1980A&AS...42..319H WESTERBORK OBSERVATIONS OF B2 RADIO SOURCES IN ABELL CLUSTERS OF GALAXIES. D.E. Harris, C. Lari, J.P. Vallee, A.S. Wilson Summary. Short observations at 1415 MHz have been made of 120 Abell clusters. This sample contains all apparent coincidences between sources from the Bologna (B2) catalogue with S_408MHz >0.2 Jy,+24d < DEC <+42d, and Abell clusters of distance class D<5. In this paper we present the results for those clusters (58) containing B2 sources which are probably associated with the cluster (i.e. identified with a galaxy of optical magnitude corresponding to cluster membership), Positions, flux densities, and optical identifications are listed for these clusters in Table 1, and contour diagrams for some of the extended sources are also included. I. INTRODUCTION Attempts to determine the statistical properties of radio sources in clusters of galaxies are usually hampered by selection effects and incompleteness. In an effort to minimize these effects we have made observations at 1415 MHz with the Westerbork Synthesis Radio Telescope (WSRT) of B2 sources (Colla et al., 1970, 1972, 1973, and Fanti et al. 1974) which coincide with Abell Clusters of distance class D<5. For inclusion in the sample we therefore required that the angular distance between a B2 source and a cluster center, r_c, was less than the corresponding Abell radius, R_A = 1.717/z arcmin (Abell, 1958). Similar surveys of Abell clusters have been completed at the National Radio Astronomy Observatory (Green Bank) and at Cambridge. Owen et al. (1977, and references therein) have published results on 89 clusters observed at 2.7 and 8 GHz. Their sample was based on a finding search at 1400 MHz supplemented by "all available radio data on rich clusters as of January 1974", and was restricted to declinations greater than 20d. McHardy (1978) and Riley (1975) have observed 53 clusters at frequencies between 0.4 and 5 GHz. Their sources were drawn from the 4C and 4CT catalogues for declinations greater than 10d. For both surveys, sources were restricted to those with rc/RA < 0.3; a constraint which is not present in our survey. The present paper presents the results of the WSRT observations for those cases where there is an optical identification from the PSS E prints with a galaxy of m_v <= m_10 <= m_10 + 2 (m_10 = the magnitude of the tenth brightest galaxy). This limit roughly corresponds to M_V<-18. In several cases follow-up observations have already been completed (e.g. Valentijn , 1979), and some statistical use of the data has also appeared (Lari and Perola, 1978), Section II contains a brief summary of the observing parameters and the reduction method. The tabular data are described in Section III and remarks on individual sources are contained in the notes to Table 1. Contour diagrams of extended sources follow Table 1. In the Appendix (Table 2) we list the remaining clusters of the original sample for which the radio sources were not clearly associated with the cluster. II OBSERVATIONS AND DATA REDUCTION The Westerbork synthesis instrument has been detailed extensively in the literature (Hogbom and Brouw, 1974; Baars and Hooghoudt, 1974; Casse and Muller, 1974) and