A&A 386, 97-113 (2002)
DOI: 10.1051/0004-6361:20020119

The Parkes quarter-Jansky flat-spectrum sample

I. Sample selection and source identifications

C. A. Jackson ¹ - J. V. Wall ² - P. A. Shaver ³ - K. I. Kellermann ⁴ - I. M. Hook ² - M. R. S. Hawkins ⁵

1 - Research School of Astronomy & Astrophysics, The Australian National University, Mount Stromlo Observatory, Canberra, Australia
2 - Department of Astrophysics, University of Oxford, Nuclear and Astrophysics Laboratory, Keble Road,
Oxford OX1 3RH, UK
3 - European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
4 - National Radio Astronomy Observatory, Edgemont Road, Charlottesville, VA 22903-2475, USA
5 - Royal Observatory, Blackford Hill, Edinburgh EH3 9HJ, UK

Received 7 November 2001 / Accepted 22 January 2002

Abstract
We present a new sample of quarter-Jansky flat-spectrum radio sources selected to search for high-redshift quasars and to study the evolution of the flat-spectrum quasar population. The sample comprises 878 radio sources selected from the Parkes catalogues with spectral indices $\alpha^{5 \rm \thinspace GHz}_{2.7 \rm\thinspace GHz} \ge -$0.4 where $S_{\nu} \propto \nu^{\alpha}$. The sample covers all right ascensions and the declination range from $-80\hbox{$.\!\!^\circ$ }0$ to $+2\hbox{$.\!\!^\circ$ }5$, excluding low galactic latitudes ( $\mid b \mid < 10^{\circ }$) and the Magellanic Cloud regions. We have obtained improved radio source positions, firstly to reconfirm the majority of the existing identifications, and secondly, using digitized sky-survey data and deep B, Gunn-i and Gunn-z CCD-imaging, to find optical identifications for 223 previously-unidentified sources. We present the final catalogue of 878 flat-spectrum sources: 827 are compact radio sources identified with galaxies, quasars and BLLac objects, 38 have either extended radio structure or are identified with Galactic objects (PN, HII or non-compact radio source), 4 are obscured by Galactic stars, and 9 (1 per cent of the total sample) remain unidentified.

Key words: catalogues - radio continuum: galaxies - BL Lac objects: general - galaxies: general - quasars: general

1 Introduction

This is the first paper in a series of three describing the results of a program to search for high-redshift quasars and study the evolution of the flat-spectrum quasar population.

This paper (Paper I) sets out the sample, discussing its selection and the identification and reconfirmation programme to determine the optical counterparts to the radio sources. Paper II (Hook et al. in preparation) presents new spectroscopic observations and redshift determinations. Paper III (Wall et al. in preparation) considers quasar space distribution, the luminosity function and its epoch dependence. An earlier version of this sample was used by Shaver et al. (1996) to study the evolution of the quasar space density at redshifts greater than 3.

We selected our radio source sample from the machine-readable version of the composite Parkes radio source catalogue (PKSCAT90: Wright & Otrupcek 1990). This catalogue comprises radio and optical data collected for 8264 radio sources for the sky south of +27$^{\circ}$, excluding the Galactic Plane and Magellanic Cloud regions. The catalogue was compiled from major radio surveys at 2.7  GHz undertaken by John Bolton and colleagues over the years 1969 to 1979 (Bolton et al. 1979 and references therein).

Samples extracted from PKSCAT90 contain source-identification information compiled over the last 30 years or more in numerous collaborations, resulting in several complete or near-complete samples, e.g. the 2-Jy sample (Wall & Peacock 1985), the Parkes Selected Regions (Downes et al. 1986; Dunlop et al. 1989, 1991) and the Parkes half-Jansky sample (Drinkwater et al. 1997).

Our goal was to obtain a spectroscopic sample of flat-spectrum radio-selected quasars, free of optical selection effects and complete at high redshifts. Starting with a sample selected from PKSCAT90 and the identifications therein we therefore had to ensure that we (i) identified the remaining PKSCAT90 sources and (ii) obtained redshifts for all candidate quasars in the sample, with priority given to those north of $-40^{\circ}$ declination.

The results of our selection, identification and confirmation programme are described in this paper as follows. Section 2 gives the selection criteria for the sample and some characteristics of the identified and empty field sources. In Sect. 3 we describe the procedure for identifying the PKSCAT90 empty-field sources and in Sect. 4 we analyse the reliability of the complete sample. In Sect. 5 we present the full catalogue and in Sect. 6 we summarise the characteristics of the final sample.

2 Radio source selection

The sample of flat-spectrum radio sources was selected from PKSCAT90 using the following criteria -

1.

$-80\hbox{$.\!\!^\circ$ }0 < \delta$ (B1950) $< +2\hbox{$.\!\!^\circ$ }5$, all right ascensions;

2.

$\alpha_{2.7 \rm\thinspace GHz}^{5.0 \rm\thinspace GHz} > -0.4$, where $S \propto \nu ^{\alpha }$;

3.

Galactic latitude $\mid b \mid > 10^{\circ}$.

Sources lying within the Magellanic Cloud regions (B1950 RA, Dec = 04 30 hrs to 06 30 hrs, -64$^{\circ}$ to -75$^{\circ}$ for the LMC and 00 hrs to 02 hrs, -69$^{\circ}$ to -76$^{\circ}$ for the SMC) were excluded from our sample. We also checked the 2.7  GHz and 5  GHz flux densities extracted from PKSCAT90 against the original survey papers listed in Table 2. A number of sources have more recent flux density measurements recorded by PKSCAT90; we replaced these with the original survey flux densities for consistency. In addition, we find 10 sources in PKSCAT90 which are not in the original survey papers (Table 1): 3 of these sources lie in regions not covered by the original Parkes surveys. The other 7 sources are within the original survey areas listed in Table 2 but are not in the original survey papers.

 

 

Table 1: PKSCAT90 sources not in original Parkes Survey papers.

Source	Region(1)
PKS B0522-030	A
PKS B0528-454	J
PKS B0549-459	J
PKS B1131-115	B
PKS B1150-723	K
PKS B1159-515	H
PKS B1718-649	X
PKS B1730-130	X
PKS B1801+010	X
PKS B2111+015	A

Notes: (1) The original Parkes survey region (see Table 2).

A cut-off value of -0.4 for the spectral index was applied to minimize the number of extended or non-core-dominated radio sources in the sample. However, such sources still contaminate the sample, due to one or more of the following reasons:

1.

Flux density uncertainties: the original Parkes survey flux densities at 2.7  GHz and 5  GHz have uncertainties of ((0.02)² + (0.03S)²)^0.5. Therefore there will be objects with $\alpha^ {5 \rm \thinspace GHz}_{2.7 \rm\thinspace GHz} < -0.4$ in the sample.

A few nearby sources have a different type of flux-density error, due to diffuse lobe emission that has been poorly mapped and errors in one or both flux densities can result in $\alpha^ {5 \rm \thinspace GHz}_{2.7 \rm\thinspace GHz} < -0.4$. PKS B0123-016 (3C40) is a case in point.

2.

Confusion: the Parkes beam sizes of 8 arcmin at 2.7  GHz and 4 arcmin at 5  GHz result in occasional instances of source confusion.

3.

Source variability: there are two effects here. The first is due to the time interval between the 2.7  GHz and 5  GHz flux density measurements; a number of steep-spectrum sources are included in our sample whilst a number flat-spectrum sources are missed as the source varied. The second effect is that neither flux density determination measured the mean source flux density, with the result that a number of sources are missed or included depending on their activity at the time of the survey. Drinkwater et al. (1997) analysed the magnitude of these effects for the 0.5-Jy Parkes survey sample which has a steeper spectral-index selection ( $\alpha_{2.7 \rm\thinspace GHz}^{5.0 \rm\thinspace GHz} > -0.5$) and concluded that 1) the time lag between the surveys includes about 3 per cent steep-spectrum sources and misses a similar proportion of true flat-spectrum sources, and 2) the difference between the Parkes survey flux densities and mean flux densities results in $\sim$11 per cent of the sample having mean flux densities below any survey area's flux density limit, whilst $\sim$8 per cent of sources are missed. The latter bias is inherent in any single-epoch flux-limited sample.

To assess the magnitude of these effects we have compared 694 sources common to our sample and NVSS (Condon et al. 1998). We find that the vast majority - 663 out of 694 (96 per cent) - are either compact (unresolved by NVSS, major axis <15 arcsec) or are extended sources with an obvious dominant radio core so that unambiguous identification is possible. Thus we conclude that the incidence of non-core dominated, steep-spectrum sources in our complete sample is less than 5 per cent.

 

 

Table 2: The Parkes Survey regions.

			$S_{\rm lim,\, 2.7~\rm GHz}$
Area	Dec range	RA range	/ Jy	Reference	N(1)
A	+2 $.\!\!^\circ$5 to -4$^{\circ}$	7$^{\rm h}$20 to 17$^{\rm h}$50, 19$^{\rm h}$40 to 6$^{\rm h}$	0.25(2)	Wall et al. (1971)	147 (+2)
B	-4$^{\circ}$ to -15$^{\circ}$	10$^{\rm h}$ to 15$^{\rm h}$	0.25	Bolton et al. (1979)	56 (+1)
C	-15$^{\circ}$ to -30$^{\circ}$	10$^{\rm h}$ to 15$^{\rm h}$	0.25	Savage et al. (1977)	65
D	-4$^{\circ}$ to -30$^{\circ}$	22$^{\rm h}$ to 5$^{\rm h}$	0.25	Wall et al. (1976)	157
E	-4$^{\circ}$ to -30$^{\circ}$	5$^{\rm h}$ to 6$^{\rm h}$30, 8$^{\rm h}$ to 10$^{\rm h}$
		15$^{\rm h}$ to 17$^{\rm h}$, 19$^{\rm h}$ to 22$^{\rm h}$	0.6	Bolton et al. (1975)	64
F	-18 $^{\circ}.8\pm2^{\circ}.6$	22 $^{\rm h}\pm2\hbox{$.\!\!^\circ$ }6$	0.10	Wall et al. (1971)	9
G	-30$^{\circ}$ to -35$^{\circ}$	9$^{\rm h}$ to 16$^{\rm h}$30, 18$^{\rm h}$30 to 7$^{\rm h}$15	0.2	Shimmins & Bolton (1974)	91
H	-33$^{\circ}$ to -75$^{\circ}$	3$^{\rm h}$, 11$^{\rm h}$, 19$^{\rm h}$, 23$^{\rm h}$	0.25	Shimmins (1971)	66 (+1)
I	-35$^{\circ}$ to -45$^{\circ}$	10$^{\rm h}$ to 15$^{\rm h}$, 19$^{\rm h}$ to 7$^{\rm h}$	0.25	Bolton & Shimmins (1973)	79
J	-45$^{\circ}$ to -65$^{\circ}$	0$^{\rm h}$ to 3$^{\rm h}$, 4$^{\rm h}$ to 8$^{\rm h}$30
		17$^{\rm h}$30 to 19$^{\rm h}$, 20$^{\rm h}$ to 23$^{\rm h}$	h 0.5	Wall et al. (1975)	74 (+2)
K	-65$^{\circ}$ to -75$^{\circ}$	0$^{\rm h}$ to 24$^{\rm h}$	0.25	Bolton & Butler (1975)	32 (+1)
L	-75$^{\circ}$ to -80$^{\circ}$	0$^{\rm h}$ to 24$^{\rm h}$	0.2	Shimmins & Bolton (1972)	28
X	all other areas	not covered by original Parkes surveys	0.25	PKSCAT90	3

Notes: (1) Number of sources each region contributes to our sample. The number in parenthesis is the number of sources which are in this region but not in the referenced paper (see Table 1). (2) Region A includes 21 sources lying in 5 regions, each of 40 square degrees with $S_{2.7 \rm ~ GHz}$ = 0.1  Jy as shown in Fig. 1.

Figure 1: Sky distribution of the Parkes quarter-Jansky flat-spectrum sources within the Parkes survey regions. Radio sources identified with galaxies and stellar objects are shown as circles with the size of the circle being proportional to the 2.7  GHz flux density. Parkes 2.7  GHz survey limits are shown in shades of grey, from dark to light, equating to $S_{2.7 \rm ~ GHz}$ of 0.10, 0.20, 0.25 and 0.60 Jy. Sources in the Magellanic Cloud regions and near the Galactic equator ( $\mid b \mid < 10^{\circ }$) are excluded from the sample.

Open with DEXTER

Figure 1 shows the distribution of the 878 quarter-Jansky sample sources within the Parkes survey regions. Of these, 645 have an optical identification given in PKSCAT90, with the majority, 535 (82 per cent), with stellar objects (quasars or BL Lacs). Moreover, it is the brighter radio sources which are identified, leaving the majority of the 247 unidentified (Parkes empty-field) sources with 2.7  GHz flux densities below 0.6  Jy (Fig. 2). In contrast, the distribution of spectral indices between identified and unidentified sources is unbiased (Fig. 3).

	Figure 2: 2.7  GHz flux density distributions for the quarter-Jansky sample (open histogram). Flux densities for our 223 new identifications shown hatched and the 9 remaining empty fields shown solid fill.
Open with DEXTER

	Figure 3: 2.7-5  GHz spectral index distributions for the quarter-Jansky sample ( $S \propto \nu ^{\alpha }$) (open histogram). Spectral indices for our 223 new identifications shown hatched and the 9 remaining empty fields shown solid fill.
Open with DEXTER

3 The identification procedure

Identification of the PKSCAT90 empty-field sources was carried out as follows:

1.

Accurate radio positions to better than 1 arcsec were obtained for all PKSCAT90 empty-field sources (Sect. 3.1).

2.

The COSMOS digitized sky survey database was interrogated at the new radio positions to find candidate source identifications (Sect. 3.2).

3.

Where no candidate was found from the COSMOS database, deep CCD images were taken through blue and red filters (Sect. 3.3).

4.

We then obtained low-dispersion spectra for all stellar identifications, as these are potential high-redshift (z > 3) quasars (Paper II).

5.

A random subset of COSMOS candidate identifications was also imaged to assess the incidence of blending of faint objects by COSMOS which would otherwise result in mis-identifications.

6.

The reliability of the total sample was then assessed (Sect. 5): (i) for the new identifications; (ii) for the existing PKSCAT90 identifications.

3.1 Radio observations

Refined radio positions are necessary to identify the empty field sources as the original Parkes radio positions are accurate only to $\sim$10-15 arcsec. We obtained these data for 72 of the empty field sources via our own observations with the Very Large Array (VLA) and Australia Telescope Compact Array (ATCA).

For 63 sources south of declination -30$^{\circ}$ the ATCA was used in the "6D'' configuration to obtain accurate radio positions. On 27 September 1993 observations were made at 4.80 and 8.64  GHz with orthogonal linear polarisations and a bandwidth of 128  MHz. The synthesised beam at 4.80  GHz was 2 arcsec FWHM (east-west). Each source was observed in typically three 45-s cuts widely spaced in hour angle, and these one-dimensional cuts were later combined to determine the source position. Secondary position calibrators were interspersed regularly throughout these observations. The flux density scale was based on the ATCA primary calibrator, PKS 1934-638.

In 1994 and 1995 we used the VLA to determine accurate positions of 29 previously unidentified sources. Most of these are are declinations north of $-30^{\circ}$ but a few are as far south as $-41^{\circ}$. The observations were made at 8.4  GHz with the VLA in its "A'' or "B''configuration with corresponding resolutions of 0.4 to 1.2 arcsec. Each programme source was covered with a single "snapshot'' scan typically of about four minutes duration, and each group of snapshots was preceded and followed by scans on a phase calibrator whose rms position uncertainty is not more than 0.1 arcsec in each coordinate. The flux density scale was based on an assumed value of 5.2 Jy for 3C 286.

The VLA data were edited and calibrated using the AIPS software package.

The remainder of the new radio positions were obtained from both previously published and unpublished results. The origin of each position is shown in the final catalogue (Appendix A). All radio positions used in the identification process are accurate to better than 1 arcsec in each coordinate. Throughout, B1950 positions were used, and where necessary the STARLINK SLALIB and COCO routines have been used to convert from other epochs and equinoxes.

Our VLA and ATCA observations revealed four sources with extended radio structures and no well-defined position or obvious optical counterpart. A further five Parkes sources were undetected at the VLA. For these, we found no evidence of any compact structure stronger than 0.5 mJy within 1 arcmin of the Parkes position. They are coded as "NCS'' (non-compact radio sources) in the final catalogue (Appendix A) and no optical identification was attempted.

3.2 Optical identifications using sky survey data

The plates of the ESO/SERC Southern Sky Survey were taken with a IIIa-J emulsion and a GG395 filter to give the photographic blue passband $B_{\rm J}$ (3950 Å-5400 Å), with a limiting magnitude ( $m_{B_{\rm J}}$) of approximately 22.5. These plates were digitized with the COSMOS plate-measuring machine at the Royal Observatory Edinburgh (Yentis et al. 1992). The COSMOS database was used to generate finding charts two arcmin-square centered on the radio position. Details of the COSMOS object nearest to the radio position were recorded.

There is an error in the stored coordinates in the COSMOS database arising from the precession calculations used to construct the database at ROE. The effect of this is that the positions stored in the COSMOS database are not J2000 but are close to B2000 (see Drinkwater et al. 1995 for a full discussion). As a result the "B1950'' positions produced from COSMOS are also incorrect. As the COSMOS positions have been constructed using the "FK4'' catalogue there is no mean systematic offset in the COSMOS positions from the (FK4) SAO catalogue. However, there is a systematic offset between COSMOS and the newer (FK5) Positions and Proper Motions (PPM) catalogue (Roeser et al. 1994). The PPM catalogue is more accurate than the SAO catalogue in that the FK5 system is closer to an inertial reference frame. For the level of astrometric accuracy required by this project, the COSMOS coordinates must be corrected by reference to an FK5 catalogue.

In order to correct the COSMOS "B1950'' positions to true B1950 positions for each field, (x,y) positions for approximately 12 of the faintest PPM stars around each radio position were measured on the ESO R survey plate using the PDS plate-measuring machine at the Royal Greenwich Observatory. The ESO R survey was chosen as the images are smaller, less saturated than deeper surveys, and hence a more accurate determination of the star centres was possible. Where the ESO R survey was not available the UKST IIIa-J survey was used. The (x,y) coordinates were transformed to (RA, Dec) coordinates using a 6-coefficient fit to Schmidt distortion geometry using STARLIB ASTROM. Each COSMOS "B1950'' position was then corrected from the average of the offsets.

With the corrections applied, we initially took the nearest COSMOS-database object to the radio position as the optical counterpart. A Gaussian fitted to the radio - optical offsets revealed an rms scatter of $\sim$1.12 arcsec in each coordinate. We therefore took a maximum offset of 3.6 arcsec ($\sim$3$\sigma$) in each coordinate as the identification criterion.

Objects which were obviously extended or were found to have narrow-line spectra (Paper II) were classified as galaxies, the remainder as stellar objects. If a candidate was close to the sky survey plate limit ($b_{\rm J}$ $\sim22$), in the absence of other data for the object we conservatively classified it as stellar.

Using the COSMOS database, we found identifications for 136 of the PKSCAT90 empty-field sources, comprising 107 stellar objects and 29 galaxies. The galaxy identifications were confirmed via visual inspection of the sky survey plates, as often faint objects in close proximity are merged by the COSMOS digitization process and then erroneously recorded in the database as a single object (usually a "galaxy'').

3.3 CCD Imaging

To identify the 87 sources which had no candidate identification from the COSMOS database we conducted a programme of deep CCD-imaging using the ESO Faint Object Spectrograph and Camera (EFOSC1) at the Cassegrain focus of the ESO 3.6m-telescope. Six observing sessions were undertaken at the telescope, as shown in Table 3.

 

 

Table 3: ESO 3.6-m imaging observations.

	Number of
Dates	nights used
20-23 April 1993	3
10-14 November 1993	4
10-12 May 1994	2
5-8 October 1994	3
26-29 April 1995	2
23-25 October 1995	3

ESO filters #552 (B), #614 (Gunn-i) and #615 (Gunn-z) were used for imaging on EFOSC1, using photometric standards from Stobie et al. (1985) and Landolt (1992). Typical integration times were 5 min in B and 10 min in Gunn-i and Gunn-z filters.

The raw FITS-format CCD images obtained with EFOSC1 were reduced using the Image Reduction and Analysis Facility ( IRAF) version 2.10, developed at NOAO. The radio source position (x,y) was aligned onto the CCD frames via the STARLINK ASTROM routine using the positions of approximately 12 faint stellar objects on the CCD frame. The corrected COSMOS B1950 positions of these stellar objects were transformed using a 6-coefficient fit which was accepted when the rms residual reduced to 0.3 arcsecs. In many cases we obtained more than one exposure per radio source so that an (x,y) solution was required for each frame. All frames were then manually examined for candidate objects.

For a source to be accepted as the optical counterpart we adopted the same 3$\sigma$ criterion as for the COSMOS identifications. For the accepted identifications we find that the CCD-based identifications have a wider Gaussian spread of radio - optical offsets as shown in Fig. 4 and Table 4 with the CCD identifications generally associated with fainter optical sources (Fig. 5).

	Figure 4: Position offsets in RA and dec for the 223 new identifications. Identifications from COSMOS are shown as "1'' and those from CCD imaging as "2''.
Open with DEXTER

 

 

Table 4: Radio-optical position offsets.

