Journal
ASTROPHYSICAL JOURNAL
Volume 788, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/788/1/48
Keywords
galaxies&COLFAML active; galaxies&COLFAML nuclei; galaxies&COLFAML Seyfert; line&COLFAML formation; line&COLFAML profiles
Categories
Funding
- National Research Foundation of Korea [2008-0060544] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1008882, 1009756] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1101216] Funding Source: National Science Foundation
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After the All-Sky Automated Survey for SuperNovae discovered a significant brightening of the inner region of NGC 2617, we began a similar to 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 H beta line width and the radius-luminosity relation, we estimate the mass of central black hole (BH) to be (4 +/- 1) x 10(7)M(circle dot). 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.
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