only a brief account is given in the following. At the time of these observations, the array consisted of twelve equatorially mounted 25m paraboloids, each with orthogonal dipole feeds at its focus, distributed along an East-West line. The ten fixed paraboloids were spaced at intervals of 144m, while the two movable ones were separated by 72m along a rail track. Combining each fixed paraboloid with each movable one gave twenty interferometers; in this configuration, the 20 spacings were integral multiples of 72m, with a minimum of 72m and a maximum of 1440m. For most fields studied, we made seven observations (lasting 3 minutes each), at uniformly distributed hour angles. This gave a reasonable sampling of the twenty ellipses on the Fourier transform (u,v) plane. The angular resolution is equivalent to a synthesized beamwidth of 23 x 23/sind arcsec (RA x DEC) at the observing frequency of 1415 MHz. About twenty fields centered on the B2 positions were observed in the summer of 1974, and the remainder were completed in the summer of 1975. The calibration followed the standards set by the WSRT Reduction Group. With a 4 MHz bandwidth, the rms noise per synthesized beam area amounted to about 3 mJy. Data reduction used the CLEAN technique (Hogbom, 1974), in which extended regions on the maps are iteratively decomposed into a set of point sources, whose effects on the maps are removed using the antenna pattern with its sidelobes and grating rings. These point sources are finally restored on the residual maps, after being convolved with a Gaussian approximating the original synthesized beam out to the first zero crossing. The maps were then corrected for the attenuation by the primary beams of the individual paraboloids (HPBW is about 36 arcmin at 1.4 GHz). Positions and intensities of all sources associated with the B2 sources were found by a Gaussian fitting routine. Global errors have been estimated as < 4 arcsec for RA, < 8 arcsec for DEC, and sqrt[(0.02S)^2 + (3)^2] mJy for the flux density, S. III. DATA PRESENTATION In order to avoid two or more tables for the same sources, and to curtail duplicate entries, we have adopted a two tiered table. Every source or component occupies two lines of data. These will be abbreviated here as "l1" and "l2". Column 1: l1 The Abell number of the cluster. l2 The distance and richness class. Column 2: l1 Redshifts of clusters. Estimated redshifts are distinguished by 2 digits only. l2 The magnitude of the 10th brightest galaxy. Column 3: l1 The B2 source name. l2 The Bautz Morgan cluster type. Column 4: l1 The radio right ascension (1950) of the source. l2 The right ascension of the optical object. Column 5: The corresponding declinations. Column 6: l1 The flux density at 408 MHz. l2 The flux density at 1415 MHz. Column 7: l1 The spectral index, alpha (S ~ nu^-alpha). l2 The projected distance of the source from the cluster center, r_c, divided by the Abell radius, R_A Column 8: l1 The radio types which are abbreviated by Cx = complex. Db = double. NC = not classified. NC is primarily used for sources weaker than 100 mJy and so the signal to noise ratio is not sufficient to determine if the source is slightly resolved or