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DISK–JET CONNECTION IN THE RADIO GALAXY 3C 120

Ritaban ChatterjeeInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USAAlan P. MarscherInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USASvetlana G. JorstadAstronomical Institute of St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, RussiaAlice R. OlmsteadInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USAIan M. McHardyDepartment of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKMargo F. AllerAstronomy Department, University of Michigan, 830 Dennison, 501 East University Street, Ann Arbor, MI 48109-1042, USAHugh D. AllerAstronomy Department, University of Michigan, 830 Dennison, 501 East University Street, Ann Arbor, MI 48109-1042, USAAnne LähteenmäkiMetsähovi Radio Observatory, Helsinki University of Technology TKK, Metsähovintie 114, FIN-02540 Kylmälä, FinlandMerja TornikoskiMetsähovi Radio Observatory, Helsinki University of Technology TKK, Metsähovintie 114, FIN-02540 Kylmälä, FinlandTalvikki HovattaMetsähovi Radio Observatory, Helsinki University of Technology TKK, Metsähovintie 114, FIN-02540 Kylmälä, FinlandKevin MarshallDepartment of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USAH. Richard MillerDepartment of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USAWesley T. RyleDepartment of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USABenjamin ChickaInstitute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USAA. J. BenkerDepartment of Physics & Astronomy, University of California, Irvine, CA 92697-4575, USAMark C. BottorffPhysics Department, Southwestern University, Georgetown, TX 78627-0770, USADavid BrokofskyDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAJeffrey S. CampbellDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USATaylor S. ChonisDepartment of Astronomy, University of Texas, Austin, TX 78712-0259, USAC. Martin GaskellDepartment of Astronomy, University of Texas, Austin, TX 78712-0259, USAEvelina R. GaynullinaUlugh Beg Astronomical Institute of the Uzbek Academy of Sciences Astronomicheskaya St. 33, Tashkent 100052, UzbekistanKonstantin N. GrankinUlugh Beg Astronomical Institute of the Uzbek Academy of Sciences Astronomicheskaya St. 33, Tashkent 100052, UzbekistanCecelia H. HedrickDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAMansur A. IbrahimovUlugh Beg Astronomical Institute of the Uzbek Academy of Sciences Astronomicheskaya St. 33, Tashkent 100052, UzbekistanElizabeth S. KlimekDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAAmanda K. KruseDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAShoji MasatoshiDepartment of Astronomy, University of Texas, Austin, TX 78712-0259, USAThomas R. MillerHong-Jian PanKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, ChinaEric A. PetersenDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USABradley W. PetersonDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAZhiqiang ShenKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, ChinaDmitriy V. Strel'nikovDepartment of Astronomy, National University of Uzbekistan, Tashkent 700095, UzbekistanJun TaoKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, ChinaAaron E. WatkinsDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USAKathleen WheelerDepartment of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588-0111, USA

The Astrophysical Journaljournal2009en

ABI

Annotatsiya

We present the results of extensive multi-frequency monitoring of the radio galaxy 3C 120 between 2002 and 2007 at X-ray (2-10 keV), optical (R and V bands), and radio (14.5 and 37 GHz) wave bands, as well as imaging with the Very Long Baseline Array (VLBA) at 43 GHz. Over the 5 yr of observation, significant dips in the X-ray light curve are followed by ejections of bright superluminal knots in the VLBA images. Consistent with this, the X-ray flux and 37 GHz flux are anti-correlated with X-ray leading the radio variations. Furthermore, the total radiative output of a radio flare is related to the equivalent width of the corresponding X-ray dip. This implies that, in this radio galaxy, the radiative state of accretion disk plus corona system, where the X-rays are produced, has a direct effect on the events in the jet, where the radio emission originates. The X-ray power spectral density of 3C 120 shows a break, with steeper slope at shorter timescale and the break timescale is commensurate with the mass of the central black hole (BH) based on observations of Seyfert galaxies and black hole X-ray binaries (BHXRBs). These findings provide support for the paradigm that BHXRBs and both radio-loud and radio-quiet active galactic nuclei are fundamentally similar systems, with characteristic time and size scales linearly proportional to the mass of the central BH. The X-ray and optical variations are strongly correlated in 3C 120, which implies that the optical emission in this object arises from the same general region as the X-rays, i.e., in the accretion disk-corona system. We numerically model multi-wavelength light curves of 3C 120 from such a system with the optical-UV emission produced in the disk and the X-rays generated by scattering of thermal photons by hot electrons in the corona. From the comparison of the temporal properties of the model light curves to that of the observed variability, we constrain the physical size of the corona and the distances of the emitting regions from the central BH. In addition, we discuss physical scenarios for the disk-jet connection that are consistent with our observations.

Mavzular

Astrophysical Phenomena and Observations Galaxies: Formation, Evolution, Phenomena Astrophysics and Cosmic Phenomena

Identifikatorlar

DOI: 10.1088/0004-637x/704/2/1689

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