1. INTRODUCTION 2. SOURCE SELECTION
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1 THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 124:285È381, 1999 October ( The American Astronomical Society. All rights reserved. Printed in U.S.A. VLA IMAGES AT 5 GHz OF 212 SOUTHERN EXTRAGALACTIC OBJECTS R. I. REID Department of Astronomy, University of Toronto, 60 St. George Street, Toronto, ON, M5S 3H8, Canada; reid=astro.utoronto.ca P. P. KRONBERG Department of Physics, University of Toronto, 60 St. George St., Toronto, ON, M5S 1A7, Canada; kronberg=physics.utoronto.ca AND R. A. PERLEY National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM, ; rperley=nrao.edu Received 1998 July 24; accepted 1999 April ABSTRACT Maps of 212 extragalactic radio sources at 4.9 GHz are shown in Stokes I along with linear polarization vectors. The objects have a declination range of 0 to [35 and were chosen from the Hewitt & Burbidge quasar catalog with a spectral index less than [0.5 and the NVSS survey with a minimum 1.4 GHz Ñux density greater than 0 mjy. The observations were made with the Very Large Array in its B conðguration, and the images have a typical resolution of 2A. One hundred ninety-ðve objects were resolved; 8 of the sources are quasars, and another 51 have been identiðed as galaxies. Subject headings: galaxies: structure È polarization È quasars: general È radio continuum: galaxies 1. INTRODUCTION Most imaging surveys of radio jets have concentrated on the northern sky, mainly because the telescopes being used were in the northern hemisphere. In this paper we focus on imaging radio jets in as much of the relatively neglected southern sky as is easily accessible by the Very Large Array (VLA). Recent improved optical and X-ray data from the Hubble Space Telescope, ROSAT, and the coming generation of powerful southern ground-based optical telescopes are, and increasingly will be, short of valuable complementary radio images. This is due to the inherent difficulty that most synthesis radio telescopes (which are in the northern hemisphere) have in imaging at negative declinations. The observations presented here are in part a concentrated e ort to redress this situation as far as the VLA can reach ÏÏ into the southern sky. Radio-extended quasars and galaxies give important clues on the AGN and radio jet phenomenon. The more extended extragalactic radio sources provide some of the best laboratories for studying the physics of radio jets, in addition to radio lobeèintergalactic medium interactions. Additionally, we are using these results to augment the number of well deðned radio jets in a study of polarization alignment breaking (a form of weak gravitational lensing) in the jets due to intervening galaxy-scale masses (Kronberg, Dyer, & Ro ser 1996). The candidates for this survey were chosen with declinations from 0 to [35, without any limits in right ascension. This region is covered by the Northern VLA Sky Survey (NVSS) (Becker, White, & Helfand 1995), but our survey uses a higher frequency and the B conðguration of the VLA to achieve a signiðcantly higher resolution of roughly 2A. This is suitable for the detection of many new radio jets. Although our declination range does not overlap the large northern patch of the FIRST survey (Condon et al. 1998), its much smaller southern patch is included in our range, at a lower frequency (1.4 GHz) and resolution (5A) than our survey SOURCE SELECTION All of the sources were selected from the declination range [[35, 0 ]. Although the VLA can observe objects at declinations as low as [, [35 was chosen as a southern limit to broaden the range of hour angles at which the southernmost sources could be observed. This gave some Ñexibility in the scheduling of exposures and allowed multiple snapshots, hence better image quality, for some objects. To minimize the reobservation of sources that had already been well imaged, 0 was picked as a northern limit. The Ðrst list of candidates was the Hewitt & Burbidge (1989) catalog of quasars (HB89), from which 80 objects were chosen within the above declination range. A further requirement for selection was that the spectral index, a, had to be less than [0.5 (S P la). This was done to maximize the probability of the objects having extended structure, since compact quasars tend to have Ñat radio spectra, while sources with jets, being dominated by optically thin synchrotron radiation, have steeper integrated spectra. More precisely, 79 quasars were selected from HB89 using NED (Helou et al. 1995),1 and one map, [062706, turned out to have a serendipitous double-lobed radio source within its Ðeld, at 13h38m11s, [6 27@13A. (J2000 equatorial coordinates will be used throughout this paper, and sources will be designated by their J2000 right ascension and declination in the form hhmmss ^ ddmmss.) No limits in right ascension were imposed on the HB89 candidates, but they should not be considered uniformly distributed in right ascension. The other 131 objects were selected from the (then) partially completed NVSS survey (Condon et al. 1998) in 1995 October. At that time, the NVSS catalog only covered 23h to 4hm in right ascension for the declination range of this survey. We used a Ñux cuto of 0 mjy at 1.4 GHz, and a requirement that the sources be at least 3% polarized. The 1
2 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * ( -1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * ( -1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * ( -1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.25 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * ( -1, 1, 4, 16, 64) FIG. 1.ÈSource maps at 4.8 GHz. in with linear polarization. The contours, separated by a factor of 4 in brightness, show Stokes I. Dashed contours are negative. The length of line segments are proportional to the linear polarization ((Q2]U2)1@2) at their centers. 286
3 MHz MHz Pol. lines: 1 arcsec = 8.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = mjy/beam Peak flux = Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16, 64, 256, 24) MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 287
4 MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * ( -1, 1, 4, 16, 64, 256) Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 288
5 MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) MHz Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 289
6 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 1.25 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 290