		$\langle\Delta {\rm RA}\rangle$	$\sigma_{\rm RA}$	$\langle\Delta {\rm Dec}\rangle$	$\sigma_{\rm Dec}$
Identification	N	/arcsec	/arcsec	/arcsec	/arcsec
COSMOS-survey	136	-0.06	0.89	-0.04	0.85
CCD images	87	0.07	1.12	0.03	0.96

	Figure 5: Position offsets (radial) for the 223 new identifications. Identifications from COSMOS are shown as "1'' and those from CCD imaging as "2''.
Open with DEXTER

Our CCD-imaging programme resulted in identifications for 87 sources. These identifications comprise 37 stellar objects and 50 galaxies. In Appendix D we show the CCD images, each 2 arcmin square, centred on the new identifications. The classification of type (stellar object/galaxy) was based on observed morphology. For 31 sources (23 stellar objects and 8 galaxies) we have confirmed their classifications via low-resolution spectroscopy (Paper II).

4 Reliability of the new identifications

There is the possibility that erroneous identifications have been made with objects lying close to the line-of-sight of the radio source. The uncertainty in the radio and optical positions and the density of objects on the survey plate or CCD exposure both determine the chance coincidence of a non-radio source being identified in error. Contamination due to foreground objects is fairly obvious where the object is a galactic star but not so obvious when the object is a faint galaxy.

The background faint-galaxy density was determined by examination of the deepest CCD exposures in each of the filters. The count of the galaxy density at the CCD imaging limit ( $m_{\rm B} = 24.5$) is found to be 12 faint galaxies per square arcmin in B, 13 per square arcmin in Gunn-i ( $m_{{\rm Gunn}-i} = 23.5$) and 9 per square arcmin in Gunn-z ( $m_{{\rm Gunn}-z} = 25.0$). There is a 10 per cent chance of a faint galaxy falling within the search area for any one identification. In the majority of identifications the candidate is a far brighter object so that the chance of it being an erroneous identification is remote. However, there are 38 faint galaxy identifications ( $m_{\rm B} \ge 23$), so that 4 are potential spurious identifications. We find that the rms radio minus optical offsets for these 38 faint galaxy identifications is larger (RA, dec: 1.19, 0.92 arcsec) than those for the brighter identifications (RA, Dec: 0.93, 0.89 arcsec).

The new identifications can therefore be considered as being reliable, although this is inevitably a function of magnitude. Additional confidence in the identifications is provided by the histogram of $m_{\rm B}$ magnitudes for the new identifications (Fig. 6). The decline in new identifications occurs around $b_{\rm J}$ =23, i.e. at about one magnitude brighter than the limiting magnitude of our CCD-images.

	Figure 6: Distribution of optical $b_{\rm J}$ magnitudes for all galaxy, quasar and BL Lac sources in the quarter-Jansky sample, with our new identifications shown hatched.
Open with DEXTER

5 The sample

5.1 Sample catalogue

The catalogue of the quarter-Jansky sample is presented in Appendix A. Finding charts, images and additional notes on individual sources are given in Appendices B, C and D.

The identification classes in our catalogue, column 8, are as follows. G = galaxy, and in this we have subsumed the PKSCAT90 classes "DB'', "E'' and "Sey'', defining sub-categories of galaxies (double, elliptical and Seyferts respectively). Q = quasar, confirmed spectroscopically or via UVX measurement, while Q* = quasar by virtue of coincidence between the position of a stellar object and an accurate radio position, and Q? is an unconfirmed quasar, a stellar object coincident with a Parkes survey radio position.

5.2 Catalogue reliability

In the course of constructing the final catalogue and subsequent to the analysis of Shaver et al. (1996) we have reassessed the data contained in the entire catalogue. Our primary aim is to ensure that we have not overlooked any z > 5 candidate quasars in the sample, particularly due to errors in PKSCAT90. For the 233 new identifications discussed in Sect. 3 we are confident in that there are no undiscovered high-redshift quasars.

We use digitized material from the UKST IIIa-J and UK SES R surveys along with the best-available radio positions to check every one of the 878 sources in our sample. The overlays of the radio position on the sky survey data is shown in Appendix C.

We find 10 radio sources for which we cannot confirm the identification (see Table 5). Of these 10, one source, PKS B0141-060 lies within an area already covered by the Sydney University Molonglo Sky Survey (SUMSS, Bock et al. 1999) at 843 MHz: This is clearly a complex, extended source so this is classified as a non-compact source (NCS).

Of the remaining 9 sources, 3 have radio positions catalogued by NVSS (Condon et al. 1998): PKS B0225-065, PKS B0415-029 and PKS B0522-030. There is no more recent radio survey data from which to confirm the validity of the other 7 sources. As an interesting point of note, three of the remaining unidentifiable PKSCAT90 sources in Table 5 do not appear in the original Parkes survey papers (Table 2): That such a significant fraction of the non-Parkes survey sources cannot be identified suggests that they are either highly variable or that their existence is questionable.

	Figure 7: Optical $b_{\rm J}$ magnitudes vs. radio flux densities ($b_{\rm J}$ vs. $S_{2.7 \rm ~ GHz}$) for 150 galaxies ($\bullet$) and 677 stellar objects ($\circ$, quasars and BLLacs) from the quarter-Jansky radio sample.
Open with DEXTER

Considering the PKSCAT90 identifications we find that two sources, PKS B0225-065 and PKS B1150-723 are identified as galaxies. However, as we find no evidence to support this, we code these sources to "e'' for an elimated PKSCAT90 identification. Another source, PKS B0551-538 is classified as "Xg'' in PKSCAT90, indicating at least one galaxy within the Parkes radio position error box. We code this as an empty-field source (X). Two sources are PKSCAT90 empty-field sources ("Xs'' and "Xsa'') and were overlooked in our identification campaign and remain empty fields (X). The remaining four PKSCAT90-blank coded sources also are coded as empty-fields (X).

 

 

Table 5: PKSCAT90 previously-identified sources de-identified as a result of arcsec-radio positions.

Original
Parkes	PKS B1950	PKSCAT90	$S_{2.7 \rm ~ GHz}$	$S_{\rm lim}$	New
survey	name	Id	/ Jy	/ Jy	Id
Y	B0141-609	Xg	0.17	0.25	NCS
Y	B0225-065	G	0.35	0.25	e
Y	B0415-029	Xs	0.16	0.25	X
N	B0522-030	Xsa	0.06	0.25	X
N	B0528-454	blank	0.39	0.25	X
N	B0549-459	blank	0.32	0.25	X
Y	B0551-538	Xg	0.27	0.25	X
Y	B0619-468	blank	0.43	0.60	X
Y	B0715-663	blank	0.43	0.25	X
N	B1150-723	G	0.82	0.25	e

For the PKSCAT90 confirmed identifications we have assessed the stellar identifications as follows: Q = quasar, confirmed spectroscopically or via UVX measurement, while Q* = quasar by virtue of coincidence between the position of a stellar object and an accurate radio position, and Q? is an unconfirmed quasar, a stellar object coincident with a Parkes survey ($\sim$10-15 arcsec) radio position.

Furthermore, we have checked all redshifts in the table by searching the original references. Numerous errors in the PKSCAT90 listing were found. Full references for the redshifts appear in Appendix A, and Appendix B gives full details of updates to PKSCAT90 data.

6 Sample characteristics

6.1 Optical magnitude distribution

The distribution of $b_{\rm J}$ magnitudes for the sample is shown in Fig. 6; our new identifications (inevitably) lie at the faint end of the distribution and show that the total distribution is mildy bimodal with a main peak at $b_{\rm J}=19.5$ mag and a subpeak near $b_{\rm J}$  = 22.5 mag.

Figure 7, a plot of the sample in $b_{\rm J}$ magnitude vs. $S_{2.7 \rm ~ GHz}$ with indication of object type, shows that galaxies dominate at faint flux densities and faint $b_{\rm J}$ magnitudes. Considering identification-fraction as a function of $b_{\rm J}$ magnitude (Fig. 8) we see that quasars dominate between $b_{\rm J}=16$ to 22, and that the spectroscopically-confirmed BL Lac objects comprise 5 to 10 per cent of the sample at all $b_{\rm J}$ magnitudes. However, this latter result should be treated as a lower limit only, as we do not have complete spectroscopic measurements for all stellar sources.

6.2 Source types as a function of 2.7 GHz flux density

As a function of flux density (Fig. 9), the galaxies are significant (i) at bright flux densities (the cores of active nearby ellipticals) and (ii) towards the faint flux densities ( $S_{2.7 \rm ~ GHz}$ $\sim$ 0.2  Jy). The increase in the galaxy fraction at fainter flux densities has also been observed in other radio samples (Falco et al. 1998) and probably comprises peaked-spectrum or compact symmetric radio galaxies.

The set of histograms of Fig. 10 shows how the $b_{\rm J}$ magnitude distribution changes with decreasing 2.7  GHz flux density. The brightest radio sources have a peaked distribution around $b_{\rm J}$  = 18.5; there is no hint of bimodality as there is little intrusion of the flat-spectrum population of faint galaxies. As radio flux density decreases and the flat-spectrum galaxies appear, the distribution takes on the bimodal shape, which continues below $S_{2.7 \rm ~ GHz}$ = 0.25  Jy. As first noted by Bolton (1970), the median of the distribution shifts to fainter magnitudes as flux density decreases, an effect seen in subsequent studies (Browne & Wright 1985; Drinkwater et al. 1997).

	Figure 8: Proportions of identified source types by optical $b_{\rm J}$ magnitude in the quarter-Jansky sample.
Open with DEXTER

	Figure 9: Proportions of the identified source types by $S_{2.7 \rm ~ GHz}$ in the quarter-Jansky sample.
Open with DEXTER

	Figure 10: Optical $b_{\rm J}$ magnitude distributions a) for sources with $S_{2.7 \rm ~ GHz}$ $\ge$ 2.0  Jy b) for sources with $S_{2.7 \rm ~ GHz}$ $\ge$ 0.50  Jy c) for sources with $S_{2.7 \rm ~ GHz}$ $\ge$ 0.25  Jy and d) for sources with $S_{2.7 \rm ~ GHz}$ < 0.25  Jy. Legend: hatched regions indicate galaxy identifications, open histogram regions quasar plus BL Lac identifications.
Open with DEXTER

6.3 Redshift distribution

The redshift distribution is shown in Fig. 11. There is some dependence on flux density in that the distribution for the fainter sources of the sample - those with flux densities in the range 0.25 $\le$ $S_{2.7 \rm ~ GHz}$ < 0.5  Jy - is flatter and biased to significantly higher redshifts than that for all sources with $S_{2.7 \rm ~ GHz}$ $\ge$ 0.25  Jy.

6.4 Spectral index distributions

The distributions of spectral indices for galaxies and stellar objects (quasars and BLLacs) are compared in Fig. 12. A K-S test reveals that there is only a 2.3 per cent probability that the two distributions are drawn from the same population. The galaxy identifications have generally steeper spectra; their distribution is suggestive simply of an extended tail to the classical (low-frequency survey) distribution with its peak around $\sim$-0.8. The quasar plus BLLac distribution gives indication of the bimodality seen so clearly in samples selected at frequencies above 2.7  GHz. In these sources the flat-spectrum peak is identified with beamed emission.

	Figure 11: Redshift distribution for the quarter-Jansky sample sources $S_{2.7 \rm ~ GHz}$ $\ge$ 0.25  Jy (unfilled histogram). For comparison sources with 0.25 $\le S_{2.7~ \rm GHz} <$ 0.50  Jy are shown hatched.
Open with DEXTER

	Figure 12: Spectral index distributions ( $\alpha^{5 \rm \thinspace GHz}_{2.7 \rm \thinspace GHz}$) by identified source types in the quarter-Jansky sample sources. Left - galaxies; right - quasars and BL Lac objects.
Open with DEXTER

7 Summary

In a sample of 878 flat-spectrum sources selected from PKSCAT90, observations to obtain accurate radio positions and optical imaging data have resulted in optical counterparts for 223 previously unidentified sources. The sample catalogue presented here contains 827 compact radio sources identified with galaxies, quasars and BLLac objects, 38 sources either resolved or identified with Galactic objects, and 4 sources whose fields are optically contaminated by bright stars. Just 9 sources (1 per cent) remain unidentified. From this total sample, complete flux-density limited samples can be selected; for example for sources north of $-40^{\circ}$ declination in regions where the survey limit is $\ge$0.25 Jy there are secure identifications for 418 out of 419 sources (99.8 per cent).

Further to our comprehensive checking of the existing PKSCAT90 data and our new identifications, we conclude that

• it contains no z > 5 objects, and
• the increasing contribution of galaxies in the sample below about 0.2 Jy is real and these are probably peaked-spectrum or compact symmetric sources.

The sample highlights why completion of optical identifications is difficult even for flat-spectrum compact samples: at faint flux-density levels ( $S_{2.7 \rm ~ GHz}$ < 0.3  Jy) a significant fraction of the host objects are faint red galaxies.

Acknowledgements

We thank Dick Hunstead, Alok Patnaik, John Reynolds, Ann Savage and Niven Tasker for providing radio positions in advance of publication. We also thank Dave McConnell and Bob Sault for assistance with the ATCA observations and analysis, Benoit Germain for his work with the optical data reduction and John Pilkington for carrying out the PDS plate measurements. This work is based on data collected at the European Southern Observatory, the Australia Telescope National Facility and the National Radio Astronomy Observatory. NRAO is operated by Associated Universities Inc. under cooperative agreement with the National Science Foundation.

  
Appendix A: The complete catalogue of the Parkes quarter-Jansky sample

Catalogue column entries:

1. PKSCAT90 B1950 source name.

2. and 3. PKSCAT90 radio source position (B1950).

4. and 5. The best radio source position (B1950).

6. The origin of the radio position given in Cols. 4 and 5:

A	ATCA observation for this project
C	ATCA calibrator (ftp.atnf.csiro.au/pub/atnfdocs/guides/at.cat)
H	R Hunstead, private communication
N	NVSS catalogue (Condon et al. 1998)
P	A Patnaik, private communication
R	J Reynolds, private communication
S	A Savage, private communication
T	N Tasker, private communication
V	VLA observation for this project
W	White (1992)

7. Origin of identification:

1: Reconfirmed PKSCAT90 identification based on the following:

1a: Sky survey data and the best radio position available as shown in the table. No offsets (radio - optical) have been determined for these sources.

1b: COSMOS sky survey and the best radio position available as shown in the table. Identification offsets (radio - optical) have been determined for these sources.

1c: CCD imaging and the best radio position available as shown in the table. Identification offsets (radio - optical) have been determined for these sources.

2: A new identification by this project using the COSMOS database.

3: A new identification by this project using CCD-imaging.

8. Identification:

Q: confirmed quasar by spectroscopy or UVX photometry

Q*: stellar object based on positional coincidence with accurate (post-PKSCAT90) radio position, although no spectrum or UVX confirmation.

Q?: PKS radio position coincident with stellar object. No spectroscopy/UVX confirmation.

BL: spectroscopically-confirmed BL Lac object.

G: Galaxy with morphological or spectroscopic confirmation.

G?: probably a galaxy based on optical colour or morphology.

X: no identification, was previously a PKSCAT90 empty-field source.

e: the best radio invalidates the PKSCAT90 identification in that there is no optical source at the best radio position.

Ob: radio position obscured by foreground star.

NCS: Non-compact radio source. The source is either a steep-spectrum or extended radio source. Refer to individual notes for full details (Appendix B).

PN: Planetary nebula.

HII: HII region.

9. and 10. Radio - optical offset of candidate identification (given for identification classes 1c, 2 and 3 in Col. 7).

11. B or $B_{\rm J}$ magnitude. The origin of these magnitudes can be determined from the entry in Col. 7 as follows: for "1'' identifications, the magnitude is from PKSCAT90 and could be B or $B_{\rm J}$, for "2'' identifications the magnitudes is from COSMOS and is a $B_{\rm J}$ magnitude, for "3'' identifications the magnitude is from our CCD-imaging and is a B magnitude.

Magnitudes prefixed with: are either (i) estimated (ii) untraceable in the literature although given in PKSCAT90 or (iii) too close to the DSS plate limit to be reliable.

12. and 13. Gunn-iand Gunn-z (instrumental) magnitudes as determined from our CCD imaging.

14. and 15. Redshift and reference. Those prefixed ":'' are from PKSCAT90 but are untraceable in the literature.

16. to 18. PKSCAT90 $S_{2.7 \rm ~ GHz}$, $S_{5~ \rm GHz}$ and $S_{\rm lim,~2.7~{\rm GHz}}$

19. Exclusion flag. If "X'' then this source is excluded from our complete sample due to one of the following conditions:

Source is non-compact radio source (NCS) as shown in Col. 8 and the individual notes for that source.

Source flux density at 2.7  GHz is below the survey area flux density limit ( $S_{2.7 \rm ~ GHz}$ $< S_{\rm lim, 2.7~{\rm GHz}}$).

Source is steep-spectrum as described in detailed notes for that source.

Source is outside of the original Parkes survey areas (in area "X'' of Table 2). In this case $S_{\rm lim,~2.7~{\rm GHz}}$ is also set to 0.0.

 

 

Table A.1: Parkes radio sources.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0000-160	00 00 53.7	-16 03 48	00 00 53.68	-16 03 47.8	P	3	G	-0.3	-0.2	22.6	20.1	21.7	0.508	83	0.30	0.26	0.25
PKS B0001-121	00 01 24.0	-12 06 36	00 01 25.89	-12 06 16.2	P	3	G	2.6	1.0	24.0					0.27	0.22	0.25
PKS B0002-170	00 02 43.6	-17 04 45	00 02 44.52	-17 04 46.9	P	1b	Q*	-0.4	-0.5	18.0					0.14	0.16	0.25 X
PKS B0002-478	00 02 03.0	-47 53 02	00 02 02.94	-47 53 02.1	C	1a	Q			19.0					0.63	0.55	0.25
PKS B0003-066	00 03 40.3	-06 40 17	00 03 40.29	-06 40 17.4	P	1b	BL	-0.5	-0.4	19.5			0.347	1	1.46	1.58	0.25
PKS B0005-239	00 05 27.5	-23 56 00	00 05 27.47	-23 56 00.1	P	1b	Q	-0.2	-0.8	17.0			1.410	2	0.58	0.53	0.25
PKS B0005-262	00 05 53.5	-26 15 53	00 05 53.48	-26 15 54.0	N	1a	Q?			20.0					0.58	0.58	0.25
PKS B0008-222	00 08 21.1	-22 13 49	00 08 21.03	-22 13 45.7	P	2	G?	0.6	0.5	21.8		22.0			0.38	0.39	0.25
PKS B0008-264	00 08 28.9	-26 29 15	00 08 28.89	-26 29 14.9	P	1b	Q	-0.1	0.1	19.0			1.096	3	0.67	0.81	0.25
PKS B0008-307	00 08 04.4	-30 44 13	00 08 03.58	-30 44 29.1	A	2	Q	0.2	-0.5	19.1			1.189	83	0.31	0.27	0.20
PKS B0011-046	00 11 20.6	-04 40 33	00 11 20.66	-04 40 33.6	N	1a	Q?			19.0					0.21	0.41	0.25 X
PKS B0012-184	00 12 30.0	-18 29 28	00 12 30.06	-18 29 31.5	P	1b	Q	0.3	-1.0	20.0			0.743	83	0.48	0.42	0.25
PKS B0013-005	00 13 37.4	-00 31 53	00 13 37.35	-00 31 52.6	P	1b	Q	-0.1	0.1	19.5			1.575	4	0.80	0.65	0.10
PKS B0013-240	00 13 33.8	-24 00 32	00 13 33.87	-24 00 31.9	N	1a	G			17.0					0.25	0.23	0.25
PKS B0014-312	00 14 55.6	-31 14 46				1a	NCS								0.15	0.15	0.20 X
PKS B0017-307	00 17 13.0	-30 47 56	00 17 12.15	-30 47 59.0	N	1a	Q			19.0			2.666	83	0.34	0.33	0.20
PKS B0022-044	00 22 12.8	-04 28 37	00 22 12.74	-04 28 38.6	P	1b	Q	-0.3	0.0	20.0			1.946	83	0.29	0.39	0.25
PKS B0026-014	00 26 29.6	-01 29 42	00 26 27.42	-01 30 16.7	P	2	G	-0.9	0.5	16.3			0.083	83	0.30	0.26	0.25
PKS B0027-024	00 27 58.9	-02 28 33	00 27 58.41	-02 28 30.2	P	2	Q*	1.1	0.5	19.6					0.22	0.18	0.25 X
PKS B0027-426	00 27 51.8	-42 41 25				1a	Q			19.0			0.495	83	0.42	0.43	0.25
PKS B0028-396	00 28 55.8	-39 39 31	00 28 57.82	-39 39 23.2	A	2	Q*	-0.4	-0.4	20.8					0.19	0.19	0.25 X
PKS B0029-414	00 29 01.3	-41 24 39				1a	Q			17.0			0.896	5	0.23	0.21	0.25 X
PKS B0035-252	00 35 46.0	-25 15 31	00 35 46.01	-25 15 31.5	P	1b	Q	-0.6	-0.6	17.5			1.196	6	0.28	0.30	0.25
PKS B0035-595	00 35 09.2	-59 34 27				1a	Q			19.0					0.26	0.21	0.25
PKS B0036-216	00 36 00.4	-21 36 33	00 36 00.45	-21 36 33.2	P	1b	G	0.0	0.2	19.0					0.53	0.60	0.25
PKS B0038-326	00 38 05.1	-32 41 40	00 38 04.09	-32 41 49.6	S	2	BL	0.8	0.8	21.5				83	0.43	0.69	0.20
PKS B0039-407	00 39 37.6	-40 47 06				1a	Q			18.5			2.478	83	0.25	0.34	0.25
PKS B0040+001	00 40 58.6	+00 08 38	00 40 58.91	+00 08 34.3	N	1a	Q			19.0			1.127	7	0.08	0.11	0.10 X
PKS B0046-315	00 46 58.3	-31 32 54	00 46 57.68	-31 32 47.0	N	1a	Q			16.5			2.718	8	0.15	0.15	0.20 X
PKS B0047+023	00 47 08.8	+02 20 43	00 47 08.87	+02 20 43.0	N	1a	BL			18.0				4	0.39	0.39	0.10
PKS B0047-051	00 47 48.8	-05 08 39	00 47 49.02	-05 08 40.0	P	1b	Q*	0.1	-0.2	18.5					0.18	0.27	0.25 X
PKS B0047-579	00 47 48.0	-57 54 47	00 47 48.16	-57 54 47.1	C	1a	Q			17.8			1.797	8	1.96	2.48	0.25
PKS B0048-071	00 48 36.2	-07 06 21	00 48 36.22	-07 06 20.9	P	1b	Q	-0.5	0.0	19.0			1.975	3	0.70	0.67	0.25
PKS B0048-097	00 48 10.0	-09 45 24	00 48 09.98	-09 45 24.3	P	1b	BL	-0.4	-0.2	17.0				3	1.44	1.92	0.25
PKS B0048-427	00 48 49.0	-42 42 52	00 48 49.02	-42 42 52.0	C	1a	Q			18.8			1.749	9	0.68	0.58	0.25
PKS B0051-077	00 51 04.6	-07 43 45	00 51 04.77	-07 43 45.9	P	3	G?	0.6	0.2	>24.5		23.0			0.21	0.19	0.25 X
PKS B0054-006	00 54 43.3	-00 40 46	00 54 43.40	-00 40 45.7	P	1b	Q	-0.5	-0.2	18.0			2.790	8	0.15	0.19	0.10
PKS B0054-451	00 54 29.0	-45 07 23				1a	G			18.5					0.46	0.39	0.25
PKS B0055-328	00 55 42.0	-32 51 17				1a	NCS								0.44	0.36	0.20 X
PKS B0056-525	00 56 45.6	-52 35 20	00 56 43.91	-52 35 36.9	A	3	BL	-1.2	-1.6	23.6	20.9	23.5		83	0.26	0.26	0.25

   
Appendix B: Notes on individual sources

0000-160 Could be interacting with a fainter galaxy to south.

