On the Nature of the NGC 1275 System

http://adsabs.harvard.edu/abs/2001AJ....122.2281C
http://iopscience.iop.org/article/10.1086/323534/fulltext/

from Introduction
NGC 1275 (Perseus A, 3C 84) is one of the most unusual early-type galaxies in the nearby universe and contains an example ofalmost every known extragalactic phenomenon. However, several of its basic observed features still remain a mystery. NGC 1275 is located at the center of the Perseus Cluster and resembles a normal elliptical galaxy on low-resolution plates (Hubble & Humason 1931). Humason (1932) and later Seyfert (1943) discovered strong emission lines in NGC 1275. Later, Minkowski (1955) found twodistinct emission-line systems toward NGC 1275: a high-velocity (HV) component at V = 8200 km s^-1 and a low-velocity (LV) one at V = 5200 km s^-1. The stellar radial velocity of NGC 1275 is 5264 ± 11 km s^-1 (Huchra, Vogeley, & Geller 1999), while the velocitydispersion of the Perseus Cluster is 1277 km s^-1 (Struble & Rood 1991). The puzzling nature of NGC 1275 was compounded by thediscovery of an extensive array of emission-line filaments projecting away from the central galaxy (Minkowski 1957; Lynds 1970). The origin of these features is still being debated (see, e.g., McNamara, O'Connell, & Sarazin 1996; Sabra, Shields, & Filippenko 2000).