Fermi Gamma-ray Space Telescope

Study of the Optical/UV and X-ray variability of NGC 1275 with Swift

Fumiya Imazato
(Yasushi Fukazawa)

Abstract:

Radio galaxies are good objects for studying jet periphery emission. NGC 1275(3C 84) is the brightest radio galaxy in the gamma-ray band. Recently, the gamma-ray flux of NGC 1275 has increased gradually. The gamma-ray emission originated from the jet, however it is still under debate whether the the optical/UV and X-ray emission is coming from the jet or accretion disk/corona. In the present work, using the optical/UV and X-ray data from Swift UVOT and XRT we have performed PSF photometry in optical/UV to estimate the contribution of AGN and host galaxy in the total observed emission. From the long-term observations, the optical/UV and X-ray fluxes gradually increase as gamma-ray flux and reddening which mean that those components could be contributed to the jet emission. Additionally, the observed steep peak in the optical/UV SED may suggest an accretion disk origin of the emission. Similar observed correlation of optical and UV flux with the X-ray flux indicates that the X-rays can be attributed to the accretion disk and or corona.