2 The cluster is elongated with a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. One foreground S/S0 galaxy is superimposed on a southwestern region of the cluster. 4 The cluster is very faint. Leir (1976) notes that the cluster is elongated. A foreground galaxy is superimposed on a northwestern region of the cluster. 6 The galaxy which we identify as the most luminous member of the cluster (#1) has several companion galaxies. 9 The cluster is faint. 10 A foreground S0/a galaxy is superimposed on the cluster. 11 The cD galaxy may be a foreground galaxy superimposed on the cluster. Two galaxy chains are located in a northern region of the cluster. 14 Four possible foreground spiral galaxies are located in the field of A1213 defined as the circle of radius R_c centered on the cluster; if these galaxies are non-members, then the RS type of the cluster is cD. 16 Two foreground galaxies (S0/a + SBbc) are superimposed on the cluster. 17 A possible subcluster of galaxies is located in a southwestern region of the cluster. The cluster is faint. 19 Four foreground spiral galaxies are superimposed on the cluster. 22 The cluster is elongated in the approximately north-south direction (not with the position angle of the line connecting the components of the two brightest members of the B_b cluster). 24 Several bright S/S0 galaxies are located in the cluster. 25 Two foreground galaxies (E + S) are superimposed on an eastern region of the cluster. 26 A foreground group of galaxies is superimposed on the cluster. 30 Leir (1976) notes that the coordinates of the Abell cluster are close to the northern of two clusters. The cD galaxy is possibly a b-galaxy. 32 The cluster is very, very faint. A32 is possibly connected to A34. 34 A foreground S/S0 galaxy is superimposed on a region near the center of the cluster. A34 is possibly connected to A32. 36 Several probable bright foreground galaxies are located in the field of A36 defined as the circle of radius R_c centered on the cluster. 37 The galaxy which we identify as the most luminous member of the cluster (#1) is located in the B subcluster and has companion galaxies. Leir (1976) notes that the cluster contains two groups of galaxies. 38 A foreground S_p galaxy is superimposed on a northwestern region of the cluster. 39 Three foreground galaxies are superimposed on the cluster. 41 A foreground group of galaxies is superimposed on A41 parallel to the line of galaxies which characterizes the L cluster. 49 The cD galaxy has a very faint envelope of luminosity. Three foreground spiral galaxies are superimposed on the cluster, one on a northern region, one on an eastern region, and one on a southern region. 50 A foreground group of spiral galaxies is superimposed on a southeastern region of the cluster. 51 A foreground group of galaxies is superimposed on a northern region of the cluster. 53 A foreground spiral galaxy is superimposed on the cluster. 54 The galaxy which we identify as the third most luminous member of the cluster (#3) is projected near a star. A possible background cluster is located in the southeastern field of A54. 56 Three foreground galaxies in a linear configuration are superimposed on a northern region of the cluster. 58 A possible background cluster is located in the field of A58 defined as the circle of radius R_c centered on the cluster. 59 This cluster is connected to A60. A foreground Sp galaxy is superimposed on a northern region of the cluster. 60 This cluster is connected to A59. Foreground S/S0 galaxies are superimposed on a northern region of the cluster. Two foreground S/S0 galaxies are superimposed on a western region of the cluster. 61 The cluster is very sparse. Two foreground galaxies (E + S) are superimposed on the cluster. 62 One foreground Sbc galaxy is superimposed on the cluster. 64 Two foreground galaxies are superimposed on a region near the center of the cluster. A64 is connected to A65. R_c is restrictive. 65 This cluster is connected to A64. 70 Two foreground spiral galaxies are superimposed on the cluster. A possible foreground b-galaxy is located in the southwestern field of the cluster. 71 The cluster is poor in spiral galaxies. 72 The cluster is very sparse. 73 The cluster is very faint. 74 Three foreground spiral galaxies are superimposed on the cluster. 75 The cluster seems closer than is indicated by distance class 5. 76 The cluster is poor in spiral galaxies. 78 The galaxy which we identify as the second most luminous member of the cluster (#2) has a faint companion galaxy. A foreground spiral galaxy is superimposed on a southeastern region of the cluster. 