1996AuJPh..49..977S A VLA Survey of Rich Clusters of Galaxies III. The Weaker Sources: Maps and Identifications O.B. Slee (1), A.L. Roy (1,2) and H. Andernach (3) 1) Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, N.S.W. 2121. 2) School of Physics, University of Sydney, N.S.W. 2006, Australia. 3) INSA, ESA-IUE Observatory, Apdo. 50727, E-28080 Madrid, Spain. Abstract We present radio and optical parameters for 737 weak sources in 60 Abell cluster fields observed with the Very Large Array (VLA) using scaled arrays at 1.5 and 4.9 GHz. The measurements extend to a lower 1.5 GHz limit of 1.0 mJy and comprise a complete sample with 1.5-GHz flux density 2.5 S1.5 < 20 mJy The combined sky area within the half-power circle on the maps is 3.5 x 10-3 sr, and the cluster fields are distributed over 24 h of right ascension and between declinations +35deg and -30deg. Contour maps of the extended sources at 1.5 GHz are presented and source parameters such as position, angular size and spectral index are tabulated. We also derive the emitted power and linear size for those sources with published redshifts. We try to identify the radio sources with optical images on the Palomar and SERC survey plates and give their accurate optical positions, morphologies and apparent magnitudes. 1. Introduction >From 1982 to 1985 Slee et al. (1989; hereafter SPS89, Paper I) used scaled arrays at the VLA to survey 60 fields near rich clusters of galaxies. The survey fields were centred on the steep-spectrum sources with spectral index alpha= -0.90 (defined by S ~ freq^alpha) discovered in earlier low-resolution surveys by Slee and Siegman (1983) and Slee et al. (1983). Fifty-three of the fields were surveyed with scaled arrays at 1.5 and 4.9 GHz ( with the C- and D-arrays respectively), using identical phase and delay centres at the two frequencies. Five fields (A 13, A 85-2, A 2354, A2399 and A 2575) were mapped only at 1.5 GHz. The half-power-beam width (HPBW) at both frequencies was ~ 14 arcsec in right ascension but was up to a factor of two larger in declination at the southern declination limit of -30deg. The VLA observations, data reduction, whole-field maps and general source statistics were described in Paper I. The results (maps, polarisation and identifications) for the stronger sources are given in Slee et al. (1994; hereafter SRS94, Paper II). This paper, the third of the series, provides similar radio and optical parameters for the weaker sources with 1.5-GHz flux densities 1< S1.5 < 20 mJy. The only other major survey of Abell clusters with similar angular resolution is that described in the three publications of Zhao et al. (1989), Owen at al. (1992) and Owen et al. (1993), who made their observations only at 1.5 GHz. Their published maps and measurements were confined to the strongest sources near the cluster centres and only a few clusters are common to both surveys. Therefore, it is more appropriate to compare their results with those on the stronger sources in our Paper II; this will be done in a future publication. The weak-source measurements are presented in Section 2, including contour maps of the more resolved sources. The optical identifications for these sources are discussed in Section 3 and a conclusion is given in Section 4. Throughout this paper computations of emitted power and linear source dimensions make use of H_0=75 km s-1 Mpc-1 and q0 =0.5. 2. Results The observations and reductions have been adequately treated in SPS89 (Paper I). The data and maps presented here come from processing further the results in Paper I and are similar to the detailed source parameters given in Paper II. The results presented here include: i elliptical Gaussian brightness distributions fitted to the sources; ii contour mapping for well-resolved sources; iii determination of spectral indices; iv computation of power output and linear size for sources with redshifts. v optical identifications. In contrast with the stronger sources in Paper II, we have no polarisation data for this sample, nor do we have any high-resolution interferometer measurements of their core components. Table 1 provides a list of the cluster fields that we observed. The more useful optical and X-ray parameters of the clusters are listed, and the positions of the VLA field centres with respect to the cluster centres are given. The rms fluctuation level over a large, relatively clear area of each VLA map is shown in columns 7 and 8; a blank in either of these columns means that no map is available at that frequency. The column headings are explained in a footnote to the table. The values of Lx followed by 'R' in column 17 