1. THE MAN BEHIND THE CURTAIN: X-RAYS DRIVE THE UV THROUGH NIR VARIABILITY IN THE 2013 ACTIVE GALACTIC NUCLEUS OUTBURST IN NGC 2617
- Author
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Shappee, BJ, Prieto, JL, Grupe, D, Kochanek, CS, Stanek, KZ, De Rosa, G, Mathur, S, Zu, Y, Peterson, BM, Pogge, RW, Komossa, S, Im, M, Jencson, J, Holoien, TW-S, Basu, U, Beacom, JF, Szczygieł, DM, Brimacombe, J, Adams, S, Campillay, A, Choi, C, Contreras, C, Dietrich, M, Dubberley, M, Elphick, M, Foale, S, Giustini, M, Gonzalez, C, Hawkins, E, Howell, DA, Hsiao, EY, Koss, M, Leighly, KM, Morrell, N, Mudd, D, Mullins, D, Nugent, JM, Parrent, J, Phillips, MM, Pojmanski, G, Rosing, W, Ross, R, Sand, D, Terndrup, DM, Valenti, S, Walker, Z, and Yoon, Y
- Subjects
galaxies&COLFAML active ,galaxies&COLFAML nuclei ,galaxies&COLFAML Seyfert ,line&COLFAML formation ,line&COLFAML profiles ,astro-ph.HE ,astro-ph.CO ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) ,Astronomy & Astrophysics - Abstract
After the All-Sky Automated Survey for SuperNovae discovered a significant brightening of the inner region of NGC 2617, we began a ∼70 day photometric and spectroscopic monitoring campaign from the X-ray through near-infrared (NIR) wavelengths. We report that NGC 2617 went through a dramatic outburst, during which its X-ray flux increased by over an order of magnitude followed by an increase of its optical/ultraviolet (UV) continuum flux by almost an order of magnitude. NGC 2617, classified as a Seyfert 1.8 galaxy in 2003, is now a Seyfert 1 due to the appearance of broad optical emission lines and a continuum blue bump. Such "changing look active galactic nuclei (AGNs)" are rare and provide us with important insights about AGN physics. Based on the Hβ line width and the radius-luminosity relation, we estimate the mass of central black hole (BH) to be (4 ± 1) × 107 M . When we cross-correlate the light curves, we find that the disk emission lags the X-rays, with the lag becoming longer as we move from the UV (2-3 days) to the NIR (6-9 days). Also, the NIR is more heavily temporally smoothed than the UV. This can largely be explained by a simple model of a thermally emitting thin disk around a BH of the estimated mass that is illuminated by the observed, variable X-ray fluxes. © 2014. The American Astronomical Society. All rights reserved..
- Published
- 2014