NGC 759. This E0 galaxy is one of the brightest members of the cluster
A262, at a distance of 66 Mpc. It forms a noninteracting pair with
NGC 753. The cluster A262 is comparable to the Virgo cluster in its
richness and has a similar X-ray luminosity. An optical spectroscopy
survey of ten galaxies in A262 (including NGC 759) showed that only one
galaxy (NGC 708) has a spectra with Balmer absorption and emission lines
showing recent star formation activity (Vigroux et al. 1989).
Nevertheless, we detect relatively strong CO emission in NGC 759,
corresponding to an H_2_ mass of 2 x 10^9^ M_sun_. The CO linewidth is
similar for both the J = 1-0 and J = 2-1 lines and the profiles are
typical for a ring or disk with constant circular rotation.
0154+361. Its structure is characterized by a diffuse emission, with a
central peak, but no compact core. This source is reminiscent of objects
presented by Wrobel & Heeschen (1988), who suggest that the radio
emission could originate from star formation, rather than from an active
nucleus. This possibility is supported in the present source by its
identification with the IRAS source 01548+3605, which has a flux of 0.8
Jy at 60 microns. The ratio between radio and infrared flux is in
agreement with that of star forming galaxies (Wrobel & Heeschen 1988).
See UGC 01434, UGC 01437
E0: (de Vaucouleurs)
Non-interacting pair with NGC 0753 at 23.5 arcmin.