1978A&AS...34..117Harris & Miley Westerbork Observations of 5 fields centred on Abell clusters of Galaxies Tables 2-6 merged into one (scanned by H.Andernach, corrected/proofed by A. Gubanov, 2/95) Field 13W RA_1950 +-s DEC1950+-" S_610/mJy S_1415/mJy alph(49/21) optID R-O_RA" R-O_DEC" Notes ----+----1----+----2----+----3----+----4----+----5----+----6----+----7----+----8----+----9----+----0 A 376 1 023711.3 0.3 +363027 4 75 7 OFF A 376 2 023752.0 0.9 +372556 18 95 25 **PLO -2 2 # A 376 3 023753.2 0.2 +361833 3 105 6 NBG A 376 4 023819.8 0.3 +372318 8 110 25 *S(b) -10 8 A 376 5 023900.7 0.3 +362551 5 32 6 **PLO 1 -6 # A 376 6 023918.2 0.4 +361138 7 95 20 # 94"@160 A 376 7 023921.6 0.2 +362200 3 58 8 *S(f) -3 13 51"@102 A 376 8 023924.8 0.3 +370631 5 24 3 NBG A 376 9 023933.9 0.4 +365506 7 50 15 EF # A 376 10 023946.5 0.4 +360214 12 90 30 # 91"@130 A 376 11 024011.7 0.4 +365034 7 26 7 EF A 376 12 024017.3 0.3 +364208 4 52 5 **G(18.5) -2 2 A 376 13 024021.3 0.4 +353817 8 160 30 EF A 376 14 024027.4 1.0 +362937 22 13 6 **G(f) -5 -11 A 376 15 024056.0 0.3 +371331 4 24 2 # A 376 16 024103.1 0.3 +371916 4 27 3 G(~16) A 376 17 024108.9 0.2 +365636 3 26 2 G(~18) A 376 18 024110.1 0.2 +363119 3 335 10 **PLO 1 -1 B2,Ohio A 376 19 024118.7 0.2 +370505 3 195 20 EF # A 376 20 024136.3 0.2 +360555 4 40 8 *db(f) 6 -13 # A 376 21 024146.1 0.2 +362429 2 23 3 *S?(f) -4 -8 A 376 22 024155.0 0.6 +362334 14 9 3 PLOs A 376 23 024156.3 0.7 +362020 12 15 2 EF 53"@71 A 376 24 024158.0 0.2 +355221 4 335 20 EF B2 A 376 25 024158.7 0.1 +363716 3 98 8 EF A 376 26 024201.0 0.2 +364110 5 13 2 EF A 376 27 024214.4 0.3 +372848 4 60 5 *S?(f) 15 15 (26"@39) A 376 28 024219.8 0.1 +363458 3 195 15 EF A 376 29 024220.6 0.2 +364648 4 64 5 *G(17.5) -8 9 A 376 30 024237.3 0.2 +371730 5 55 15 # A 376 31 024301.0 0.2 +364908 2 42 4 EF # A 376 32 024305.4 0.1 +370302 3 46 8 S?(f) -3 12 18"@85 A 376 33 024314.1 0.2 +355736 3 45 3 NBG A 376 34 024316.5 0.2 +352348 3 310 20 OFF A 376 35 024318.1 0.2 +361543 4 21 2 G(~17)+ A 376 36 024318.9 0.2 +363751 3 125 20 **G?(17)+ -0.4 24 # 51"@178 A 376 37 024322.9 0.2 +370152 3 82 6 PLOs A 376 38 024344.8 0.5 +363233 5 75 10 # 69"@84 A 376 39 024345.8 0.3 +362644 5 26 4 EF A 376 40 024347.5 0.1 +361054 2 65 15 EF A 376 41 024349.7 0.5 +373329 9 50 12 EF # (B2) A 376 42 024351.4 0.3 +363033 4 12 1 NBG A 376 43 024358.1 0.1 +363127 2 63 4 EF A 376 44 024358.6 0.2 +355609 3 55 4 EF A 376 45 024358.6 0.3 +361042 5 17 2 NBG A 376 46 024400.5 0.2 +373534 3 176 10 S 12 0 # (B2) A 376 47 024423.5 0.2 +374223 4 1160 70 EF B2,4C,Ohio A 376 48 024433.0 0.2 +365438 5 37 7 EF A 376 49 024435.2 0.2 +363228 3 120 8 EF A 376 50 024444.9 0.6 +371347 11 31 6 **G(f) -4 -11 A 376 51 024458.7 0.4 +354717 6 260 40 **PLO -5 -3 # B2 A 376 52 024503.1 0.6 +365840 8 19 4 **S(f) -12 -11 (33"@93) A 376 53N 024505.4 0.3 +364702 6 20 3 EF A 376 53S 024506.0 0.2 +364428 5 19 3 EF A 376 54 024517.5 0.3 +354400 5 83 7 OFF A 376 55 024529.8 0.2 +370526 3 146 10 *G(f) 4 9 A 376 56 024552.2 0.2 +365703 2 54 10 EF A 376 57 024620.6 0.4 +363254 6 18 9 EF # A 376 58 024630.5 0.7 +370104 6 100 50 **S(f) 4 8 A 376 59 024630.7 0.1 +363655 2 28 5 EF # A 376 60 024630.7 0.2 +361751 4 115 15 EF A 376 61 024636.7 1.0 +365206 10 30 10 **PLO 2 4 A 376 62 024654.8 0.4 +355311 8 190 40 **G(f) 5 4 34"@97 A 376 63 024757.0 0.2 +363422 3 55 14 # A 407 64 025249.0 0.5 +353358 12 280 40 **PLO 2 2 B2 A 407 65 025305.3 0.2 +363027 3 500 40 EF B2 A 407 66 025332.3 0.3 +354553 4 75 8 **S(b) -4 3 A 407 67 025443.7 0.1 +362724 2 321 16 **G(f) 0 -3 B2 A 407 68 025454.9 0.5 +350150 9 130 20 EF B2 A 407 69 025512.4 0.2 +354328 4 310 20 **G(18) 1 2 # B2 A 407 70 025525.3 0.1 +353102 3 700 60 *G(18) -4 5 B2 A 407 71W 025548.7 0.3 +355150 6 65 20 # A 407 71E 025551.5 0.6 +355140 8 75 20 # typo in DEC-arcmin in publ.paper A 407 72 025605.0 0.4 +351600 8 60 10 **db(18) 0 -4 # A 407 73 025606.3 0.2 +361936 3 59 4 EF A 407 74 025610.0 0.4 +354902 7 43 6 PLO(blue) A 407 75 025630.1 0.3 +354531 4 450 100 G(16.5)+ # B2 A 407 76 025640.7 0.2 +352810 4 22 2 **db(15.7)+ # A 407 77 025649.5 0.2 +363728 3 132 9 **G(14) -5 7 A 407 78 025649.9 0.5 +350304 13 50 6 **PLO 6 0 A 407 79 025654.2 0.2 +352358 3 25 5 EF A 407 80 025716.0 0.1 +350318 3 185 15 EF A 407 81 025718.6 0.3 +350844 6 130 30 **G?