are ROSAT logarithmic luminosities (Ebeling 1993) that have been transformed to the EINSTEIN luminosity scale. This was done by finding the average difference between EINSTEIN and ROSAT logarithmic luminosities for the 11 clusters in Table 1 that were observed by both telescopes. The average difference ROSAT - EINSTEIN = +0.45 in Log Lx was then subtracted from the ROSAT logarithmic luminosities for those clusters with no EINSTEIN observations. This gives a more complete, self-consistent set of X-ray luminosities for subsequent analysis. ------------------------------------------------------------------------ Table 1. * The RA is from Abell et al. (1989). The incorrect RA of Abell (1958) was used for the radio field centre - hence the large offset. R_clu is the cluster radius from the Palomar Sky Survey (Struble & Rood 1987 =1987ApJS...63..555S) except that the Abell radius (approximately 1.72/z arcmin) is quoted for A3528, Zw1518.8, A4038. # Data from Abell et al. (1989) × Data from "Catalogue of Galaxies and of Clusters of Galaxies" (Zwicky et al. 1961) and Slee & Quinn (1979) =1979PASAu...3..332S R ROSAT measurement converted to the Einstein luminosity scale (see text Section 2). Column headings : 1. The cluster of galaxies nearest the observed radio field. The name of the Zwicky cluster Zw1518.8+0747 was shortened here to "Z1518.8" 2,3. The centroid position (B1950) of the optical cluster, mainly from Abell (1958), but data for three clusters come from Abell et al. (1989) and Zwicky et al. (1961). 4,5,6. The angular distance (in arcmin) and position angle (in degs. positive from north through east) of the centre of the radio field with respect to the optical centroid in columns 2 & 3. 7,8. The rms levels over a large clear area of the maps at 1.5 and 4.9 GHz, both in microJansky per beam. 9,10. The richness and distance class of the cluster, mainly from Abell (1958), but for three clusters we obtain the data from Abell et al. (1989) or Slee & Quinn (1979). 11. The magnitude of the tenth brightest galaxy in the cluster, mainly from Abell (1958), but in three cases cases from Abell et al. (1989) or Zwicky et al. (1961). 12. The Bautz-Morgan classification of the cluster, mainly from Abell et al. (1989), but for Zw1518.8+0747 from Slee & Quinn (1979). 13. The angular radius of the cluster in arcmin as quoted by Struble & Rood (1987). 14. The linear radius of the cluster in Mpc. 15,16. The mean redshift of the cluster and a corresponding reference. 17. The EINSTEIN X-ray luminosity in the energy range 0.5-4.5 keV and out to a radius of 1Mpc from the cluster centre. The data (adjusted for H_o=75 km/s/Mpc) are from Jones & Forman (1995, unpubl.). 18. The ROSAT X-ray luminosity from Ebeling (1993, PhD MPE Garching). Redshift references : 1 Struble & Rood 1991 =1991ApJS...77..363S 2 From the m10-z relation =1994AuJPh..47..145S (Slee, Roy & Savage 1994; SRS94, Paper II) 3 Melnick & Quintana 1981 =1981A&AS...44...87M 4 Abell et al. 1989 =1989ApJS...70....1A 5 Beers et al. 1991 =1991AJ....102.1581B 6 Slee & Reynolds 1984 =1984PASAu...5..516S 7 Reynolds 1986 =1986USydn.T00J....R 8 Postman et al. 1992 =1992ApJ...384..404P Table 1. Properties of the observed clusters Map-rms Cluster RADec_B1950 Radio Offset PA muJy/beam R D m10 BMclass R_clu Redshift Log Lx (erg/s) Field nts h m d ' ' R/Rc deg 1.5GHz 4.9GHz R ' Mpc z Refz Einstein ROSAT (1) (2) (3) (4) (5) (6) (7) (8)(9)(10)(11) (12) (13) (14) (15) (16) (17) (18) ----+----1----+----2----+----3----+----4----+----5----+----6----+----7----+----8----+----9----+----0----+ A0013 00 11.1 -19 47 2.5 0.15 -81.1 58 2 5 16.6 III 17 1.59 0.0945 6 43.97 R 44.42 A0076 00 37.2 +06 30 31.8 0.93 16.3 105 42 0 3 15.0 II-III 34 1.53 0.0416 1 A0085-1 00 39.1 -09 37 30.6 0.90 -157.3 97 44 1 4 15.7 I 34 2.00 0.0556 1 A0085-2 00 39.1 -09 37 2.1 0.06 -127.1 30 1 4 15.7 I 34 2.00 0.0556 1 44.60 45.07 A0086 00 40.2 -22 04 11.4 0.46 -145.2 71 47 0 4 15.9 II-III 25 1.64 0.0627 1 42.92 A0115 00 53.3 +26 03 5.6 0.37 -21.3 288 43 3 6 17.3 III 15 2.51 0.1971 1 44.51 A0133 01 00.3 -22 09 1.2 0.04 -64.1 78 33 1 5 15.9 I 27 1.61 0.0566 1 44.11 A0154-1 01 08.3 +17 24 27.0 0.48 65.5 100 45 1 3 15.6 II 56 3.73 0.0638 1 A0154-2 01 08.3 +17 24 18.6 0.33 43.9 198 64 1 3 15.6 II 56 3.73 0.0638 1 A0196 01 24.5 +22 57 1.5 0.11 -37.1 159 41 1 6 17.5 III 14 1.97 0.156 2 A0240 01 39.3 +07 22 15.7 0.60 -64.3 68 38 0 3 15.6 II-III 26 1.68 0.0618 1 A0278 01 54.4 +31 59 1.2 0.04 149.2 130 33 0 3 15.6 III 27 2.42 0.0894 8 43.66 A0357 02 26.7 +13 01 8.0 0.30 -117.3 145 41 0 5 16.8 27 2.88 0.110 2 A0362 02 29.1 -05 05 1.8 0.16 145.8 79 36 1 6 17.7 II-III 11 1.66 0.172 2 A0407 02 58.6 +35 38 