0001-121 Faint galaxy from CCD imaging, on B frame only. However, the NVSS catalogues 2 bright radio sources, offset 87 and 297 arcsecs respectively with nothing closer to the Parkes or Patnaik position. The nearest NVSS radio source is coincident with a galaxy on DSS, with $B_{\rm J}$ mag approx 21.0. It is probable that this is the correct radio source id, the Parkes beam being confused by 2 close compact radio sources. For the time being we leave the id as the faint galaxy and estimate the B mag.

0005-262 PKSCAT90 galaxy is an incorrect identification: Identified as a stellar object on K-band image by Drinkwater et al. (1997).

0008-222 Classified as galaxy in the COSMOS survey, as probably extended on our Gunn-z image and also brighter on B.

0014-312 Undetected by our VLA observations, nothing in NVSS.

0026-014 A gE galaxy identified in the COSMOS survey, disturbed/interacting. Has smaller companion galaxy at same redshift.

0027-426 The redshift given in NED (from Hewitt et al. 1989) is wrong. New redshift obtained by us (Paper II).

0051-077 Not present on B image. Classed as a galaxy as it is probably extended on Gunn-z image.

0055-328 Double radio source (NVSS). No compact core component at PKSCAT90 position.

0056-525 BL Lac object (Paper II), stellar on Gunn-i and Gunn-z images, very faint on B.

0059-287 Re-observed with VLA 1.4 GHz April 95, showing steep radio spectrum; variable quasar?

0100-760 The correct redshift is given in Wilkes et al. (1983) and is not that of Jauncey et al. (1978).

0111-385 Galaxy identification from CCD frames. Our VLA observations indicate the source has a double radio structure; there is a candidate identification coincident with one component and is a faint diffuse red object. The NVSS survey also catalogues this as a double radio source and thus it is excluded from our complete sample.

0113-310 Original PKS survey catalogues this source as confused with 0112-310. NVSS catalogues this source 84 arcsec offset from the PKS position in RA: it is a compact radio source coincident with a stellar object.

0115-016 Extended (or compound) image appears on the Gunn-i and Gunn-z, stellar on B.

0115-357 Nothing at position in NVSS survey, nearest NVSS source is 250 arcsec offset. Excluded from our complete sample.

0115-368 Extended, probably bent double radio source (NVSS). Excluded from our complete sample.

0123-016 = NGC545/7; it is a very extended FRI radio source, and the apparent flat spectrum only comes about through inaccurate flux-density integration at 2.7 and 5.0 GHz. Excluded from our complete sample.

0128-132 Extended (bent double?) radio source (NVSS). Excluded from our complete sample.

0130-447 Low-surface-brightness galaxy identification from CCD imaging; red and very diffuse.

0143-061 Galaxy identified from the COSMOS survey with narrow-line spectrum (Paper II). Our VLA observations reveal an extended radio structure for the source, agreeing with NVSS. Excluded from our complete sample.

0144-219Low-surface-brightnessgalaxy,mostobviousonGunn-iframe.Possiblyinteractingwithnearby,brighterS0.

0156-144 Faint galaxy, from B frame but not on Gunn-z. Galaxy is actually a steep-spectrum source: the PKSCAT90 2.7 GHz flux density is wrong (0.90 Jy vs. the original PKS survey value of 1.01 Jy). Our VLA observations reveal a steep-spectrum source, thus it is exluded from our complete sample.

0202-337 Scattered light from a nearby bright star creates a ghost ring covering the radio position, but the morphology is reasonably clear.

0203-520 Erroneous redshift given in PKSCAT90. Updated in our table to the correct value and reference.

0215+015 Extremely variable BLLac object (Bolton & Wall 1969; Gaskell 1982).

0215-015 Looks stellar on B and Z; no signal in our optical spectrum (Paper II) and thus unconfirmed quasar.

0218-683 Candidate is very close to bright star and its scattered light makes morphological classification difficult.

0225-065 The NVSS catalogues a compact source 3 arcsec from the PKSCAT90 position, at B1950 $02^{\rm h} 25^{\rm m} 15\hbox{$.\!\!^{\rm s}$ }22$, $-06^{\circ} 34' 32\hbox{$.\!\!^{\prime\prime}$ }3$, 0.513 Jy at 1.4 GHz. DSS shows a very faint object, possibly extended, close to this position; but it cannot be claimed as the identification.

0230-790 A suspect redshift: Browne & Savage (1977) found a single line at 5800 Å and it was pointed out by Jauncey et al. (2000) that if this were identified with MgII $\lambda 2798$ then the redshift is 1.07.

0231+022 Double radio source (NVSS), excluded from our complete sample.

0238-084 NGC1052 LINER-type elliptical with inverted radio spectrum.

0239-553 Faint (possibly double) galaxy based on our ATCA position which notes it as a double radio source. The centroid position is used for the identification. The relatively large radio-optical offset is probably due to the extended radio structure. Excluded from our complete sample.

0240-060 The redshift given in Strittmatter et al. (1974) is wrong. New redshift obtained by us (Paper II).

Appendix C Finding charts for all sources

 

Finding charts for all 878 sources presented in Appendix A. Charts are oriented North up, East left, and the scale is in arcmins. Position of the best radio position is marked (+).

   
Appendix D: Newly-identified sources with CCD images

Images are oriented North up, East left, and scale is in arcseconds. Images are 2 arcminutes square, centered on the identification ($\circ$).

References

 
• Abraham, R. G., Crawford, C. S., & McHardy, I. M. 1991, MNRAS, 252, 482(35) In the text NASA ADS  
• Allington-Smith, J. R., Peacock, J. A., & Dunlop, J. S. 1991, MNRAS, 253, 287(19) In the text NASA ADS  
• Baker, J. C., Hunstead, R. W., Kapahi, V. K., & Subrahmanya, C. R. 1999, ApJS, 122, 29(55) In the text NASA ADS  
• Baldwin, J. A., Wampler, E. J., & Burbridge, E. M. 1981, ApJ, 243, 76(63) In the text NASA ADS  
• Barbieri, C., Capaccioli, M., & Zambon, M. 1975, Mem. Soc. Astron. Ital., 46, 461 In the text NASA ADS  
• Bergeron, J., & Kunth, D. 1984, MNRAS, 207, 263(61) In the text NASA ADS  
• Bock, D. C.-J., Large, M. I., & Sadler, E. M. 1999, AJ, 117, 1578 In the text NASA ADS  
• Bolton, J. G., & Butler, P. W. 1975, Aust. J. Phys. Astrophys. Suppl, 34, 33 In the text  
• Bolton, J. G., & Ekers, J. A. 1966, Austr. J. Phys., 19, 275 In the text  
• olton, J. G., Kinman, T. D., & Wall, J. V. 1968, ApJ, 154, L105(23) In the text  
• Bolton, J. G., Savage, A., & Wright, A. E. 1979, Aust. J. Phys. Suppl., 46, 1 In the text  
• Bolton, J. G., & Shimmins, A. J. 1973, Aust. J. Phys. Astrophys. Suppl., 30, 1 In the text NASA ADS  
• Bolton, J. G., Shimmins, A. J., & Wall, J. V. 1975, Australian J. Phys. Astrophys. Suppl., 34, 55 In the text  
• Bolton, J. G., & Wall, J. V. 1969, Astrophys. Lett., 3, 177 In the text  
• Bolton, J., & Wall, J. V. 1970, Aust. J. Phys., 23, 789 In the text NASA ADS  
• Bowyer, S., Brodie, J., Clarke, J. T., & Henry, J. P. 1984, ApJ, 278, L103(77) In the text NASA ADS  
• Browne, I. W. A., & Savage, A. 1977, MNRAS, 179, 65P(22) In the text  
• Browne, I. W. A., Savage, A., & Bolton, J. G. 1975, MNRAS, 173, 87P(12) In the text  
• Browne, I. W. A., & Wright, A. E. 1985, MNRAS, 213, 97 In the text NASA ADS  
• Burbidge, E. M. 1970, ApJ, 160, L33(68) In the text NASA ADS  
• Burbidge, E. M., & Strittmatter, P. A. 1972a, ApJ, 172, L37(72) In the text NASA ADS  
• Burbidge, E. M., & Strittmatter, P. A. 1972b, ApJ, 174, L57(73) In the text NASA ADS  
• Chu, Y. Q., Zhu, X. F., & Butcher, H. 1986, Chinese Astron. Astrophys., 10, 196(28) In the text  
• Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, AJ, 115, 1693 In the text NASA ADS  
• Condon, J. J., Hicks, P. D., & Jauncey, D. L. 1977, AJ, 82, 692 In the text NASA ADS  
• Condon, J. J., Jauncey, D. L., & Wright, A. E. 1978, AJ, 83, 1036 In the text NASA ADS  
• Cristiani, S., & Koehler, B. 1987, A&AS, 68, 339(29) In the text  
• da Costa, L. N., Willmer, C., Pellegrini, P. S., & Chincarini, G. 1987, AJ, 93, 1338(62) In the text NASA ADS  
• Danziger, I. J., & Goss, W. M. 1979, MNRAS, 186, 93(71) In the text NASA ADS  
• de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H. G., et al. 1991, Reference Catalogue of Bright Galaxies, 3rd edition (Springer Verlag), 14 In the text  
• Dekker, H., & D'Odorico, S. 1984, The Messenger, 37, 7(54) In the text NASA ADS  
• di Serego-Alighieri, S., Danziger, I. J., Morganti, R., & Tadhunter, C. N. 1994, MNRAS, 269, 998(65) In the text NASA ADS  
• Downes, A. J. B., Peacock, J. A., Savage, A., & Carrie, D. R. 1986, MNRAS, 218, 31 In the text NASA ADS  
• Dressler, A. 1991, ApJS, 75, 241(69) In the text NASA ADS  
• Drinkwater, M. J., Barnes, D. G., & Ellison, S. L. 1995, Proc. Astron. Soc. Aust., 12, 248 In the text  
• Drinkwater, M. J., Webster, R. L., Francis, P. J., et al. 1997, MNRAS, 284, 85(20) In the text NASA ADS  
• Dunlop, J. S., Peacock, J. A., Savage, A., et al. 1989, MNRAS, 238, 1171(4) In the text NASA ADS  
• Ekers, R. D., & Ekers, J. A. 1973, A&A, 24, 247 In the text NASA ADS  
• Eracleous, M., & Halpern, J. P. 1994, ApJS, 90, 1(16) In the text NASA ADS  
• Fairall, A. P., Willmer, C. N. A., Calderon, J. H., et al. 1992, AJ, 103, 11(59) In the text NASA ADS  
• Falco, E. E., Kochanek, C. S., & Munoz, J. A. 1998, ApJ, 494, 47 In the text NASA ADS  
• Falomo, R., Maraschi, L., Treves, A., & Tanzi, E. G. 1987, ApJ, 318, L39(74) In the text NASA ADS  
• Fisher, K. B., Huchra, J. P., Strauss, M. A., et al. 1995, ApJS, 100, 69(57) In the text NASA ADS  
• Fricke, K. J., Kollatschny, W., & Witzel, A. 1983, A&A, 117, 60(24) In the text NASA ADS  
• Gaskell, C. M. 1982, ApJ, 252, 447 In the text NASA ADS  
• Goncalves, A. C., Veron, P., & Veron-Cetty, M. P. 1998, A&AS, 127, 107(82) In the text NASA ADS  
• Heckman, T. M., O'Dea, C. P., Baum, S. A., & Laurikainen, E. 1994, ApJ, 428, 65(39) In the text NASA ADS  
• Hewitt, A., & Burbidge, G. 1993, ApJS, 87, 451 In the text NASA ADS  
• Hewitt, P. C., Webster, R. L., Harding, M. E., et al. 1989, ApJ, 346, 1959 In the text  
• Hook, I. M., Shaver, P. A., Jackson, C. A., Wall, J. V., & Kellermann, K. I. 2002, in preparation  
• Hunstead, R. W., & Murdoch, H. S. 1980, MNRAS, 192, 31P(64) In the text  
• Hunstead, R. W., Murdoch, H. S., & Shobbrook, R. R. 1978, MNRAS, 185, 149(26) In the text NASA ADS  
• Jauncey, D. L., Batty, M. J., Gulkis, S., & Savage, A. 1982, AJ, 87, 763(58) In the text NASA ADS  
• Jauncey, D. L., Batty, M. J., Wright, A. E., Peterson, B. A., & Savage, A. 1984, ApJ, 286, 498(6) In the text NASA ADS  
• Jauncey, D. L., Kedziora-Chudczer, L. L., Macquart, J. P., et al. 2000, in IAU Symp., 205, E7 In the text  
• Jauncey, D. L., Savage, A., Morabito, D. D., et al. 1989, AJ, 98, 54 In the text NASA ADS  
• Jauncey, D. L., Wright, A. E., Peterson, B. A., & Condon, J. J. 1978, ApJ, 219, L1(5) In the text  
• Junkkarinen, V. 1984, PASP, 96, 539(66) In the text NASA ADS  
• Kollgaard, R. I., Feigelson, E. D., Laurent-Muehleisen, S. A., et al. 1995, ApJ, 449, 61 In the text NASA ADS  
• Landolt, A. U. 1992, AJ, 104, 340 In the text NASA ADS  
• Lanzetta, K. M., McMahon, R. G., Wolfe, A. M., et al. 1991, ApJS, 77, 1(70) In the text NASA ADS  
• Lynds, C. R. 1967, ApJ, 147, 837(21) In the text NASA ADS  
• Lynds, C. R., Hill, S. J., Heere, K., & Stockton, A. N. 1966, ApJ, 144, 1244(51) In the text NASA ADS  
• Lynds, C. R., Stockton, A. N., & Livingston, W. C. 1965, ApJ, 142, 1667(53) In the text NASA ADS  
• Maza, J., Ruiz, M. T., Gonzalez, L. E., Wischnjewsky, M., & Antezana, R. 1993, Rev. Mex. Astron. Astrofis., 25, 51(79) In the text  
• McAlpine, G. M., & Feldman, F. R. 1982, ApJ, 261, 412(13) In the text NASA ADS  
• Morton, D. C., Savage, A., & Bolton, J. G. 1978, MNRAS, 185, 735(36) In the text NASA ADS  
• Murdoch, H. S., Hunstead, R. W., Blades, J. C., & Pettini, M. 1986, Ap&SS, 118, 501(18) In the text NASA ADS  
• O'Dea, C. P., Baum, S. A., Stanghellini, C., et al. 1990, A&AS, 84, 549 In the text NASA ADS  
• Osmer, P. S., & Smith, M. G. 1980, ApJS, 42, 333(80) In the text NASA ADS  
• Owen, F. N., Ledlow, M. J., & Keel, W. C. 1995, AJ, 109, 14(44) In the text NASA ADS  
• Perlman, E. S., Padovani, P., Giommi, P., et al. 1998, AJ, 115, 1253(37) In the text NASA ADS  
• Peterson, B. A., & Bolton, J. G. 1972, ApJ, 173, L19(25) In the text NASA ADS  
• Peterson, B. A., Jauncey, D. L., Wright, A. E., & Condon, J. J. 1976, ApJ, 207, L5(8) In the text NASA ADS  
• Peterson, B. A., Wright, A. E., Jauncey, D. L., & Condon, J. J. 1979, ApJ, 232, 400(45) In the text NASA ADS  
• Postman, M., & Lauer, T. R. 1995, ApJ, 440, 28(56) In the text NASA ADS  
• Quintana, H., & Ramirez, A. 1995, ApJS, 96, 343(43) In the text NASA ADS  
• Reimers, D., Koehler, T., & Wisotzki, L. 1996, A&AS, 115, 235(48) In the text NASA ADS  
• Roeser, S., Bastian, U., & Kuzmin, A. 1994, A&AS, 105, 301 In the text NASA ADS  
• Savage, A., & Bolton, J. G. 1979, MNRAS, 188, 599(17) In the text NASA ADS  
• Savage, A., Bolton, J. G., & Trett, J. 1982, Aust. J. Phys., 35, 207 In the text NASA ADS  
• Savage, A., Browne, I. W. A., & Bolton, J. G. 1976, MNRAS, 177, 77P(30) In the text  
• Savage, A., Clowes, R. G., Cannon, R. D., et al. 1985, MNRAS, 213, 485(11) In the text NASA ADS  
• Savage, A., & Wright, A. E. 1981, MNRAS, 196, 927(75) In the text NASA ADS  
• Savage, A., Wright, A. E., & Bolton, J. G. 1977, Aust. J. Phys. Astrophys. Suppl, 4, 21 In the text  
• Schmidt, M. 1963, Nature, 197, 1040(52) In the text NASA ADS  
• Schmidt, M. 1977, ApJ, 217, 358(34) In the text NASA ADS  
• SDSS 2001, Sloan Digital Sky Survey (early-release data), In the text http://archive.stsci.edu/sdss/  
• Searle, L., & Bolton, J. G. 1968, ApJ, 154, L101(76) In the text NASA ADS  
• Shaver, P. A., Wall, J. V., Kellermann, K. I., Jackson, C. A., & Hawkins, M. R. S. 1996, Nature, 384, 439 In the text NASA ADS  
• Shimmins, A. J. 1971, Aust. J. Phys. Astrophys. Suppl., 21, 1 In the text NASA ADS  
• Shimmins, A. J., & Bolton, J. G. 1972, Aust. J. Phys. Astrophys. Suppl., 26, 1 In the text NASA ADS  
• Shimmins, A. J., & Bolton, J. G. 1974, Aust. J. Phys. Astrophys. Suppl., 32, 1 In the text NASA ADS  
• Smith, A. G., & Nair, A. D. 1995, PASP, 107, 863 In the text NASA ADS  
• Stanghellini, C., Baum, S. A., O'Dea, C. P., & Morris, G. B. 1990, A&A, 233, 379 In the text NASA ADS  
• Stickel, M., Fried, J. W., & Kuehr, H. 1993a, A&AS, 98, 393(78) In the text NASA ADS  
• Stickel, M., Fried, J. W., & Kuehr, H. 1989, A&AS, 80, 103(1) In the text NASA ADS  
• Stickel, M., Kuehr, H., & Fried, J. W. 1993b, A&AS, 97, 483(38) In the text NASA ADS  
• Stickel, M., & Kuhr, H. 1993, A&AS, 101, 521(41) In the text NASA ADS  
• Stobie, R. S., Sagar, R., & Gilmore, G. 1985, A&AS, 60, 503 In the text NASA ADS  
• Strittmatter, P. A., Carswell, R. F., & Gilbert, G. 1974, ApJ, 190, 509(27) In the text NASA ADS  
• Tadhunter, C. N., Morganti, R., di Serego-Alighieri, S., Fosbury, R. A. E., & Danziger, I. J. 1993, MNRAS, 263, 999(42) In the text NASA ADS  
• Thompson, D. J., Djorgovski, S., & de Carvalho, R. 1990, PASP, 102, 1235 In the text NASA ADS  
• Veron, P., Veron-Cetty, M. P., Djorgovski, S., et al. 1990, A&AS, 86, 543(32) In the text NASA ADS  
• Veron-Cetty, M. P., & Veron, P. 1989, QSO list (ESO Scientific Report, Garching: European Southern Observatory (ESO), 1989, 4th ed.) In the text  
• Veron-Cetty, M.-P., & Veron, P. 1993, A&AS, 100, 521 In the text NASA ADS  
• Veron-Cetty, M. P., & Veron, P. 1998, A Catalogue of quasars and active nuclei (A Catalogue of quasars and active nuclei, Edition: 8th ed., Publisher: Garching: European Southern Observatory (ESO), 1998, Ser. ESO Scientific Report Ser. Vol. 18) In the text  
• Wall, J. V., & Peacock, J. A. 1985, MNRAS, 216, 273 In the text  
• Wall, J. V., Shaver, P. A., Jackson, C. A., Kellermann, K. I., & Hook, I. M. 2002, in preparation  
• Wall, J. V., Shimmins, A. J., & Bolton, J. G. 1975, Aust. J. Phys. Astrophys. Suppl., 34, 55 In the text NASA ADS  
• Wall, J. V., Shimmins, A. J., & Merkelijn, J. K. 1971, Aust. J. Phys. Suppl., 19, 1 In the text  
• Wall, J. V., Wright, A. E., & Bolton, J. G. 1976, Aust. J. Phys. Astrophys. Suppl., 39, 1 In the text NASA ADS  
• White, G. L. 1992, Proc. Astron. Soc. Aust., 10, 140 In the text  
• White, G. L., Jauncey, D. L., Savage, A., et al. 1988, ApJ, 327, 561(9) In the text NASA ADS  
• Wilkes, B. 1986, MNRAS, 218, 331(31) In the text NASA ADS  
• Wilkes, B. J., Wright, A. E., Jauncey, D. L., & Peterson, B. A. 1983, Proc. Astron. Soc. Aust., 5, 2(10) In the text  
• Wills, B. J., & Wills, D. 1979, ApJS, 41, 689(81) In the text NASA ADS  
• Wills, D., & Lynds, R. 1978, ApJS, 36, 317(7) In the text NASA ADS  
• Wills, D., & Wills, B. J. 1976, ApJS, 31, 143(2) In the text NASA ADS  
• Wright, A. E., Ables, J. G., & Allen, D. A. 1983, MNRAS, 205, 793(3) In the text NASA ADS  
• Wright, A. E., Jauncey, D. L., Bolton, J. G., & Savage, A. 1982, Aust. J. Phys., 35, 177 In the text NASA ADS  
• Wright, A. E., Jauncey, D. L., Peterson, B. A., & Condon, J. J. 1977, ApJ, 211, L115(15) In the text NASA ADS  
• Wright, A. E., & Otrupcek, R. E. 1990, Parkes Catalogue, Australia Telescope National Facility, CSIRO In the text  
• Wright, A. E., Peterson, B. A., Jauncey, D. L., & Condon, J. J. 1978, ApJ, 226, L61(40) In the text NASA ADS  
• Wright, A. E., Peterson, B. A., Jauncey, D. L., & Condon, J. J. 1979, ApJ, 229, 73(33) In the text NASA ADS  
• Yentis, D. J., Cruddace, R. G., Gursky, H., et al. 1992, in Digitized Optical Sky Surveys, ed. H. T. McGillivray, & E. B. Thomson (Kluwer, Dordrecht) In the text  
• Young, P., Sargent, W. L. W., & Boksenberg, A. 1982, ApJS, 48, 455(49) In the text NASA ADS  
• Zickgraf, F. J., Voges, W., Krautter, J., et al. 1997, A&A, 323, L21(47) In the text NASA ADS