80 Two foreground spiral galaxies are superimposed on a northwestern region of the cluster. 82 A foreground Sbc galaxy is superimposed on the cluster. 83 The galaxy which we identify as the most luminous member of the cluster (#1) is an S + S0 binary galaxy. The cluster is elongated. 87 Three foreground spiral galaxies are superimposed on the cluster. 88 Abell (1958) originally specified distance class 3 for the cluster. 89 Several possible foreground spiral galaxies are located in the field of A89 defined as the circle of radius R_c centered on the cluster. The cluster also overlaps A85, a distance class 4 cluster. 91 Four foreground galaxies (2 S + cE + b) are superimposed on the cluster. 96 A foreground group of galaxies is superimposed on a western region of the cluster. 97 An elongated double star is located in the field of A97 defined as the circle of radius R_c centered on the cluster. 100 The cluster is very sparse. 101 A foreground SBbc galaxy is superimposed on the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is also a possible foreground galaxy superimposed on the cluster. 102 A large and edge-on foreground spiral galaxy is superimposed on the northwestern part of the cluster. 104 The L5 subcluster may be a foreground group observed along the line-of-sight adjacent to the C7 cluster. 110 Three foreground spiral galaxies are superimposed on the cluster. 111 Three foreground spiral galaxies are superimposed on the cluster. 113 One large foreground spiral galaxy is superimposed on the cluster. Several smaller foreground galaxies are superimposed on a southern region of the cluster. 115 Two foreground galaxies (E/S0 and diffuse object) are superimposed on the cluster. 117 The cD galaxy may actually be a foreground elliptical galaxy superimposed on the cluster; it is NOT centrally located. 118 Two foreground galaxies (P + S) are superimposed on the cluster. 119 The gE galaxy is an outlier from the main concentration of galaxies. 122 Is A122 a cD cluster in the making? Two possible foreground spiral galaxies are located in the field of A122 defined as the circle of radius R_c centered on the cluster. 124 A rectangle of galaxies is located in the C8 subcluster. 126 The cluster is very elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 127 Three foreground galaxies are superimposed on a western region of the cluster; one foreground elliptical galaxy is superimposed on a southern region of the cluster, one foreground galaxy is superimposed on a northeastern region of the cluster. 131 Two foreground spiral galaxies are superimposed on the cluster. 132 A foreground group of galaxies is superimposed on a western region of the cluster. 135 The cluster is faint. 136 The galaxy which we identify as the most luminous member of the cluster (#1) has three faint companion galaxies in its envelope of luminosity. The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 137 Foreground galaxies are superimposed on a southern region of the cluster. 138 Several foreground spiral galaxies are superimposed on the cluster. 139 A bright foreground E/S0 galaxy is superimposed on the cluster. Four b-galaxies are located within one subclump of galaxies in the cluster. 142 Four foreground spiral galaxies are superimposed on the cluster. 145 Two foreground S0 galaxies are superimposed on the cluster. An I_c cluster is located 25 mm (on plates of the POSS) to the east of A145. 146 The cluster is sparse. A foreground b-galaxy is superimposed on an eastern region of the cluster. 148 One foreground spiral galaxy is superimposed on the cluster. 151 Haufen A cluster. Three possible foreground spiral galaxies are located in the field of A151 defined as the circle of radius R_c centered on the cluster. 153 A foreground elliptical galaxy is superimposed on an eastern region of the cluster. 154 Each of the two brightest members of the B cluster has several fainter galaxies within its envelope of luminosity; there is also possible circumfrential alignment of galaxies with respect to these two brightest members. 156 A foreground group of galaxies overlaps the cluster which makes it is difficult to separate populations. 163 Three foreground galaxies are superimposed on an eastern region of the cluster. A163 is possibly connected to A167. 164 Two foreground spiral galaxies are superimposed on the cluster. 165 The cluster is elongated with a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. A165 is possibly closer than is indicated by distance class 6. 167 Two foreground galaxies are superimposed on an eastern region of the cluster. A167 is possibly connected to A163. 168 A possible foreground arc or chain of galaxies is located in the field of A168 defined as the circle of radius R_c centered on the cluster. 