(f) # 64"x30"@155 A 407 82 025719.3 0.3 +353557 4 285 30 EF # 49"@70 A 407 83 025719.4 0.2 +354210 5 30 5 EF A 407 84 025724.0 0.2 +360936 2 260 30 S7(f) 11 1 B2 A 407 85 025730.6 0.2 +355022 4 19 2 EF A 407 86 025735.0 0.2 +353606 10 36 EF # A 407 87 025737.4 0.2 +351850 5 90 15 EF A 407 88 025739.4 0.2 +361014 2 85 15 **G(16)+ 1 -1 A 407 89 025740.3 0.3 +353803 6 45 EF # A 407 90 025742.3 0.3 +351342 2 50 10 **G(18) -1 0 33"@110 A 407 91 025743.0 0.2 +353355 3 310 20 *S(f) 6 -10 # B2 A 407 92 025752.5 0.3 +355333 3 27 2 *S(f) -6 -6 A 407 93 025753.7 0.3 +360451 4 23 2 EF A 407 94 025758.1 0.2 +361549 4 135 25 EF A 407 95 025811.6 0.3 +360104 4 20 2 EF A 407 96 025814.0 0.2 +355650 3 49 4 EF A 407 97 025817.2 0.2 +351115 3 31 2 *G(f) 6 7 A 407 98 025835.3 0.2 +350033 3 2800 100 **G(13.5) 0 -1 # 4C,B2 A 407 99 025839.0 0.3 +365329 4 187 20 EF A 407 100 025844.2 0.2 +353841 3 1750 100 # 46"@122 A 407 101 025855.7 0.3 +355409 4 20 2 **G(15)+ A 407 102 025857.5 0.3 +361753 5 240 30 **PLO 0 4 # A 407 103 025857.5 0.1 +351722 2 250 30 **G(f) 1 2 A 407 104 025906.2 0.2 +345631 4 408 30 **PLO -3 0 B2 A 407 105 025913.4 0.2 +360940 4 92 6 *db(f) 1 -10 A 407 106 025926.2 0.2 +352611 4 410 40 *G(f) 6 4 # B2 A 407 107 030006.4 0.1 +362000 3 90 9 EF A 407 108 030012.2 0.2 +350309 3 42 3 EF A 407 109 030017.2 0.3 +353438 4 23 2 **G(15)+ -4 -2 A 407 110 030020.4 0.4 +361814 8 53 7 EF A 407 111 030020.8 0.1 +343531 3 1090 50 EF 4C,B2 A 407 112 030037.1 0.2 +362252 3 77 5 EF A 407 113 030039.3 0.3 +355100 7 42 8 EF A 407 114 030048.0 0.2 +353541 8 70 7 *PLO -5 -7 A 407 115 030144.9 0.1 +350031 3 960 40 EF 4C,B2 A 407 116 030207.8 0.3 +350954 4 55 5 EF A 407 117 030213.2 0.1 +361328 10 390 50 *G(17) -4 -1 B2 A 407 118 030328.7 0.3 +353606 4 86 8 EF A 407 119 030401.9 0.3 +351723 4 144 14 EF B2 A1035 120 102515.7 0.2 +401715 3 85 12 EF A1035 121 102529.4 1.0 +410332 11 57 12 **S?(f) 6 0 A1035 122 102541.7 0.2 +400856 3 46 4 EF A1035 123 102556.4 0.3 +392615 13 140 30 EF A1035 124 102606.4 0.3 +411136 5 68 15 EF A1035 125 102700.1 0.3 +401556 3 26 2 EF A1035 126 102721.8 0.5 +391321 8 500 100 PLO # B2 A1035 127 102744.7 0.2 +400510 5 45 5 EF A1035 128 102806.6 0.2 +405304 2 41 2 EF A1035 129 102807.3 0.2 +401622 5 540 50 EF 60"@22, B2 A1035 130 102808.6 0.2 +411248 3 41 3 **S(f) 2 5 A1035 131 102821.8 0.1 +400223 4 306 30 EF B2 A1035 132 102900.3 0.2 +402213 3 23 6 **G?(15.5)+ -4 3 A1035 133 102902.9 0.5 +412344 9 30 10 **S(b) 2 2 A1035 134 102910.9 0.4 +405828 7 18 4 EF A1035 135 102928.2 0.5 +404437 17 9 3 EF # A1035 136 102933.0 0.2 +393122 4 61 6 **PLO 1 6 A1035 137 102934.1 0.3 +404634 8 10 2 # A1035 138 102935.2 0.2 +402154 3 17 1 EF A1035 139 102936.8 0.3 +413221 8 120 12 **S(b) -4 15 (75"@26) A1035 140 102946.3 0.4 +403606 7 20 4 EF # A1035 141 102951.6 0.2 +403842 6 16 2 EF A1035 142 102956.5 0.3 +401509 4 67 6 EF A1035 143 103007.9 0.2 +413135 3 830 30 **BSO(f) 1 0 A1035 144 103023.6 0.2 +404124 13 13 3 A1035 145 103027.5 0.2 +395121 3 525 25 *PLO -6 -4 B2 A1035 146 103040.1 0.2 +394047 3 43 3 **PLO 3 6 A1035 147 103049.1 0.2 +403645 3 15 1 EF A1035 148 103059.8 0.2 +402051 3 16 1 EF A1035 149 103103. +3931 43 # A1035 150 103104.1 0.1 +400412 2 55 8 EF A1035 151 103110.7 0.4 +402301 15 25 10 **PLO -5 -6 A1035 152 103112.5 0.3 +403038 5 32 4 **PLO -3 -3 A1035 153 103112.6 0.1 +401055 5 46 4 **S?