not. NR = not resolved. This type normally refers to sources stronger than 100 mJy and implies that the angular size is <15"(RA) and <30"(DEC). R = resolved. The angular size is > 2 beam sizes. SR = slightly resolved. The deconvolved size is < 2 beam sizes. TRG= tailed radio galaxy. WAT= wide angle tail. l2 The optical type D = a D galaxy. Db = a double galaxy. E = elliptical. Ep = peculiar E galaxy. NC = not classified. (Usually because the galaxy is too faint.) Column 9: l1 The apparent visual magnitude. When the symbol "a" precedes m_v, this indicates that the galaxy is the brightest in the cluster. l2 The absolute visual magnitude (H_o = 100 km/s/Mpc) Column 10: l1 The largest angular size of the radio structure (NR = not resolved). l2 The largest linear size'. Column 11: l1 The position angle for the entry in 10(l1). l2 The identification classification: 0 = good positional agreement and the galaxy is probably a cluster member. 1 = good positional agreement, but cluster association is in doubt. 2 = multiple optical objects are present and cluster association is probable. 3 = poor positional agreement but the optical galaxy is probably a cluster member. Column 12: l1 Log of the 408 MHz power (H_o = 100 km/s/Mpc). When two components are found at 1415 MHz for a single B2 source, the 408 #Hz powers have been calculated on the basis of the relative intensities at 1415 MHz. l2 Notes - a dagger indicates that comments on the source follow the table. - a capital "C" indicates that a contour diagram is given. - lower case letters code the references to radio data at other freguencies. Table I. - Sources Associated with Clusters 1 2 3 4 5 6 7 8 9 10 11 12 A z B2 RA_r DEC_r S408 alpha type_r mV LAS PA logP D R m10 BM RA_o DEC_o S1415 d/Ra type_o Mv LLS Id_cl Notes ----+----1----+----2----+----3----+----4----+----5----+----6----+----7----+----8----+-- A7 .14 0009+32 000910.2+320847 320 1.4 NC 18.5 NR - 24.8 5 1 17.1 III 000910.4+320846 57 .04 NC -19.6 < 30 0 +C, f A7 0008+32 000831.9+320024 1150 .97 WAT? 16.6 400" 110 25.5 000843.6+320034 304 .60 E -21.5 640 2 +C, c A7 0009+31 000853 +315901 670 * * * * * * * * 241 * * * * * * A82 .14 0038+25A 003817.8+250126 260 1.35 NC 16.5 NR - 24.7 5 2 17.1 III 003817.8+250111 48 .56 E -21.6 <30 3 + A104 .07 0047+24 004703.0+240958 460 .92 R 15.4 60" 170 24.4 4 1 15.9 II-III 004703.2+240957 146 .26 E -21.3 55 0/2 C A278 .090 0154+31B 015423.1+320008 1080 1.33 SR 16.6 35" 140 24.96 3 0 15.6 III 015422.4+320010 205 .02 E6 -20.6 40 0 c d f A318 .12 0209+26B 021000.9+261140 580 .97 NR 16.7 NR - 24.96 5 1 16.9 III 021001.5+261155 173 .16 E -21.1 <28 3 c f A346 .12 0219+26 021924.6+260759 420 1.05 NR 16.7 NR - 24.82 5 1 16.9 II-III 021925.0+260759 113 .23 E -21.1 <28 0 f A439 .1070 0327+24B 032733.0+243740 1180 1.24 TRG? a16.5 40" 90 25.14 5 0 17.0 III 032732.2+243735 252 .09 E -21.0 61 3 d f A567 .12 0658+33A 065817.1+325920 400 .97 Db 16.6 88" 60 24.74 5 1 16.9 III 065814.7+325911 119 .34 E -21.3 126 0 +C c i A567 0658+33B 065850.7+330202 790 1.1 WAT? 16.5 90" 90 25.08 065852.6+330147 198 .71 E -21.4 129 0 * A568 .078 0704+35 070423.6+350815 1360 .94 Cx 14.8 80" 90 24.93 3 0 15.4 I-II 070423.0+350817 420 .06 E -22.2 80 0/2 +C