2.0 0.06 85.3 141 42 0 2 14.7 II 34 1.69 0.0463 1 43.34 43.67 A0416 03 04.9 -16 54 3.7 0.37 56.6 93 60 0 6 17.7 I-II 10 1.51 0.172 2 A0474 * 04 09.6 -16 49 58.7 6.52 -87.4 117 37 0 5 17.1 II: 9 1.08 0.128 2 A0496 04 31.3 -13 21 0.4 0.09 141.0 166 42 1 3 15.3 I: 45 1.62 0.0327 1 44.16 44.55 A0514 04 45.7 -20 31 11.0 0.32 126.3 110 33 1 4 15.2 II-III 34 2.54 0.0728 7 43.65 A0519 04 51.2 +00 36 1.1 0.05 119.5 75 33 0 5 17.0 23 2.67 0.122 2 A0531 04 58.8 -03 37 1.8 0.10 45.3 60 41 1 5 17.0 III 18 2.09 0.122 2 A0658 08 21.0 +15 50 6.8 0.49 150.4 78 30 1 5 17.0 III 14 1.62 0.122 2 A0912 09 58.6 +00 08 10.4 0.42 6.9 292 38 0 4 15.9 25 1.81 0.070 2 A1142 10 58.3 +10 49 20.5 0.60 100.5 177 53 0 3 15.4 II-III: 34 1.31 0.0353 1 A1171 11 04.9 +03 13 11.6 0.41 -146. 86 36 0 4 16.2 28 2.13 0.0741 1 A1189 11 08.5 +01 24 1.1 0.04 0.0 135 45 0 5 17.0 25 2.90 0.122 2 A1238 11 20.4 +01 22 1.6 0.11 -38.7 102 37 1 4 16.0 III 15 1.14 0.074 2 A1273 11 26.8 -06 46 1.8 0.16 -105.5 195 54 1 6 17.6 III 11 1.61 0.164 2 A1620 12 47.2 -01 19 4.7 0.21 65.2 128 43 0 5 17.2 III 22 2.75 0.134 2 A1631 12 50.2 -15 10 5.9 0.21 7.1 54 29 0 3 15.4 I 28 1.40 0.0465 1 43.28 43.84 A3528 # 12 51.6 -28 45 13.4 0.36 156.1 53 1 4 16.3 II 37 2.00 0.0506 3 A1689 13 09.0 -01 06 2.0 0.18 -61.5 67 33 4 6 17.6 II-III: 11 1.74 0.1832 1 44.98 45.47 A1772 13 39.4 -10 50 1.9 0.15 156.6 59 35 1 5 17.0 II-III 13 1.51 0.122 2 A1775 13 39.6 +26 37 1.2 0.04 -47.6 55 35 2 4 15.7 I 28 2.07 0.0717 1 44.01 44.48 A1791 13 46.0 -25 12 1.7 0.06 100.3 111 38 1 6 17.0 I 26 3.01 0.122 2 A1913 14 24.5 +16 54 3.6 0.16 46.8 56 40 1 4 16.0 III 22 1.23 0.0528 1 43.39 A2009 14 58.0 +21 34 1.3 0.12 53.8 29 29 1 5 17.2 I-II: 11 1.52 0.1530 1 44.63 45.09 A2029 15 08.5 +05 57 1.5 0.07 -152.8 190 32 2 4 16.0 I 22 1.73 0.0768 1 44.85 45.31 A2052 15 14.3 +07 11 1.6 0.07 9.0 764 260 0 3 15.0 I-II 22 0.84 0.0348 1 43.95 44.39 Z1518.8 x 15 18.8 +07 47 10.1 0.24 59.5 29 31 4 2 15.2 II 42 2.00 0.0440 5 44.02 A2082 15 28.2 +03 37 12.4 0.48 51.8 79 39 0 5 17.0 26 3.01 0.122 2 A2091 15 31.9 +10 24 2.9 0.32 9.8 38 58 1 6 17.5 III 9 1.27 0.156 2 A2094 15 34.0 -01 52 2.2 0.20 34.0 58 42 1 5 16.7 III 11 1.13 0.105 2 A2103 15 37.3 -02 00 12.6 0.48 -96.5 93 44 0 5 17.1 26 3.13 0.128 2 A2108 15 37.8 +18 03 17.3 1.08 57.0 68 39 0 4 15.7 III 16 1.47 0.0919 1 A2151 16 03.0 +17 53 35.6 1.27 42.9 92 37 2 1 13.8 III 28 1.12 0.0368 1 A2249 17 07.9 +34 31 2.4 0.09 160.0 71 38 0 3 15.4 III 26 2.13 0.0809 1 44.21 R 44.66 A2354 21 33.1 -15 08 2.1 0.19 -110.4 54 2 5 17.1 III 11 1.33 0.128 2 A2396 21 53.2 +12 15 2.7 0.30 26.5 110 136 1 6 17.5 9 1.27 0.156 2 A2399 21 54.9 -08 02 31.3 1.20 -161.1 99 1 3 15.6 III 26 1.62 0.0594 7 A2443 22 23.7 +17 05 1.5 0.13 -14.0 83 47 2 5 16.5 II 12 1.13 0.095 2 43.96 R 44.41 A2456 22 32.4 -15 33 1.1 0.14 166.9 54 52 1 5 17.2 I 8 1.00 0.134 2 A2457 22 33.2 +01 13 11.8 0.45 139.0 56 48 1 4 16.0 I-II: 26 1.97 0.074 2 A2575 23 17.1 -22 19 2.1 0.30 129.1 166 0 6 17.9 III 7 1.14 0.190 2 A2593 23 22.0 +14 22 0.5 0.02 78.3 70 98 0 3 15.1 II 28 1.27 0.0421 1 43.63 44.02 A2622 23 32.4 +27 09 3.4 0.17 138.5 100 56 0 4 15.9 II-III: 20 1.45 0.070 2 43.56 R 44.01 A2626 23 34.0 +20 53 1.0 0.04 167.7 74 25 0 3 15.2 I-II 25 1.51 0.0573 1 43.76 44.30 A2657 23 42.3 +08 52 27.3 1.05 125.4 68 70 1 3 14.9 III 26 1.17 0.0414 1 A4038 # 23 45.1 -28 25 0.5 0.01 -2.5 68 43 2 2 14.2 III 64 2.00 0.0283 4 A2670 23 51.6 -10 41 20.0 0.91 -128.1 78 60 3 4 15.7 I-II 22 1.71 0.0761 1 ----------------------------------------------------------------------------- The optical angular radius of the cluster, Rc, is not the Abell radius that is usually quoted in cluster publications, but is the value obtained from galaxy counts on the PSS plate by Struble and Rood (1987). The Abell radius assumes that all clusters have a linear radius of 2 Mpc (H0 = 75 km/s/Mpc, q0=0.5), but we prefer to preserve the differences between clusters by using their measured angular radii. For comparison with the Abell radius, the mean linear radius derived from Rc in Table 1 is 1.79 Mpc with a standard deviation of 0.64 Mpc. (2a) Radio Parameters of the Sample Table 2 contains the basic radio measurements of the detected sources, excluding the radio positions, which are given in Table 5. Sources in this paper include: i) all sources listed in Paper I with S1.5 < 20 mJy. A few of them (e.g. A13_6a/b/c) were also in Paper II because of a special interest in them; ii) a number of weak sources that had been accidentally omitted from Paper II; iii) a significant number of sources with S1.5 > 20 mJy (usually located near the field edges), which had been deliberately omitted from Paper II. We omitted a few of the weak sources