170 A foreground group of four spiral galaxies is superimposed on the cluster. 171 Two probable foreground spiral galaxies are located in the field of A171 defined as the circle of radius R_c centered on the cluster. 173 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. A173 is a very faint cluster. 175 Five foreground galaxies (3 E, S, P) are superimposed on the cluster. 176 Several probable foreground galaxies are located in the field of A176 defined as the circle of radius R_c centered on the cluster; it is difficult to separate populations. 177 A foreground group of elliptical and S0 galaxies is superimposed on a southeastern region of the cluster. 181 The RS type of the cluster is possibly C7. Two diffuse objects are located in a southern region of the cluster. 182 A foreground spiral galaxy is superimposed on a western region of the cluster. 184 A foreground sprial galaxy is superimposed on a northeastern region of the cluster. 187 A possible foreground group of galaxies is located east of the cluster. 188 A foreground SB0/a galaxy is superimposed on the cluster. 189 Two large foreground galaxies (SBc, E/S0) are superimposed on the cluster. 192 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy. 196 The cluster is elongated in the approximately east-west direction. 199 The position angle of major axis of the cluster is similar to the position angle of the line connecting the two brightest members of the B cluster. The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) are possibly connected to each other by a bridge of luminosity. 201 Two foreground S/S0 galaxies are superimposed on the cluster. 202 Three foreground galaxies (2 Sc + SB) are superimposed on the cluster. The components of the t-galaxy, which we identify as the first brightest galaxy (#1), are aligned collinearly. 203 Two foreground galaxies (S0/a + Sc) are superimposed on the cluster. 204 The galaxy which we identify as the most luminous member of the C10 cluster (#1) is part of the chain of galaxies which characterizes the cluster. Two foreground S0/E galaxies are superimposed on the cluster. Leir (1976) notes that the Abell cluster is possibly two clusters. 206 One foreground galaxy is superimposed on a southern region of the cluster. 208 Two foreground galaxies (SB + S) are superimposed on the cluster. 209 Is this a possible pre-cD cluster? A foreground cE galaxy is superimposed on a western region of the cluster. 210 The cD galaxy is circularly symmetric. The cluster is elongated. A diffuse foreground Sd galaxy is superimposed on a northern region of the cluster. 211 One foreground Sab galaxy is superimposed on the cluster. 212 Is the distance class of the cluster possibly D=6? Three foreground S/S0 galaxies are superimposed on an eastern region of the cluster. 213 A foreground SBc galaxy is superimposed on the cluster. 214 The galaxy which we identify as the third most luminous member of the cluster (#3) has faint companion galaxies. 215 Several spiral galaxies are located in the cluster. 218 The cluster is very faint. A foreground diffuse P galaxy is superimposed on a northern region of the cluster. 220 Two foreground spiral galaxies are superimposed on an eastern region of the cluster. A defect on the E-plate of the POSS is located in the western field of the cluster. 223 Both subclusters are compact and good examples of RS type C. Three foreground E/S0 galaxies are superimposed on the cluster. 226 A foreground Sbc galaxy is superimposed on a southwestern region of the cluster. A226 overlaps and is possibly confused with A228. 227 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy. The envelope of luminosity on the cD galaxy is faint. 228 A foreground Sbc galaxy is superimposed on a northern region of the cluster. R_c is very restrictive because A228 overlaps A226 causing possible confusion in determining the membership of each cluster. 229 A foreground spiral galaxy is superimposed on the cluster. 232 Two foreground spiral galaxies are superimposed on the cluster. 234 Several foreground galaxies are superimposed on northwestern and southeastern regions of the cluster. 236 A foreground spiral galaxy is superimposed on the cluster. 238 A foreground group of galaxies is superimposed on the cluster. 240 A possible foreground S0/a galaxy is located in the field of A240 defined as the circle of radius R_c centered on the cluster. 241 R_c is restrictive. We adopted our revised estimate R_c~~10 mm on plates of the POSS. 242 The cluster is faint. A foreground spiral galaxy is superimposed on a northern region of the cluster. 