2022ApJ...925..207Z

The nearby Seyfert type galaxy NGC 1275 contains a bright radio nucleus at its center, revealed through high-spatial resolution imaging to be the source of the jets emanating from the galaxy. Coincident with the emergence of a new component C3 in the nucleus since 2005, flux densities from NGC 1275, at least at radio, millimeter, and γ-ray frequencies, had been increasing up through 2017 and leveled off afterwards. We analyze the long-term light curves of the nucleus that span the rising trend to 2015 July, and find a pair of approximately year-long quasi-periodic oscillations, with periods of P_l ≃ 345 days and P_h ≃ 386 days, respectively, in emission at 1.3 mm wavelength. We discuss the case that there would be a long precession period, P_prec ≃ 9 yr, causing the appearance of P_h that is slightly higher than P_l. The accretion disk around the central supermassive black hole (SMBH) would be precessing at P_prec, induced by either the Lense-Thirring effect or the existence of a companion SMBH. In the two scenarios, P_l would be the jet wobbling timescale or the SMBH binary period, respectively. The finding, which could be verified through high-spatial resolution millimeter imaging, would not only identify the nature of the jet variation but also help reveal the full features of the galaxy.