listed in Paper I because subsequent analysis showed that they were probably spurious. To avoid later confusion, the additional sources are inserted in the Table at the correct right ascension but are given an extra lower case Roman numeral. For example, the source A13_13 in Table 2 of Paper I is now A13_13i, while an added source of slightly later RA, called A13_13ii, has been inserted in Table 2 of this paper. The column headings are explained in a footnote to the table. On the basis of the statistical analysis of Paper I, only a few of the present sources are expected to be cluster members, i.e. for cluster membership, the integrated 1.5-GHz flux density should be >=20 mJy and R/R_c<=0.28 ( see explanation of R_c in Section 1) . Many sources are close to the cluster centres in angular spacing, but only those that can be optically identified with galaxies with published redshifts, agreeing with the cluster redshifts, can be accepted as cluster members. Accordingly, there are few computations of emitted power and linear size in Table 2. The angular size parameters in columns 8, 9 & 10 of Table 2 were found by fitting a single Gaussian ellipse to the 1.5-GHz brightness distribution, making allowance in the deconvolution for the beam width and bandwidth smearing. A base level was subtracted during the fitting procedure. In most cases the fitted position (given in Table 5) is close to that of the centroid of the distribution, but in some well-resolved doubles this position is that of the peak of the dominant component. In these cases we have omitted the angular diameter but retained the position as a reference point for the optical identifications in Table 5. The deconvolution of the fitted ellipse for the beam shape and bandwidth smearing did not converge for many of the weaker sources. In these sources ( indicated by blanks in the Gaussian-fitted parameters in Table 2), the fitting errors can be so large that the parameters of the derived ellipse may not be consistent with the beam shape and smearing magnitude. The integrated flux densities given in columns 5 & 6 in Table 2 were not obtained from the Gaussian fitting but from the AIPS task IMEAN, which sums the pixel amplitudes in a small box placed around the source image. This method ensures a more accurate result when the source shape departs markedly from an elliptical Gaussian. The spectral index in column 7 of Table 2 was preferentially computed from our 1.5- and 4.9- GHz measurements of flux density with scaled arrays. If we did not have a 4.9-GHz flux density (because of the smaller primary beam), we combined our 1.5-GHz flux density with other measurements from the references in column 11. The tabulations of 1.5-GHz spectral power density and linear size in columns 12 and 13, use the few published redshifts of the brighter galaxy identifications. Most of these redshift references are identified in the NASA/IPAC Extragalactic Database(#) (NED) or the compilation of Andernach et al. (1995), but a few more redshifts were obtained from an independent scan of the literature. (2b) Components of Double Sources The detailed parameters of the doubles included in Table 2 are set out in Table 3. The column headings are explained in a footnote to the table. Component 'a' of a double is that with the higher 1.5-GHz flux density. Our angular resolution (~ 14 arcsec FWHP) is too low to refine the morphological classification. As for the fitting of the single ellipses described in Section 2a, the Gaussian fits to the components often had errors large enough to prevent the convergence of the deconvolution for beam shape and bandwidth smearing. Unlike the stronger sources in Paper II, far fewer of the sources identified with optical galaxies (see Table 5) are double sources; only 18 of the 174 galaxy identifications (10%) have definite double structure. For the star-like identifications, 9 out of a total of 61 (15%) are doubles. The larger fraction of doubles 35/62 (56%) remains unidentified. A plausible explanation of this difference is that the weaker sources in this sample are correspondingly more distant so that the angular scale of their lobe structure can not now be resolved. Alternatively, these are intrinsically weak radio sources and may have correspondingly small linear dimensions (see the radio power - linear size relationship for the stronger sources shown in Paper I). (2c) Components of Triple and Quadruple Sources Table 4 gives the parameters of the 6 triple and quadruple sources; one of these (A1631_a/b/c/d) has a total flux density S1.5=32.7 mJy and was accidentally omitted from Paper II. Only two of the six sources can