(f) 2 -3 A1035 154 103124.5 0.4 +400909 7 74 14 BSO(f) (59"@27) A1035 155 103144.4 0.2 +395405 5 57 10 **S(b) 2 5 61"@53 A1035 156 103147.8 0.2 +405542 3 145 8 EF A1035 157 103158.0 0.3 +400238 7 45 15 EF A1035 158 103208.8 0.2 +404652 3 50 12 *G(f) 7 1 # A1035 159 103212.8 0.3 +403327 6 180 20 EF (38"@63) A1035 160 103225.6 0.2 +402326 5 115 15 EF A1035 161 103228.9 0.4 +403030 7 54 5 EF A1035 162 103237.9 0.4 +402932 7 22 4 EF A1035 163 103313.3 0.6 +405737 10 32 6 EF A1035 164N 103326.1 0.2 +395608 5 64 10 EF A1035 164S 103327.2 0.4 +395229 7 65 8 EF A1035 165 103331.1 0.1 +405108 3 610 40 EF VRO A1035 166 103341.0 0.6 +410843 12 45 7 EF A1035 167 103418.7 0.2 +402714 3 1440 70 EF 4C,VRO A1035 168 103455.0 0.4 +403525 7 66 6 EF A1035 169 103455.1 0.4 +404612 8 57 8 EF A1035 170 103505.6 0.5 +403239 7 150 20 EF A1035 171 103524.0 0.6 +394836 11 120 20 EF B2 A1035 172 103525.0 0.2 +403916 3 220 20 EF A1035 173 103621.4 0.2 +404720 2 240 16 EF A1904 174 141353.5 0.3 +491048 3 390 40 EF A1904 175 141452.6 0.2 +481643 2 1990 200 EF 4C A1904 176W 141744. 3. +485120 18 80 20 # A1904 176E 141749.4 0.4 +485149 4 115 15 # A1904 177 141755.8 0.5 +475455 7 300 40 *G(16.2) -18 -33 # A1904 178 141803.6 0.5 +485423 10 84 14 EF ~50"@~170 A1904 179 141808.2 0.4 +491233 4 32 4 EF A1904 180 141838.8 0.2 +485502 3 33 5 EF A1904 181 141924.7 0.7 +492900 3 120 20 EF 34"@~70 A1904 182 141925.2 0.3 +485316 3 27 3 EF A1904 183 141932.2 0.5 +484321 4 15 2 EF A1904 184 141934.4 0.4 +490903 3 164 16 EF 61"@114 A1904 185 141957.1 0.3 +490147 4 25 5 *PLO 9 4 A1904 186 141957.6 0.2 +480435 3 120 20 EF A1904 187 142002.2 0.2 +490557 3 136 6 *PLO 0 -11 A1904 188 142016.7 0.2 +481324 3 60 6 **PLO 4 0 30"@33 A1904 189 142046.6 0.2 +484128 3 128 5 EF A1904 190 142054.7 0.2 +475559 2 140 12 EF A1904 191 142103.4 0.3 +481938 4 25 4 EF A1904 192 142105.3 0.3 +490056 4 23 3 EF A1904 193 142115.7 0.1 +481546 2 490 20 **PLO 2 -1 # A1904 194 142128.4 0.1 +484350 2 383 12 **PLO 0 -1 A1904 195 142130.6 0.6 +485355 10 23 3 EF (40"@0) A1904 196 142133.5 0.3 +491018 4 22 3 EF A1904 197 142133.9 0.2 +492721 4 80 12 *PLO -6 5 A1904 198 142146.7 0.5 +483931 4 18 4 *G(15.3)+ -3 -13 (98"@90) A1904 199 142155.9 0.6 +483036 8 12 4 *G?(f) -16 16 A1904 200 142204.6 0.3 +491407 4 27 3 EF A1904 201 142204.6 0.7 +475619 8 38 10 EF A1904 202 142206.4 0.3 +480138 4 72 7 EF A1904 203 142213.0 0.3 +483711 3 49 4 EF (11"@102) A1904 204 142218.1 0.2 +474803 2 144 15 EF A1904 205 142233.6 0.2 +484344 4 17 3 EF A1904 206 142245.9 0.3 +491512 5 31 3 EF A1904 207 142246.9 0.2 +484715 5 17 4 EF A1904 208 142251.4 0.6 +481816 6 18 4 **G(f) 9 7 A1904 209 142255.2 0.3 +494446 3 345 20 EF A1904 210 142309.5 0.2 +490426 3 49 5 EF # A1904 211 142314.2 0.2 +485647 2 41 4 EF A1904 212 142314.8 0.5 +490606 10 29 3 EF # A1904 213 142315.4 0.4 +492312 4 28 3 *S(f) 9 3 A1904 214 142317.4 0.1 +474945 2 156 20 EF A1904 215 142340.5 0.3 +493247 5 60 10 EF A1904 216 142412.5 0.2 +492806 3 47 4 EF A1904 217 142412.5 0.3 +483759 4 55 7 EF A1904 218 142431.8 0.4 +491210 5 35 6 EF (102"@8) A1904 219 142435.5 0.3 +492144 3 66 6 EF 19"@93 A1904 220 142438.4 0.2 +485018 3 17 3 EF A1904 221 142456.4 0.4 +494604 4 88 10 **db(f) 7 2 A1904 222 142505.1 0.3 +492158 3 55 10 *G?