 

Online Material

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0000-160	00 00 53.7	-16 03 48	00 00 53.68	-16 03 47.8	P	3	G	-0.3	-0.2	22.6	20.1	21.7	0.508	83	0.30	0.26	0.25
PKS B0001-121	00 01 24.0	-12 06 36	00 01 25.89	-12 06 16.2	P	3	G	2.6	1.0	24.0					0.27	0.22	0.25
PKS B0002-170	00 02 43.6	-17 04 45	00 02 44.52	-17 04 46.9	P	1b	Q*	-0.4	-0.5	18.0					0.14	0.16	0.25 X
PKS B0002-478	00 02 03.0	-47 53 02	00 02 02.94	-47 53 02.1	C	1a	Q			19.0					0.63	0.55	0.25
PKS B0003-066	00 03 40.3	-06 40 17	00 03 40.29	-06 40 17.4	P	1b	BL	-0.5	-0.4	19.5			0.347	1	1.46	1.58	0.25
PKS B0005-239	00 05 27.5	-23 56 00	00 05 27.47	-23 56 00.1	P	1b	Q	-0.2	-0.8	17.0			1.410	2	0.58	0.53	0.25
PKS B0005-262	00 05 53.5	-26 15 53	00 05 53.48	-26 15 54.0	N	1a	Q?			20.0					0.58	0.58	0.25
PKS B0008-222	00 08 21.1	-22 13 49	00 08 21.03	-22 13 45.7	P	2	G?	0.6	0.5	21.8		22.0			0.38	0.39	0.25
PKS B0008-264	00 08 28.9	-26 29 15	00 08 28.89	-26 29 14.9	P	1b	Q	-0.1	0.1	19.0			1.096	3	0.67	0.81	0.25
PKS B0008-307	00 08 04.4	-30 44 13	00 08 03.58	-30 44 29.1	A	2	Q	0.2	-0.5	19.1			1.189	83	0.31	0.27	0.20
PKS B0011-046	00 11 20.6	-04 40 33	00 11 20.66	-04 40 33.6	N	1a	Q?			19.0					0.21	0.41	0.25 X
PKS B0012-184	00 12 30.0	-18 29 28	00 12 30.06	-18 29 31.5	P	1b	Q	0.3	-1.0	20.0			0.743	83	0.48	0.42	0.25
PKS B0013-005	00 13 37.4	-00 31 53	00 13 37.35	-00 31 52.6	P	1b	Q	-0.1	0.1	19.5			1.575	4	0.80	0.65	0.10
PKS B0013-240	00 13 33.8	-24 00 32	00 13 33.87	-24 00 31.9	N	1a	G			17.0					0.25	0.23	0.25
PKS B0014-312	00 14 55.6	-31 14 46				1a	NCS								0.15	0.15	0.20 X
PKS B0017-307	00 17 13.0	-30 47 56	00 17 12.15	-30 47 59.0	N	1a	Q			19.0			2.666	83	0.34	0.33	0.20
PKS B0022-044	00 22 12.8	-04 28 37	00 22 12.74	-04 28 38.6	P	1b	Q	-0.3	0.0	20.0			1.946	83	0.29	0.39	0.25
PKS B0026-014	00 26 29.6	-01 29 42	00 26 27.42	-01 30 16.7	P	2	G	-0.9	0.5	16.3			0.083	83	0.30	0.26	0.25
PKS B0027-024	00 27 58.9	-02 28 33	00 27 58.41	-02 28 30.2	P	2	Q*	1.1	0.5	19.6					0.22	0.18	0.25 X
PKS B0027-426	00 27 51.8	-42 41 25				1a	Q			19.0			0.495	83	0.42	0.43	0.25
PKS B0028-396	00 28 55.8	-39 39 31	00 28 57.82	-39 39 23.2	A	2	Q*	-0.4	-0.4	20.8					0.19	0.19	0.25 X
PKS B0029-414	00 29 01.3	-41 24 39				1a	Q			17.0			0.896	5	0.23	0.21	0.25 X
PKS B0035-252	00 35 46.0	-25 15 31	00 35 46.01	-25 15 31.5	P	1b	Q	-0.6	-0.6	17.5			1.196	6	0.28	0.30	0.25
PKS B0035-595	00 35 09.2	-59 34 27				1a	Q			19.0					0.26	0.21	0.25
PKS B0036-216	00 36 00.4	-21 36 33	00 36 00.45	-21 36 33.2	P	1b	G	0.0	0.2	19.0					0.53	0.60	0.25
PKS B0038-326	00 38 05.1	-32 41 40	00 38 04.09	-32 41 49.6	S	2	BL	0.8	0.8	21.5				83	0.43	0.69	0.20
PKS B0039-407	00 39 37.6	-40 47 06				1a	Q			18.5			2.478	83	0.25	0.34	0.25
PKS B0040+001	00 40 58.6	+00 08 38	00 40 58.91	+00 08 34.3	N	1a	Q			19.0			1.127	7	0.08	0.11	0.10 X
PKS B0046-315	00 46 58.3	-31 32 54	00 46 57.68	-31 32 47.0	N	1a	Q			16.5			2.718	8	0.15	0.15	0.20 X
PKS B0047+023	00 47 08.8	+02 20 43	00 47 08.87	+02 20 43.0	N	1a	BL			18.0				4	0.39	0.39	0.10
PKS B0047-051	00 47 48.8	-05 08 39	00 47 49.02	-05 08 40.0	P	1b	Q*	0.1	-0.2	18.5					0.18	0.27	0.25 X
PKS B0047-579	00 47 48.0	-57 54 47	00 47 48.16	-57 54 47.1	C	1a	Q			17.8			1.797	8	1.96	2.48	0.25
PKS B0048-071	00 48 36.2	-07 06 21	00 48 36.22	-07 06 20.9	P	1b	Q	-0.5	0.0	19.0			1.975	3	0.70	0.67	0.25
PKS B0048-097	00 48 10.0	-09 45 24	00 48 09.98	-09 45 24.3	P	1b	BL	-0.4	-0.2	17.0				3	1.44	1.92	0.25
PKS B0048-427	00 48 49.0	-42 42 52	00 48 49.02	-42 42 52.0	C	1a	Q			18.8			1.749	9	0.68	0.58	0.25
PKS B0051-077	00 51 04.6	-07 43 45	00 51 04.77	-07 43 45.9	P	3	G?	0.6	0.2	>24.5		23.0			0.21	0.19	0.25 X
PKS B0054-006	00 54 43.3	-00 40 46	00 54 43.40	-00 40 45.7	P	1b	Q	-0.5	-0.2	18.0			2.790	8	0.15	0.19	0.10
PKS B0054-451	00 54 29.0	-45 07 23				1a	G			18.5					0.46	0.39	0.25
PKS B0055-328	00 55 42.0	-32 51 17				1a	NCS								0.44	0.36	0.20 X
PKS B0056-525	00 56 45.6	-52 35 20	00 56 43.91	-52 35 36.9	A	3	BL	-1.2	-1.6	23.6	20.9	23.5		83	0.26	0.26	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0056-572	00 56 38.9	-57 15 21	00 56 38.58	-57 15 22.4	C	1a	Q			18.3					0.77	1.07	0.25
PKS B0059-287	00 59 28.3	-28 47 30	00 59 28.18	-28 47 27.9	P	3	Q	0.6	-0.1	23.2	21.0	22.7	1.694	83	0.44	0.36	0.25
PKS B0059-628	00 59 14.6	-62 49 14				1a	Q			19.3					0.28	0.25	0.25
PKS B0100-270	01 00 31.5	-27 02 42	01 00 31.62	-27 02 42.8	P	1b	Q	-0.3	0.7	17.5			1.597	5	0.26	0.24	0.25
PKS B0100-413	01 00 58.5	-41 20 38				1a	Q			18.5					0.15	0.13	0.25 X
PKS B0100-760	01 00 55.8	-76 02 59				1a	Q			18.2			1.015	10	0.43	0.55	0.20
PKS B0102-245	01 02 32.8	-24 32 33	01 02 32.78	-24 32 32.3	P	1b	Q*	-0.9	0.0	18.5					0.24	0.22	0.25 X
PKS B0104-275	01 04 02.1	-27 34 14	01 04 02.07	-27 34 13.9	P	1b	Q	-0.8	0.0	19.0			2.492	11	0.29	0.37	0.25
PKS B0104-408	01 04 27.6	-40 50 21				1a	Q			19.0			0.584	9	0.57	0.85	0.25
PKS B0106+013	01 06 04.5	+01 19 01	01 06 04.50	+01 18 59.6	N	1a	Q			18.0			2.094	7	4.24	4.76	0.25
PKS B0107-395	01 07 26.3	-39 34 27	01 07 27.83	-39 34 35.3	A	3	G?	-0.5	-0.5	23.5					0.19	0.15	0.25 X
PKS B0107-610	01 07 16.8	-61 05 46	01 07 17.16	-61 05 46.9	C	1a	Q			21.4					0.28	0.37	0.25
PKS B0108-079	01 08 19.0	-07 57 38	01 08 19.01	-07 57 37.6	P	1b	Q	-1.2	-0.1	19.0			1.776	3	1.02	0.89	0.25
PKS B0108-635	01 08 22.9	-63 31 49	01 08 22.86	-63 31 53.9	T	1c	Q	-1.3	1.1	19.4					0.29	0.24	0.25
PKS B0110-668	01 10 32.6	-66 50 36				1a	Q			17.7					0.34	0.31	0.25
PKS B0111+021	01 11 08.6	+02 06 25	01 11 08.57	+02 06 24.6	P	1b	G	-1.4	0.0	16.3			0.047	2	0.63	0.65	0.25
PKS B0111-256	01 11 18.7	-25 39 51	01 11 18.77	-25 39 51.9	P	1b	Q	-0.7	0.5	19.5			1.030	83	0.26	0.23	0.25
PKS B0111-385	01 11 58.5	-38 33 21	01 12 01.79	-38 34 11.8	V	1a	NCS	-1.2	-0.1		22.9	24.9			0.23	0.18	0.25 X
PKS B0112-017	01 12 43.9	-01 42 55	01 12 43.93	-01 42 55.0	P	1b	Q	-0.1	-0.3	18.0			1.365	7	0.94	1.10	0.25
PKS B0113-118	01 13 43.2	-11 52 05	01 13 43.22	-11 52 04.6	P	1b	Q	-1.3	-0.1	18.5			0.670	3	1.78	1.88	0.25
PKS B0113-283	01 13 01.6	-28 20 45	01 13 01.53	-28 20 45.5	P	1b	Q	-0.8	-0.5	19.0			2.555	83	0.29	0.43	0.25
PKS B0113-310	01 13 19.0	-31 05 04	01 13 25.56	-31 05 9.1	N	1a	Q?			20.2					0.39	0.32	0.20
PKS B0114-351	01 14 17.7	-35 11 35	01 14 18.35	-35 12 49.7	A	2	Q*	-0.6	-0.3	18.7					0.07	0.07	0.25 X
PKS B0115-016	01 15 42.2	-01 36 15	01 15 42.21	-01 36 16.6	P	3	Q	-0.2	0.4	22.5	20.9	22.6	1.162	83	0.64	0.56	0.25
PKS B0115-342	01 15 25.6	-34 12 53	01 15 25.75	-34 12 54.0	N	1a	Q			19.0			0.647	83	0.27	0.26	0.20
PKS B0115-357	01 15 46.0	-35 44 27				1a	NCS								0.07	0.09	0.25 X
PKS B0115-368	01 15 45.3	-36 53 57				1a	NCS								0.08	0.07	0.25 X
PKS B0116-219	01 16 32.4	-21 57 15	01 16 32.41	-21 57 15.4	P	1b	Q	-0.4	-0.2	19.0			1.165	3	0.57	0.51	0.25
PKS B0118-272	01 18 09.5	-27 17 07	01 18 09.54	-27 17 07.6	P	1b	BL	0.3	-0.2	16.5				83	0.96	1.18	0.25
PKS B0120-078	01 20 24.0	-07 49 30	01 20 23.23	-07 49 15.4	N	1a	Q?			19.0					0.11	0.12	0.25 X
PKS B0122-003	01 22 55.2	-00 21 31	01 22 55.18	-00 21 31.3	P	1b	Q	-0.4	-0.4	17.0			1.08	12	1.19	1.29	0.25
PKS B0122-005	01 22 43.6	-00 34 04	01 22 43.58	-00 34 04.6	P	1b	Q	-0.4	0.0	18.5			2.280	13	0.28	0.23	0.25
PKS B0122-042	01 22 03.2	-04 16 33	01 22 02.78	-04 16 41.8	N	1a	Q			18.0			0.561	31	0.14	0.25	0.25 X
PKS B0122-514	01 22 53.5	-51 28 50				1a	Q			19.2					0.35	0.29	0.25
PKS B0123-016	01 23 27.2	-01 36 17	01 23 27.47	-01 36 27.1	N	1a	NCS			13.0			0.018	14	2.17	1.78	0.25 X
PKS B0123-226	01 23 51.2	-22 38 07	01 23 51.29	-22 38 07.7	P	1b	Q	0.0	-0.8	18.5			0.720	26	0.48	0.40	0.25
PKS B0124-249	01 24 16.5	-24 55 45	01 24 15.88	-24 55 56.3	P	1b	G	0.1	-0.9	18.0					0.22	0.19	0.25 X
PKS B0128-132	01 28 36.7	-13 17 01				1a	NCS								0.28	0.22	0.25 X
PKS B0130-106	01 30 56.9	-10 41 21	01 30 57.01	-10 41 40.1	N	1a	G			16.5					0.24	0.19	0.25 X
PKS B0130-171	01 30 17.7	-17 10 12	01 30 17.69	-17 10 12.0	P	1b	Q	0.0	0.3	19.0			1.020	3	0.99	0.97	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0130-447	01 30 54.5	-44 46 25	01 30 52.90	-44 46 05.9	A	3	G	-0.6	-1.2	24.3		22.9			0.59	0.49	0.25
PKS B0131-522	01 31 05.6	-52 15 26	01 31 05.61	-52 15 26.6	C	1a	Q			20.3					1.09	1.18	0.25
PKS B0133-204	01 33 13.6	-20 24 04	01 33 13.64	-20 24 04.3	P	1b	Q	-0.3	-0.5	18.0			1.144	3	0.68	0.63	0.25
PKS B0135-247	01 35 17.1	-24 46 09	01 35 17.11	-24 46 08.8	P	1b	Q	0.2	-0.4	16.9			0.837	3	1.37	1.65	0.25
PKS B0136-059	01 36 20.9	-05 55 21	01 36 20.90	-05 55 21.0	P	1b	Q	-0.4	-0.9	20.0			2.004	83	0.30	0.36	0.25
PKS B0136-231	01 36 35.2	-23 09 57	01 36 35.47	-23 09 59.9	P	1b	Q	-0.7	-1.0	18.0			1.893	31	0.33	0.28	0.25
PKS B0138-097	01 38 56.9	-09 43 52	01 38 56.86	-09 43 51.7	P	1b	BL	-0.1	-0.4	18.0				83	0.71	1.19	0.25
PKS B0140-059	01 40 08.0	-05 59 12	01 40 08.06	-05 59 07.3	P	1b	BL	-0.6	-0.4	18.5				83	0.27	0.25	0.25
PKS B0141-609	01 41 17.6	-60 59 56				1a	NCS								0.17	0.15	0.25 X
PKS B0142-278	01 42 45.0	-27 48 35	01 42 44.97	-27 48 35.9	N	1b	Q			18.5			1.155	3	0.82	0.90	0.25
PKS B0143-061	01 43 46.5	-06 06 18	01 43 45.56	-06 06 09.8	V	1a	NCS	-0.1	0.6	21.8			0.499	83	0.28	0.23	0.25 X
PKS B0144-219	01 44 45.7	-21 59 43	01 44 45.56	-21 59 39.7	P	3	G	-0.4	-0.2	:24.0	18.7	23.0	0.262	83	0.28	0.22	0.25
PKS B0150-144	01 50 06.1	-14 27 22	01 50 06.23	-14 27 25.8	P	2	Q	-0.7	0.3	19.8			1.349	83	0.39	0.37	0.25
PKS B0150-334	01 50 57.0	-33 25 11	01 50 56.97	-33 25 10.1	N	1a	Q			16.5			0.610	15	0.92	0.86	0.20
PKS B0152-513	01 52 25.4	-51 22 32				1a	Q			18.8			1.581	16	0.29	0.38	0.25
PKS B0153-663	01 53 09.7	-66 18 57				1a	Q			18.2					0.37	0.40	0.25
PKS B0155-549	01 55 02.0	-54 54 14				1a	G			19.5					0.48	0.47	0.25
PKS B0156-144	01 56 18.1	-14 27 37	01 56 18.34	-14 27 40.5	P	3	G	0.3	-0.6	23.6					0.90	0.73	0.25 X
PKS B0157+011	01 57 29.5	+01 10 43	01 57 29.44	+01 10 41.4	N	1a	Q			18.5			1.170	2	0.38	0.40	0.25
PKS B0158-519	01 58 04.3	-51 58 06				1a	Q			18.5			2.390	17	0.17	0.15	0.25 X
PKS B0200-127	02 00 36.8	-12 47 02	02 00 38.38	-12 47 34.8	N	1a	G			18.5					0.21	0.17	0.25 X
PKS B0202-172	02 02 34.5	-17 15 39	02 02 34.52	-17 15 39.5	P	1b	Q	0.0	-0.4	18.0			1.740	3	1.40	1.38	0.25
PKS B0202-337	02 02 18.6	-33 43 14	02 02 17.67	-33 43 11.0	A	3	G	-0.1	-0.4	23.1					0.34	0.31	0.20
PKS B0203-520	02 03 00.8	-52 01 14				1a	Q			18.0			1.420	17	0.12	0.16	0.25 X
PKS B0206-688	02 06 47.7	-68 52 06	02 06 47.88	-68 52 06.4	A	1c	Q	0.3	-0.4	19.6					0.31	0.32	0.25
PKS B0207-149	02 07 58.8	-14 59 05	02 07 58.90	-14 59 06.3	P	3	G	-1.7	0.7	24.1		24.6			0.37	0.50	0.25
PKS B0208-512	02 08 57.1	-51 15 06	02 08 56.96	-51 15 07.8	C	1a	Q			17.6			1.003	8	3.56	3.21	0.25
PKS B0213-026	02 13 09.9	-02 36 52	02 13 09.88	-02 36 51.5	P	3	Q	-0.1	0.1	21.6		20.9	1.177	83	0.54	0.77	0.25
PKS B0214-085	02 14 34.3	-08 34 43	02 14 34.46	-08 34 43.7	P	1b	BL	0.0	-0.4	17.5				83	0.43	0.34	0.25
PKS B0214-330	02 14 38.5	-33 01 35	02 14 38.55	-33 01 32.4	N	1a	Q			18.0			1.331	83	0.25	0.24	0.20
PKS B0214-522	02 14 17.2	-52 14 05	02 14 17.21	-52 14 05.5	W	3	G	1.2	0.6	23.0					0.70	0.55	0.25
PKS B0215+015	02 15 14.1	+01 31 00	02 15 14.14	+01 31 00.0	P	1b	BL	-0.2	-0.1	18.5			1.715	18	0.73	1.06	0.25
PKS B0215-015	02 15 22.0	-01 35 39	02 15 22.22	-01 35 40.1	P	3	Q*	-1.3	-0.2	22.9		21.9			0.27	0.22	0.25
PKS B0216+011	02 16 32.5	+01 07 13	02 16 32.43	+01 07 12.9	N	1a	Q			20.0			1.623	19	0.62	0.73	0.25
PKS B0217-189	02 17 00.2	-18 56 24	02 17 00.33	-18 56 24.4	P	1b	BL	0.0	-0.3	19.5				83	0.40	0.46	0.25
PKS B0218-220	02 18 16.8	-22 04 54	02 18 16.80	-22 04 54.6	P	1b	Q*	0.1	0.1	18.5					0.22	0.21	0.25 X
PKS B0218-683	02 18 44.0	-68 20 02	02 18 43.48	-68 20 01.4	A	3	G	0.7	-0.3	23.1					0.30	0.29	0.25
PKS B0219-164	02 19 38.2	-16 28 55	02 19 38.29	-16 28 55.5	P	1b	Q	-0.7	-0.9	19.0			0.70	31	0.33	0.38	0.25
PKS B0219-474	02 19 37.0	-47 26 37				1a	Q?			18.0					0.33	0.31	0.25
PKS B0219-637	02 19 37.8	-63 43 59				1a	Q			18.3					0.51	0.46	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0220-349	02 20 49.6	-34 55 04	02 20 49.59	-34 55 4.5	N	1a	Q			22.0			1.49	20	0.60	0.61	0.20
PKS B0221-171	02 21 21.7	-17 10 06	02 21 21.96	-17 10 12.3	P	1b	Q*	-0.5	-1.1	19.5					0.22	0.23	0.25 X
PKS B0222+000	02 22 34.1	+00 03 37	02 22 34.17	+00 03 35.7	N	1a	Q			19.0			0.523	8	0.14	0.11	0.10
PKS B0223+012	02 23 34.9	+01 16 03	02 23 35.02	+01 15 58.0	N	1a	Q			19.0			1.369	4	0.21	0.17	0.10
PKS B0225-065	02 25 15.2	-06 34 35	02 25 15.22	-06 34 32.3	N	1a	e								0.35	0.28	0.25
PKS B0226-038	02 26 22.0	-03 50 57	02 26 22.08	-03 50 58.5	P	1b	Q	-0.4	-0.3	17.5			2.064	21	0.77	0.71	0.25
PKS B0226-559	02 26 46.8	-55 59 25				1a	Q			17.6					0.43	0.45	0.25
PKS B0227-369	02 27 24.9	-36 57 03	02 27 24.85	-36 57 17.1	N	1a	Q			19.0			2.115	83	0.25	0.27	0.25
PKS B0229-398	02 29 52.0	-39 48 59	02 29 52.07	-39 48 58.5	N	1a	Q			22.3			1.646	20	0.64	0.68	0.25
PKS B0230-790	02 30 28.9	-79 00 59	02 30 28.73	-79 01 00.9	C	1a	Q			18.6			:1.07	22	0.57	0.77	0.20
PKS B0231+022	02 31 13.3	+02 15 48	02 31 13.51	+02 16 16.3	N	1a	NCS			17.5			0.322	23	0.07	0.11	0.10 X
PKS B0233-478	02 33 18.7	-47 50 12	02 33 18.49	-47 50 12.7	A	2	Q*	0.4	-2.2	17.3					0.46	0.37	0.25
PKS B0234-301	02 34 21.5	-30 06 56	02 34 21.61	-30 06 56.1	N	1a	Q			18.0			2.102	8	0.42	0.53	0.20
PKS B0235-618	02 35 37.6	-61 49 14	02 35 37.76	-61 49 13.5	C	1a	Q			17.8					0.55	0.59	0.25
PKS B0237-027	02 37 13.7	-02 47 33	02 37 13.72	-02 47 32.9	P	1b	Q	-0.8	-0.1	19.0			1.116	24	0.68	1.16	0.25
PKS B0238-052	02 38 26.2	-05 17 30	02 38 26.32	-05 17 30.8	P	1b	BL	-0.9	-0.5	18.5				83	0.33	0.41	0.25
PKS B0238-084	02 38 37.3	-08 28 09	02 38 37.36	-08 28 09.0	P	1b	G	0.4	-0.9	11.6			0.004	3	0.58	1.40	0.25
PKS B0239-553	02 39 15.0	-55 21 00	02 39 16.84	-55 20 30.9	A	1a	NCS	-1.7	-2.3	23.7					0.16	0.16	0.25 X
PKS B0240-021	02 40 15.0	-02 10 12	02 40 15.45	-02 10 33.1	N	1a	Q			19.0			0.617	4	0.12	0.10	0.10
PKS B0240-060	02 40 43.2	-06 03 38	02 40 43.25	-06 03 37.5	P	1b	Q	-1.0	-0.5	19.0			1.805	83	0.53	0.52	0.25
PKS B0240-217	02 40 19.3	-21 45 10	02 40 19.34	-21 45 09.7	P	1b	G	0.2	-0.6	17.0			0.314	3	0.97	0.82	0.25
PKS B0241-513	02 41 33.8	-51 17 56	02 41 34.06	-51 17 57.3	A	1c	Q	0.3	-1.4	20.1					0.40	0.56	0.25
PKS B0244-128	02 44 34.7	-12 49 02	02 44 34.70	-12 49 02.2	P	1b	Q	-0.9	-0.2	18.5			2.201	6	0.32	0.32	0.25