be identified with galaxies (see Table 5). Neither galaxy has a published redshift, so we are unable to derive an emitted power or linear size. (2d) Contour Maps The contour maps in Fig. 1 have been assigned numbers, which also appear in Tables 2, 3 and 4 for the relevant sources. The maps have been corrected for primary beam attenuation but not for image distortion caused by bandwidth smearing in the outer regions of the radio fields. The map numbers accompanied by daggers in Tables 2 and 3 are those for which the source centroid position was >=7.0 arcmin from the delay and phase centre, so that the smearing was >=7 arcsec in the radial direction. The resulting image distortion depends upon the true angular dimensions of the source and on the position angle of the major axis of the restoring beam with respect to the radial direction from the map centre. Naturally, sources with angular dimensions appreciably greater than the smeared beam will not be much distorted. The parameters of the fitted Gaussians in Tables 2 and 3 have been corrected for the smearing. Unlike Paper II, very few of these sources could be mapped at 4.9 GHz so that Fig. 1 contains only 1.5-GHz maps. The radio positions (mainly centroids) are depicted in Fig. 1 as large, open, 7-pointed stars on the maps, while the smaller, filled, 13-pointed stars show the positions of optical objects within the radio contours. The radio and optical positions are listed in Table 5, together with the morphologies of the optical objects. (2e) Errors in the Parameters of Table 2 Errors in the flux density, spectral index and the Gaussian-fitted parameters result from a number of causes, the effects of which we estimate here. Flux density measurements are affected by : i) A systematic multiplicative error in the flux density of our primary flux calibrator (3C 48). Baars et al. (1977) give this as < 3-4 percent. We adopt an error of 3 percent. ii) Flux bootstrapping from the primary to the secondary calibrators contributes a random multiplicative error of ~ 4 percent. iii) Pointing errors of 10 arcsec rms can generate a random multiplicative error of up to ~ 1 percent for sources out near the half-power points in the primary beam. (iv) Deconvolution in the mapping process can contribute a random multiplicative error of ~ 3 percent. (v) Error from map noise and side lobes was estimated using the AIPS task IMEAN with a number of enclosing boxes having various areas and centre-offsets from the source. The resulting 1s random additive error was ~ 2 times the map rms (given in Table 1). The effective map noise increases with distance from the map centre (primary beam attenuation), so the errors calculated below should be increased to account for this effect. In deriving errors in parameters such as spectral index and emitted radio power from the flux densities in this paper, one adds in quadrature the errors from (i) to (iv) to obtain a total multiplicative error of 6 percent, to which one adds in quadrature the random additive error in (v). As an example, a source with S1.5 =9.0 mJy, S4.9 =3.0 mJy from maps with rms = 78 mJy/beam has a spectral index alpha =-0.93+/-0.12. The errors in the Gaussian-fitted parameters were found from a statistical analysis of fit- errors from 83 sources drawn from 1.5 GHz maps having a wide range of map rms. First, simple power-law regressions were made between fit-error and the several parameters that could possibly influence the error. We found that errors in the major and minor axes depended mainly on flux density/rms and ellipse area. The error in the position angle of the major axis depended on flux density/rms and axial ratio. Secondly, multiple regressions were then made to obtain the following best-fit, power-law equations : D_Maj = 0.36 (S/N)^-0.52 (Maj*Min)^+0.56 (1) D_Min = 5.08 (S/N)^-0.56 (Maj*Min)^+0.12 (2) D_PA = 117.2 (S/N)^-0.61 (AR)^-1.07 (3) where: D_Maj = error (arcsec) in the major axis (Maj) D_Min = error (arcsec) in the minor axis (Min) D_PA = error (degrees) in the position angle AR = axial ratio of the fitted ellipse (Maj/Min) S/N = flux density/rms As an example, we compute the 1s errors in the Gaussian-fitted parameters for a source with S = 5.0 mJy from a map with rms = 78 mJy/beam and having Maj*Min = 20 * 10 arcsec2. Substituting in equations (i) to (iii) we find : D_Maj = 0.80 arcsec, D_Min. = 0.93 arcsec, D_PA = 4.4 deg 3. Optical Identifications We examined the Palomar and SERC sky survey plates for optical counterparts to the sources in Table 2. The optical fields surrounding ~ 95% of the sources had been checked on the plates in connection with the preparation of Papers