243 A defect on the E-plate of the POSS is located in a field near the center of the cluster. 248 A foreground spiral galaxy is superimposed on a northern region of the cluster. 249 A foreground group of galaxies is superimposed on a southern region of the cluster. 250 A foreground S0 galaxy is superimposed on the cluster. 253 The galaxy which we identify as the most luminous member of the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. The cluster is elongated with a position angle of major axis similar to that of the cD galaxy. The cluster is very faint. 254 The galaxy which we identify as the most luminous member of the cluster (#1) may have streamers of luminosity to other companion galaxies. 255 A chain of galaxies is located near the center of the cluster. 256 Several foreground spiral galaxies are superimposed on the cluster. 257 The cluster seems closer than is indicated by distance class 5. 258 The cluster is sparse. Several foreground spiral galaxies are superimposed on the cluster. 259 A foreground spiral galaxy is superimposed on the cluster. 260 The cluster is probably nearer than is indicated by distance class 4. 261 Might the cD galaxy actually be a gS0 galaxy? 265 This cluster is the more distant of two clusters with the locational coordinates specified by Abell (1958). The two L subclusters are parallel to each other. 265X This is a foreground cluster of galaxies superimposed on A265. Is the distance class of A265X D=4? 267 A foreground group of galaxies is superimposed on an eastern region of the cluster. 268 A foreground spiral galaxy is superimposed on the cluster. A268 seems farther than is indicated by distance class 5. 271 A foreground SB galaxy is superimposed on the cluster. 274 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. 275 Two foreground spiral galaxies are superimposed on the cluster. 276 The two B subclusters are separated by 19.8 mm on plates of the POSS. 277 A probable foreground group of spiral galaxies is located in the field of A277 defined as the circle of radius R_c centered on the cluster. The Ep galaxy has a luminous jet. 278 The cluster is rich in spiral galaxies. 280 The cluster is elongated. 281 A foreground spiral galaxy is superimposed on the cluster. 282 The cluster is faint. 284 A foreground b-galaxy is superimposed on the cluster. 287 Two foreground spiral galaxies are superimposed on the cluster. 288 Two foreground galaxies are superimposed on the cluster. 290 Two foreground spiral galaxies are superimposed on the cluster. The cluster contains some subclusters of galaxies. 292 Three foreground spiral galaxies are superimposed on the cluster. 293 The L subclusters are approximately parallel to each other. A foreground E/S0 galaxy is superimposed on a northern region of the cluster. The cluster looks closer than is indicated by distance class 6. 294 The cluster is sparse. A foreground Sp galaxy is superimposed on a region near the center of the cluster. 295 Is the cluster closer than is indicated by distance class 5? 298 Two foreground Sc galaxies are superimposed on the cluster. 301 A foreground galaxy is superimposed on a southeastern region of the cluster. 302E The galaxy which we identify as the most luminous member of the subcluster (#1) is located at one end of a chain of galaxies. The subcluster is very small. 303 The cluster is sparse. Leir's (1976) correction to the rectangular coordinates of the cluster as registered on plates of the POSS is for A308; the original coordinates are correct; Leir's (1976) BM type is correct. The galaxy which we identify as the most luminous member of the cluster (#1) is surrounded by six companion galaxies. 306 A foreground spiral galaxy is superimposed on a northern region of the cluster. 307 A foreground galaxy is superimposed on a northern region of the cluster. A307 is elongated with a position angle of major axis similar to that of the line connecting the two brightest members of the B_b cluster. 309 Two foreground galaxies are superimposed on an eastern region of the cluster. A defect on the E-plate of the POSS is located in the field of A309 defined as the circle of radius R_c centered on the cluster; this plate defect looks like an elliptical galaxy. 312 Three foreground galaxies (E + S + b) are superimposed on the cluster. 313 Two foreground galaxies are superimposed on a western region of the cluster. 314 A foreground group of galaxies is superimposed on the cluster. A foreground SBc galaxy is superimposed in a northern region of the cluster. 315 Several foreground spiral galaxies are superimposed on the cluster. 317 Three foreground galaxies are superimposed on the cluster. 