The VSOP 5 GHz Active Galactic Nucleus Survey. III. Imaging Results for the First 102 Sources (original) (raw)

J0927+3902: (4C39.25) An image made from VSOP GOT data can be found in VSOPPR. The main component is slightly asymmetric, with a small component that is east of the main body of the source. Higher frequency USNO images suggest that the core is the more central, stronger component. J1058+0133: See VLBApls, USNO ,VLBA2cm1, and VLBA2cm2 for more detailed images of the extended emission to the northwest. Based upon the USNO higher frequency images, the core appears to be the easternmost component. J1107−4449: The image from the complete GOT data-set is given in VSOPsth. J1118+1234: See VLBA2cm2 for a more detailed image. The area subtended by the core is < 0.1 mas 2. J1146−2447: This is a GPS source (Stanghellini et al. 1997). The secondary component to the south coincides with the extended emission seen in the VLBApls and 8 GHz USNO images. J1147−0724: The core region extends westward towards the extended emission seen in the VLBApls, USNO and VLBA2cm1 images. J1147−3812: Faint emission to the east is also seen in some of the 8 GHz USNO images. J1215−1731: Stickel & Kühr (1996) were able to get an optical ID for this source, despite the close proximity of the star gamma Corvus. J1229+0203: (3C273) A VSOP image made from GOT data can be found in Lobanov & Zensus (2001). The four component model-fit does not include the large-scale structure. J1230+1223: (3C274, M87) A VSOP image made from GOT data can be found in Junor et al. (2000). The four component model fit only accounts for the small-scale structure. The faint core is unresolved subtending an area of < 0.05 mas 2. J1246−2547: The extension from the core is in the same direction as the extended emission seen in the VLBApls and VLBA2cm2 images. J1256−0547: (3C279) For the GOT images of this source see Piner et al. (2000). The core has been identified as the stronger, easternmost component (Piner et al. 2000). J1310+3220: Based upon 8, 24, and 43 GHz USNO images we have assumed the core to be the more easterly component. J1337−1257: The faint component to the west of the main component is seen in VLBA2cm1-15images after 1999, so it is probably a new component. J1357−1744: A VLBA image at 5 GHz (Frey et al. 1997) shows a weak, 10-mas scale bent jet extending towards the southeast and east. J1407+2827: (OQ208) The area subtended by the faint core is < 0.04 mas 2. J1507−1652: VLBA2cm1 images, as well as the 8 and 15 GHz USNO images, show extended structure to the south and southeast. This extended structure is not as apparent in our image due to poor sampling of the short (u, v) spacings. J1510−0543: The extended emission to the east seen in the VLBApls, VLBA2cm1, and VLBA2cm2 images is not seen in our image, probably due to the paucity of data on shorter baselines.