I and II, and Polaroid copies had been made if any optical object appeared within ~ 20 arcsec of the radio position. The remaining 5% of the sources were checked for optical counterparts on the COSMOS (Drinkwater et al. 1995) or APM (Irwin et al. 1994) digital versions of the surveys. We utilized both the catalogues and digital images on CD-ROM. A detailed account of our optical position measurements and magnitude estimates is given in Paper II. An important difference in our treatment of these results is that the coordinates of optical objects within 20 arcsec of the radio position were obtained from the digitised surveys. We believe that these yield about the same accuracy ( ~1 arcsec ) in either coordinate as we obtained with the Bolton machine for the identifications in Paper II. One advantage of the digitised SERC survey lay in our ability to make use of the SERC plates for radio sources with declinations as far north as +2=B0 (copies of the SERC Equatorial Survey were not available in Sydney). In 95% of the sources we were able to check from Polaroid prints that the digital parameters gave a true description of the optical morphology and whether the digital position was affected by image blends; for those fields in the SERC Equatorial Survey, we checked the images on CD-ROM. If blending did occur, we estimated positions by offsetting from well-positioned sources on the Polaroids, whose scale of 3.4 arcsec/mm was accurately known. The morphologies of faint objects are difficult to assess, both from the Polaroids and the digital surveys. It is very difficult to distinguish between galaxies and stars when the images are near the plate limit and so our classifications in such cases are subjective and should be treated with appropriate caution. Table 5 presents the radio source positions and the parameters of all optical objects detected on the sky survey plates within ~ 20 arcsec of the radio position. The column headings are explained at the foot of the table. The magnitudes of the objects listed in Table 5 were estimated in the same way as used in Paper II, supplemented by the digital estimates from COSMOS and APM. Our primary magnitude estimates are based on visual estimates from the Polaroids, using a 'fly-spanker' constructed for Paper II. In the southern section of our radio survey, we sometimes had Polaroids from both the SERC and Palomar I plates, enabling us to make independent brightness estimates of the same object. We estimate that the 'fly-spanker' estimates are accurate to about 0.5 mag, based on our tests outlined in Paper II. In summary, we think the radio and optical positions in Table 5 are accurate to about 1 arcsec and the magnitude estimates to about 0.5 mag. For each radio source Table 5 lists between zero (Blank Field) and seven optical candidates. We tried in Paper II to outline detailed identification criteria, but in Paper III we accepted any optical object within 10 arcsec of an unresolved radio source ( i. e. < 10 arcsec in major axis) as a possible identification. In the case of some of the more extended sources such as those shown in Fig. 1, we accepted optical objects further from the radio position as possible identifications. These likely identifications are printed in bold type. From past experience, galaxies rather than star-like images are much more likely to be associated with radio sources, but the low flux-density limit of the present survey means that it is possible to detect more true stellar emission than was likely in the stronger sources of Paper II. In addition, the lower flux-density limit of the present list may enable us to detect the so-called radio-quiet QSOs, so that coincidences with star-like images may be more frequent; one could only distinguish between stars and QSOs from their optical spectra. Morphologies for 95% of the optical objects in Table 5 were estimated from the polaroid copies, the remaining 5 per cent being digital estimates from COSMOS or APM. We used the following criteria for the Polaroid estimates: i) galaxies which were visibly extended, being surrounded by a diffuse structureless halo with an axial ratio less than ~2, were classified as elliptical (E); ii) galaxies satisfying the above definition but which were several times larger than all neighbouring galaxies were classified as 'cD' if near the cluster centre, or 'D' if well away from the cluster centre; iii) images showing two barely resolved ellipticals were classed as 'DB'. iv) a galaxy which satisfied the definition of an elliptical, except that the axial ratio was greater than ~ 2, was classified as 'S0'; v) a galaxy with considerable structure in the halo was classified as a spiral (Sp). vi) an image that was diffuse but too faint to assign to the above galaxy classes was called 'G'; vii) An image with a sharp circular boundary and sometimes showing diffraction spikes was classified as stellar (St). Some of these could, of course, be very compact ellipticals or QSOs. It should be noted that very faint images are difficult to assign to the G or St categories and often the choice is rather arbitrary. 