cef A587 .11 0729+39A 072936.3+393135 290 .87 NR a16.8 NR - 24.57 5 1 16.6 I-II 072936.6+393138 98 .18 E -20.7 <27 0 f A610 .10 0756+27 075609.6+271717 1020 .71 Db a15.8 140" 80 24.98 4 0 16.4 II-III 075613 +271730 160 .05 D -21.5 174 0 C cdf A610 075616.4+271732 * * * * * * * * * 260 * * * * * * A690 .079 0836+29 083613.3+290138 1500 .5 WAT a14.2 360" 20 24.98 5 1 16.9 I 083613.4+290117 808 .05 cD -22.7 366 0 +cdfi A695 .068 0838+32A 083806.5+323542 1610 .71 Cx a14.1 260" - 24.88 5 1 17.1 I 083806.8+323539 667 .50 cDm -22.4 236 0 +ei A923 .1165 1003+26 100349.4+260915 300 1.32 NC a16.2 NR - 24.62 5 1 17.2 I 100349.4+260924 58 .12 D -21.5 <28 0 +f A1081 .14 1042+35 104152.1+355614 340 .72 R 16.1 35" 90 24.12 5 2 17.2 II 104152.3+355604 26 .38 Db -22.1 58 0 C A1081 104205.3+355644 * * R 17.1 60" 30 24.76 104205.9+355640 112 .38 E -21.1 97 0 * A1097 .08 1045+31 104525.0+314420 470 1.37 NC 16.8 NR - 24.46 4 0 16.0 II 104522.2+314415 85 .14 E -20.1 <20 3/0 +f A1179 .11 1106+24B 110642.0+241137 340 .79 R 17.1 80" 170 24.64 5 0 16.6 III 110641.6+241124 127 .5 E -20.4 107 0 A1190 .075 1108+41 110852.7+410637 3030 1.03 TRG? 14.6 57" 0 25.22 5 2 16.6 II 110853.5+410643 766 .12 D -22.2 55 0 C cgi A1190 110853.4+410341 * * Db 15.9 40" 30 24.50 110854.3+410326 70 * E -20.9 39 0 +Ccgi A1213 .049 1113+29 111354 +293157 4210 .66 Db a13.9 78" 70 25.01 2 1 14.5 III 111353.4+293134 1840 .04 Db -21.9 52 0 +cef A1267 .06 1125+27 112505.8+271531 400 1.64 NC 17.4 NR - 24.10 3 0 15.4 112506.2+271539 52 .22 Ep -18.8 <16 1 + A1336 .08 1137+32A 113710.0+324017 470 .84 Db 16.3 90" 60 24.46 4 0 16.0 III 113707.5+323956 165 .20 E -20.6 92 0 +C A1455 .15 1201+28 120104.5+281240 610 1.07 NR 16.8 NR - 25.17 5 2 17.2 II-III 120103.4+281315 160 .30 E -21.4 <34 0/3 A1547 .15 1225+26B 122534.0+265900 330 .59 SR 18.2 30" 0 24.90 5 1 17.2 I 122534.0+265902 158 .56 E -20.0 51 0 A1608 .15 1243+33 124317.1+334045 720 1.01 Db 15.8 70" 55 25.24 5 0 17.2 II-III 124316.7+334051 203 .08 E -22.4 1 19 0 +Ccf A1609 .089 1243+26B 124354.6+264333 1200 1.00 WAT a15.0 270" 30 24.99 5 1 16.8 III 124354.6+264339 342 .12 E -22.1 304 0 +cfi A1610 .15 1244+30 124425.3+302147 370 .99 SR 16.5 30" 160 24.90 5 1 17.2 III 124425.8+302143 108 .29 E -21.7 51 0 A1632 .15 1250+29 125011.4+290806 1090 .72 NR 17.5 NR - 25.37 5 2 17.2 II-III 125011.4+290808 444 .39 E -20.7 <34 0 c A1685 .15 1306+35 130607.9+351003 250 1.12 NC 18.5 NR - 24.78 5 0 17.2 II-III 130608.4+351002 62 .74 NC -19.7 <34 0 A1775 .072 1339+26B 133931.0+263733 1260 1.15 TRG a13.8 43 6 24.85 4 2 15.7 I 133930.7+263735 300 .04 Db -22.9 40 0 +acfhj A1785 .15 1342+38B 134249.0+382402 260 1.88 NC 17.2 - - 24.75 5 2 17.2 I-II 134248.8+382412 25 .18 NC -21.0 26 0 A1795 .063 1346+26 134633.8+265025 3150 1.01 NR a13.6 NR - 25.11 4 2 16.0 I 134634.1+265028 890 .08 cD -22.8 <17 0 +aef A1797 .13 1347+25A 134721.1+252239 280 1.00 SR 16.8 46" 170 24.69 5 1 17.0 III 134720.9+252240 80 .47 E -21.2 70 0 C A1797 1347+25C 134744.5+252424 340 .92 Db? 17.2 120" 30 24.79 134743.8+252325 108 .73 E -20.8 183 3 +C A1799 .15 1347+35B 134706.4+353907 260 .5 NC 18.2 NR - 24.65 5 1 17.2 II 134706.8+353909 100 .45 E -20.0 <34 0 f A1799 134716.0+354233 * * NC 18.6 NR 24.25 134716.1+354241 