0316+413 (3C84, Perseus A) is a nearby Seyfert galaxy (z=0.0172) with a compact radio source in excess of 30 Jy at 22 GHz, which accounts for the great majority of the total flux density of the source. The sub-pc-scale structure consists of a bright core component and a strong jet-like elongation extending approximately 10 mas from the core toward the south. A newly discovered component to the north of the core has been detected at 8.4 and 22 GHz. This component has been identified as a pc-scale counterjet [Walker, Romney, & Benson 1994; Vermeulen, Readhead, & Backer 1994]. The spectral index of the counterjet suggests that a free-free absorbing disk or torus is partly obscuring our view of it [Vermeulen, Readhead, & Backer 1994]. Subluminal motions have been observed on the pc-scale ranging from 0.14 h 
c [Vermeulen, Readhead, & Backer 1994] to 0.58 h c [Marr et al. 1989].
0402+372 (z=0.0504) has a complex pc-scale morphology consisting of a jet-like structure approximately 40 mas long at a position angle of approximately 30 
[Polatidis et al. 1995]. Only a single epoch of VLBI imaging was found from the literature. The kpc-scale radio structure has been imaged with the VLA [Xu et al. 1995], revealing a bright core component and a diffuse, double-lobed structure which straddles the core along a position angle of approximately 30 and has a lobe-to-lobe angular extent of approximately 15''.
0430+052 (3C120) is a Seyfert galaxy (z=0.033) with an associated radio structure consisting of a jet which is observable on scales between 0.5 pc and 100 kpc, and diffuse lobes on scales up to 400 kpc [Walker, Benson, & Unwin 1987]. The kpc-scale structure is complex, the jet bending significantly. On the pc-scale, a strong, one-sided, 50 mas jet is directed to the west, away from a bright core component. Measurements of the apparent motion of components in the jet have yielded speeds between 2 and 4 times the speed of light [Walker, Benson, & Unwin 1987]. 3C120 is therefore the lowest red shift extragalactic superluminal radio source. The closest superluminal source is, of course, GRO J1655-40.
1228+127 (M87, NGC 4486, Virgo A) is the closest active radio source which is easily accessible with Northern Hemisphere VLBI arrays, at a distance of approximately 16 Mpc. On the kpc-scale, a complex radio and optical jet has been imaged with the VLA and HST [Sparks, Biretta, & Macchetto 1994]. On the pc-scale, a strongly one-sided jet has been observed with VLBI [Reid et al. 1989]. A subluminal, 
0.3c, speed has been measured for components within the pc-scale jet. Limb brightening and oscillations in the pc-scale surface brightness distribution have also been observed.
1652+398 (z=0.038) is a core dominated radio source associated with a BL Lac type object. The pc-scale morphology is extremely complex, consisting of a bright core component and a series of four elongated components ( 40 mas each) which extend away from the core for over 100 mas, separated by approximately 30 mas, at a position angle of approximately 45 . However, each of the components is orientated with major axes at position angles of approximately 135 . The kpc-scale radio structure has been imaged by Ulvestad, Johnston, & Weiler [1983], revealing a bright core and weak diffuse extended ( 10'') emission either side of the core at a position angle of approximately 45 .
1807+698 (z=0.051) is another core dominated radio source associated with a BL Lac type object. The pc-scale morphology consists of a bright core component and a straight jet at a position angle of approximately 
and extending 50 mas. The kpc-scale radio structure has been imaged [Ulvestad & Johnston 1984], revealing a bright core component with a surrounding diffuse halo of radius approximately 1'.