for different lines. In this paper, we find: (1) a 24:32 ratio of turn-on to turn-off CL AGNs; (2) an upper-limit transition timescale ranging from 330 to 5762 days in the rest frame; and (3) the majority of CL AGNs follow the bluer-when-brighter trend. Our results greatly increase the current CL census (similar to 30%) and would be conducive to exploring the underlying physical mechanism.
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页数:18
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