40 .01 NC -19.6 <34 1 * A1800 .0724 1347128 134756.3+283136 520 .73 SR 14.9 42" 25 24.44 3 0 15.4 I-II 134756.5+283138 210 .43 E -21.8 40 0 A1819 .15 1352+24 135243.6+243920 490 .80 NR a15.3 NR - 25.02 5 1 17.2 III 135243.6+243920 180 .26 Db -22.9 <34 0 df A1832 .15 1356+29 135652.9+295006 410 .80 NC 17.3 NR - 24.88 5 1 17.2 III 135653.4+295013 116 .16 NC -20.9 <34 0 C f A1832 135651.6+294818 * * NC 17.8 NR - 24.37 135652.3+294808 36 * NC -20.4 <34 3 +C f A1856 .15 1404+25A 140408.0+252337 440 .84 NR 17.5 NR - 24.97 5 1 17.2 III 140409.3+252324 155 .34 NC -19.5 <34 3 A1886 .15 1412+27 141255.6+272009 370 1.07 NC 16.6 80" 95 24.90 5 1 17.2 II-III 141256.4+272022 71 .44 E -21.6 136 0 C A1886 141300.5+271957 * * * * * * * * 26 * * * * * * A1898 .13 1418+25A 141826.2+252226 350 .41 NC a14.1 NR - 24.52 5 1 17.0 III 141826.3+252227 111 .44 D -23.9 <30 0 C A1898 141826.2+251420 * * NC 17.5 NR - 24.47 141825.8+251417 100 .68 E -20.5 <30 0 * A1914 .15 1424+38 142404.0+380226 670 - NC 17.7 - - 25.20 5 2 17.2 II 142403.6+380245 >15 .05 NC -20.5 - 2 +Cf A1939 .0881 1435+25 143501.7+250508 600 .75 R 16.2 90" 125 24.57 5 1 16.6 III 143502.7+250506 177 .04 E -21.1 120 0 C acf A1939 143501.5+245858 * * Db 16.5 150" 25 24.09 143501.4+245831 58 .16 E -20.8 200 0 * A1979 .15 1448+31B 144852.0+313003 360 1.76 NC a16.6 NR - 24.34 5 2 17.2 II-III 144852.5+313003 20 .00 D -21.6 <34 0 C A1979 144854.0+313337 * * NC 17.7 NR - 24.81 144853.2+313335 60 .27 NC -20.5 <34 0 * A1984 .1265 1450+28 145023.5+281013 380 .75 Db? a15.7 40" 135 24.79 5 2 17.2 I-II 145023.8+281010 150 .20 Db -22.2 60 0 +f A1990 .15 1451+28 145123.1+281612 420 .77 NR 18.9 NR - 24.95 5 3 17.2 III 145122.7+281608 160 .2 NC -19.3 <34 0 cf A2022 .06 1502+28 150211.2+284714 1920 .66 TRG 14.6 120" 20 24.90 3 1 15.6 III 150208.3+284551 837 .24 E -21.8 163 0 +C ci A2025 .15 1504+34 150443.7+343925 470 .69 SR a15.6 48" 180 25.00 5 1 17.2 I-II 150444.0+343954 200 .06 D -22.6 82 3 C ef A2034 .12 1507+33 150755.5+333824 510 1.04 Db 16.7 80" 30 24.90 5 2 16.9 II-III 150758.4+333906 82 .33 E -21.2 115 0 C A2034 150758.4+333920 * * * * * * * 58 * * * * * * A2042 .15 1509+36 150929.3+364455 380 .86 SR a17.3 20" 90 24.91 5 1 17.2 III 150928.8+364451 130 .12 NC -20.9 34 0 f A2062 .11 1519+32 151925.0+320827 240 1.06 NC 17.9 - - 24.44 5 1 16.6 151924.7+320838 64 .47 NC -19.6 <27 1 A2079 .0653 1525+29 152539.8+290526 430 .60 SR 15.4 20" 90 24.27 3 1 15.4 III 152539.6+290528 204 .16 E -21.1 17 0 acj A2083 .1143 1527+30 152743.1+305248 370 1.31 NC 15.2 - - 24.69 5 1 16.9 II 152743.3+305249 72 .32 E -22.5 <28 0 + A2089 .07 1530+28 153039.1+281351 790 .66 SR 16.5 50" 20 24.61 4 1 15.8 I-II 153039.4+281352 349 .13 E -20.2 46 0 cf A2096 .13 1533+37 153324.8+373314 280 1.33 NC 16.8 - - 24.18 5 2 17.0 II-III 153325.3+373308 16 .24 E -21.2 <31 0 C c A2096 153325.9+373526 * * * - - - * 37 * - - - - * A2142 .0896 1556+27 155609.0+272454 420 1.18 TRG 16.1 70" 90 24.42 4 2 16.0 II 155609.9+272454 97 .16 E -20.7 72 0 C ab A2249 .080 1707+34 170750.0+342934 1940 .89 R 16.2 28" 90 25.10 3 0 15.4 III 170749.3+342934 643 .08 E -20.7 29 0 cef A2250 .0621 1709+39 170917.4+394517 1800 .93 TRG a14.8 300" 105 24.85 5 1 16.5 III 170916.8+394507 566 .10 