4. Conclusion We have listed the parameters of 737 sources detected in 60 VLA fields, which were located near 58 Abell clusters; 715 of the sources have flux densities < 20 mJy at 1.5 GHz. The measurements in this paper (Paper III) and in Paper II constitute a large database from which we can assemble a complete flux limited sample of radio sources in or near rich clusters of galaxies. In a forthcoming paper, we will use such a sample to explore the complex relationships between the radio, optical and X-ray measurements. We thank Dr. G.S. Tsarevsky for his help with the literature search. The referee's thorough and competent reading of the manuscript has resulted in significant improvements to the paper. 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Zwicky, F., Herzog, E., and Wild, P. 1961, Catalogue of Galaxies and Clusters of Galaxies, V. 1, (California Institute of Technology). * The VLA is operated by the National Radio Astronomy Observatory for Associated Universities Inc., by co-operative agreement with the National Science Foundation. # The NASA/IPAC Extragalactic Database is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. ////////////////////////////////////////////////////////////////////// 1994AuJPh..47..145Slee, Roy, Savage: VLA Survey of Rich Clusters of Galaxies II. The stronger sources 1996AuJPh..49..977Slee, Roy, Andernach: VLA Survey of Rich Clusters of Galaxies III. The weaker sources VLA radio source measurements and identifications reformatted 29-Mar-96 by H.Andernach ( paper 3 <20 mJy; paper 2 >= 20 mJy; corrections included according to emails of B.Slee 2-Apr-96, 25-Apr-96, 23-Jul-96 and 22-Oct-96) # = sequence number of opt. ID for same source Cluster Source Radio Centroid Paper Ang. 1.5 4.9GHz Sp ell.Gauss-fit Probable OptID ra-opt offset Field Number RADec_1950 Dist. Flux Flux Index maj min PA Morph PSSE SRC Ang PA Helio. h m s d ' " R/Rc mJy mJy " " deg Cl Rmag B_J Dist deg Redshift (1) (2) (3) (4) (5) (6) (7) (8) (9)(10)(11)(12)(13) (14) (15) (16) (17) ----+----1----+----2----+----3----+----4----+----5----+----6----+----7----+----8----+----9----+----0----+--- A0013_1 000938.97 -194042.4 2 1.30 84.0 17 3 89 A0013_2i 000941.73 -195459.8 3 1.29 7.0 A0013_2ii 000943.95 -193150.5 3 1.44 22.2 A0013_3 001002.81 -193737.2 3 1.08 1.9 A0013_4 001031.71 -195206.5 3 0.59 3.4 A0013_5 001051.14 -193903.5 3 0.54 1.6 E 20.8 3 22 A0013_6_abc 001054.51 -194647.7 23 0.19 3.9 -2.1 53 20 99 E 17.7 18 -85 A0013_7 001056.68 -194014.1 2 0.45 21.1 7 3 48 A0013_8 001104.67 -195313.4 3 0.36 1.4 A0013_9i 001111.87 -194623.6 3 0.07 1.0 E 20.8 2 11 A0013_9ii #1 001115.03 -195144.2 3 0.30 1.1 St 19.0 8 -114 A0013_9ii #2 001115.03 -195144.2 3 0.30 1.1 Stx2 18.5 2 -122 A0013_10 001131.18 -195718.5 3 0.68 1.0 A0013_11 001150.49 -193200.3 3 1.09 16.7 St 20.6 6 180 A0013_12 001158.53 -195915.6 3 1.00 7.8 17 6 203 A0013_13i 001209.05 -195922.0 3 1.11 18.5 14 5 118 A0013_13ii_ab 001211.66 -194308.9 3 0.94 9.2 A0013_14 001215.17 -194355.5 3 0.96 8.1 St 18.8 2 -39 A0076_1 003639.42 +065632.7 2 0.82 31.8 0.0 13 4 74 A0076_2 003659.05 +065619.0 3 0.78 2.9 21 10 67 G 19.5 5 -170 A0076_3 003712.65 +065714.2 3 0.80 3.4 A0076_4 003712.89 +065254.9 3 0.67 4.8 A0076_5_ab 003717.56 +070832.7 2 1.14 20.7 53 7 38 A0076_6i 003721.02 +070924.5 3 1.16 8.5 14 7 48 A0076_6ii #1 003723.21 +065747.5 3 0.82 3.0 E 17.3 9 130 A0076_6ii #2 003723.21 +065747.5 3 0.82 3.0 G 19.5 9 43 A0076_7 003724.24 +070322.5 3 0.99 1.3 G 18.5 4 143 A0076_8 003731.45 +070331.9 2 1.00 24.6 10.1 -0.7 8 2 134 A0076_9 003732.43 +065706.2 3 0.81 7.5 3 3 73 A0076_10 003740.48 +070247.0 3 0.99 0.6 St 19.5 5 -10 A0076_11 003740.69 +071000.8 3 1.20 2.4 A0076_12 003747.47 +070147.2 3 0.97 2.1 0.3 -1.5 18 9 77 A0076_13_ab 003747.96 +070008.3 2 0.93 157.0 51.6 -0.9 50 8 104 A0076_14 003759.25 +070548.1 3 1.11 2.2 14 7 40 E 18.2 0 A0076_15 003805.76 +070546.1 3 1.13 8.1 4.2 -0.6 A0076_16 003816.79 +071126.3 3 1.31 3.9 20 7 5 A0076_17_ab 003817.31 +064826.9 2 0.72 29.6 34 7 71 A0076_18 003823.45 +070601.7 3 1.18 3.3 12 5 68 G 19.3 3 60 A0076_19 003857.38 +064133.0 3 0.84 123.0 0.3 A0085_1 003708.09 -100557.6 2 1.21 37.3 -0.9 8 5 83 G 18.6 4 152 A0085_2i 003750.49 -101819.9 3 