(f) -2 -5 51"@143 A1904 223 142528.5 0.7 +490953 11 30 12 EF A1904 224 142609.5 0.2 +492213 2 420 50 **PLO -1 0 11"@86 A1904 225 142615.5 0.2 +485446 2 115 12 EF A1904 226 142620.5 0.2 +491458 3 150 30 EF A1904 227 142638.1 0.2 +490540 4 88 8 **PLO 2 -1 A1904 228 142638.6 0.4 +492657 4 77 7 EF A1904 229 142640.1 0.3 +484339 4 85 15 EF A1904 230 142645.6 0.2 +490029 2 95 15 EF A1904 231 142646.0 2.0 +492250 4 68 8 EF A1904 232 142711.4 0.5 +485202 7 100 30 EF A2319 233 191227.9 0.2 +435415 3 1200 400 PLOs # 42"@174 A2319 234 191250.7 0.3 +434504 3 1900 200 S(f) # (43"@85) A2319 235 191329.7 0.2 +431905 4 440 40 stars A2319 236 191334.4 0.4 +435745 5 140 15 EF A2319 237 191518.1 0.2 +431046 3 410 40 stars A2319 238 191523.2 0.1 +434204 2 83 12 EF # A2319 239 191545.2 0.4 +440340 4 19 2 G(f) A2319 240 191553.0 0.3 +433807 3 50 5 *G(18) 9 10 ## A2319 241 191558.2 0.3 +435447 4 58 6 **S(17) 4 -5 A2319 242 191604.6 0.1 +434258 2 225 15 EF A2319 243 191605.3 0.2 +443132 2 480 15 G?(f) 14 0 # (4C) A2319 244 191605.4 0.1 +432301 2 445 20 **G?(18) 0 -1 A2319 245 191637.9 0.3 +443304 5 190 30 **G(18) -3 1 # A2319 246 191717.9 0.2 +443150 3 725 25 **S?(f) -1 -2 (4C) A2319 247 191725.9 0.2 +441249 2 77 7 20 5 1.6 0.4 EF A2319 248 191734.0 0.3 +443316 3 43 3 EF A2319 249 191742.4 0.1 +435202 1 55 7 25 2 0.9 0.2 EF A2319 250 191744.3 0.1 +433956 2 7.5 1.5 G(f) (14"@37) A2319 251 191803.5 0.2 +441926 2 32 4 PLO A2319 252 191804.7 0.3 +423035 2 380 50 EF A2319 253 191813.1 0.2 +444635 2 74 7 EF A2319 254 191823.3 0.3 +430023 2 45 3 PLO A2319 255 191831.6 0.1 +435458 2 10 2 4.0 0.6 1.1 0.3 star A2319 256 191831.9 0.5 +441138 9 30 6 EF (87"x32"@19) A2319 257 191838.5 0.2 +435412 2 13 3 2.8 0.4 1.8 0.4 stars A2319 258 191840.4 0.7 +424526 12 60 15 EF A2319 259 191842.3 0.2 +435728 3 170 30 90 6 0.8 0.2 # typo in RA-min in publ.paper A2319 260 191842.8 0.1 +432601 1 114 6 35 2 1.4 0.1 PLOs A2319 261 191843.8 0.2 +424112 3 250 40 EF A2319 262 191845.0 0.1 +434302 2 13 2 4.0 0.5 1.4 0.3 G?(17)+ A2319 263 191850.3 0.1 +440521 1 38 4 18 2 0.9 0.2 **G(f) -2 2 A2319 264 191854.5 0.3 +434654 4 1.3 0.2 star A2319 265 191859.0 0.1 +434753 2 1.9 0.3 EF 17"@172 A2319 266 191859.3 0.2 +434901 2 2.5 0.3 EF A2319 267 191900.0 0.1 +432608 1 18 3 10.5 1.0 0.6 0.2 **G(15)+ 1 0 # A2319 268 191902.8 0.1 +433750 2 3.2 0.3 PLO A2319 269 191907.0 0.2 +440356 2 5.3 0.5 2.8 0.5 0.8 0.3 EF A2319 270 191920.2 0.1 +434650 1 74 6 32 2 1.0 0.2 EF A2319 271 191922.5 0.4 +430215 6 30 10 **G(13.5) 3 1 NGC6792 A2319 272 191932.5 0.2 +435901 2 2.5 0.5 PLO A2319 273 191935.3 0.2 +434723 2 65 10 26 4 1.1 0.3 **G(15.8)+ 9 5 # A2319 274 191935.8 0.1 +432757 1 46 4 131 7 -1.2 0.1 **G?(f) 0 -1 # A2319 275 191937.6 0.1 +432340 2 30 6 11 3 1.2 0.5 stars 35"@80 (610 MHz) A2319 276 191938.8 0.2 +433912 2 2.1 0.3 star A2319 277 191939.2 0.1 +435056 1 65 20 20 1 1.4 0.3 EF # A2319 278 191946.0 0.1 +435240 1 20 10 4.0 0.5 1.9 0.6 EF (15"@157) A2319 279 191946.7 0.2 +432938 3 8 3 G(15)+ # A2319 280 191950.7 0.3 +430929 5 70 G # A2319 281W 191951.9 0.2 +440402 3 5 A2319 281 191953.2: +440347: 33 6 1.3 0.4 # A2319 281E 191955.3 0.1 +440331 2 6 A2319 282 191958.7 0.2 +435400 2 4.2 1.0 **G(15.5)+ 1 1 18"@90 A2319 283 191959.9 0.1 +435221 2 230 30 100 7 1.0 0.2 EF # A2319 284 192000.9 1.1 +430655 13 50 G # A2319 285 192002.6 0.3 +432954 5 5 2 G(15)+ # A2319 286 192003.3 0.3 +432625 2 38 10 21 5 0.7 0.5 **G(f) 1 -1 # A2319 287 192004.7 0.1 +434900 3 2.2 0.3 star A2319 288 192006.1 0.2 +434726 2 1.6 0.4 PLO A2319 289 192006.2 0.6 +430807 5 70 G # A2319 290 192008.7 0.4 +433947 4 1.6 0.4 EF A2319 291 192009.1 0.1 +435206 1 40 8 16 4 1.1 0.4 **G(15)+ 9 4 # 15"@80 A2319 292 192011.0 0.2 +433734 2 1.6 0.4 PLO A2319 293 192012.3 0.1 +435120 1 1.7 0.3 *G(17)+ -5 2 # A2319 294 192013.8 0.1 +440626 1 13 2 6.0 0.6 0.9 0.3 stars # 11"@96 A2319 295 192016.0 0.1 +440433 1 9.5 0.4 EF A2319 296 192023.0 0.3 +450038 4 320 70 EF A2319 297 192025.0 0.1 +440839 1 12 3 7.0 0.7 0.6 0.3 **G(f) 0 0 # A2319 298 192028.3 0.3 +442906 5 106 10 EF A2319 299 192028.4 0.1 +432709 1 20 2 11 2 0.7 0.2 EF 17"@101 A2319 300 192028.7 0.2 +440202 2 30 6 14 2 0.9 