PKS B0244-297	02 44 12.9	-29 47 38	02 44 12.88	-29 47 38.7	P	1a	NCS	-0.4	-0.4	22.5					0.36	0.34	0.25 X
PKS B0244-470	02 44 13.4	-47 03 50				1a	Q?			18.5					0.73	0.59	0.25
PKS B0245-167	02 45 47.2	-16 44 15	02 45 47.28	-16 44 14.2	P	1b	BL	-1.0	0.2	20.0				83	0.34	0.32	0.25
PKS B0248-266	02 48 24.2	-26 40 02	02 48 24.34	-26 40 03.1	P	1b	Q*	0.5	0.2	19.0					0.21	0.28	0.25 X
PKS B0248-412	02 48 51.0	-41 15 56				1a	Q			19.0					0.23	0.22	0.25 X
PKS B0250-602	02 50 11.2	-60 12 19				1a	Q			19.0					0.28	0.32	0.25
PKS B0252-549	02 52 00.2	-54 54 02	02 52 00.26	-54 54 02.4	C	1a	Q			17.9			0.537	5	0.76	0.80	0.25
PKS B0253-218	02 53 57.5	-21 49 35	02 53 57.51	-21 49 32.9	P	1b	Q	-0.7	0.4	18.5			1.470	31	0.30	0.25	0.25
PKS B0253-754	02 53 32.3	-75 25 26				1a	Q			21.6					0.34	0.28	0.20
PKS B0254-334	02 54 39.2	-33 27 12	02 54 39.41	-33 27 23.0	N	1a	Q			17.0			1.915	8	0.37	0.42	0.20
PKS B0256-005	02 56 55.4	-00 31 52	02 56 55.12	-00 31 54.2	P	1b	Q	-1.3	-1.0	17.5			1.998	25	0.27	0.23	0.25
PKS B0256-393	02 56 18.9	-39 21 44	02 56 18.47	-39 21 37.8	A	2	Q	-0.5	-0.2	19.6			3.449	83	0.32	0.36	0.25
PKS B0257-128	02 57 32.0	-12 48 29	02 57 32.13	-12 48 27.7	P	1b	G	-0.3	0.3	17.0					0.30	0.24	0.25
PKS B0257-510	02 57 02.5	-51 03 58				1a	Q			20.8					0.45	0.39	0.25
PKS B0258+011	02 58 49.0	+01 06 52	02 58 48.85	+01 06 47.2	N	1a	Q			20.5			1.221	83	0.37	0.32	0.25
PKS B0258-018	02 58 24.8	-01 51 10	02 58 24.59	-01 51 09.4	P	1b	G	0.2	-2.2	19.0					0.16	0.14	0.25 X
PKS B0258-184	02 58 48.5	-18 24 06	02 58 48.60	-18 24 06.7	P	1b	Q	0.1	-0.2	19.0			1.627	83	0.25	0.31	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0258-344	02 58 34.7	-34 25 58	02 58 34.61	-34 25 54.9	N	1a	Q			18.0			1.704	83	0.35	0.33	0.20
PKS B0259-316	02 59 11.5	-31 38 29	02 59 11.50	-31 38 5.2	N	1a	G			18.5					0.39	0.42	0.20
PKS B0300-186	03 00 34.0	-18 36 07	03 00 33.97	-18 36 14.5	N	1a	G			17.0			0.089	26	0.20	0.17	0.25 X
PKS B0301-721	03 01 31.4	-72 08 17	03 01 31.52	-72 08 18.0	A	1c	Q	1.0	-0.9	18.6					0.39	0.40	0.25
PKS B0302-623	03 02 48.0	-62 23 03	03 02 48.14	-62 23 04.1	C	1a	Q			19.1					1.11	1.47	0.25
PKS B0305-131	03 05 00.9	-13 09 47	03 05 01.12	-13 09 51.1	N	1a	NCS			18.5					0.47	0.38	0.25 X
PKS B0308-611	03 08 51.2	-61 09 57	03 08 51.29	-61 09 58.3	C	1a	Q			18.6					0.85	1.32	0.25
PKS B0310+013	03 10 08.7	+01 22 11	03 10 08.55	+01 22 4.7	N	1a	Q			18.5			0.660	27	0.42	0.46	0.25
PKS B0312-770	03 12 56.4	-77 02 59				1a	Q			17.2			0.223	5	0.50	0.59	0.20
PKS B0313-107	03 13 32.5	-10 42 43	03 13 32.53	-10 42 41.1	P	1b	Q*	-0.5	-0.1	18.5					0.23	0.19	0.25 X
PKS B0313-171	03 13 09.1	-17 07 32	03 13 09.28	-17 07 32.9	P	2	Q*	-0.1	0.0	18.4					0.22	0.25	0.25 X
PKS B0315-282	03 15 26.9	-28 14 14	03 15 26.88	-28 14 13.5	N	1b	Q			20.0			1.166	83	0.40	0.41	0.25
PKS B0318-388	03 18 53.4	-38 48 15	03 18 53.70	-38 48 14.9	A	3	Q*	-0.1	1.4	20.7					0.38	0.31	0.25
PKS B0320+015	03 20 34.6	+01 35 13	03 20 34.62	+01 35 12.5	P	3	G	0.5	0.4	23.5	22.9	23.4			0.49	0.42	0.25
PKS B0323-244	03 23 03.2	-24 26 22	03 23 03.11	-24 26 18.4	P	2	Q	-0.1	0.2	21.6			1.161	83	0.29	0.26	0.25
PKS B0324-489	03 24 18.0	-48 57 47	03 24 17.87	-48 58 00.8	A	3	G	0.0	0.2	:24.5	22.3	23.8			0.26	0.23	0.25
PKS B0325-222	03 25 47.5	-22 12 26	03 25 47.50	-22 12 27.3	P	1b	Q	-0.3	-0.3	19.0			2.220	10	0.40	0.41	0.25
PKS B0327-241	03 27 43.9	-24 07 23	03 27 43.88	-24 07 23.1	P	2	Q	-0.1	0.3	18.8			0.888	20	0.63	0.73	0.25
PKS B0328-469	03 28 41.5	-46 58 10				1a	Q?			18.0					0.18	0.18	0.25 X
PKS B0329-255	03 29 00.5	-25 34 53	03 29 00.46	-25 34 53.2	P	1b	Q	-0.4	-0.6	17.1			2.685	5	0.41	0.38	0.25
PKS B0331-448	03 31 55.6	-44 48 57	03 31 54.95	-44 49 01.9	A	3	G	1.5	1.8	23.2	21.5	22.6			0.28	0.22	0.25
PKS B0331-654	03 31 07.1	-65 28 12	03 31 06.89	-65 28 14.4	A	1c	Q	1.0	4.1	20.1					0.73	0.59	0.25
PKS B0332-403	03 32 25.2	-40 18 24	03 32 25.24	-40 18 23.8	C	1a	Q			18.5			:1.445		1.96	2.60	0.25
PKS B0333-729	03 33 03.2	-72 59 04	03 33 03.25	-72 59 04.4	A	1c	Q	0.6	-0.7	19.3					0.43	0.65	0.25
PKS B0334-131	03 34 13.7	-13 11 55	03 34 13.86	-13 11 55.0	N	1a	Q			19.0			1.303	83	0.33	0.42	0.25
PKS B0334-546	03 34 35.9	-54 40 17	03 34 36.04	-54 40 17.1	C	1a	Q			20.4					0.56	0.63	0.25
PKS B0335-122	03 35 33.5	-12 13 59	03 35 33.37	-12 13 51.1	P	2	Q	-0.8	-0.6	21.5		21.8	3.450	28	0.34	0.38	0.25
PKS B0335-364	03 35 00.0	-36 25 55	03 35 00.02	-36 25 54.4	N	1a	Q			18.0			1.537	29	0.46	0.46	0.25
PKS B0336-019	03 36 58.9	-01 56 17	03 36 58.96	-01 56 16.9	P	1b	Q	-1.0	-0.8	18.4			0.852	7	2.58	2.75	0.25
PKS B0338-214	03 38 23.3	-21 29 08	03 38 23.29	-21 29 07.9	P	1b	BL	-0.5	-0.3	17.5				10	0.82	0.94	0.25
PKS B0340-600	03 40 24.0	-60 03 43	03 40 22.86	-60 03 40.8	A	2	Q*	0.0	0.3	18.6					0.25	0.26	0.25
PKS B0341-256	03 41 12.0	-25 39 44	03 41 12.16	-25 39 44.3	P	1b	Q	0.0	-0.3	19.0			1.419	83	0.40	0.38	0.25
PKS B0342-528	03 42 29.5	-52 50 43				1a	G			18.5					0.37	0.31	0.25
PKS B0346-163	03 46 21.8	-16 19 25	03 46 21.83	-16 19 25.6	P	1b	BL	-0.1	-1.4	18.0				83	0.54	0.55	0.25
PKS B0346-279	03 46 34.0	-27 58 21	03 46 34.03	-27 58 21.0	P	1b	Q	0.5	-0.4	19.5			0.991	9	1.10	0.96	0.25
PKS B0347-211	03 47 45.7	-21 11 47	03 47 45.78	-21 11 50.5	P	2	Q	0.3	0.0	21.1			2.944	83	0.37	0.52	0.25
PKS B0348-120	03 48 49.2	-12 02 21	03 48 49.17	-12 02 21.4	P	1b	Q	-0.7	-0.1	19.5			1.520	3	0.50	0.54	0.25
PKS B0348-326	03 48 45.2	-32 41 57	03 48 45.39	-32 41 58.8	S	3	G	2.9	-0.6	22.9	21.0	23.1	0.927	83	0.27	0.23	0.20
PKS B0350-518	03 50 06.1	-51 51 50				1a	Q			20.2					0.36	0.41	0.25
PKS B0351-701	03 51 52.7	-70 08 30	03 51 52.69	-70 08 27.1	A	3	Q	0.8	0.1	22.4		20.5	0.455	83	0.32	0.29	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0352-153	03 52 13.7	-15 23 01	03 52 14.77	-15 23 01.1	P	1b	G	-0.3	0.2	18.0					0.29	0.25	0.25
PKS B0352-164	03 52 07.9	-16 25 09	03 52 07.96	-16 25 09.0	P	1b	Q	-0.9	-0.1	19.0			1.187	6	0.40	0.40	0.25
PKS B0352-255	03 52 00.2	-25 31 04	03 51 57.26	-25 31 39.8	N	1a	Q?			19.5					0.18	0.15	0.25 X
PKS B0353-474	03 53 30.9	-47 27 46	03 53 31.66	-47 27 47.4	A	2	Q*	1.2	0.5	21.6					0.22	0.22	0.25 X
PKS B0354-263	03 54 46.1	-26 21 29	03 54 46.13	-26 21 21.6	N	1a	G			18.5					0.23	0.20	0.25 X
PKS B0355-079	03 55 17.5	-07 59 49	03 55 17.53	-07 59 48.9	P	1b	Q	-1.0	-0.7	18.0			1.050	31	0.34	0.43	0.25
PKS B0355-483	03 55 52.5	-48 20 49	03 55 52.51	-48 20 49.2	C	1a	Q			17.5			1.016	30	0.61	0.57	0.25
PKS B0355-669	03 55 27.8	-66 54 12	03 55 27.83	-66 54 12.1	C	1a	Q			18.7					0.74	0.62	0.25
PKS B0357-264	03 57 28.4	-26 23 58	03 57 28.47	-26 23 58.1	P	2	BL	-0.2	-0.1	21.7				83	0.58	0.47	0.25
PKS B0400-319	04 00 23.6	-31 55 42	04 00 23.61	-31 55 42.0	C	1c	Q	0.3	-0.5	19.5			1.288	83	1.14	1.03	0.20
PKS B0402-362	04 02 02.6	-36 13 12	04 02 02.62	-36 13 11.5	N	1a	Q			16.5			1.417	8	1.04	1.29	0.25
PKS B0403-132	04 03 14.0	-13 16 19	04 03 13.99	-13 16 18.2	P	1b	Q	-0.7	-0.5	17.1			0.571	21	3.15	3.24	0.25
PKS B0403-179	04 03 57.4	-17 58 00	04 03 57.43	-17 57 59.7	P	1b	Q	-0.7	0.0	19.0			1.640	10	0.38	0.32	0.25
PKS B0405-331	04 05 38.5	-33 11 42	04 05 38.50	-33 11 41.8	N	1a	Q			19.0			2.562	20	0.70	0.63	0.20
PKS B0405-385	04 05 12.1	-38 34 25	04 05 11.95	-38 34 26.1	N	1a	Q			18.0			1.285	32	1.02	1.06	0.25
PKS B0405-712	04 04 19.2	-71 17 15				1a	Q			19.0					0.31	0.25	0.25
PKS B0406-056	04 06 31.7	-05 37 32	04 06 31.65	-05 37 32.0	P	1b	G	-0.6	-0.2	18.5			0.304	83	0.41	0.34	0.25
PKS B0406-127	04 06 45.3	-12 46 39	04 06 45.33	-12 46 39.1	P	1b	Q	0.1	-0.8	18.5			1.563	33	0.59	0.61	0.25
PKS B0406-311	04 06 27.5	-31 08 33	04 06 27.63	-31 08 44.0	S	1a	NCS	0.8	-0.9	23.7	22.6				0.55	0.55	0.20 X
PKS B0409-045	04 09 22.0	-04 32 02	04 09 20.54	-04 31 56.6	N	1a	Q?			19.5					0.14	0.15	0.25 X
PKS B0410-519	04 10 19.1	-51 57 01				1a	Q			17.5					0.48	0.59	0.25
PKS B0410-756	04 10 47.8	-75 41 33	04 10 49.34	-75 41 32.3	A	3	G	-0.6	0.8	23.3	21.6	22.8			0.25	0.21	0.20
PKS B0411-462	04 11 17.4	-46 12 32	04 11 18.53	-46 12 24.4	A	2	Q	-0.4	-0.3	20.4			2.223	83	0.42	0.33	0.25
PKS B0414-189	04 14 23.3	-18 58 30	04 14 23.36	-18 58 29.7	P	1b	Q	-0.6	-0.5	18.0			1.536	26	1.18	1.31	0.25
PKS B0414-467	04 14 27.8	-46 45 05	04 14 28.63	-46 45 11.5	T	2	G	1.7	-0.4	:23.0					0.45	0.36	0.25
PKS B0415-029	04 15 26.5	-02 57 30	04 15 27.51	-02 57 35.8	N	1a	X								0.16	0.14	0.25 X
PKS B0418-151	04 18 00.8	-15 08 33	04 18 00.93	-15 08 33.7	P	1b	Q*	-0.5	0.3	20.5					0.16	0.28	0.25 X
PKS B0420+022	04 20 16.1	+02 12 29	04 20 16.04	+02 12 30.0	N	1a	Q			19.5			2.277	83	0.33	0.67	0.25
PKS B0420-014	04 20 43.5	-01 27 29	04 20 43.54	-01 27 28.7	P	1b	Q	-0.8	-0.3	18.0			0.914	7	2.14	4.15	0.25
PKS B0420-484	04 20 01.0	-48 25 15	04 20 01.95	-48 25 05.9	A	2	Q	0.2	-0.1	17.5			0.527	83	0.29	0.29	0.25
PKS B0421+019	04 21 32.7	+01 57 33	04 21 32.69	+01 57 33.0	N	1a	Q			17.5			2.048	34	0.83	0.73	0.25
PKS B0422+004	04 22 12.5	+00 29 17	04 22 12.50	+00 29 17.1	N	1a	BL			16.0			:0.31	35	1.28	1.60	0.25
PKS B0422-380	04 22 56.2	-38 03 09	04 22 56.29	-38 03 09.9	N	1a	Q			16.5			0.780	15	0.49	0.81	0.25
PKS B0422-389	04 22 49.1	-38 55 30	04 22 49.10	-38 55 30.9	N	1a	Q			18.0			2.346	83	0.47	0.37	0.25
PKS B0423-163	04 23 37.6	-16 19 24	04 23 37.66	-16 19 25.1	P	3	Q*	-0.8	-1.6	24.6	21.8	23.3			0.55	0.44	0.25
PKS B0426-380	04 26 54.7	-38 02 52	04 26 54.67	-38 02 52.3	N	1a	BL			18.0				83	1.04	1.14	0.25
PKS B0427-435	04 27 49.7	-43 35 02				1a	Q			18.0			1.423	83	0.30	0.25	0.25
PKS B0431-512	04 31 04.2	-51 15 44				1a	Q			17.7			0.557	30	0.68	0.57	0.25
PKS B0432-440	04 32 30.2	-44 02 03	04 32 29.42	-44 01 58.2	A	2	Q	-0.7	0.3	19.6			2.649	83	0.29	0.25	0.25
PKS B0432-606	04 32 50.3	-60 36 25				1a	Q			19.0					0.43	0.39	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0434-188	04 34 49.0	-18 50 48	04 34 48.97	-18 50 48.2	P	1b	Q	-0.3	-0.5	20.0			2.702	3	1.05	1.19	0.25
PKS B0435-083	04 35 43.8	-08 23 24	04 35 43.13	-08 24 44.9	V	3	G	-0.7	-0.9	>24.0		24.4			0.20	0.22	0.25 X
PKS B0436-089	04 36 13.8	-08 54 14	04 36 13.88	-08 54 14.8	P	1b	G	-0.6	-0.1	20.0					0.35	0.31	0.25
PKS B0436-129	04 36 15.5	-12 56 56	04 36 15.60	-12 56 56.8	P	1b	Q	-0.4	-0.3	19.0			1.277	31	0.40	0.43	0.25
PKS B0436-203	04 36 39.6	-20 18 14	04 36 39.84	-20 18 18.5	P	3	Q	-1.8	1.4	22.8		23.1	2.146	83	0.36	0.30	0.25
PKS B0437-454	04 37 30.6	-45 28 12	04 37 30.64	-45 28 12.4	W	2	Q*	0.0	-0.2	20.8					1.22	1.37	0.25
PKS B0438-436	04 38 43.2	-43 38 53	04 38 43.19	-43 38 53.5	C	1a	Q			19.5			2.863	36	6.50	7.00	0.25
PKS B0439-299	04 39 21.9	-29 58 17	04 39 21.93	-29 58 17.8	P	1b	G	-0.5	-1.0	19.5					0.41	0.33	0.25
PKS B0439-433	04 39 43.6	-43 19 10				1a	Q			16.5			0.593	31	0.32	0.30	0.25
PKS B0439-501	04 39 52.4	-50 09 50	04 39 53.69	-50 09 44.4	A	2	Q*	-0.7	-0.1	20.6					0.25	0.21	0.25
PKS B0440-285	04 40 38.0	-28 31 06	04 40 38.06	-28 31 07.0	P	1b	Q	-0.3	-1.4	19.0			1.952	9	0.34	0.45	0.25
PKS B0440-520	04 40 45.0	-52 00 34				1a	Q?			17.5					0.32	0.33	0.25
PKS B0445-019	04 45 11.6	-01 58 01	04 45 11.00	-01 58 03.5	P	1b	Q	-0.2	0.1	19.0					0.23	0.18	0.25 X
PKS B0446-175	04 46 50.8	-17 34 25	04 46 50.53	-17 34 23.8	P	2	G	-0.2	0.2	23.3		22.1			0.24	0.19	0.25 X
PKS B0446-212	04 46 08.4	-21 15 02	04 46 08.27	-21 14 57.8	P	1b	Q	0.0	0.1	19.5			1.971	37	0.29	0.28	0.25
PKS B0446-370	04 46 30.1	-37 04 29	04 46 29.19	-37 04 14.3	A	2	Q	0.1	-0.9	18.9			0.561	83	0.27	0.26	0.25
PKS B0447-010	04 47 10.4	-01 02 28	04 47 10.27	-01 02 30.2	P	1b	Q	-0.9	-0.8	19.5			0.487	83	0.41	0.35	0.25
PKS B0448-187	04 48 23.8	-18 42 07	04 48 23.68	-18 42 03.9	P	1b	Q	0.1	-0.7	19.0			2.05	31	0.43	0.43	0.25
PKS B0448-392	04 48 00.4	-39 16 15	04 48 00.47	-39 16 15.4	N	1a	Q			17.5			1.288	15	0.89	0.89	0.25
PKS B0450-230	04 50 37.7	-23 03 10	04 50 38.31	-23 03 00.6	N	2	Q?	-1.0	2.4	21.2					0.23	0.19	0.25 X
PKS B0450-469	04 50 27.8	-46 58 16	04 50 27.91	-46 58 16.2	C	1a	Q?			19.0					0.69	0.58	0.25
PKS B0451-282	04 51 15.1	-28 12 29	04 51 15.14	-28 12 29.4	P	1b	Q	0.5	-1.1	19.0			2.564	24	2.38	2.50	0.25
PKS B0454-234	04 54 57.3	-23 29 28	04 54 57.31	-23 29 28.3	P	1b	Q	0.0	0.5	18.5			1.003	1	1.76	2.00	0.25
PKS B0455-395	04 55 47.0	-39 32 05	04 55 48.02	-39 32 09.9	T	2	Q	-0.2	-0.1	18.6			0.570	9	0.15	0.14	0.25 X
PKS B0458-020	04 58 41.3	-02 03 34	04 58 41.35	-02 03 33.9	P	1b	Q	-1.2	0.2	20.0			2.286	27	1.89	2.19	0.25
PKS B0459-308	04 59 12.1	-30 51 50	04 59 11.75	-30 51 55.9	N	1a	Q?			19.0					0.17	0.14	0.20 X
PKS B0500+019	05 00 45.2	+01 58 54	05 00 45.18	+01 58 53.9	W	3	G	-0.3	-0.8	22.8	19.5	21.3	0.584	83	2.46	2.04	0.25
PKS B0503-608	05 03 24.0	-60 53 57				1a	Q			19.3					0.58	0.74	0.25
PKS B0509+011	05 09 23.0	+01 07 10	05 09 22.54	+01 07 16.1	N	1a	G			18.0					0.39	0.35	0.25
PKS B0510-006	05 10 29.5	-00 36 00	05 10 29.44	-00 35 54.2	N	1a	G			19.4					0.33	0.31	0.25
PKS B0511-220	05 11 41.8	-22 02 41	05 11 41.82	-22 02 41.2	P	1b	Q	-0.6	-0.6	19.5			1.296	1	1.21	1.27	0.60
PKS B0512-013	05 12 39.0	-01 22 57	05 12 38.97	-01 23 22.4	P	1b	Q*	-0.3	0.4	18.5					0.15	0.13	0.25 X
PKS B0514-161	05 14 01.1	-16 06 23	05 14 01.08	-16 06 22.6	P	1b	Q	-0.6	-0.2	18.0			1.278	2	0.80	0.76	0.60
PKS B0516-621	05 16 15.4	-62 10 13	05 16 15.38	-62 10 14.4	A	1c	Q	0.4	-0.8	21.0					0.38	0.44	0.25
PKS B0519+011	05 19 42.3	+01 10 41	05 19 42.36	+01 10 41.9	N	2	G?	0.0	-0.8	:22.2					0.55	0.55	0.25
PKS B0522-030	05 22 08.8	-03 03 35	05 22 08.11	-03 03 40.0	N	1a	X								0.06	0.11	0.25 X
PKS B0522-611	05 22 00.2	-61 10 42	05 22 00.39	-61 10 41.4	C	1a	Q			19.0			1.400	33	0.71	0.67	0.25
PKS B0524-433	05 24 23.0	-43 20 35				1a	Q			18.0			2.164	83	0.29	0.27	0.25
PKS B0524-460	05 24 06.0	-46 00 28				1a	Q			17.3			1.479	38	0.91	0.99	0.25
PKS B0524-485	05 24 56.5	-48 33 06				1a	Q?			20.0					0.45	0.48	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0525-127	05 25 09.4	-12 44 16	05 25 09.39	-12 44 17.0	N	1a	PN			10.0					1.63	1.78	0.60
PKS B0528-250	05 28 05.2	-25 05 44	05 28 05.21	-25 05 44.6	P	1b	Q	-0.4	-0.9	19.0			2.813	15	1.32	1.13	0.60
PKS B0528-454	05 28 58.5	-45 26 45				1a	X								0.39	0.34	0.25
PKS B0529-305	05 29 20.5	-30 34 16	05 29 20.62	-30 34 23.6	S	2	G	2.6	-1.4	22.4					0.38	0.31	0.20
PKS B0532-378	05 32 35.2	-37 49 22	05 32 35.26	-37 49 21.4	C	1c	Q	-1.1	0.1	19.5			1.668	20	0.70	0.59	0.25