1.33 8.9 14 6 49 A0085_2ii 003751.54 -100929.7 3 1.09 3.1 G 21.9 10 -63 A0085_3 003752.46 -093152.9 2 0.57 101.0 -0.9 23 3 118 G 18.4 2 229 A0085_4 003756.25 -101539.5 3 1.24 9.7 16 7 133 A0085_5 003758.25 -094102.3 3 0.51 6.4 A0085_6 003758.89 -095640.1 3 0.75 2.9 A0085_7_abc 003759.24 -101726.1 2 1.27 85.7 -1.0 91 14 8 A0085_8 003811.79 -100736.9 3 0.98 3.6 1.6 -0.7 8 4 13 A0085_9_ab 003811.02 -093946.8 3 0.41 1.7 30 4 120 A0085_10 003812.51 -094607.0 3 0.47 8.7 10 5 48 A0085_11 003815.66 -092907.9 3 0.45 3.4 G 19.5 22.3 6 -46 A0085_12_ab 003817.42 -100507.2 2 0.89 331.0 84.3 -1.1 A0085_13 003819.50 -095718.9 2 0.68 40.9 -1.2 4 3 61 A0085_14 003822.65 -092002.4 3 0.61 3.6 -3.0 A0085_15 003823.24 -101254.7 3 1.10 3.2 A0085_16 003823.80 -100117.3 3 0.77 1.7 A0085_17 003827.66 -100028.5 3 0.74 7.3 13 6 4 G >19.5 21.4 4 -45 A0085_18 003828.58 -100549.4 3 0.88 17.1 4.0 -1.2 5 2 150 A0085_19 003834.92 -094511.6 3 0.32 8.7 -0.6 4 1 119 A0085_20i 003841.87 -095030.5 3 0.43 0.7 G 21.8 5 -144 A0085_20ii 003842.45 -092935.4 3 0.30 1.9 G >19.5 21.9 1 180 A0085_21i 003848.22 -093552.1 3 0.13 0.5 A0085_21ii_ab 003848.69 -092721.4 3 0.33 1.1 A0085_22_abc 003849.70 -095230.6 3 0.46 5.8 23 2 6 A0085_23i 003852.29 -101309.7 3 1.06 4.4 A0085_23ii 003855.33 -094255.0 3 0.19 0.5 St 18.6 9 -39 A0085_24 003856.77 -092929.0 3 0.25 0.6 A0085_25_abc 003857.03 -093844.4 23 0.08 7.8 -2.4 97 16 143 A0085_26i 003858.48 -093215.4 3 0.17 6.6 8 2 133 cD 15.2 3 -31 0.0448 A0085_26ii 003858.62 -095710.1 3 0.60 1.8 A0085_27 003901.11 -094426.8 3 0.21 1.4 A0085_28 003904.80 -095548.4 3 0.55 11.0 -0.2 7 4 122 G 19.5 22.7 9 104 A0085_29 003902.21 -101143.2 3 1.01 5.6 -1.3 G 18.2 21.2 7 4 A0085_30i 003901.81 -095613.1 3 0.54 1.4 St 16.8 16.9 6 38 A0085_30ii 003903.12 -093650.2 3 0.02 0.5 A0085_31 003907.08 -093917.0 3 0.05 1.6 6 3 169 A0085_32i 003909.86 -093039.5 3 0.21 2.2 A0085_32ii 003912.21 -092716.9 3 0.29 1.1 A0085_33i 003914.12 -094908.9 3 0.36 0.6 A0085_33ii 003916.14 -093309.9 2 0.15 49.1 -1.4 31 2 171 E 16.1 17.4 20 170 0.0529 A0085_34i 003916.25 -093711.0 3 0.07 6.7 8 4 127 A0085_34ii 003917.15 -095238.6 3 0.47 1.3 E 21.9 4 -174 A0085_35_ab 003918.66 -093438.4 2 0.13 46.2 -1.2 8 4 27 cD 13.5 14.6 0 0.0557 A0085_36_ab 003919.28 -094215.0 2 0.17 91.1 -1.7 40 28 67 E 16.0 17.5 14 274 0.0579 A0085_37 003921.34 -094131.5 23 0.16 2.5 8 2 111 A0085_38i #1 003921.29 -094554.8 3 0.27 1.3 E 16.5 17.1 4 134 0.0525 A0085_38i #2 003921.29 -094554.8 3 0.27 1.3 E >19.5 20.6 8 21 A0085_38ii_ab 003921.89 -102102.9 3 1.30 28.5 24 7 137 A0085_39 003923.65 -092140.8 3 0.49 3.2 A0085_40 003926.39 -093322.8 3 0.19 2.5 S0 >19.5 21.9 3 42 A0085_41 003927.00 -095544.0 3 0.56 5.5 A0085_42i 003927.41 -094017.6 3 0.17 1.0 A0085_42ii_abc #1 003929.30 -093525.3 3 0.17 3.2 83 17 85 E 20.6 6 139 A0085_42ii_abc #2 003929.30 -093525.3 3 0.17 3.2 83 17 85 E 20.2 4 87 A0085_43 003932.14 -093114.3 3 0.27 1.6 G 21.2 9 132 A0085_44 003934.17 -095542.3 3 0.57 4.1 A0085_45_ab 003936.11 -094859.0 2 0.40 27.6 -0.7 34 8 34 A0085_46 003937.39 -095719.4 2 0.63 20.7 9 5 127 A0085_47i 003938.79 -094402.1 3 0.32 0.7 A0085_47ii 003939.35 -093300.8 3 0.28 0.8 A0085_47iii 003940.87 -092708.5 3 0.38 0.8 A0085_48i 003941.12 -092441.2 3 0.44 1.1 A0085_48ii 003942.28 -094909.4 3 0.43 3.3 -2.6 A0085_49 003944.24 -094254.7 3 0.32 1.0 A0085_50 003944.74 -094209.8 3 0.31 1.7 A0085_51i 003947.50 -095047.1 2 0.49 48.1 -1.0 11 3 109 A0085_51ii 003948.08 -092602.4 3 0.44 1.3 A0085_52 003949.57 -092048.5 3 0.59 6.4 St 18.8 19.3 9 -152 A0085_53i 003953.25 -094328.6 3 0.39 1.1 -3.8 5 3 48 A0085_53ii 003955.40 -095236.8 3 0.58 1.4 A0085_54i 003956.87 -092846.6 3 0.44 1.1 A0085_54ii 003958.61 -093827.9 2 0.38 81.2 0.1 11 5 86 A0085_55 003959.40 -095029.2 3 0.54 4.1 A0085_56i 004001.90 -093836.4 3 0.41 1.6 A0085_56ii 004004.03 -092812.9 3 0.49 1.4 A0085_57 004009.05 -094137.2 3 0.47 2.8 A0086_1 003832.53 -220955.0 3 0.86 11.0 A0086_2 003853.40 -220314.7 3 0.64 2.7 A0086_3 003924.64 -221620.2 3 0.59 2.0 A0086_4i 003934.00 -221210.1 3 0.48 1.3 G 21.5 8 -120 A0086_4ii 003940.02 -220751.0 3 0.24 2.6 9 6 138 A0086_5_ab 003941.61 -221315.2 2 0.39 136.0 43.5 -1.0 34 5 51 A0086_6 #1 003944.27 -221840.6 3 0.59 2.0 19 4 3 G 20.4 5 -26 A0086_6 #2 003944.27 -221840.6 3 0.59 2.0 19 4 3 G 21.0 7 -138 A0086_7 003945.41 -220331.9 3 0.16 3.2 St 19.5 1 -145 A0086_8 003946.82 -222330.4 3 0.78 16.5 -1.1 A0086_9 003956.22 -221624.6 3 0.48 2.0 E 18.8 3 154 A0086_10 003958.05 -215853.1 3 0.24 3.6 -1.8 A0086_11i 004001.49 -221910.6 3 0.59 3.3 A0086_11ii 004008.52 -220946.9 3 0.23 2.2 14 6 7 E 18.2 7 -165 A0086_12 004018.30 -221247.2 2 0.36 32.1 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