E -21.6 248 0 +Ccfh A2622 .0607 2332+27 233231.9+270546 730 1.32 NC a14.2 - - 24.17 4 0 15.9 I-II 233231.6+270543 72 0.00 D -22.1 <16 0 C ef A2622 233231.9+271017 * * NC 17.0 - - 24.15 233232.4+271002 68 .20 E -19.4 <16 0 * A2672 .14 2352+26 235258.0+260620 940 .94 Db 18.2 220" 120 25.29 5 1 17.1 III 235251.6+260734 165 .37 D -19.9 355 1 C c A2672 235245.0+260821 * * * * * * * * 125 * * * * * * NOTES TO TABLE 1 + A dagger indicates that comments on the source are included below. # An asterisk is used to indicate that the corresponding entry above applies to this radio component as well. E.g. when one optical object is thought to be associaSed with two radio components. an asterisk is found for the second entry. Often two components are not resolved at 408 MHz and an asterisk indicates that the first entry is the total flux density for both components. a An alpha preceeding m_v indicates that the galaxy is the brightest in the cluster. a,b,etc: lower case letters designate references to radio data at other frequencies: a 1980A&AS...41..339Andernach et al. b 1978A&AS...31...99Haslam et al. c 1975AJ.....80..263Owen d 1975AJ.....82..677Owen et al. e 1975MNRAS.170...53Riley f 1976A&A....50..165Roland et al. g 1977AJ.....82....1Rudnick and Owen h 1979MNRAS.188..637Simon i 1979A&ASS..38...31Valentijn j 1979A&AS...36..237Waldthausen et al. k 1978MNRAS.184..387Birkinshaw l 1978A&AS...34..117Harris & Miley m 1974AJ.....79..427Owen COMMENTS ON INDIVIDUAL SOURCES A7 0009+32: Several other galaxies are close by. That indicated in the contour diagram is located at RA = 00 09 09.1, DEC =+32 08 45 0008+32 and 0009+31: For the tabular entries, we have interpreted these two sources as being associated. They are shown in Figure 1. A82 Another source (RA=003836.2, DEC=+250950, S_1415MHz ~ 40 mJy lies close to the cluster center. However, it is not a B2 source and the nearest galaxy is 43" away. A439 0327+24B: Since the right ascensions of the galaxy and the radio positions at 2695, 1415 and 408 MHz follow an increasing progression, we agree with Owen et al. (1977) who remark that 0327+246 may be a narrow tail. Occultation observations have been published by Kapahi et al. (1973). A567 0658+33 A and B: Both sources have two components (see figure 3). The tabulated positions refer to the stronger components, but the flux densities are the sums. The positions of the weaker components are 0658+33A (SW): 065812.1+325846 0658+33B (E) : 065858.1+330141 Finding charts and 610 MHz maps have been published by Valentijn (1979). A568 0704+35: The galaxy listed in the table is one of the 3 shown in the finding chart of Riley (1975). The second galaxy (mv = 15.4) indicated in figure 5 is at B070424.6+350823. The weaker radio component is at B070427.1+350830. The tabulated flux densities refer to the sum of both components. A690 0836+29: The data for this complex source are given in Fanti et al. (1978). The tabulated position is for the brightest component at 1415 MHz but the flux densities are summed over all components. A695 0838+32A: See the note above for A690. A923 1003+26: The tabulated data are taken from Fanti et al. (1978). A1097 1045+31: The tentative identification is with a