PKS B0533-120	05 33 13.1	-12 04 31	05 33 13.74	-12 04 14.2	P	1b	G	-0.3	-0.5	17.8			0.157	39	0.80	0.64	0.60
PKS B0534-340	05 34 39.6	-34 02 58	05 34 39.57	-34 02 58.1	W	2	Q	-0.3	-0.3	18.3			0.683	83	0.41	0.73	0.20
PKS B0534-611	05 34 02.4	-61 07 59				1a	Q			18.8					0.42	0.47	0.25
PKS B0537-158	05 37 17.1	-15 52 05	05 37 17.17	-15 52 04.6	P	1b	Q	-0.6	0.0	18.0			0.947	33	0.63	0.61	0.60
PKS B0537-286	05 37 56.9	-28 41 28	05 37 56.94	-28 41 28.0	P	1b	Q	-0.7	-0.5	20.0			3.110	40	0.74	0.99	0.60
PKS B0537-441	05 37 21.1	-44 06 45	05 37 21.08	-44 06 44.6	C	1a	Q			15.0			0.894	8	3.84	3.80	0.25
PKS B0539-057	05 39 11.0	-05 43 15	05 39 11.00	-05 43 15.0	P	1b	Q	-0.3	0.0	20.0			0.893	41	0.65	1.51	0.60
PKS B0549-459	05 49 52.3	-45 56 54				1a	X								0.32	0.31	0.25
PKS B0549-575	05 49 20.8	-57 33 11				1a	Q			19.5					0.35	0.41	0.25
PKS B0551-538	05 51 33.8	-53 50 07				1a	X								0.27	0.22	0.25
PKS B0557-454	05 57 45.0	-45 28 27	05 57 45.79	-45 29 47.0	A	2	Q	-0.4	0.1	17.9			0.687	67	0.24	0.19	0.25 X
PKS B0601-172	06 01 44.8	-17 16 19	06 01 44.77	-17 16 15.8	P	1b	Q	-0.4	-0.8	20.0			2.711	83	0.40	0.55	0.60 X
PKS B0602-424	06 02 52.4	-42 25 14	06 02 52.49	-42 25 14.1	C	1a	Q			19.0			0.611	83	0.35	0.84	0.25
PKS B0605-063	06 05 19.2	-06 22 38	06 05 19.80	-06 22 34.3	N	1a	HII								5.60	6.94	0.60
PKS B0605-085	06 05 36.0	-08 34 20	06 05 36.03	-08 34 20.2	P	1b	Q	-1.6	-2.6	18.0			0.872	38	2.90	3.39	0.60
PKS B0606-223	06 06 53.4	-22 19 46	06 06 53.39	-22 19 46.2	P	1b	Q	-0.6	0.4	20.0			1.926	33	1.00	1.36	0.60
PKS B0607-157	06 07 26.0	-15 42 03	06 07 25.99	-15 42 03.3	P	1b	Q	2.3	-2.9	18.0			0.324	26	2.20	1.77	0.60
PKS B0607-605	06 07 19.5	-60 31 18	06 07 19.56	-60 31 18.7	A	1c	Q	0.0	0.3	18.2					0.34	0.45	0.60 X
PKS B0610-316	06 10 37.0	-31 38 07	06 10 36.98	-31 38 06.6	N	1a	Q			18.5			0.873	83	0.47	0.51	0.20
PKS B0610-436	06 10 58.3	-43 36 58	06 10 58.46	-43 36 57.1	C	1a	Q			19.0			3.461	83	0.35	0.64	0.25
PKS B0613-312	06 13 27.0	-31 16 23	06 13 26.02	-31 16 18.8	N	1a	BL			17.0				83	0.32	0.33	0.20
PKS B0615-305	06 15 45.7	-30 30 16	06 15 45.97	-30 30 18.0	A	3	G	-1.5	1.5	23.6		23.4			0.27	0.23	0.20
PKS B0618-252	06 18 29.7	-25 13 53	06 18 29.77	-25 13 52.2	P	1b	Q	-0.4	-0.5	18.2			:1.90		0.81	0.73	0.60
PKS B0619-468	06 19 50.0	-46 50 30				1a	X								0.43	0.56	0.60 X
PKS B0621-786	06 21 29.7	-78 41 33				1a	Q			17.5			0.942	5	0.16	0.18	0.20 X
PKS B0622-441	06 22 02.7	-44 11 23				1a	Q			17.5			0.688	15	0.77	0.89	0.60
PKS B0625-401	06 25 17.3	-40 11 57	06 25 17.19	-40 10 57.9	T	3	G	-0.2	-0.8	23.4	20.3	22.1			0.25	0.23	0.25
PKS B0627-199	06 27 14.1	-19 57 16	06 27 14.12	-19 57 16.2	P	2	BL	-0.1	0.0	21.1				83	0.57	0.75	0.60 X
PKS B0628-627	06 28 32.7	-62 46 40	06 28 32.76	-62 46 39.4	A	1c	G?	-0.2	0.3	21.5					0.37	0.44	0.60 X
PKS B0629-418	06 29 37.7	-41 52 14	06 29 37.67	-41 52 14.3	C	1a	Q			17.0			1.416	6	0.53	0.74	0.25
PKS B0630-261	06 30 05.0	-26 11 45	06 30 05.37	-26 11 58.4	P	3	Q	2.7	0.1	20.5	19.0	20.2	0.717	83	0.44	0.44	0.60 X
PKS B0637-337	06 37 31.2	-33 43 12	06 37 31.16	-33 43 12.8	N	1a	BL			20.5				83	0.54	0.70	0.20
PKS B0637-752	06 37 23.3	-75 13 37				1a	Q			17.2			0.651	30	5.90	5.49	0.20
PKS B0642-349	06 42 37.4	-34 56 33	06 42 37.45	-34 56 34.0	N	1a	Q			18.5			2.165	15	0.94	0.99	0.20
PKS B0644-390	06 44 50.4	-39 00 06	06 44 50.25	-39 00 22.0	N	1a	Q			18.5			0.681	83	0.28	0.26	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0644-671	06 44 30.3	-67 09 44				1a	G?			21.7					0.32	0.41	0.25
PKS B0646-306	06 46 19.2	-30 40 54	06 46 19.22	-30 40 54.3	W	2	Q	-0.2	-0.9	20.4			1.153	83	0.95	1.06	0.20
PKS B0700-465	07 00 07.5	-46 30 14	07 00 08.86	-46 30 13.5	R	2	Q	0.0	0.0	19.5			0.822	83	0.55	0.64	0.60 X
PKS B0700-661	07 00 23.6	-66 06 26	07 00 23.46	-66 06 23.6	T	1c	Q	-1.4	-1.8	19.2					0.25	0.45	0.25
PKS B0715-663	07 15 06.5	-66 22 44				1a	X								0.43	0.36	0.25
PKS B0726-476	07 26 57.3	-47 39 13	07 26 57.91	-47 39 02.5	T	3	Q	0.1	-0.3	22.4		22.2	2.282	83	0.38	0.30	0.60 X
PKS B0731-465	07 31 16.3	-46 33 53	07 31 15.66	-46 33 45.7	C	2	Q?			22.0					0.83	0.76	0.60
PKS B0736+017	07 36 42.5	+01 44 00	07 36 42.52	+01 44 00.2	P	1b	Q	0.2	-0.2	18.0			0.191	21	2.24	1.85	0.25
PKS B0736-770	07 36 37.3	-77 04 28	07 36 37.07	-77 04 27.3	T	1c	Q	0.4	-0.1	21.6					0.26	0.21	0.20
PKS B0738-674	07 38 49.7	-67 28 50				1a	Q			19.8			1.663	31	0.45	0.56	0.25
PKS B0743-006	07 43 21.0	-00 36 56	07 43 21.05	-00 36 55.7	P	1b	Q	-0.2	-0.8	18.0			0.994	9	1.01	1.31	0.25
PKS B0744-691	07 44 25.4	-69 11 47				1a	Q			21.5					0.38	0.43	0.25
PKS B0748-006	07 48 37.0	-00 39 09	07 48 37.21	-00 39 08.6	P	1b	Q	0.1	-0.2	20.5					0.20	0.23	0.25 X
PKS B0800-098	08 00 16.1	-09 49 44	08 00 08.76	-09 49 06.3	N	1a	NCS			18.5					1.20	0.99	0.60 X
PKS B0802-010	08 02 42.9	-01 02 50	08 02 40.26	-01 02 37.8	P	1b	NCS	-0.3	0.0	17.5			0.088	43	0.33	0.33	0.25 X
PKS B0805-077	08 05 49.5	-07 42 22	08 05 49.56	-07 42 22.3	P	1b	Q	-0.2	-0.4	19.0			1.837	9	1.10	1.01	0.60
PKS B0805-119	08 05 14.4	-11 58 59	08 05 14.41	-11 58 58.4	P	1a	NCS	-0.1	0.0	19.1					0.51	0.44	0.60 X
PKS B0806-710	08 06 46.3	-71 03 30	08 06 46.59	-71 03 26.9	A	1c	Q	-0.2	0.4	20.0			0.330	83	0.44	0.40	0.25
PKS B0808+019	08 08 51.1	+01 55 51	08 08 51.14	+01 55 51.2	P	1b	BL	0.0	-0.6	17.0			:0.93		0.40	0.59	0.25
PKS B0813-741	08 13 14.2	-74 11 07	08 13 15.57	-74 11 05.2	A	1a	NCS	-4.3	-1.0	23.2					0.40	0.38	0.25 X
PKS B0818-128	08 18 36.2	-12 49 25	08 18 36.26	-12 49 25.0	P	1b	BL	-0.7	-0.1	18.0					0.87	0.81	0.60
PKS B0819+012	08 19 01.1	+01 12 28	08 19 00.37	+01 12 08.4	N	2	G	1.0	2.7	17.0					0.10	0.08	0.25 X
PKS B0819-032	08 19 09.5	-03 13 39	08 19 09.46	-03 13 36.2	P	1b	Q	-0.8	-0.8	18.2			2.352	15	0.37	0.30	0.25
PKS B0834-201	08 34 24.6	-20 06 30	08 34 24.64	-20 06 29.6	N	1b	Q			19.0			2.752	24	4.15	3.42	0.60
PKS B0834-223	08 34 38.5	-22 22 40	08 34 38.52	-22 22 40.1	P	2	Q	0.0	-1.4	18.0			0.837	83	0.50	0.47	0.60 X
PKS B0837+012	08 37 14.6	+01 15 04	08 37 14.81	+01 15 06.3	N	1a	Q			19.0			1.123	44	0.45	0.39	0.25
PKS B0845-051	08 45 29.5	-05 09 28	08 45 29.52	-05 09 27.7	N	1a	Q			19.5			1.242	33	0.49	0.40	0.60 X
PKS B0855-716	08 55 04.1	-71 37 31				1a	Q			19.3					0.33	0.38	0.25
PKS B0858-004	08 58 52.8	-00 25 12	08 58 52.50	-00 25 13.6	N	1a	Q			20.0					0.24	0.19	0.25 X
PKS B0858-771	08 58 39.5	-77 07 42				1a	Q			18.0			0.489	31	0.42	0.33	0.20
PKS B0859-140	08 59 54.9	-14 03 39	08 59 54.95	-14 03 38.7	P	1b	Q	-0.2	-0.1	16.6			1.333	31	2.93	2.29	0.60
PKS B0902-256	09 02 40.9	-25 40 51	09 02 40.89	-25 40 51.3	P	1b	Q	-0.2	-0.1	18.0			1.635	33	0.50	0.47	0.60 X
PKS B0906+015	09 06 35.2	+01 33 48	09 06 35.19	+01 33 48.2	P	1b	Q	0.0	-1.0	18.0			1.020	15	0.97	1.20	0.25
PKS B0907+022	09 07 04.1	+02 12 19	09 07 04.42	+02 12 19.3	N	1a	BL			19.0				83	0.26	0.43	0.25
PKS B0909-745	09 09 33.2	-74 32 49				1a	Q			21.0					0.31	0.28	0.25
PKS B0913+003	09 13 18.0	+00 19 55	09 13 17.78	+00 19 45.4	N	2	Q	-0.8	0.0	21.7			3.074	83	0.27	0.25	0.25
PKS B0915-213	09 15 10.3	-21 18 57	09 15 10.44	-21 18 57.0	P	1b	Q	-0.4	-0.5	18.5			0.847	33	0.59	0.54	0.60 X
PKS B0919-260	09 19 16.7	-26 05 55	09 19 16.71	-26 05 54.4	P	1b	Q	-0.2	-1.0	19.0			2.300	33	1.15	1.28	0.60
PKS B0921-213	09 21 21.8	-21 22 47	09 21 21.83	-21 22 52.2	P	1b	G	-0.1	-0.5	16.5			0.052	45	0.53	0.42	0.60 X
PKS B0922+005	09 22 33.7	+00 32 12	09 22 33.68	+00 32 12.9	N	1a	Q			18.5			1.720	23	0.82	0.70	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B0925-203	09 25 33.5	-20 21 45	09 25 33.55	-20 21 44.8	P	1b	Q	0.2	-0.8	16.3			0.348	45	0.81	0.70	0.60
PKS B0926-039	09 26 01.8	-03 55 52	09 26 02.61	-03 56 02.2	V	2	Q*	0.3	0.5	20.3					0.14	0.13	0.60 X
PKS B0928+008	09 28 18.1	+00 48 12	09 28 17.99	+00 48 12.6	N	1a	Q			19.0			0.505	6	0.30	0.33	0.25
PKS B0930-338	09 30 29.0	-33 52 31	09 30 30.03	-33 52 38.6	S	2	Q	-1.7	-0.8	19.5			0.936	83	0.34	0.31	0.20
PKS B0931-114	09 31 08.8	-11 26 03	09 31 08.91	-11 26 04.0	P	3	G	-2.9	-1.0	23.0	20.7	22.1			0.45	0.44	0.60 X
PKS B0933-333	09 33 01.1	-33 19 08	09 33 01.71	-33 19 12.0	V	2	Q	-0.8	-0.3	20.0		20.8	2.906	83	0.31	0.32	0.20
PKS B0938-002	09 38 07.3	-00 14 56	09 38 06.96	-00 14 21.6	P	2	Q*	-0.3	0.6	20.4		21.5			0.24	0.22	0.25 X
PKS B0945-321	09 45 58.9	-32 09 49	09 45 58.86	-32 09 48.5	N	1a	Q			19.0			2.14	9	0.58	0.83	0.20
PKS B0952-691	09 52 20.0	-69 10 12	09 52 19.88	-69 10 12.7	A	1c	Q	0.8	-0.2	19.1					0.27	0.22	0.25
PKS B0958-314	09 58 27.4	-31 25 26	09 58 27.69	-31 25 23.9	N	1a	G			12.7					0.48	0.51	0.20
PKS B0959-307	09 59 26.1	-30 44 07	09 59 26.07	-30 43 59.7	N	1a	NCS								0.61	0.49	0.20 X
PKS B1004-018	10 04 31.7	-01 52 31	10 04 31.72	-01 52 30.5	P	1b	Q	-0.2	0.1	19.2			1.212	7	0.59	0.53	0.25
PKS B1004-217	10 04 25.8	-21 44 39	10 04 25.50	-21 44 40.3	P	1b	Q	0.0	-0.2	16.4			0.330	22	0.30	0.30	0.25
PKS B1005-333	10 05 17.5	-33 18 15	10 05 18.54	-33 18 26.9	N	1a	Q			18.0			1.837	83	0.27	0.31	0.20
PKS B1005-739	10 05 22.6	-73 55 03	10 05 22.16	-73 55 04.0	A	1c	Q	1.0	0.3	20.1					0.40	0.48	0.25
PKS B1008+013	10 08 41.6	+01 21 28	10 08 41.19	+01 21 31.1	N	1a	BL			19.0				83	0.27	0.23	0.25
PKS B1008-041	10 08 58.0	-04 08 41	10 08 58.79	-04 08 38.2	P	1b	Q	-0.1	-0.4	18.5					0.17	0.21	0.25 X
PKS B1009-321	10 09 41.8	-32 08 44	10 09 41.78	-32 08 44.0	N	1a	Q			18.1			1.742	30	0.32	0.27	0.20
PKS B1009-328	10 09 53.1	-32 49 30	10 09 51.97	-32 49 25.4	V	2	Q	-0.4	-0.5	19.0		20.0	1.745	83	0.26	0.22	0.20
PKS B1010-255	10 10 54.0	-25 32 20	10 10 53.92	-25 32 01.5	V	2	G	0.3	0.7	21.9		24.1			0.21	0.17	0.25 X
PKS B1010-427	10 10 32.3	-42 43 39				1a	Q			17.5			2.954	83	0.38	0.43	0.25
PKS B1016-268	10 16 50.3	-26 53 46	10 16 49.41	-26 53 50.9	P	2	BL	0.0	-0.1	18.3				83	0.29	0.36	0.25
PKS B1016-311	10 16 12.6	-31 08 51	10 16 12.53	-31 08 51.3	N	1a	Q			18.5			0.794	20	0.62	0.65	0.20
PKS B1021-323	10 21 45.6	-32 18 58	10 21 44.13	-32 19 1.6	N	1a	Q			19.5			1.568	83	0.46	0.37	0.20
PKS B1022-102	10 22 29.6	-10 16 25	10 22 27.60	-10 16 27.9	P	1b	Q	-0.4	-0.8	16.8			2.00	46	0.27	0.27	0.25
PKS B1022-183	10 22 21.5	-18 23 03	10 22 21.47	-18 23 17.4	N	1a	PN			9.0					0.92	0.81	0.25
PKS B1026-084	10 26 09.3	-08 29 15	10 26 09.03	-08 29 16.9	P	2	Q	0.5	0.4	21.4			4.276	47	0.27	0.22	0.25
PKS B1027-186	10 27 08.3	-18 37 29	10 27 08.18	-18 37 27.0	P	1b	Q	0.2	-0.7	19.0			1.784	83	0.26	0.21	0.25
PKS B1029-222	10 29 28.1	-22 13 12	10 29 29.00	-22 12 57.8	P	3	G	1.4	2.6	>23.0		22.6			0.34	0.27	0.25
PKS B1030-357	10 30 52.1	-35 46 27	10 30 51.80	-35 46 31.1	N	1a	Q			20.5			1.455	6	0.66	0.57	0.25
PKS B1031-019	10 31 51.9	-01 55 36	10 31 51.56	-01 55 31.6	V	2	G	-0.6	-0.9	20.7					0.14	0.14	0.25 X
PKS B1032-199	10 32 37.4	-19 56 02	10 32 37.37	-19 56 02.0	P	1b	Q	-0.2	-0.6	18.5			2.198	33	1.10	1.15	0.25
PKS B1034-058	10 34 16.4	-05 50 07	10 34 16.34	-05 50 06.2	P	1b	G?	-0.5	-0.6	20.0					0.46	0.58	0.25
PKS B1034-293	10 34 55.8	-29 18 27	10 34 55.83	-29 18 26.8	P	1b	Q	0.2	-0.1	17.0			0.312	1	1.33	1.51	0.25
PKS B1034-374	10 34 38.2	-37 28 40	10 34 38.16	-37 28 35.1	N	1a	Q			18.5			1.821	6	0.54	0.44	0.25
PKS B1035-728	10 35 57.0	-72 49 55	10 35 56.69	-72 49 54.9	A	1c	Q*	-1.3	-0.8	19.5					0.43	0.39	0.25
PKS B1036-154	10 36 39.5	-15 25 28	10 36 39.48	-15 25 28.0	P	1b	Q	-0.3	-0.7	19.5			0.525	20	0.75	0.78	0.25
PKS B1036-431	10 36 03.5	-43 09 39	10 36 03.06	-43 10 08.8	S	2	Q	1.8	0.4	18.5			1.356	83	0.42	0.39	0.25
PKS B1044-128	10 44 35.6	-12 52 41	10 44 35.09	-12 52 42.1	P	1b	Q	-0.4	-0.7	18.0			1.288	48	0.28	0.33	0.25
PKS B1045+019	10 45 48.4	+01 57 40	10 45 48.43	+01 57 40.0	V	3	G	-0.1	-0.5	>24.5	22.4				0.49	0.43	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B1045-188	10 45 40.1	-18 53 44	10 45 40.10	-18 53 43.9	P	1b	Q	-0.1	-0.5	19.0			0.595	38	0.94	1.11	0.25
PKS B1046-222	10 46 58.6	-22 15 01	10 46 56.61	-22 15 13.9	P	2	Q	0.5	-0.2	21.7		21.1	1.609	83	0.29	0.24	0.25
PKS B1048-313	10 48 43.4	-31 22 19	10 48 43.39	-31 22 18.5	W	2	Q	-0.4	-0.1	18.5			1.429	20	0.80	0.73	0.20
PKS B1049-349	10 49 09.4	-34 58 00	10 49 12.07	-34 58 06.3	V	3	G	-1.1	-2.2	21.8		21.7			0.30	0.24	0.20
PKS B1049-726	10 49 16.7	-72 38 36	10 49 16.33	-72 38 36.5	A	1c	Q	-0.3	0.0	20.4					0.27	0.22	0.25
PKS B1055+018	10 55 55.3	+01 50 04	10 55 55.32	+01 50 03.6	P	1b	Q	0.5	-0.9	18.2			0.888	7	3.15	3.16	0.25
PKS B1055-243	10 55 29.9	-24 17 45	10 55 29.94	-24 17 44.5	P	2	Q	-0.4	0.1	19.9			1.086	20	0.77	0.61	0.25
PKS B1055-248	10 55 29.6	-24 53 50	10 55 28.89	-24 53 24.6	P	2	Q	0.0	0.4	18.7		19.8	0.593	83	0.32	0.31	0.25
PKS B1055-301	10 55 38.3	-30 08 57	10 55 37.28	-30 08 51.0	N	1a	Q			19.5			2.523	83	0.36	0.43	0.20
PKS B1056-113	10 56 42.3	-11 18 17	10 56 42.30	-11 18 17.0	P	1b	BL	-0.4	-0.5	17.5				83	0.37	0.61	0.25
PKS B1057-797	10 57 50.0	-79 47 48	10 57 49.73	-79 47 47.7	C	1c	Q	0.5	0.5	19.0					1.13	1.57	0.20
PKS B1101-325	11 01 07.8	-32 35 01	11 01 08.43	-32 35 8.1	N	1a	Q			15.4			0.355	15	0.93	0.73	0.20
PKS B1102-242	11 02 19.8	-24 15 14	11 02 19.81	-24 15 13.7	P	1b	Q	-0.3	-0.7	19.3			1.666	20	0.50	0.57	0.25
PKS B1104-445	11 04 50.4	-44 32 53	11 04 50.38	-44 32 52.8	C	1a	Q			18.0			1.598	45	1.84	2.03	0.25
PKS B1105-304	11 05 18.8	-30 27 12	11 05 19.45	-30 27 21.0	S	2	Q	0.6	1.7	20.2			0.740	83	0.26	0.26	0.20
PKS B1106-227	11 06 43.3	-22 45 28	11 06 43.34	-22 45 28.6	P	2	Q	0.5	-0.1	20.8			1.875	83	0.32	0.29	0.25
PKS B1110-217	11 10 21.7	-21 42 10	11 10 21.71	-21 42 09.2	P	2	G	0.4	0.1	22.5					0.94	0.76	0.25
PKS B1110-355	11 10 37.6	-35 33 30	11 10 37.70	-35 33 23.1	N	1a	Q			19.0			1.695	83	0.26	0.34	0.25
PKS B1112-080	11 12 00.8	-08 00 25	11 12 00.74	-08 00 17.4	P	3	G	-1.1	1.2	22.6		21.9			0.26	0.34	0.25
PKS B1115-122	11 15 46.1	-12 16 29	11 15 46.13	-12 16 29.5	P	1b	Q	-0.3	-1.0	19.0			1.739	20	0.67	0.63	0.25
PKS B1115-306	11 15 55.9	-30 38 12	11 15 54.25	-30 38 34.2	N	1a	Q?			18.5					0.22	0.18	0.20
PKS B1117-124	11 17 41.4	-12 27 14	11 17 40.99	-12 27 11.5	P	2	G	0.3	-0.2	22.1		21.4			0.26	0.29	0.25
PKS B1117-270	11 17 48.8	-27 02 59	11 17 48.54	-27 02 39.9	P	1b	Q	1.6	-0.2	19.0			1.881	83	0.42	0.34	0.25
PKS B1118-056	11 18 52.1	-05 38 30	11 18 52.52	-05 37 29.2	P	2	Q	-0.6	-0.4	19.4			1.297	20	0.66	0.57	0.25
PKS B1118-140	11 18 24.8	-14 04 02	11 18 24.77	-14 04 03.0	P	1b	Q	-0.3	-0.3	17.5			1.114	83	0.34	0.59	0.25
