The Seyfert Galaxy NGC 1275: Superfine Structure

Based on VLBA observations (NRAO archive) at lambda = 2 cm, we have constructed radio maps of the Seyfert galaxy NGC 1275 with a resolution of 25 mu as, the epochs of 1995-2015, and at lambda = 7 mm (Boston University archive), the epochs of 2000-2015, with a resolution of 20 mu as. We have identified a ring structure with a diameter phi approximate to 2 mas (1 pc) inclined at 60 degrees to the plane of the sky that includes three centers of activity, vortices. The surrounding relativistic plasma comes to the main northern center along two arms and is ejected in the southward direction X approximate to -10 degrees of a hollow tube, a jet with a diameter phi approximate to 0.12 mas. The second center of activity, a vortex whose plane is parallel to the jet, is located in the remote part of the jet at a distance rho approximate to 2.5 mas. An excess angular momentum is carried away by a coaxial flow with null (21) approximate to 0.8 mas and null (22) approximate to 0.3 mas in the eastward direction X approximate to -90 degrees, where the third center of activity is formed. A coaxial flow with null (31) approximate to 0.7 mas and null (32) approximate to 0.35 mas is ejected in the northward direction. The projections of both coaxial flows form mesh points on the plane of the sky. The nozzle splitting in the first system is observed at a resolution of 3 mu as. The sizes of the two succeeding centers of activity are 80 x 40 and 80 x 120 mu as. The results of our studies of the fine structure of galaxies in polarized emission will be published in the next paper (II).