bright, double galaxy. However, there is a difference of > 30 arcsec between the optical and radio RA. There is a possible radio extension of very low brightness in PA = 90 . A1190 1108+41: The second entry for the radio position refers to the center of the southern double source (see figure 6). A1213 1113+29: This is 4C29.41B (Riley, 1975). The tabulated position is the centroid of the two lobes (the W lobe is twice as strong as the E lobe at 1415 MHz). See Fanti et al. (1977) for details. A1267 1125+27: A second, fainter component at RADEC50=112502.0+271505, with S(1415) = 16 mJy is not clearly related to the main component. A1336 1137+32A: The radio coordinates are those of the radio centroid. A1455 1201+28: There may be low level emission extending to the north. A1608 1243+33: The tabulated position is the centroid of the almost equal double shown in figure 8. A1609 1243+26B: The radio and optical data are from Fanti et al. (1978). The tabulated position is that of the strongest component, but the flux densities listed are for all the detected components. A second galaxy is at RADEC50=124352.7+264332 (m_v=16). A1775 1339+26B: The optical position refers to the SE galaxy of a close pair. WSRT maps and data have been published in Miley and Harris (1977) and Harris et al. (1980). A1795 1346+26: The tabulated data are from Fanti et al. (1977). A1797 1347+25C: The listed position is for the NE component. The weaker (SW) component contributes 16 mJy to the total flux density of 108 mJy at 1415 MHz. A1832 1356+29: The fainter, southern component is 20 arcsec east of the brightest galaxy in the cluster. A1914 1424+38: The radio source is of low surface brightness at 1415 MHz, and is probably extended (~2 arcmin). Our peak intensity of 15 mJy may be compared with 0.14 Jy as measured with the NRAO 300' telescope by Tovmassian (1973). The total power spectrum may be approximated by a power law with a = 1.75 between 26 and 2700 MHz. There are several more galaxies close to the one listed. A1984 1450+28: The tabulated data are from Fanti et al. (1978). The optical position refers to the midpoint of the two galaxies. A2022 1502+28: The position given is for the radio centroid. More extensive WSRT observations are reported by Valentijn (1979). A2079 1525+29: The radio data are taken from Fanti et al. (1977). A second radio galaxy (B2 1528+29) (see Fanti et al. 1978) is probably a background source. A2083 1527+30: The radio and optical data are from Fanti et al. (1978). A2249 1707+34: A second source (B2 1708+34) at 0.68 Abell radii from the cluster center, has not been detected in the present observations. A2250 1709+39: Other maps have been published by Miley and Harris (1977). Harris et al. (1980), and Rudnick and Owen (1976). Appendix. Table 2 is a list of additional clusters, which, together with those in Table 1, comprised the original sample. The two clusters of distance class D=6 (indicated by an asterisk) were added as filler observations. In additiona to the basic clusters parameters (first 5 columns) we give the status of the WSRT 1415 MHz observations. NO = no observation. Some of these were intentionally dropped because higher sensitivity maps already existed. C = a preliminary contour diagram is available P = the position of the strongest source is available DM = a digital map is available The last column of the table contains letters indicating references to other observations 1415 MHz observations. NO = no observation. Some of these were intentionally dropped because higher sensitivity maps already existed. C = a preliminary contour diagram is available P = the position of the strongest source is available DM = a digital map is available The last column of the table contains letters indicating references to other observations a 1980A&AS...41..339Andernach et al. b 1978A&AS...31...99Haslam et al. c 1975AJ.....80..263Owen d 1975AJ.....82..677Owen et al. e 1975MNRAS.170...53Riley f 1976A&A....50..165Roland et al. g 1977AJ.....82....1Rudnick and Owen h 1979MNRAS.188..637Simon i 1979A&ASS..38...31Valentijn j 1979A&AS...36..237Waldthausen et al. k 1978MNRAS.184..387Birkinshaw l 1978A&AS...34..117Harris & Miley m 1974AJ.....79..427Owen TABLE 2. Additional Clusters CLUSTER POSITION m10 D R Status Other Observations ----+----1----+----2----+----3----+----4----+----5----+----6 A 156 0108+33 16.9 5 1 C,P A 260 0149+32 15.8 4 1 C,P m A 407 0258+35 14.7 2 0 NO a,c,e,f,g,h,j,l *A 584 0725+26 17.3 6 1 C,P c,f A 602 0750+29 15.8 4 0 DM a,j,m A 603 0752+33 16.8 5 1 C,P m A 605 0753+27 16.7 5 0 DM A 607 0754+39 16.9 5 0 DM A 612 0757+34 16.5 5 1 C,P m A 628 0806+35 15.9 4 0 DM A 654 0820+39 17.1 5 1 C,P A 683 0833+31 17.1 5 0 DM A 702 0844+25 17.1 5 1 C,P A 846 0938+22 17.0 5 1 C,P A 879 0947+29 17.2 5 1 C,P m A 943 1009+33 17.2 5 2 C,P A 963 1014+39 17.2 5 3 NO c,e,f A 964 1013+25 17.2 5 1 C,P A1026 1027+40 17.2 5 1 C,P l A1031 1028+39 17.2 5 0 DM A1033 1028+35 17.2 5 2 NO f A1099 1046+35 17.0 5 1 C,P c,e,f A1185 1108+28 14.3 2 1 C,P A1187 1108+39 15.6 3 1 C,P c,m,optical cluster not found A1228 1118+34 13.8 1 1 C,P m A1257 1123+35 15.0 3 0 C,P A1275 1127+36 15.7 4 0 DM A1305 1130+35 17.2 5 0 DM A1401 1149+37 17.0 5 3 C,P A1420 1154+26 17.2 5 1 C,P A1423 1154+33 16.5 5 1 C,P A1425 1155+26 17.2 5 1 N0 e,f A1433 1157+26 17.1 5 1 C,P A1441 1158+35 17.2 5 1 C,r A1567 1233+27 17.2 5 0 DM *A1667 1300+32 17.6 6 2 C,P c,d,r,i,m A1672 1302+33 17.2 5 1 DM A1691 1309+39 15.4 3 1 DM A1694 1309+34 17.2 5 1 P A1715 1318+38 17.0 5 1 DM A1723 1319+37 17.0 5 0 DM A1769 1336+28 17.2 5 1 C,P f A1781 1342+30 15.4 3 0 DM A1840 1359+30 17.2 5 0 DM A1863 1405+27 17.2 5 0 DM m A1873 1409+28 16.3 4 0 DM A1902 1419+37 17.2 5 2 DM A1908 1421+26 17.1 5 1 C A1909 1421+25 16.8 5 1 DM m A1927 1428+25 16.0 4 1 DM c,m A1944 1435+30 17.2 5 1 DM m A2004 1456+25 17.0 5 0 DM f A2019 1500+27 16.3 4 0 DM m A2065 1520+27 15.6 3 2 DM m A2067 1521+31 15.7 4 1 N0 A2092 1530+31 15.7 4 1 N0 m A2106 1537+33 17.2 5 1 C A2124 1543+36 15.6 3 1 C A2141 1555+35 17.2 5 1 DM f A2145 1558+33 16.6 5 0 DM A2148 1601+25 15.4 3 0 C A2175 1618+30 16.2 4 1 C A2178 1619+24 17.1 5 1 C A2241 1658+32 15.6 3 0 N0 a,c,e,j A2243 1700+35 17.1 5 1 DM A2244 1700+34 16.6 5 2 DM f,m A2245 1700+33 16.5 5 1 DM m A2257 1716+32 17.1 5 1 DM A2584 2319+27 17.1 5 0 N0 c,e,f A2647 2338+25 17.1 5 0 DM A2650 2339+25 17.1 5 1 C A2666 2348+27 13.8 1 0 C c,k,m (OCR, proof, reformatting by H.Andernach 1/96)