PKS B1119-069	11 19 09.9	-06 54 52	11 19 09.79	-06 54 39.0	P	2	BL	0.0	-0.6	20.3		20.1		83	0.34	0.42	0.25
PKS B1124-073	11 24 39.3	-07 18 41	11 24 39.98	-07 18 40.9	P	3	Q*	0.8	-0.3	:23.0		21.8			0.37	0.49	0.25
PKS B1124-186	11 24 34.1	-18 40 46	11 24 34.02	-18 40 46.2	P	1b	Q	0.0	-0.9	19.0			1.048	20	0.61	0.84	0.25
PKS B1124-382	11 24 18.8	-38 12 05	11 24 18.38	-38 12 13.8	V	2	G	-0.1	-0.1	22.0		22.1			0.26	0.26	0.25
PKS B1127-145	11 27 35.7	-14 32 54	11 27 35.67	-14 32 54.3	P	1b	Q	-1.3	-0.1	16.9			1.184	31	5.97	5.46	0.25
PKS B1128-047	11 28 57.5	-04 43 46	11 28 57.50	-04 43 45.8	P	1b	G	-0.3	-0.6	20.0			0.266	20	0.74	0.90	0.25
PKS B1131-088	11 31 03.0	-08 48 52	11 31 03.51	-08 48 48.3	P	2	Q*	1.0	0.5	21.5		21.7			0.35	0.31	0.25
PKS B1131-115	11 31 25.4	-11 34 52				1a	NCS								0.27	0.25	0.25 X
PKS B1133-032	11 33 51.3	-03 13 51	11 33 51.25	-03 13 53.1	P	1b	Q	-0.1	-0.5	19.5			1.648	83	0.26	0.39	0.25
PKS B1133-172	11 33 31.6	-17 16 36	11 33 31.60	-17 16 36.4	P	2	Q	-0.1	-0.5	22.4			1.024	20	0.65	0.52	0.25
PKS B1133-739	11 34 01.4	-73 59 09	11 34 01.43	-73 59 08.7	W	2	Q*	0.4	0.1	21.6					0.80	0.63	0.25
PKS B1136-135	11 36 38.6	-13 34 09	11 36 38.52	-13 34 05.9	P	1b	Q	-0.5	-0.4	16.0			0.557	31	2.76	2.22	0.25
PKS B1136-156	11 36 57.7	-15 36 22	11 36 57.61	-15 36 13.8	P	1b	Q	-0.2	-1.0	20.0			2.625	83	0.34	0.51	0.25
PKS B1141+011	11 41 34.8	+01 11 18	11 41 34.79	+01 11 14.9	N	1a	G			19.4					0.34	0.27	0.25
PKS B1142-225	11 42 50.2	-22 33 52	11 42 50.23	-22 33 51.3	P	3	Q	0.2	0.5	22.3		22.1	1.141	20	0.54	0.63	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B1143-245	11 43 36.4	-24 30 53	11 43 36.37	-24 30 52.7	P	1b	Q	-0.3	-0.2	18.0			1.940	20	1.32	1.18	0.25
PKS B1143-287	11 43 54.8	-28 42 39	11 43 54.81	-28 42 38.2	P	1b	Q	1.0	-0.6	20.0			0.45	10	0.43	0.60	0.25
PKS B1144-379	11 44 30.9	-37 55 31	11 44 30.83	-37 55 31.0	N	1a	BL			18.0			1.048	1	1.03	0.90	0.25
PKS B1145-071	11 45 18.3	-07 08 01	11 45 18.30	-07 08 00.5	P	1b	Q	0.6	-1.5	18.5			1.342	31	1.09	1.21	0.25
PKS B1146-037	11 46 22.4	-03 47 30	11 46 22.38	-03 47 28.7	P	1b	Q	-0.5	-1.0	16.4			0.340	15	0.42	0.34	0.25
PKS B1147-192	11 47 59.3	-19 14 29	11 47 58.88	-19 14 08.2	P	2	Q	-0.3	0.0	19.4		22.4	2.489	83	0.28	0.27	0.25
PKS B1148-001	11 48 10.1	-00 07 13	11 48 10.13	-00 07 13.0	P	1b	Q	-0.2	-0.4	17.6			1.978	49	2.40	1.90	0.25
PKS B1148-171	11 48 30.4	-17 07 19	11 48 30.38	-17 07 18.4	P	1b	Q	-0.3	-0.5	19.0			1.751	33	0.60	0.50	0.25
PKS B1149-084	11 49 43.5	-08 24 23	11 49 43.83	-08 24 22.5	N	1b	Q			18.5			2.370	83	0.39	0.56	0.25
PKS B1149-480	11 49 07.5	-48 05 28	11 49 07.23	-48 05 24.0	T	3	G?	3.0	-0.2	23.8					0.25	0.24	0.25
PKS B1150-723	11 50 30.7	-72 22 43				1a	e			19.0					0.82	0.65	0.25
PKS B1156-094	11 56 39.1	-09 24 10	11 56 39.06	-09 24 09.8	P	2	Q*	-0.5	-0.1	22.0					0.75	0.66	0.25
PKS B1156-221	11 56 37.8	-22 11 55	11 56 37.76	-22 11 54.5	P	1b	Q	-0.2	-0.4	20.0			0.565	33	0.71	0.78	0.25
PKS B1157-215	11 57 18.3	-21 32 12	11 57 18.32	-21 32 11.3	P	1b	Q	-0.4	-0.3	18.5			0.927	30	0.49	0.66	0.25
PKS B1159-515	11 59 09.2	-51 33 53	11 59 09.36	-51 33 51.9	C	1a	Q			20.3					0.33	0.54	0.25
PKS B1200-051	12 00 00.4	-05 11 20	12 00 00.43	-05 11 20.2	P	1b	Q	-0.1	-0.4	18.0			0.381	33	0.50	0.46	0.25
PKS B1203+011	12 03 14.8	+01 10 24	12 03 14.82	+01 10 25.7	N	1a	Q			18.0			0.933	7	0.13	0.14	0.10
PKS B1205+011	12 05 59.8	+01 11 05	12 05 59.94	+01 11 03.6	P	3	G	0.4	0.3	>22.5		21.8			0.25	0.25	0.10
PKS B1205-008	12 05 07.8	-00 49 55	12 05 07.89	-00 49 54.8	P	1b	Q	-0.4	-0.5	18.5			1.002	15	0.22	0.20	0.10
PKS B1206-202	12 06 39.5	-20 16 09	12 06 39.99	-20 15 57.2	P	3	G	1.7	0.2	22.1	19.0	20.3	0.404	83	0.38	0.65	0.25
PKS B1206-238	12 06 27.7	-23 49 39	12 06 27.68	-23 49 38.9	P	1b	Q	0.1	-0.2	18.0			1.299	83	0.49	0.71	0.25
PKS B1206-399	12 06 59.4	-39 59 30				1a	Q			16.1			0.966	5	0.59	0.53	0.25
PKS B1207-319	12 07 04.8	-31 58 03	12 07 04.79	-31 58 11.5	V	3	Q*	1.0	2.3	24.1		23.7			0.32	0.28	0.20
PKS B1209-191	12 09 22.0	-19 09 32	12 09 22.89	-19 09 26.4	P	3	G	1.0	0.1	23.6		21.7			0.21	0.36	0.25 X
PKS B1210-097	12 10 49.1	-09 46 48	12 10 48.56	-09 46 44.3	P	3	BL	-1.1	0.8	21.5		21.7		83	0.27	0.28	0.25
PKS B1213-102	12 13 51.0	-10 16 48	12 13 49.83	-10 16 35.4	P	3	Q	-0.7	0.0	21.8		21.6	0.636	83	0.29	0.31	0.25
PKS B1213-172	12 13 11.7	-17 15 05	12 13 11.76	-17 15 6.0	N	1a	Ob								1.33	1.28	0.25
PKS B1215-002	12 15 24.8	-00 13 08	12 15 24.94	-00 13 06.7	P	1b	G	-0.4	0.2	18.5			0.417	4	0.33	0.28	0.10
PKS B1216-010	12 16 01.1	-01 03 14	12 16 01.07	-01 03 14.9	P	1b	Q	-0.2	-0.1	17.7			0.415	50	0.15	0.16	0.10
PKS B1217+023	12 17 38.3	+02 20 21	12 17 38.77	+02 20 20.5	N	1a	Q			16.5			0.240	51	0.51	0.44	0.10
PKS B1218-136	12 18 56.0	-13 37 29	12 18 55.90	-13 37 23.2	P	1b	G	0.6	-1.3	17.0					0.18	0.16	0.25 X
PKS B1224-443	12 24 45.3	-44 20 10	12 24 45.57	-44 19 56.9	T	2	BL	1.4	1.0	21.5	20.5	22.1		83	0.32	0.36	0.25
PKS B1226+023	12 26 33.2	+02 19 43	12 26 32.96	+02 19 40.0	N	1a	Q			12.8			0.158	52	40.90	36.70	0.25
PKS B1226-028	12 26 02.5	-02 48 06	12 26 02.75	-02 48 04.1	P	1b	Q	0.2	-0.4	19.0					0.18	0.16	0.25 X
PKS B1226-062	12 26 18.0	-06 15 02	12 26 17.54	-06 15 11.2	N	1a	Ob								0.24	0.22	0.25 X
PKS B1228-113	12 28 20.1	-11 22 36	12 28 20.04	-11 22 35.8	P	2	Q	-0.5	-0.8	22.0			3.528	20	0.55	0.46	0.25
PKS B1228-310	12 28 05.7	-31 04 39	12 28 06.03	-31 04 49.8	N	1a	Q			19.0			2.276	9	0.29	0.27	0.20
PKS B1229-439	12 29 59.6	-43 54 55	12 30 00.39	-43 55 00.6	A	3	G	0.4	-0.3	24.0		21.1			0.27	0.23	0.25
PKS B1230-101	12 30 37.4	-10 08 53	12 30 37.72	-10 08 45.8	P	2	Q	-0.2	-0.7	19.8			2.394	83	0.43	0.34	0.25
PKS B1237-101	12 37 07.3	-10 07 01	12 37 07.28	-10 07 00.4	P	1b	Q	-0.5	-0.5	18.0			0.753	2	1.35	1.13	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B1240-059	12 40 58.4	-05 57 02	12 40 59.61	-05 56 56.9	V	3	G	-0.1	-0.7	14.4	17.0	18.3	0.139	83	0.20	0.16	0.25 X
PKS B1240-394	12 40 50.1	-39 25 33	12 40 50.29	-39 25 27.0	S	2	Q	-0.2	-0.6	21.0			1.387	83	0.26	0.26	0.25
PKS B1241-399	12 41 45.0	-39 56 21	12 41 45.07	-39 56 21.6	S	2	Q	-2.4	-1.3	17.2			0.191	83	0.26	0.21	0.25
PKS B1243-072	12 43 28.8	-07 14 23	12 43 28.79	-07 14 23.3	P	1b	Q	-0.3	-0.8	18.0			1.286	10	0.79	1.11	0.25
PKS B1243-160	12 43 16.1	-16 00 18	12 43 16.24	-16 00 22.3	P	2	G?	0.6	-0.6	22.5					0.30	0.36	0.25
PKS B1244-255	12 44 06.7	-25 31 27	12 44 06.72	-25 31 26.5	P	1b	Q	0.3	-1.2	17.0			0.633	30	1.34	1.55	0.25
PKS B1245-062	12 45 47.4	-06 15 25	12 45 47.69	-06 15 48.6	P	2	Q	0.1	-0.8	19.5		21.3	0.762	83	0.41	0.33	0.25
PKS B1248-350	12 48 55.5	-35 02 13	12 48 55.06	-35 02 21.9	S	2	Q	1.9	0.4	21.2			0.410	83	0.37	0.32	0.25
PKS B1250-330	12 50 14.9	-33 03 42	12 50 14.90	-33 03 42.0	N	1c	Q	-1.0	-1.2	21.4			0.859	83	0.52	0.49	0.20
PKS B1251-407	12 51 12.8	-40 43 11	12 51 12.62	-40 43 14.7	V	3	Q	-0.5	0.1	23.7	19.3	22.9	4.464	83	0.25	0.22	0.25
PKS B1252-441	12 52 09.2	-44 08 39				1a	G			15.5					0.32	0.35	0.25
PKS B1253-055	12 53 35.8	-05 31 08	12 53 35.84	-05 31 07.8	P	1b	Q	-0.5	-0.9	17.8			0.536	53	12.00	13.00	0.25
PKS B1254+006	12 54 30.8	+00 40 46	12 54 29.74	+00 40 50.8	N	1a	Q			18.0			1.257	9	0.13	0.13	0.25 X
PKS B1255-316	12 55 15.2	-31 39 05	12 55 15.20	-31 39 03.5	N	1a	Q			18.5			1.924	6	1.49	1.68	0.20
PKS B1256-015	12 56 32.3	-01 34 46	12 56 32.35	-01 34 47.8	P	3	G	-0.9	-0.2	:22.5		23.4			0.25	0.20	0.25
PKS B1256-177	12 56 00.2	-17 43 42	12 55 59.21	-17 43 52.1	V	3	Q	-0.7	0.2	20.2		21.3	1.956	83	0.45	0.45	0.25
PKS B1256-220	12 56 13.9	-22 03 20	12 56 13.94	-22 03 20.2	P	1b	Q	0.0	-0.6	20.0			1.306	54	0.65	0.79	0.25
PKS B1256-229	12 56 27.6	-22 54 28	12 56 27.61	-22 54 27.9	P	1b	Q	-0.5	-0.5	18.0			1.365	20	0.50	0.54	0.25
PKS B1256-243	12 56 31.3	-24 19 55	12 56 31.27	-24 19 54.9	P	1b	Q	-0.4	-0.4	19.5			2.263	55	0.44	0.36	0.25
PKS B1258-321	12 58 16.2	-32 10 20	12 58 15.89	-32 10 19.3	N	1a	G			13.0			0.017	56	0.92	0.79	0.20
PKS B1259-312	12 59 41.3	-31 14 45	12 59 41.13	-31 14 36.7	V	3	G	-0.2	-2.7	>22.5	21.6	23.0			0.25	0.21	0.20
PKS B1300-105	13 00 37.0	-10 35 27	13 00 36.73	-10 35 11.2	P	3	BL	0.2	1.1	22.9	20.6	22.2		83	0.32	0.36	0.25
PKS B1302-034	13 02 08.7	-03 29 59	13 02 08.72	-03 29 58.4	P	1b	Q	-0.2	-1.1	19.4			1.250	7	0.60	0.54	0.25
PKS B1302-102	13 02 55.8	-10 17 16	13 02 55.85	-10 17 16.2	P	1b	Q	-0.2	-0.3	15.2			0.286	12	0.89	1.00	0.25
PKS B1302-208	13 02 18.5	-20 50 40	13 02 18.29	-20 50 38.5	P	2	Q*	-1.6	-0.4	21.8					0.49	0.43	0.25
PKS B1302-285	13 02 24.2	-28 34 40	13 02 24.66	-28 34 38.3	P	2	Q*	-0.7	-0.5	22.5		24.5			0.30	0.30	0.25
PKS B1306-241	13 06 01.3	-24 07 16	13 05 59.59	-24 06 59.8	N	1a	G			16.0			0.014	57	0.28	0.22	0.25
PKS B1307+010	13 07 54.9	+01 00 10	13 07 54.99	+01 00 7.1	N	1a	Q?			20.0					0.21	0.25	0.25 X
PKS B1313-333	13 13 20.0	-33 23 10	13 13 20.05	-33 23 09.5	P	1b	Q	0.0	-0.3	19.5			1.21	58	1.00	1.32	0.20
PKS B1316-120	13 16 34.0	-12 01 42	13 16 33.51	-12 01 47.1	P	1b	Q*	0.0	-0.5	18.0					0.32	0.41	0.25
PKS B1317+019	13 17 53.7	+01 56 20	13 17 53.72	+01 56 19.6	N	1a	Q			19.5			1.232	20	0.59	0.59	0.25
PKS B1318-263	13 18 28.9	-26 20 29	13 18 28.91	-26 20 28.2	P	2	Q	1.2	0.0	20.4			2.027	20	0.65	0.64	0.25
PKS B1319-093	13 19 59.8	-09 22 57	13 19 59.27	-09 21 57.8	P	1b	Q	-0.4	-0.4	18.0			1.864	83	0.37	0.53	0.25
PKS B1320-338	13 20 28.0	-33 51 28	13 20 27.79	-33 51 33.9	N	1a	Q			20.0			1.346	83	0.31	0.36	0.20
PKS B1321-105	13 21 48.4	-10 34 51	13 21 47.65	-10 33 46.6	N	1a	Q			18.5			0.872	83	0.34	0.64	0.25
PKS B1324-047	13 24 19.4	-04 45 27	13 24 18.76	-04 45 25.8	P	1b	Q	-0.2	-0.6	19.0			1.882	83	0.30	0.28	0.25
PKS B1325-222	13 25 54.6	-22 16 00	13 25 53.86	-22 16 01.8	P	2	G	-1.9	-0.8	20.6					0.25	0.21	0.25
PKS B1327-311	13 27 30.0	-31 07 31	13 27 29.97	-31 07 31.0	N	1a	Q			18.5			1.326	45	0.52	0.56	0.20
PKS B1328-034	13 28 53.6	-03 25 53	13 28 53.81	-03 25 48.4	P	1b	Q	-0.4	-0.2	19.0			1.352	7	0.35	0.29	0.10
PKS B1328-263	13 28 25.3	-26 23 57	13 28 25.19	-26 23 43.1	P	1b	Q	0.3	-0.4	17.4			0.883	22	0.34	0.37	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B1329-137	13 29 50.7	-13 46 47	13 29 50.75	-13 46 49.1	P	2	Q*	0.6	0.2	22.1		21.7			0.25	0.30	0.25
PKS B1330-143	13 30 44.0	-14 20 40	13 30 43.34	-14 20 59.0	N	1a	BL			19.0				83	0.31	0.42	0.25
PKS B1331-115	13 31 25.5	-11 34 52	13 31 24.97	-11 34 52.9	P	2	Q	-0.3	0.0	20.5		20.5	1.402	83	0.27	0.25	0.25
PKS B1333-049	13 33 21.2	-04 56 20	13 33 20.33	-04 56 23.6	P	3	BL	2.2	0.3	21.8	19.4	21.3		83	0.39	0.31	0.25
PKS B1333-082	13 33 30.5	-08 14 34	13 33 30.54	-08 14 34.1	P	1b	G	-0.8	-0.2	13.0			0.023	59	0.50	0.59	0.25
PKS B1334+008	13 34 58.0	+00 50 43	13 34 57.98	+00 50 43.1	N	1a	G			19.0			0.299	4	0.10	0.11	0.25 X
PKS B1334-127	13 34 59.8	-12 42 10	13 34 59.81	-12 42 09.6	P	1b	Q	-0.6	-0.9	18.5			0.541	6	2.01	2.18	0.25
PKS B1335+023	13 35 07.0	+02 22 09	13 35 06.97	+02 22 12.5	N	1a	Q			17.5			1.353	7	0.10	0.10	0.10
PKS B1336-000	13 36 59.7	-00 01 12	13 37 00.66	-00 01 17.4	N	1a	NCS			19.0			1.808	31	0.12	0.12	0.10 X
PKS B1336-237	13 36 15.7	-23 46 01	13 36 15.75	-23 46 01.2	P	1b	Q	0.0	-0.6	19.0			0.657	83	0.38	0.41	0.25
PKS B1336-260	13 36 32.5	-26 05 18	13 36 32.49	-26 05 18.2	P	1b	Q	0.1	-0.2	20.5			1.51	20	0.71	0.77	0.25
PKS B1337-013	13 37 30.1	-01 22 36	13 37 30.12	-01 22 35.9	P	1b	Q	0.2	0.0	19.1			1.619	7	0.35	0.37	0.10
PKS B1339-206	13 39 20.1	-20 36 28	13 39 20.21	-20 36 22.4	P	1b	Q	-0.1	-0.3	19.0			1.582	83	0.33	0.31	0.25
PKS B1339-287	13 39 25.6	-28 45 40	13 39 25.88	-28 45 34.7	P	1b	Q	0.0	-0.6	19.5			1.442	83	0.37	0.53	0.25
PKS B1339-299	13 39 30.5	-29 55 09	13 39 28.72	-29 55 09.0	N	1a	NCS								0.25	0.20	0.25 X
PKS B1346-113	13 46 51.3	-11 18 01	13 46 51.54	-11 18 01.1	P	1b	Q	0.0	-0.4	17.5			0.34	60	0.42	0.58	0.25
PKS B1346-139	13 46 34.0	-13 58 48	13 46 34.64	-13 58 23.6	P	2	G	1.5	-1.1	21.0		20.0	0.253	83	0.21	0.17	0.25 X
PKS B1348+007	13 48 31.1	+00 46 06	13 48 31.04	+00 46 08.7	V	3	Q	-0.9	0.3	22.7		22.9	2.084	4	0.21	0.17	0.10
PKS B1348-289	13 48 55.7	-28 57 29	13 48 55.86	-28 57 29.0	P	1b	Q	-0.1	-0.7	20.0			1.034	83	0.48	0.40	0.25
PKS B1349-145	13 49 10.8	-14 34 27	13 49 10.76	-14 34 27.2	N	1a	Ob								1.04	0.93	0.25
PKS B1349-439	13 49 52.5	-43 57 54	13 49 52.53	-43 57 54.0	C	1a	BL			:18.0					0.54	0.76	0.25
PKS B1351+021	13 51 18.8	+02 06 36	13 51 18.91	+02 06 38.1	N	1a	Q			19.0			1.606	7	0.33	0.26	0.10
PKS B1351-018	13 51 32.0	-01 51 20	13 51 32.04	-01 51 19.9	P	1b	Q	-1.0	-0.3	20.9			3.709	4	1.00	0.82	0.10
PKS B1351-237	13 51 44.5	-23 43 27	13 51 42.68	-23 43 06.0	P	3	G	0.0	-0.6	21.5		21.7			0.27	0.22	0.25
PKS B1352-104	13 52 06.8	-10 26 21	13 52 06.83	-10 26 20.6	P	1b	Q	-0.9	-0.3	17.5			0.332	12	0.79	0.98	0.25
PKS B1353-341	13 53 09.8	-34 06 31	13 53 09.84	-34 06 30.6	N	1a	G			18.5			0.223	9	0.64	0.67	0.20
PKS B1354-107	13 54 07.3	-10 47 05	13 54 06.85	-10 46 51.4	P	3	Q	1.0	0.2	19.2		19.9	3.006	83	0.26	0.27	0.25
PKS B1356+022	13 56 54.7	+02 14 26	13 56 54.60	+02 14 26.4	P	1b	Q	-0.2	0.0	18.3			1.329	7	0.75	0.68	0.25
PKS B1358-090	13 58 26.6	-09 02 08	13 58 26.19	-09 02 03.0	P	2	Q	-0.1	0.4	19.8		20.0	0.667	83	0.41	0.33	0.25
PKS B1358-298	13 58 41.3	-29 50 05	13 58 41.90	-29 50 09.0	P	2	Q	-0.2	0.3	19.7	18.7	20.6	0.689	83	0.32	0.28	0.25
PKS B1359-281	13 59 10.7	-28 08 00	13 59 10.60	-28 07 58.3	P	2	Q	-1.7	1.2	20.9		21.3	0.803	20	0.82	0.67	0.25
PKS B1401+000	14 01 38.2	+00 00 55	14 01 38.29	+00 00 56.3	P	1b	Q	-0.1	-0.4	19.0			1.221		0.42	0.47	0.25
PKS B1402-012	14 02 11.3	-01 16 02	14 02 11.30	-01 16 01.6	P	1b	Q	-0.2	-0.7	18.2			2.518	7	0.73	0.60	0.25
PKS B1402-144	14 02 51.1	-14 25 49	14 02 50.15	-14 25 59.5	P	1b	Q*	-0.7	-0.3	17.5					0.19	0.20	0.25 X
PKS B1403-085	14 03 21.7	-08 33 50	14 03 21.65	-08 33 49.3	P	1b	Q	-0.4	-0.4	18.5			1.763	33	0.71	0.58	0.25
PKS B1404-267	14 04 37.9	-26 46 52	14 04 38.28	-26 46 49.7	P	1b	G	-1.6	2.5	13.5			0.022	62	0.50	0.40	0.25
PKS B1404-342	14 04 57.1	-34 17 15	14 04 57.20	-34 17 14.2	S	2	Q	-0.4	-1.1	17.7			1.122	9	0.67	0.60	0.20
PKS B1405-287	14 05 56.3	-28 46 08	14 05 56.39	-28 46 12.0	P	1b	Q	0.2	-0.2	18.5			0.575	33	0.34	0.29	0.25
PKS B1406-076	14 06 17.9	-07 38 16	14 06 17.90	-07 38 15.8	P	1b	Q	-0.2	-0.2	20.0			1.494	45	0.96	1.05	0.25
PKS B1406-230	14 06 23.0	-23 01 37	14 06 23.09	-23 01 39.1	P	1b	G			17.5					0.44	0.35	0.25