7 MHz MHz Pol. lines: 1 arcsec = 0.5 Jy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Peak flux = E-02 Jy/beam Levs =6.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs =5.0E-04 * (-1, 1, 4, 16, 64) 291
8 MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 292
9 MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 6.32 mjy/beam Levs = 4.0E-04 * (-1, 1, 4) Pol. lines: 1 arcsec = 0.25 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 293
10 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) 294
11 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 295
12 MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256, 24) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 4.18E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 296
13 MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Peak flux = E-02 Jy/beam Levs = 5.0E-04 * ( -1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16) 297
14 MHz Pol. lines: 1 arcsec = mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 298
15 MHz MHz Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 1.25 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 299
16 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec =.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256, 24) 0
17 MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = 9.41 mjy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 1
18 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = 4.77E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = mjy/beam Levs = 4.0E-04 * (-1, 1, 4, 16) 2
19 MHz MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 3
20 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256, 24) MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 5.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256, 24) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 4
21 MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) A MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 1.0E-03 * ( -1, 1, 4, 16, 64) 5
22 B MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = mjy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) Pol. lines: 1 arcsec = mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16) 6
23 MHz MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 7
24 MHz MHz Pol. lines: 1 arcsec = 1.25 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 8
25 MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 9
26 MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 3
27 MHz MHz Pol. lines: 1 arcsec = mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.25 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64, 256) Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.1 mjy/beam Peak flux = mjy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 311
28 MHz Pol. lines: 1 arcsec =.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256, 24) 312
29 MHz Peak flux = 1.76E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16) MHz MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16) Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 313
30 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 314
31 MHz Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 8.0E-04 * (-1, 1, 4, 16, 64) 3
32 MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 316
33 MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Peak flux = Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64, 256) 317
34 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 318
35 MHz MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 3.97E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = 1.46E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16) MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 319
36 MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64, 256) 320
37 MHz MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 321
38 MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 4.89E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 322
39 MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = mjy/beam Levs = 4.0E-04 * (-1, 1, 4, 16) MHz MHz Pol. lines: 1 arcsec = 0.8 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = 0.2 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) 323
40 MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16) 324
41 MHz Pol. lines: 1 arcsec = 0.8 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 325
42 MHz MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Peak flux = E-02 Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64) 326
43 MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 327
44 MHz Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 328
45 MHz Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 329
46 MHz MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = 0.6 Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 8.0 mjy/beam Peak flux = 2.20 Jy/beam Levs = 8.0E-04 * (-1, 1, 4, 16, 64, 256, 24) MHz Pol. lines: 1 arcsec = 0.64 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 3
47 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = mjy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 331
48 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = E-02 Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16, 64) 332
49 MHz Peak flux = E-02 Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 333
50 MHz MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Peak flux = E-02 Jy/beam Levs = 4.0E-04 * ( -1, 1, 4, 16, 64) 334
51 MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 335
52 MHz Pol. lines: 1 arcsec = 0.32 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 336
53 MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) 337
54 MHz Pol. lines: 1 arcsec = 0.4 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16) 338
55 MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.1 mjy/beam Peak flux = mjy/beam Levs = 5.0E-04 * (-1, 1, 4) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 339
56 MHz Pol. lines: 1 arcsec = 0.8 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 1.25 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 3
57 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 341
58 MHz Peak flux = E-02 Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256, 24) 342
59 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.2 mjy/beam Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 343
60 MHz MHz Pol. lines: 1 arcsec = 6.25 mjy/beam Peak flux = Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16, 64, 256, 24) Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) 344