0.3 **S(b) -8 0 23"@125 A2319 301 192041.4 0.2 +434431 2 2.0 0.7 EF A2319 302 192041.6 0.1 +432659 1 44 4 18 2 1.1 0.2 **G(f) 2 -2 # A2319 303 192041.7 0.1 +434235 2 16 4 5.6 0.8 1.2 0.4 **G(~16)+ 0 -3 # A2319 304 192041.7 0.2 +440549 2 170 12 74 7 1.0 0.2 PLO ~12"@~70 A2319 305 192043.9 0.1 +435925 1 12 5 14 2 -0.2 0.5 star A2319 306 192051.2 0.2 +434407 2 16 4 5.3 0.5 1.3 0.3 EF A2319 307 192055.7 0.1 +433659 2 6 3 4.5 0.7 0.3 0.5 EF 26"@90 A2319 308 192056.6 0.1 +435939 1 14 3 7 1 0.8 0.3 PLO A2319 309 192057.0 0.1 +440820 1 13 3 7 2 0.7 0.5 EF A2319 310 192102.7 0.2 +442308 2 85 12 35 6 1.1 0.3 EF A2319 311 192103.4 0.2 +434926 3 3.0 0.6 G(f) A2319 312 192109.4 0.1 +434902 1 120 10 56 2 0.9 0.1 EF A2319 313 192110.6 0.4 +425936 3 34 4 NBG A2319 314 192112.8 0.1 +433927 2 24 10 8 2 1.3 0.5 EF 22"x7"@27 A2319 315 192122.7 0.1 +434202 2 72 10 32 3 1.0 0.2 EF # A2319 316 192132.4 0.1 +433645 1 < 170 25 51 3 EF (16"@157) A2319 317 192135.3 0.6 +433559 9 < 170 25 7 2 star # A2319 318 192137.8 0.6 +434434 7 130 15 65 10 0.8 0.3 EF # A2319 319 192141.1 0.2 +433453 3 105 10 51 3 0.9 0.2 EF 19"x8"@164 A2319 320 192153.7 0.3 +432453 3 25 2 EF A2319 321 192235.2 0.2 +440954 4 75 10 EF A2319 322 192239.9 0.4 +440326 7 28 6 EF A2319 323 192255.4 0.3 +441114 5 80 20 EF # A2319 324 192421.7 0.3 +433403 3 56 4 G(18) # A2319 325 192429.5 0.3 +432936 3 61 5 EF A2319 326 192502.5 0.2 +435323 2 85 6 PLO A2319 327 192647.5 0.3 +440556 3 269 24 OFF =========================================================================== NOTES =========================================================================== 1978A&AS...34..117Harris & Miley Westerbork Observations of 5 fields centred on Abell clusters of Galaxies (scanned by H. Andernach 2/95) Notes to Table 2-6: 2 The suggested identification is not the brightest of what appears to be a distant cluster. 5 There is also a db(f) 5"E and 15"S. 6 There are two faint galaxies: one at each end of the inner, elliptical contours of this extended source. 9 A 1415 MHz map of this peculiar source is shown on page 503 of Willis et al. (1976). 10 There are 2 faint galaxies (mV = 17.5 and 18.5) and a stellar image within 3 sigma of the radio position. 15 To the north of the radio position there is a faint object within the contours. 19 Low level contours extend about 1.5' to the NE. There is a S(f) and a G?(f) about 50" to the SW. 20 This source is probably extended towards the north-east. 30 The listed flux density includes a contribution of about 20 mJy from a component which lies about 2' to the SW. A PLO, a G(f). and a G?(17) all lie within 3 sigma of the radio position. 31 Birkinshaw (private communication) has observed this source at 1407 MHz. Since the flux density at that frequency is about 50 mJy, the spectrum is flat or inverted. 36 Birkinshaw (private communication) has resolved this source at 1407 MHz into a N-S double with a component separation of about 58". The suggested identification lies just to the north of the southern component. 38 This source is probably an unequal double (separation 1.1'). However it could be of the "head-tail" type morphology. Two faint galaxies (mV ~18.5) Iie near the peak of the radio brightness and a stellar image is 50" to the east. 41 There is a G(17) about midway between 41 and 46. The image on the O-print is comet shaped. 46 There is a G(17) about midway between 41 and 46. The image on the O-print is comet shaped. 51 There is a weak feature extending 1.5' to the north-west which contains about 80 of the 260 mJy. 57 There is a faint stellar image one-half way between 57 and 59. 59 There is a faint stellar image one-half way between 57 and 59. 63 A galaxy and two stars are within 5 sigma of the radio position. 