 

Table A.1: continued.

	PKSCAT90 B1950		New radio position B1950					Offsets
Name	RA	Dec	RA	Dec		Ident		RA	Dec	B	Gunn-i	Gunn-z	z	zRef	S2.7	S5	$S_{\rm lim}$
PKS B1406-267	14 06 58.4	-26 43 28	14 06 58.43	-26 43 27.7	P	1b	Q			21.8			2.43	20	0.57	0.90	0.25
PKS B1407+022	14 07 32.2	+02 17 16	14 07 32.24	+02 17 14.9	P	1b	BL	-0.4	-0.8	18.7					0.39	0.35	0.25
PKS B1412-096	14 12 39.1	-09 41 53	14 12 40.68	-09 42 02.5	P	1b	Q	-0.8	-0.4	17.5			2.001	83	0.33	0.35	0.25
PKS B1412-368	14 12 24.8	-36 51 49	14 12 25.12	-36 51 49.5	A	3	G	-0.5	0.5	>22.5		23.8			0.39	0.56	0.25
PKS B1413-168	14 13 50.5	-16 51 25	14 13 49.25	-16 51 53.1	N	2	Q?	1.7	-0.2	20.0					0.26	0.22	0.25
PKS B1415-349	14 15 58.8	-34 55 56	14 15 58.71	-34 55 54.4	N	1a	Q			19.5			1.544	83	0.43	0.49	0.25
PKS B1418-064	14 18 29.1	-06 29 56	14 18 29.55	-06 30 14.8	P	1b	Q	-0.1	0.1	18.5			3.689	83	0.38	0.34	0.25
PKS B1422-250	14 22 29.3	-25 00 13	14 22 30.87	-24 59 35.9	P	2	Q	0.2	-0.2	19.6	18.5	20.5	1.884	83	0.31	0.25	0.25
PKS B1424-418	14 24 46.7	-41 52 54	14 24 46.72	-41 52 54.4	C	1a	Q			18.0			1.522	9	2.63	2.12	0.25
PKS B1427-448	14 27 53.0	-44 48 02	14 27 46.33	-44 47 44.5	A	2	BL	-1.3	0.0	19.9		20.7		83	0.43	0.34	0.25
PKS B1427-742	14 27 22.5	-74 14 25				1a	G			15.5					0.37	0.34	0.25
PKS B1430-155	14 30 36.1	-15 35 35	14 30 36.12	-15 35 34.7	P	3	Q	-0.5	0.3	22.8	21.6	22.8	1.583	83	0.55	0.66	0.25
PKS B1430-178	14 30 10.7	-17 48 24	14 30 10.65	-17 48 24.2	P	1b	Q	-0.6	-0.4	19.0			2.331	33	1.00	0.93	0.25
PKS B1434-325	14 34 14.0	-32 31 44	14 34 13.85	-32 31 40.8	V	1a	NCS	-1.5	-3.7		23.5				0.22	0.20	0.20 X
PKS B1435-218	14 35 18.7	-21 51 58	14 35 18.66	-21 51 57.7	P	1b	Q	0.1	0.2	17.9			1.194	30	0.79	0.81	0.25
PKS B1435-311	14 35 11.4	-31 09 29	14 35 11.35	-31 09 30.3	N	1a	Q			20.0			1.287	58	0.30	0.25	0.20
PKS B1437-153	14 37 11.2	-15 18 59	14 37 11.34	-15 18 58.7	P	1b	BL	-0.3	-0.4	19.0				82	0.72	0.64	0.25
PKS B1438-328	14 38 19.3	-32 50 39	14 38 18.17	-32 50 37.9	S	3	Q	1.5	1.0	19.5		19.6	1.479	83	0.30	0.29	0.20
PKS B1438-347	14 38 20.3	-34 43 57	14 38 20.39	-34 43 56.9	N	1a	Q			18.0			1.159	58	0.50	0.45	0.20
PKS B1440-389	14 40 45.7	-38 55 33	14 40 48.15	-38 55 58.2	T	2	G	-1.2	+1.0	17.0					0.20	0.19	0.25 X
PKS B1443-032	14 43 06.1	-03 17 21	14 43 06.08	-03 17 23.8	P	2	Q*	-0.2	0.1	20.8					0.21	0.18	0.25 X
PKS B1446-005	14 46 42.3	-00 32 36	14 46 42.31	-00 32 54.4	P	2	G?	0.1	-0.4	22.7		22.7			0.40	0.40	0.25
PKS B1449-012	14 49 12.6	-01 15 18	14 49 12.57	-01 15 17.8	P	1b	Q	-0.2	-0.2	18.0			1.319	7	0.46	0.42	0.25
PKS B1451-248	14 51 51.5	-24 52 59	14 51 51.56	-24 53 03.3	P	2	Q	-0.9	-2.4	21.7			1.216	83	0.33	0.32	0.25
PKS B1451-375	14 51 18.3	-37 35 22	14 51 18.47	-37 35 24.2	N	1a	Q			16.4			0.321	12	1.51	1.84	0.25
PKS B1451-400	14 51 20.6	-40 00 22	14 51 20.58	-40 00 21.1	C	1c	Q	0.3	-1.2	18.5			:1.81		0.71	0.61	0.25
PKS B1452-168	14 52 15.3	-16 48 01	14 52 15.08	-16 48 05.8	P	2	Q*	-2.2	-0.5	21.1		21.7			0.31	0.28	0.25
PKS B1452-367	14 52 01.1	-36 43 47	14 52 01.60	-36 42 59.5	V	3	G	0.4	0.6	17.2