61 MHz Peak flux = E-02 Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = mjy/beam Levs = 4E-04 * ( -1, 1, 4, 16, 64) 3
62 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 346
63 MHz Peak flux = Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = mjy/beam Peak flux = Jy/beam Levs = 8.0E-04 * (-1, 1, 4, 16, 64, 256) 347
64 MHz MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 4.0E-03 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) 348
65 MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) 349
66 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 3.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 350
67 MHz Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 351
68 MHz MHz Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64) Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64) 352
69 MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 353
70 MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) Peak flux = mjy/beam Levs = 6.0E-04 * (-1.00, 1.000, 4.000) MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 354
71 MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec =.0 mjy/beam Peak flux = Jy/beam Levs = E-03 * (-1, 1, 4, 16, 64, 256) 355
72 MHz MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 8.0E-04 * (-1, 1, 4, 16, 64, 256) Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 8.0E-04 * (-1, 1, 4, 16, 64, 256) MHz MHz Pol. lines: 1 arcsec =.0 Jy/beam Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64, 256, 24) Peak flux = Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64, 256) 356
73 MHz Pol. lines: 1 arcsec = 4.0 mjy/beam Peak flux = Jy/beam Levs = 7.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 25.0 mjy/beam Peak flux = Jy/beam Levs =2.5E-03 * (-1, 1, 4, 16, 64, 256, 24) 357
74 MHz Pol. lines: 1 arcsec = 5.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256, 24) MHz Peak flux = Jy/beam Levs =7.0E-04 * (-1, 1, 4, 16, 64) 358
75 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = 0.6 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 359
76 MHz MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256, 24) Pol. lines: 1 arcsec = 5.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64, 256) 360
77 MHz Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz MHz Pol. lines: 1 arcsec = 0.25 mjy/beam Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) Pol. lines: 1 arcsec = 5.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 361
78 MHz MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 362
79 MHz Pol. lines: 1 arcsec =.0 mjy/beam Peak flux = Jy/beam Levs = 1.0E-03 * (-1, 1, 4, 16, 64, 256, 24) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 363
80 MHz Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 364
81 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 365
82 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64, 256) 366
83 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 6.27E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 367
84 MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = 7.20E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 368
85 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16) 369
86 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 370
87 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 5.0 mjy/beam Peak flux = Jy/beam Levs = 6.00E-04 * (-1, 1, 4, 16, 64, 256) 371
88 MHz Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) 372
89 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 373
90 MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) MHz Pol. lines: 1 arcsec = 2.0 mjy/beam Peak flux = E-02 Jy/beam Levs = 6.0E-04 * (-1, 1, 4, 16, 64) 374
91 MHz Peak flux = E-02 Jy/beam Levs = 4.0E-04 * (-1, 1, 4, 16, 64) 375
92 376 REID, KRONBERG, & PERLEY MHz Pol. lines: 1 arcsec = 0.5 mjy/beam Peak flux = E-02 Jy/beam Levs = 5.0E-04 * (-1, 1, 4, 16, 64) latter criterion favors the selection of objects with detectable radio jets. Preference was given to objects that showed any structure in the NVSS images, which have a resolution of A FWHM. The NVSS images were also examined to remove sources that were too large for us to properly image at 5 GHz in B array, and to amalgamate entries where one system would have its components listed as separate sources in the NVSS. 3. OBSERVATIONS AND DATA REDUCTION The observations were made using the VLA in its B con- Ðguration. They were split into two sessions, the Ðrst from 18: to 6: LST on 1995 November 3È4, and the second from 7:00 to :00 LST on 1995 November 29. Our choice of observing band was a compromise between two competing trends. The sample sources have steep spectra (a ¹ [0.5) which favored observing at a long wavelength. A short wavelength, however, provides better resolution and simultaneously reduces Faraday rotation (Pj2). We decided to observe in the 6 cm band, with sky frequencies of and GHz. This 0 MHz separation permits the detection of any extreme cases of Faraday rotation. No estimation of rotation measures has been done, however, and all polarization angles are presented as observed. Each object was nominally observed for 2 minutes (with some variation due to telescope travel time), but 11 received two snapshots, and seven received three snapshots for improved UV coverage and signal to noise. The choice of sources to bestow multiple snapshots upon was based on their right ascension (especially whether they were in the overlap zone between the November 3 and 29 observations) and the required telescope travel time. The typical rms noise in the images is 0.5 mjy beam~1, or 0.3 mjy beam~1 for the multiple snapshot images. A handful of maps have a higher limiting surface brightness of 1 mjy beam~1 due to the presence of a very bright source and CLEANing and/or calibration errors. The sensitivity of each map can be estimated from the lowest contour, which is set to where negative contours begin appearing. The data were calibrated before imaging using AIPS, partly at the NRAOÏs Array Operations Center in Socorro, NM, and partly at the University of Toronto. 3C 48 was observed for three minutes as a Ñux and polarization angle calibrator for the November 3 observation, and 3C 286 was observed for 6 minutes as the Ñux and polarization angle calibrator for the November 29 observation. The antenna polarization was calibrated by observing 0042]232 and 0854]198 (J2000) at several parallactic angles in the Ðrst and second sessions, respectively.