318 A foreground P galaxy is superimposed on the cluster. 319 Two foreground galaxies are superimposed on a western region of the cluster. 320 Four foreground galaxies are superimposed on the cluster, two on an eastern region and two on a western region. 325 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 327 A foreground b-galaxy and spiral galaxy are superimposed on the cluster. 328 Four foreground galaxies are superimposed on a northern region of the cluster. 329 The locational surface distribution of observed galaxies in the cluster has a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 332 Three foreground spiral galaxies are superimposed on an eastern region of the cluster. 333 The cluster is faint. 335 R_c is restrictive as is indicated by R_A' = 11.5 mm on plates of the POSS. Defects on the E-plate of the POSS are located in the northern and western fields of the cluster. 337 R_c is restrictive. 338 The cluster is faint. A large foreground P galaxy is superimposed west of the cluster. 339 R_c is restrictive. Two bright foreground galaxies are superimposed on the cluster. 340 A small chain of galaxies is located in the cluster. A foreground group of galaxies is superimposed on an eastern region of the cluster. Small defects on the E-plate of the POSS are located in the field of A340 defined as the circle of radius R_c centered on the cluster. 341 Two foreground galaxies are superimposed on an eastern region of the cluster. 342 The cluster is faint. 344 The b-galaxy identified as the brightest member of the cluster (#1) is located at the southern end of the cluster. A344 is elongated with a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B_b cluster. 345 A foreground group of galaxies is superimposed on an eastern region of the cluster. 348 Three foreground E/S0 galaxies are superimposed on a region near the center of the cluster. 349 Three foreground spiral galaxies are superimposed on a southern region of the cluster. 352 Leir (1976) notes that a cluster is located 20 mm (on plates of the POSS) to the northwest of A352. R_c is restrictive; we estimate a revised R_c = 12 mm on plates of the POSS. 353 The cluster is elongated in the approximately north-south direction with an approximate position angle of major axis similar to that of the faint envelope of luminosity on the cD galaxy. 359 This cluster is connected to A361. 360 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. A foreground Sb galaxy is superimposed on the western part of the cluster. 361 This cluster is connected to A359. 363 The t-galaxy is part of a chain of galaxies. Several spiral and elliptical galaxies are superimposed on the cluster. 368 The cluster is elongated with a position angle of major axis similar to that of the line connecting the two brightest members of the B_b cluster. A foreground spiral galaxy is superimposed on the eastern part of the cluster. 370 The cluster is very faint. The galaxy which we identify as the second most luminous member of the cluster (#2) is diffuse; the galaxy which we identify as the third most luminous member of the cluster (#3) is compact. 371 A foreground E/S0 galaxy is superimposed on the cluster. 373 Much of the E-plate of the POSS is out of focus. The 13 b-galaxies are located within a radius of 12 mm (on plates of the POSS) from the center of the cluster. 375 It is difficult to separate populations because (a) foreground galaxies are superimposed on the cluster and (b) much of the E-plate of the POSS is out of focus which makes it difficult to separate stars from galaxies. 376 A376 is not an I cluster as listed by Rood and Sastry (1971); the RS type of the cluster is C cluster because it has a definite core of brighter galaxies. Two foreground but outlying spiral galaxies are superimposed on the cluster. 378 A foreground galaxy is superimposed west of the cluster. 380 Four foreground spiral galaxies (two at each end of the line of galaxies which characterizes the cluster) are superimposed on A380. 384 A foreground group of galaxies is superimposed on the western part of the cluster. 385 Two foreground galaxies are superimposed on a region near the line of galaxies which defines the L subcluster. 386 Two foreground spiral galaxies are superimposed on the cluster. 393 A foreground group of seven spiral galaxies is superimposed on the cluster. 394 The cluster is elongated with a position angle of major axis similar to that of the line connecting the two brightest members of the B_b cluster. A foreground galaxy is superimposed on the eastern part of the cluster. 396 Is the cluster closer than is indicated by distance class 5? A foreground group of galaxies is superimposed on the cluster. 