69 There is also a blue stellar image at offset (-6",+1"). 71 A contour diagram of this double source is included in figure 2. There is a galaxy (mV ~16.5) just to the SE of the peak of 71E and a very faint galaxy near the peak of 71W. These galaxies were inadvertantly omitted when measuring positions of optical objects. 72 A plate limit jet extends in PA ~240 degrees from the southern image. 75 There are 3 galaxies (mV ~16.5) within the contours of this crescent-shaped source. Figure 2 shows the contour diagram. 76 The entries in the optical identification column refer to the centre of 2 galaxies which are almost touching. Two additional galaxies lie just to the north. 81 The suggested identification is the northern object of two overlapping images. 82 There is a galaxy located on the western edge of the radio contours (about 1' E of the radio peak). 86 86 and 89 are probably two components of a double source. The total flux density is 85 +- 15 mJy. 89 86 and 89 are probably two components of a double source. The total flux density is 85 +- 15 mJy. 91 From a comparison of the O- and E- prints, this star appears to be blue. Rudnick and Owen (1977) resolve this source into a double. The suggested identification is about 1.5" from the peak of the weaker, NW component. 98 NGC 1167, a foreground Sc galaxy with z=0.016 (Sargent 1973). 100 This is the cluster centre (see figure 1). Higher frequency maps and finding charts are given by Riley (1975) and by Rudnick and Owen (1977). 101 This is a bright lenticular galaxy for which Zwicky and Kowal (1968) give mP = 14.7. 102 There is a weak companion source of about 25 mJy, 2' to the north. 106 There is a weak component 2' to the SE. 126 The optical position of the PLO was not measured because it was off the edge of the print. 135 There are several faint galaxies close to the position of 137 and a fairly bright stellar image between 137 and 135. 137 There are several faint galaxies close to the position of 137 and a fairly bright stellar image between 137 and 135. 140 The flux density includes 12 mly from a component at the listed position and 8 mJy from a component 3.5' to the south-west. 144 Since the radio position is 52" from a fifth magnitude star, no optical identification was possible. 149 Accurate parameters for this source were not measured. 158 The suggested identification is the brightest member of what appears to be a plate limit cluster of galaxies. 176 There is a PLO near the midpoint of 176E and W. 177 This source is extended: 50" in PA = 28 degrees. The galaxy lies near the head of the contours. The 1400 MHz flux density (Maslowski (1972)) is 0.17 Jy (sp. index = 0.68). 193 The blue image is much brighter than the red. The 1400 MHz flux density (Maslowski (1972)) is 0.49 Jy so the spectrum is flat. 210 210 and 212 may be two components of an unequal double. 212 210 and 212 may be two components of an unequal double. 233 Low level contours extend 1.5' to the south. 234 On the E-print a plate limit plume is seen at PA ~20 degrees. 238 Halfway between 238 and 240 there are 3 G? and a lenticular G(17). 240 Halfway between 238 and 240 there are 3 G? and a lenticular G(17). The galaxy measured has the appearance of a left handed comma. Close to the west is a star. 243 On the E-print a jet-like feature appears at PA ~200 degrees. 245 Low level contours extend 30" to the north-east. 259 This source could be an unequal double (separation ~33"). The two-dimentional gaussian fits give 53", PA=131 degrees (610 MHz) and 70"x22", PA=132 degrees (1415 MHz). Figure 3 includes this source (in the north-west corner). The only optical object of interest is a galaxy (mV ~15.5) towards the south-east end of the source. If this galaxy is associated with the radio emission, it could be interpreted as a head-tail morphology. 