93 TABLE 1 OBJECT PARAMETERS R.A. Decl. Total Core Spectral Cat (J2000) (J2000) LAS z ID Morph Flux (Jy) Flux (Jy) Index Comments (1) (2) (3) (4) (5) (6) (7) (8) (9) () (11) HB [ Q P [0.85,c PKS HB [ Q P [0.76,c PKS NVSS [ G 2L]CJ [0.58,b PKS NVSS [ U 2L]C [0.63,a PKS,PMN,MRC,TXS NVSS [ U B ,b Same dir. as A2699. NVSS [ Q P ,b HB [ Q 2L [0.72,c 1987MNRAS S NVSS [ U P ,b NVSS [ U 2L [0.70,a NVSS [ Q P [0.00,b QCC NVSS [ G 2LJ]C [0.34,b Arp 256 gal pair NVSS [ Q 2L]J? [1.88,b * NVSS [ E 2L]C [0.88,b PKS NVSS [ U B [0.83,b PKS NVSS [ G 2L [0.35,b PKS * NVSS [ Q 2LJ]C [0.78,b PKS NVSS [ G 2LJ [0.7,a PKS * HB [ A 2L [0.71,b PKS, 4C, TXS, LBQS NVSS [ U 2L [0.92,a PKS NVSS [ U 2LJ]C [1.1,a PKS,MRC,PMN,TXS NVSS [ E 2L 0.38 [1.12,b PKS NVSS [ G 2L 0.11 [0.99,b PKS NVSS [ Q 2LJ]C? [0.81,b QCC NVSS [ U 2L]C [0.97,b PMN NVSS [ U C]2J [0.59,b PKS HB [ Q 2LJ]C [0.84,b NVSS [ G 2LJ]C [1.02,b 3C, 4C[01.03 NVSS [ Q P ,c PKS NVSS [ G 2L]JC [0.9,a * HB [ Q 2L]JC [0.82,b NVSS [ G 2L]C [0.98,b MCG[02[03[018 IRAS NVSS [ G CJ [0.93,b EDCC482 PKS NVSS [ Q 2L]C [0.89,b 4C06.04 NVSS [ U 2LJ]C [0.9,a PMN, MRC NVSS [ U 2LJ 0.37 [1.12,a 4C[03.02 PKS MRC IRAS NVSS [ U 2LJ]C [0.9,a PMN, MRC NVSS [ U 2LJ]C [0.85,a PKS NVSS [ G 2L [1.00,b PKS * NVSS [ U 2LJ [1.21,a PKS HB [ Q 2LJ]C [1.12,c PKS HB [ Q CJL? [0.90,c NVSS [ U 2L [1.20,a PKS NVSS [ Q 2LJ]C [0.46,c PKS, HB93 NVSS [ Q CL [0.28,c PKS NVSS [ Q B 0.83 [0.80,b * NVSS [ U 2JL]C [0.90,b NVSS [ G 2LJ]C [0.08,b MCG[02[04[0 NVSS [ U CJL [0.7,a NVSS [ U 2LJ]C [0.7,a 4C[05.04 NVSS [ U 2LJ]C [0.75,b NVSS [ G 2LJ]C [0.67,b PKS 4C[00.07 MRC TXS NVSS [ U 2LJ [1.0,a Core? NVSS [ G 2LJ [1.1,a * NVSS [ Q P ,b QCC NVSS [ U B [1.21,a PKS HB [ Q 2LJ]C [0.57,c PKS NVSS [ G 2L]CJ [1.00,b OC237 HB [ Q 2L]CJ [0.78,b PKS NVSS [ G 2LJ]C C[01.08 A0198, lost Ñux * HB [ Q 2LJ]C [0.54,c PKS NVSS [ G 2LJ]C [0.83,b PKS * NVSS [ U 2LJ]C 0. [1.32,a 4C[02.06 NVSS [ Q 2LJ]C [0.57,b QCC NVSS [ U 2L [0.92,b IRAS, 18 mjy P 0 ÏÏ to SW HB [ Q 2L]JC [0.61,c PKS NVSS [ G 2L 0.62 [1.00,a PKS * NVSS [ G 2LJ]C [0.96,a PKS, OC266 * NVSS [ G 2L]JC? [0.93,b 4C[01.09, Gal. pair NVSS [ G 2L]C [1.00,a PKS * NVSS [ Q 2L 0.78 [0.97,b TXS NVSS [ U 2LJ 0.22 [0.8,a PMN