398 Several foreground spiral and elliptical galaxies are superimposed on the periphery of the cluster; it is difficult to separate populations. 402 The cluster is very faint. 403 There appear to be three populations of galaxies: (a) a population of galaxies with sharp images (foreground galaxies), (b) a population of galaxies with diffuse images (members of the cluster A403C), and (c) a population of galaxies with small images (members of A403). 404 A foreground I cluster and debris(?) are located to the north of the B cluster. Is a possible background cluster superimposed on A404? 405 A large foreground galaxy is superimposed on the eastern part of the cluster. 407 The RS type of the cluster is NOT C as listed by Rood and Sastry (1971) because many bright galaxies are distributed THROUGHOUT the cluster. 408 Nine b-galaxies are located in the C5 subcluster. Three foreground spiral galaxies are superimposed on the cluster. The I_s subcluster is sparse. 409 A large foreground Sab galaxy is superimposed on the cluster. 411 Two foreground Sc galaxies are superimposed on the eastern part of the cluster. 412 Two foreground Sbc galaxies are superimposed on the cluster. 415 A possible foreground Sbc(r) galaxy is located in the field of A415 defined as the circle of radius R_c centered on the cluster. 417 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. A foreground spiral galaxy and a diffuse object (possibly an IB galaxy) are superimposed on the cluster. A417 is very elongated in the approximately north-south direction. 420 Two b galaxies are located in a northern region of the cluster. 424 Several sprial galaxies are located in the cluster. 425 Two foreground galaxies are superimposed on the northern part of the cluster. 426 Perseus cluster. 427 The cluster is very faint. 428 A foreground SBc galaxy is superimposed on the cluster. 430 A large foreground Sbc galaxy is superimposed on the cluster. 431 Four galaxies (3 S + E) are superimposed on the cluster. 432 A foreground b-galaxy is superimposed on the southeastern part of the cluster. 433 R_A' = 15 mm (Abell 1979) compared with R_c = 9 mm (Leir and van den Bergh 1977) on plates of the POSS. 434 Two foreground galaxies are superimposed on a region between the two subclusters. 435 Two foreground galaxies (S + b) are superimposed west of the field of A435 defined as the circle of radius R_c centered on the cluster. 436 A foreground S/I galaxy is superimposed on the cluster. 441 Two foreground galaxies are superimposed on the eastern part of the cluster. A441 is a good example of an I_s cluster. 443 The cluster is very sparse. A foreground S0 galaxy is superimposed on the southern part of the cluster. 445 Is the cluster a pre-cD cluster? A foreground b-galaxy is superimposed on the western part of the cluster. 446 This cluster is a good example of an I_s cluster. 447 The cluster is elongated with a position angle of major axis similar to that of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). Several foreground spiral galaxies are superimposed on the northern and southeastern parts of the cluster. 449 The cluster is very sparse. 450 The cluster is very sparse. 451 Foreground galaxies are superimposed on the southern part of the cluster. 453 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. A small chain of galaxies is located in one subcluster within the cluster. A foreground spiral galaxy and b-galaxy are superimposed on the western part of the cluster. 454 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy in a faint envelope of luminosity (Is this galaxy a pre-cD galaxy?). A454 looks closer than is indicated by distance class 6. 456 The galaxy which we identify as the third most luminous galaxy in the cluster (#3) has a companion galaxy. 458 The locational surface distribution of most observed galaxies in the cluster has a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. The cluster is T-shaped. 459 The two L subclusters are approximately parallel to each other. 462 This cluster is connected to A464. Two foreground galaxies are superimposed on the cluster. 463 The E-plate of the POSS which registers A463 is poorly focused. 464 This cluster overlaps A462. 467 The E-plate of the POSS which registers A467 is poorly focused. 469 The E-plate of the POSS which registers A469 is poorly focused. 470 Two foreground spiral galaxies are superimposed on the cluster. 471 The cluster is elongated with a position angle of major axis similar to that of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). Leir (1976) notes that a bright foreground galaxy is superimposed on the northern part of the cluster. 