000131583 001__ 131583
000131583 005__ 20241125101138.0
000131583 0247_ $$2doi$$a10.1051/0004-6361/202346475
000131583 0248_ $$2sideral$$a136967
000131583 037__ $$aART-2023-136967
000131583 041__ $$aeng
000131583 100__ $$aBrogan, R.
000131583 245__ $$aStill alive and kicking: A significant outburst in changing-look AGN Mrk 1018
000131583 260__ $$c2023
000131583 5060_ $$aAccess copy available to the general public$$fUnrestricted
000131583 5203_ $$aContext. Changing-look active galactic nuclei (AGN) have been observed to change their optical spectral type. Mrk 1018 is particularly 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 Hβ and Hα 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 explain the multi-wavelength response to the outburst, in particular: i) the unchanged Hβ and Hα 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.
000131583 540__ $$9info:eu-repo/semantics/openAccess$$aby$$uhttp://creativecommons.org/licenses/by/3.0/es/
000131583 590__ $$a5.4$$b2023
000131583 592__ $$a1.896$$b2023
000131583 591__ $$aASTRONOMY & ASTROPHYSICS$$b11 / 84 = 0.131$$c2023$$dQ1$$eT1
000131583 593__ $$aSpace and Planetary Science$$c2023$$dQ1
000131583 593__ $$aAstronomy and Astrophysics$$c2023$$dQ1
000131583 594__ $$a10.2$$b2023
000131583 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000131583 700__ $$aKrumpe, M.
000131583 700__ $$aHoman, D.
000131583 700__ $$aUrrutia, T.
000131583 700__ $$aGranzer, T.
000131583 700__ $$aHusemann, B.
000131583 700__ $$aNeumann, J.
000131583 700__ $$aGaspari, M.
000131583 700__ $$aVaughan, S. P.
000131583 700__ $$aCroom, S. M.
000131583 700__ $$aCombes, F.
000131583 700__ $$0(orcid)0000-0001-5654-0266$$aPérez Torres, M.
000131583 700__ $$aCoil, A.
000131583 700__ $$aMcElroy, R.
000131583 700__ $$aWinkel, N.
000131583 700__ $$aSingha, M.
000131583 773__ $$g677 (2023), A116 [19 pp.]$$pAstron. astrophys.$$tAstronomy and Astrophysics$$x0004-6361
000131583 8564_ $$s1850836$$uhttps://zaguan.unizar.es/record/131583/files/texto_completo.pdf$$yVersión publicada
000131583 8564_ $$s3052662$$uhttps://zaguan.unizar.es/record/131583/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000131583 909CO $$ooai:zaguan.unizar.es:131583$$particulos$$pdriver
000131583 951__ $$a2024-11-22-12:01:31
000131583 980__ $$aARTICLE