Jet Directions in Seyfert Galaxies

Abstract

We present the study of the relative angle between the accretion disk (or\nradio jet) and the galaxy disk for a sample of Seyfert galaxies selected from a\nmostly isotropic property, the 60$\\mu$m flux. For each galaxy we have a pair of\npoints ($i$,$\\delta$), which are the inclination of the galaxy relative to the\nline of sight and the angle between the jet projected into the plane of the sky\nand the host galaxy major axis, respectively. This data is combined with a\nstatistical technique to determine the distribution of $\\beta$ angles {\\it in 3\ndimensions}, the angle between the jet and the host galaxy plane axis. The\nanalysis of the data, not differentiating between Seyfert 1's and 2's, showed\nthat the observed distribution of $i$ and $\\delta$ values can be well\nrepresented by a homogeneous $\\beta-$distribution in the range\n$0^{\\circ}\\leq\\beta\\leq90^{\\circ}$. However, when we distinguished between\nSeyfert 1's and 2's, the models could not represent Seyfert 1's adequately. It\nwas necessary to introduce viewing angle restrictions, that a galaxy can only\nbe recognized as a Seyfert 1 if the angle between the jet and the line of sight\n($|\\phi|$) is smaller than a given angle $\\phi_c$ and that the galaxy\ninclination $i$ is smaller than an angle $i_c$, in order to have statistically\nacceptable models. This is a direct and independent confirmation of the\nunderlying concepts of the Unified Model. We discuss several ways to explain\nthe misalignment between the accretion disk axis and the host galaxy disk axis.\n