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NGC 1275 is a gamma-ray-emitting radio galaxy at the center of the Perseuscluster. Its multi-wavelength spectrum is similar to that of blazers, and thusa jet-origin of gamma-ray emissions is believed. In the optical and X-rayregion, NGC 1275 also shows a bright core, but their origin has not beenunderstood, since a disk emission is not ruled out. In fact, NGC 1275 exhibitsoptical broad emission lines and a X-ray Fe-K line, which are typical forSeyfert galaxies. In our precious studies of NGC 1275 with Suzaku/XIS, no X-raytime variability was found from 2006 to 2011, regardless of moderate gamma-rayvariability observed by {it Fermi}-LAT~\cite{Yamazaki}. We have continuedmonitoring observations of NGC 1275 with Suzaku/XIS. In 2013-2014, MeV/GeVgams-ray flux of NGC 1275 gradually increased and reached the maximum at thebeginning of 2014. Correlated with this recent gamma-ray activity, we foundthat X-ray flux also increased, and this is the first evidence of X-rayvariability of NGC 1275. Following these results, we discuss the emissioncomponent during the time variability, but we cannot decide the origin of X-rayvariability correlating with gamma-ray. Therefore, for future observation, itis important to observe NGC 1275 by using Fermi gamma-ray, XMM-Newton, NuStar,ASTRO-H X-ray, CTA TeV gamma-ray and Kanata optical telescope.

Suzaku X-Ray Monitoring of Gamma-Ray-Emitting Radio Galaxy, NGC 1275