267 The optical image is triangular with one vertex pointing to the south. On the O-print there appears to be a narrow shaft extending across the image at PA ~135 degrees. 273 This source is included in both figures 3 and 4. It is almost certainly a tailed radio galaxy (see discussion in the text). 274 Dickinson (private communication) has determined a flux density of 131 mJy for this source at 10.48 GHz. 277 At 610 MHz the two-dimensional gaussian fit gives 65"x65", and thus the listed flux density (65+-20 mJy) may be overestimated because of "contamination" from the halo. The flux density obtained by fitting the antenna pattern to the map is only 47 mJy. The brightest galaxy in the cluster lies 29" to the west. See figures 3 and 4. 279 The galaxy suggested as an identification lies 11" south-west of the midpoint of 279 and 285. It is galaxy #33 of Faber and Dressler (1977) and belongs to their cluster "A". 280 280, 284, and 289 are components of the complex source shown in figure 5. Both of the galaxies (mV(north)=14.7, mV(south)=15.5) near the source centroid are misshapen. The total flux of this source is 300+-60 mJy. 281 On the O-print, a PLO is visible close to the centroid or this double source. 283 This source is 1.5% polarized (PA ~25 degrees) at 1415 MHz. From observations at 2695 MHz with the 5 km telescope (Birkinshaw, private communication), it is seen that the source is an E-W double with a separation of about 4.8". See figures 3 and 4. 284 280, 284, and 289 are components of the complex source shown in figure 5. Both of the galaxies (mV(north)=14.7, mV(south)=15.5) near the source centroid are misshapen. The total flux of this source is 300+-60 mJy. 285 The galaxy suggested as an identification lies 11" south-west of the midpoint of 279 and 285. It is galaxy #33 of Faber and Dressler (1977) and belongs to their cluster "A". 286 This source is extended ( ~13" in PA ~30 degrees). The suggested identification appears to be a member of a distant cluster. 289 280, 284, and 289 are components of the complex source shown in figure 5. Both of the galaxies (mV(north)=14.7, mV(south)=15.5) near the source centroid are misshapen. The total flux of this source is 300+-60 mJy. 291 This galaxy have been shown to be a cluster member (No. 3 of Faber and Dressler 1977). It is almost certainly a tailed radio galaxy: see figures 3 and 4. 293 The suggested identification is a lenticular galaxy having its major axis in a SE-NW direction. It is the eastern-most source (one contour) in figure 4. 294 At 1415 MHz there is a component of about 1 mJy just preceding 294. 297 The suggested identification appears to be two faint galaxies in contact. 302 The suggested identification is a group of four faint galaxies in a common envelope. 303 The suggested identification, galaxy No. 24 of Faber and Dressler (1977), is a cluster member. 314 314, 315, and 318 may be components of a triple source. The SW component (314) lies in PA=221 degrees, 410" from 318. The SW component is very weak but the lowest contour shows a short extension pointing back towards 318 (PA ~35 degrees). The "centre" component (315) lies 28" west of the midpoint of the outer components. The NE component (318) is a well resolved head-tail source. The tail extends about 50" in PA=221 degrees. There are several plate-limit objects near the head of the NE component: a neutral star (mV ~18) with a possible blue jet in PA ~45 degrees near the midpoint of the outer components, several stars near the position or the "centre" component, and no objects near the SW component. If this is a triple source, the intensity ratios (NE: centre: SW) would be 8:4:1. lf the sources are unrelated, the absence of a bright galaxy at the head of 318 is difficult to explain (the tail would be ~75 kpc long if it were associated with A2319). However, it would be possible to hypothesize that 318 is a tailed radio galaxy in what appears to be a plate limit cluster of galaxies. 