94 TABLE 1ÈContinued R.A. Decl. Total Core Spectral Cat (J2000) (J2000) LAS z ID Morph Flux (Jy) Flux (Jy) Index Comments (1) (2) (3) (4) (5) (6) (7) (8) (9) () (11) NVSS [ G 2LJ [0.72,a PKS * HB [ Q 2LJ]C [0.79,c PKS NVSS [ G 2L 0.64 [0.9,a PMN * NVSS [ RG 2L]JC? [1.03,b Markarian gal nearby HB Q P [0.76,b MKN14 HB [ Q 2L]JC [0.68,c 3C57 NVSS [ U 2L]C [1.07,a PKS NVSS [ U 2LJ [0.4,a * NVSS [ G 2LJ]C [0.75,a PKS * NVSS [ U 2L]JC [1.00,a PKS NVSS [ G 2L 0.36 [0.61,b PKS * NVSS [ U 2L]JC [1.12,a PKS NVSS [ E 2L]C [0.70,b 3C62 HB [ Q 2LJ]C [0.72,c MC NVSS [ U 2L [1.1,a PMN HB [ Q 2LJ]C [0.65,c PKS HB Q P [0.68,c PKS NVSS [ U 2LJ]C [1.20,ab PKS HB [ Q 2L]CJ [0.80,c 4C01.11 NVSS [ U 2L]J [1.1,a PKS NVSS [ U 2L]JC 0.19 [0.9,a PMN NVSS [ U 2L]J [1.07,a PKS NVSS [ U 2L]C [1.00,a 4C[03.08 NVSS [ G 2L]C [1.,a PKS * HB [ Q 2L]JC [0.67,c PKS 4C[04.06, G ÏÏ away HB [ Q 2LJ? [0.79,c 4C02.12, LJ? NVSS [ G 2L [0.94,b PKS NVSS [ G 2L]JC [1.02,a PKS * NVSS [ Q CL ,c PKS HB [ Q 2L]CJ [0.53,c PKS NVSS [ G 2L [0.97,a PKS * NVSS [ U 2LJ]C [0.8,a PMN MRC TXS NVSS [ G 2LJ [1.6,a PKS * NVSS [ G 2L]J [0.76,a PMN * NVSS [ U 2L]J? [0.88,b MRC HB [ Q 2L]JC [0.70,c PKS NVSS [ U 2L]C [0.7,a PKS NVSS [ E 2L]C [0.41,b IRAS NVSS [ U 2L]C [1.05,a PKS NVSS [ E Fuzzy [1.12,b ESO NVSS [ Q CL [1.20,b PKS HB [ Q 2L]CJ [1.02,a PKS NVSS [ Q CJ [0.47,b * NVSS [ U CL? [1.12,a PKS, 2L? NVSS [ U 2L]C [1.,a 4C[03.12 NVSS [ G 2L]C [0.00,b PKS NVSS [ G 2L [0.13,b Sy2 NVSS [ Q CJ ,c PKS NVSS [ Q CL [0.18,b NVSS [ U 2L [1.02,a PKS, other source 3Ï to SW. NVSS [ Q 2L [0.88,b MRC PMN NVSS [ G 2L 0.69 [0.93,a PKS * NVSS [ E 2LJ]C [1.02,b PKS 4C[04.13 NVSS [ E 2L]C [0.08,b GSP 022 HB [ Q 2L]C [1.00,c HB [ Q 2L]JC [1.08,c 3C94 NVSS [ G 2L]JC [1.09,b PKS 4C[05., N galaxy NVSS [ G CJL [0.79,b PKS MRC TXS NVSS [ U 2L]CJ [1.02,a PKS NVSS [ Q 2LJ]C [0.83,b PKS 4C[05.16 NVSS [ U 2LJ]C [0.96,a PKS NVSS [ Q 2L]C [0.94,b PKS PMN MRC TXS 4C[02.16 HB [ Q 2LJ]C [0.75,c PKS HB Q P? 0.08 [0.63,c BL Lac NVSS [ U 2L]CJ [1.,a 3C112 HB [ Q P [0.95,c PKS HB [ Q 2LJ]C [0.90,c MC1, A0514 nearby HB [ Q P? [1.13,c HB [ Q 2LJ]C [0.78,c PKS HB [ Q 2L]JC [0.59,c PKS HB [ Q CJL [0.54,c PKS, VLBI ref HB [ Q Fuzzy [ [0.54,c PKS, BL Lac 378
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