Статья

THE MAN BEHIND THE CURTAIN: X-RAYS DRIVE THE UV THROUGH NIR VARIABILITY IN THE 2013 ACTIVE GALACTIC NUCLEUS OUTBURST IN NGC 2617

B. J. ShappeeDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]Jose L. PrietoDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USAD. GrupeDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAC. S. KochanekCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAK. Z. StanekCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAG. De RosaDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]S. MathurCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAY. ZuDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]B. M. PetersonCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAR. W. PoggeCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAS. KomossaMax-Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, GermanyM. ImCEOU/Department of Physics and Astronomy, Seoul National University, Seoul 151-742, KoreaJ. JencsonDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]T.W-S. HoloienDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]U. BasuDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]J. F. BeacomCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USAD. M. SzczygiełWarsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, PolandJ. BrimacombeS. AdamsDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]A. CampillayCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileC. ChoiCEOU/Department of Physics and Astronomy, Seoul National University, Seoul 151-742, KoreaC. ContrerasCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileM. DietrichDepartment of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USAM. DubberleyLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAM. ElphickLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAS. FoaleLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAM. GiustiniXMM-Newton Science Operation Centre, European Space Astronomy Centre (ESAC)/ESA, Villanueva de la Cañada, E-28691 Madrid, SpainC. GonzalezCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileE. HawkinsLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAD. A. HowellDepartment of Physics, University of California, Santa Barbara, CA 93106, USAE. Y. HsiaoCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileM. KossInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAK. M. LeighlyHomer L. Dodge Department of Physics and Astronomy, The University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USAN. MorrellCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileD. MuddDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]D. MullinsLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAJ. M. NugentHomer L. Dodge Department of Physics and Astronomy, The University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USAJ. ParrentLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAM. M. PhillipsCarnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, ChileG. PojmanskiWarsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, PolandW. RosingLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAR. RossLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAD. SandPhysics Department, Texas Tech University, Box 41051, Lubbock, TX 79409-1051, USAD. M. TerndrupDepartment of Astronomy, The Ohio State University, Columbus, OH 43210, USA; [email protected]S. ValentiDepartment of Physics, University of California, Santa Barbara, CA 93106, USAZ. WalkerLas Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USAY. YoonCEOU/Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea

2014en

ABI

Аннотация

After the All-Sky Automated Survey for SuperNovae (ASAS-SN) 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 (AGN)" are rare and provide us with important insights about AGN physics. Based on the Hbeta line width and the radius-luminosity relation, we estimate the mass of central black hole to be (4 +/- 1) x 10^7 M_sun. 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 black hole of the estimated mass that is illuminated by the observed, variable X-ray fluxes.

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Идентификаторы

DOI: 10.1088/0004-637x/788/1/48

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Цитирований: 10Использованных источников: 0

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