Please use this identifier to cite or link to this item: http://hdl.handle.net/2445/99902
Title: Suzaku and Multi-Wavelength Observations of OJ 287 during the Periodic Optical Outburst in 2007
Author: Bosch i Ramon, Valentí
Paredes i Poy, Josep Maria
Ribó Gomis, Marc
Keywords: Galàxies
Raigs X
Forats negres (Astronomia)
Galaxies
X-rays
Black holes (Astronomy)
Issue Date: 2009
Publisher: Astronomical Society of Japan
Abstract: Suzaku observations of the blazar OJ 287 were performed in 2007 April 10-13 and November 7-9. They correspond to a quiescent and a flaring state, respectively. The X-ray spectra of the source can be well-described with single power-law models in both exposures. The derived X-ray photon index and the flux density at 1 keV were found to be Γ = 1.65±0.02 and S1keV = 215±5 nJy in the quiescent state. In the flaring state, the source exhibited a harder X-ray spectrum (Γ = 1.50±0.01) with a nearly doubled X-ray flux density of S1keV = 404+6-5nJy. Moreover, significant hard X-ray signals were detected up to 27 keV. In cooperation with Suzaku, simultaneous radio, optical, and very-high-energy γ-ray observations of OJ 287 were performed with the Nobeyama Millimeter Array, the KANATA telescope, and the MAGIC telescope, respectively. The radio and optical fluxes in the flaring state (3.04±0.46 Jy and 8.93±0.05 mJy at 86.75 Hz and in the V-band, respectively) were found to be higher by a factor of 2-3 than those in the quiescent state (1.73±0.26 Jy and 3.03±0.01 mJy at 86.75 Hz and in the V-band, respectively). No notable γ-ray events were detected in either observation. The spectral energy distribution of OJ 287 indicated that the X-ray spectrum was dominated by inverse Compton radiation in both observations, while synchrotron radiation exhibited a spectral cutoff at around the optical frequency. Furthermore, no significant difference in the synchrotron cutoff frequency was found between the quiescent and flaring states. According to a simple synchrotron self-Compton model, the change of the spectral energy distribution is due to an increase in the energy density of electrons with small changes of both the magnetic field strength and the maximum Lorentz factor of electrons.
Note: Versió postprint del document publicat a: http://dx.doi.org/10.1093/pasj/61.5.1011
It is part of: Publications of the Astronomical Society of Japan, 2009, vol. 61, num. 5, p. 1011-1022
Related resource: http://dx.doi.org/10.1093/pasj/61.5.1011
URI: http://hdl.handle.net/2445/99902
ISSN: 0004-6264
Appears in Collections:Articles publicats en revistes (Física Quàntica i Astrofísica)

Files in This Item:
File Description SizeFormat 
574423.pdf598.08 kBAdobe PDFView/Open


Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.