315 314, 315, and 318 may be components of a triple source. The SW component (314) lies in PA=221 degrees, 410" from 318. The SW component is very weak but the lowest contour shows a short extension pointing back towards 318 (PA ~35 degrees). The "centre" component (315) lies 28" west of the midpoint of the outer components. The NE component (318) is a well resolved head-tail source. The tail extends about 50" in PA=221 degrees. There are several plate-limit objects near the head of the NE component: a neutral star (mV ~18) with a possible blue jet in PA ~45 degrees near the midpoint of the outer components, several stars near the position or the "centre" component, and no objects near the SW component. If this is a triple source, the intensity ratios (NE: centre: SW) would be 8:4:1. lf the sources are unrelated, the absence of a bright galaxy at the head of 318 is difficult to explain (the tail would be ~75 kpc long if it were associated with A2319). However, it would be possible to hypothesize that 318 is a tailed radio galaxy in what appears to be a plate limit cluster of galaxies. 316, 317, and 319 are almost certainly components of a triple source. The SE component (319) is resolved with a tail extending almost back to the centre component (317). The total flux densities are 275 mJy (610 MHz) and 122 mJy (1415 MHz), yielding a spectral index of 1.0. The excess flux density at 1415 MHz comes from extended emission around 316 and 317. 317 316, 317, and 319 are almost certainly components of a triple source. The SE component (319) is resolved with a tail extending almost back to the centre component (317). The total flux densities are 275 mJy (610 MHz) and 122 mJy (1415 MHz), yielding a spectral index of 1.0. The excess flux density at 1415 MHz comes from extended emission around 316 and 317. 318 314, 315, and 318 may be components of a triple source. The SW component (314) lies in PA=221 degrees, 410" from 318. The SW component is very weak but the lowest contour shows a short extension pointing back towards 318 (PA ~35 degrees). The "centre" component (315) lies 28" west of the midpoint of the outer components. The NE component (318) is a well resolved head-tail source. The tail extends about 50" in PA=221 degrees. There are several plate-limit objects near the head of the NE component: a neutral star (mV ~18) with a possible blue jet in PA ~45 degrees near the midpoint of the outer components, several stars near the position or the "centre" component, and no objects near the SW component. If this is a triple source, the intensity ratios (NE: centre: SW) would be 8:4:1. lf the sources are unrelated, the absence of a bright galaxy at the head of 318 is difficult to explain (the tail would be ~75 kpc long if it were associated with A2319). However, it would be possible to hypothesize that 318 is a tailed radio galaxy in what appears to be a plate limit cluster of galaxies. 319 316, 317, and 319 are almost certainly components of a triple source. The SE component (319) is resolved with a tail extending almost back to the centre component (317). The total flux densities are 275 mJy (610 MHz) and 122 mJy (1415 MHz), yielding a spectral index of 1.0. The excess flux density at 1415 MHz comes from extended emission around 316 and 317. 323 The flux density listed includes a contribution from a weak companion source, 2.5' to the south. 324 The suggested identification appears to be two faint galaxies in contact.