tokens: and wiggles a few times before ending at a hotspot 15′′ from the core. No corresponding features are detected in the X-ray band. Similarly, there are no clear knot associations in the HST image. 1116+128 (4C+12.39). The extended radio emission consists of a single knot at 25 northwest of the core. The knot is not detected in the Chandra data. No features are apparent in the HST image at the radio knot. 1303−827 (PKS 1302−82). The extended radio emission consists of a single knot at 65 southeast of the core and a knot pair about 16′′ north-northwest of the core. The X-ray jet searched was set to the southeast to include the closest knot. No knots are detected by Chandra . In the HST image, there is faint, resolved flux from the closer of the north-northwest knot pair, shown in a inset in Figure 6 . 1502+106 (B2 0954+25A). The VLBI jet is oriented at a PA of 120°, while the kpc-scale jet is at a PA of 160° (see Table 10 ) and is marginally detected. The VLA image of the jet published by Cooper et al. ( 2007 ) shows a continuous jet all the way to the termination, about 9′′ from the core. Lister et al. ( 2013 ) found a maximum apparent speed of VLBI knots of 17.5 c . The HST image shows no clear detection of any part of the kpc-scale jet. 1622−297 (PKS B1622−297). The kpc radio jet is weak and not detected with Chandra . There is a pc-scale jet at a PA of −70°, with a maximum apparent speed of 18.6 c (Lister et al. 2013 ). There are no apparent features in the HST image that are associated with radio or X-ray emission. 1823+568 (4C+56.27). There is a pc-scale jet at a PA of −160° with a maximum apparent speed of 26.17 c (Lister et al. 2013 ). The kpc-scale jet is first oriented almost due south, but bends about 1′′ from the core to the east, where it is clearly detected in the Chandra image at 25 from the core. There are no apparent features in the HST image that are associated with radio or X-ray emission, although the southern portion lies along a diffraction spike. 2201+315 (4C+31.63). The X-ray image was first published by Hogan et al. ( 2011 ). This quasar has VLBI components with apparent velocities up to 8.3 c along a PA of −145° (Lister et al. 2013 ). In the VLA image, the jet is −37′′ long at a PA of −110°, terminating in a hotspot (Cooper et al. 2007 ). To the northeast, there is a lobe about 45′′ from the core. The radio jet is detected in the Chandra data only out to about 4′′ from the core. The quasar was not part of our observing program, so we do not have an HST image of it. 2230+114 (CTA 102, 4C+11.69). There is a pc-scale jet at a PA of 160° with a maximum apparent speed of 8.6 c (Lister et al. 2013 ). There are radio-emitting knots to the northwest and southeast sides of the core but no clear association with X-ray emission. There are no apparent features in the HST image that are associated with the radio knots. 4. Discussion 4.1. Detection Statistics We detected 9 X-ray emitting jets among the 17 sources that complete our
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