472 Subclumps of galaxies are elongated in the approximate direction of the major axis of the cluster. A472 is connected to A473. 473 This cluster is connected to A472. 474 The cluster is sparse (Is the cluster possibly misidentified?). 478 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. This is a good example of a rich cD cluster with this alignment. 480 Two bright foreground spiral galaxies are superimposed on the northern part of the cluster. 481 Several foreground cE galaxies are superimposed on the cluster. 482 Leir (1976) notes that the cluster is characterized by two subclusters. 483 Leir (1976) notes that a bright foreground elliptical galaxy is superimposed on a region near the center of the cluster. 484 A large foreground spiral galaxy is superimposed on a northern region of the cluster. 485 The cluster is sparse. 487 Two foreground S/S0 galaxies are superimposed on the cluster. 489 Two foreground spiral galaxies are superimposed on the western part of the cluster. 490 Is the distance class of the cluster possibly D=6? A possible foreground b-galaxy is located in the field of A490 defined as the circle of radius R_c centered on the cluster. 491 Several foreground galaxies are superimposed on the cluster. 492 The rectangular coordinates of the cluster as registered on plates of the POSS are X = 228 mm, Y = 80 mm. 495 A foreground spiral galaxy is superimposed on the cluster. 497 Is the distance class of the cluster possibly D=6? 503 The cluster is very sparse (if extant at all). Many possible foreground galaxies are located in the field of A503 defined as the circle of radius R_c centered on the cluster. 506 Two chains of galaxies are located in the southeastern part of the cluster. 507 The cluster is sparse. 510 A possible foreground elliptical galaxy is located at the center of two clumps of galaxies. 512 A foreground spiral galaxy is superimposed on the cluster. 513 The cluster contains two compact clumps of galaxies. A foreground b-galaxy is superimposed on the eastern part of the cluster. 514 The cluster is characterized by three separate collinear clumps of galaxies. 516 A foreground group of galaxies is superimposed on the northeastern part of the cluster. A faint chain of galaxies is located in the southeastern part of the cluster. 517 Several chains of galaxies are located in the cluster. 524 A probable foreground spiral galaxy is located in the field of A524 defined as the circle of radius R_c centered on the cluster. 530 The distance class of the cluster is D=7. The locational surface distribution of faint galaxies is centered on #1, the galaxy which we identify as the most luminous member of the cluster. 532 A foreground SBc galaxy is superimposed on the cluster. 535 The galaxy which we identify as the third most luminous member of the cluster (#3) has a companion galaxy. 541 This cluster is connected to A542. 542 This cluster is connected to A541. 543 Two possible foreground E/S0 galaxies are located in the field of A543 defined as the circle of radius R_c centered on the cluster. 546 R_c is very restrictive. Foreground spiral galaxies are superimposed on a southern field of the cluster. 549 The cluster is sparse. 550 The photographic images of the stars as registered on the E-plate of the POSS are elongated in the field of A550 defined as the circle of radius R_c centered on the cluster. 551 A foreground SBc galaxy and b-galaxy are superimposed on the cluster. 558 A foreground Sab galaxy is superimposed on the cluster. 562 Two foreground spiral galaxies are superimposed on the cluster. 563 One foreground Sbc galaxy is superimposed on the cluster. 565 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. The galaxy which we identify as the second most luminous member (#2) is possibly a t-galaxy. A large foreground spiral galaxy is superimposed on the cluster. 568 Gemini cluster. Two possible foreground galaxies (E + S0/E) are located in the field of A568 defined as the circle of radius R_c centered on the cluster. The t-galaxy may be a pre-cD galaxy. 570 The cluster is sparse. Leir (1976) notes that there may be a possible misidentification and asks whether the ordinate of the cluster on plates of the POSS is Y = 120 mm. The original position for the cluster listed by Abell (1958) may actually be the position of a subcluster of galaxies in a larger cluster to the north of A570. 572 A foreground group of galaxies is superimposed on a northern region of the cluster. 573 The cluster is sparse. Leir (1976) notes that the cluster has possibly been mis-identified; we believe that the original coordinates are correct. 575 A background cluster is superimposed on a southeastern region of A575. 