Still alive and kicking: A significant outburst in changing-look AGN Mrk 1018

被引：9

作者：

Brogan, R. ^{[1
,2
]}

Krumpe, M. ^{[1
]}

Homan, D. ^{[1
]}

Urrutia, T. ^{[1
]}

Granzer, T. ^{[1
]}

Husemann, B. ^{[3
]}

Neumann, J. ^{[4
]}

Gaspari, M. ^{[5
]}

Vaughan, S. P. ^{[6
,7
,8
,9
]}

Croom, S. M. ^{[9
,10
]}

Combes, F. ^{[11
]}

Torres, M. Perez ^{[12
,13
,14
]}

Coil, A. ^{[15
]}

McElroy, R. ^{[16
]}

Winkel, N. ^{[4
]}

Singha, M. ^{[17
]}

机构：

[1] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany

[2] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[3] EUMETSAT, Eumetsat Allee 1, D-64295 Darmstadt, Germany

[4] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[5] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[6] Macquarie Univ, Sch Math & Phys Sci, Sydney, NSW 2109, Australia

[7] Macquarie Univ, Astron Astrophys & Astrophoton Res Ctr, Sydney, NSW 2109, Australia

[8] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Sch Sci, Hawthorn, Vic 3122, Australia

[9] ARC Ctr Excellence All Sky Astrophys 3 Dimens ASTR, Mt Stromlo Rd, Stromlo, ACT 2611, Australia

[10] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia

[11] Sorbonne Univ, PSL Univ, Coll France, Observ Paris,LERMA,CNRS, F-75014 Paris, France

[12] Inst Astrofis Andalucia IAA CSIC, Glorieta Astron S-N, Granada 18008, Spain

[13] Univ Zaragoza, Fac Ciencias, Pedro Cerbuna 12, Zaragoza 50009, Spain

[14] European Univ Cyprus, Sch Sci, Diogenes St, CY-1516 Nicosia, Cyprus

[15] Univ Calif San Diego, Dept Astron, San Diego, CA 92092 USA

[16] Univ Queensland, Sch Math & Phys, St Lucia, Qld 4072, Australia

[17] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 677卷

基金：

美国国家航空航天局;

关键词：

accretion; accretion disks; black hole physics; galaxies: active; galaxies: Seyfert; galaxies: nuclei; X-rays: galaxies; REFERENCE SURVEY CARS; BLACK-HOLE MASS; INFRARED-SURVEY-EXPLORER; ACTIVE GALACTIC NUCLEI; BROAD H-ALPHA; SEYFERT-GALAXIES; LINE; ACCRETION; VARIABILITY; EMISSION;

D O I：

10.1051/0004-6361/202346475

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Changing-look active galactic nuclei (AGN) have been observed to change their optical spectral type. Mrk 1018 is partic-ularly unique: first classified as a type 1.9 Seyfert galaxy, it transitioned to being a type 1 Seyfert galaxy a few years later before returning to its initial classification as a type 1.9 Seyfert galaxy after -30 years.Aims. We present the results of a high-cadence optical monitoring programme that caught a major outburst in 2020. Due to sunblock, only the decline could be observed for -200 days. We studied X-ray, UV, optical, and infrared data before and after the outburst to investigate the responses of the AGN structures.Methods. We derived a u'-band light curve of the AGN contribution alone. The flux increased by a factor of -13. We confirmed this in other optical bands and determined the shape and speed of the decline in each waveband. The shapes of H/3 and Ha were analysed before and after the event. Two XMM-Newton observations (X-ray and UV) from before and after the outburst were also exploited.Results. The outburst is asymmetric, with a swifter rise than decline. The decline is best fit by a linear function, ruling out a tidal disruption event. The optical spectrum shows no change approximately eight months before and 17 months after. The UV flux is increased slightly after the outburst but the X-ray primary flux is unchanged. However, the 6.4 keV iron line has doubled in strength. Infrared data taken 13 days after the observed optical peak already show an increased emission level as well.Conclusions. Calculating the distance of the broad-line region and inner edge of the torus from the supermassive black hole can ex-plain the multi-wavelength response to the outburst, in particular: i) the unchanged H/3 and Ha lines, ii) the unchanged primary X-ray spectral components, iii) the rapid and extended infrared response, as well as iv) the enhanced emission of the reflected 6.4 keV line. The outburst was due to a dramatic and short-lasting change in the intrinsic accretion rate. We discuss different models as potential causes.

引用

页数：19

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