580 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 584 A possible foreground group of galaxies is located in the field of A584 defined as the circle of radius R_c centered on the cluster. The cluster looks closer than is indicated by distance class 6. 585 Four foreground galaxies are superimposed on the cluster. 586 The cluster is elongated with a position angle of major axis similar to that of the line connecting the two brightest members of the B_b cluster. 587 Two foreground spiral galaxies are superimposed on the cluster. 588 A foreground group of galaxies is superimposed on an eastern region of the cluster. 589 Two foreground elliptical galaxies are superimposed on the cluster. 590 Foreground diffuse spiral galaxies are superimposed on the southern part of the cluster. Defects on the E-plate of the POSS are located in the northern field of the cluster. 591 One foreground spiral galaxy is superimposed on the cluster. 593 Leir (1976) notes that the cluster does not look like a richness class 3 cluster. 594 A large foreground spiral galaxy is superimposed on the cluster. Foreground galaxies are possibly superimposed on the field of A594 defined as the circle of radius R_c centered on the cluster; it is difficult to separate populations. A594 looks like a cluster of distance class 5. 595 Possible foreground galaxies are located in the field of A595 defined as the circle of radius R_c centered on the cluster. 596 One foreground Sc galaxy is superimposed on the cluster. 597 The cluster seems more distant than is indicated by distance class 5. 599 A foreground SB galaxy is superimposed on the cluster. 600 A foreground SBc galaxy is superimposed on the cluster. 605 One foreground spiral galaxy is superimposed on the cluster. 606 The cluster is sparse. A foreground galaxy is superimposed on the southeastern part of the cluster. 610 Several possible foreground E or S0 galaxies are located in the field of A610 defined as the circle of radius R_c centered on the cluster. 611 The cluster is very faint. 612 One foreground elliptical galaxy is superimposed on the cluster. 613 A foreground Sa galaxy is superimposed on the southern part of the cluster. Three small subgroups of bright, mostly spiral galaxies are located in the cluster. 614 Two foreground spiral galaxies are superimposed on the cluster. 616 A foreground group of galaxies is superimposed on the cluster. 621 The cluster is elongated. A621 looks like a cluster of distance class 5. 626 Three foreground spiral galaxies are superimposed on an eastern region of the cluster. 627 A foreground group of galaxies is superimposed on the cluster. 632 Two foreground galaxies (S/S0 + I) are superimposed on the cluster. 634 Several possible foreground galaxies are located in the field of A634 defined as the circle of radius R_c centered on the cluster. 635 The cD_sp galaxy has several companion galaxies. Two foreground Sc galaxies are superimposed on the cluster. 640 The cluster is very faint. The rectangular coordinates of A640 as registered on plates of the POSS are X = 250 mm, Y = 180 mm [halfway between the coordinates listed by Leir (1976) and by Sastry & Rood (1971)]. 641 The cluster is sparse. The rectangular coordinates of the cluster as registered on plates of the POSS are X = 270 mm, Y = 125 mm. 642 The rectangular coordinates of the cluster as registered on plates of the POSS are X = 225 mm, Y = 195 mm according to Leir (1976). 643 A foreground spiral galaxy is superimposed on the cluster. 649 A foreground Sab galaxy is superimposed on the southeastern part of the cluster. The cluster is sparse. 650 R_c is restrictive. Two foreground galaxies are superimposed on a region near the center of the cluster. A foreground spiral galaxy is superimposed on the northern part of the cluster. 651 The galaxy which we identify as the second most luminous member of the cluster (#2) is connected by a tail of luminosity to a companion galaxy. 652 The cluster looks closer than is indicated by distance class 6. 655 Three b-galaxies are located near the cD galaxy. The locational surface distribution of observed galaxies in the cluster has a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 657 This cluster is connected to A658, a cluster of distance class 5. 660 A foreground group of galaxies is superimposed on the cluster. 661 A foreground group of galaxies is superimposed on the northern part of the cluster. 662 Three foreground galaxies are superimposed on the northern part of the cluster. 663 This cluster is connected to A668. Is A663 closer than is indicated by distance class 6? 665 This cluster is a good example of a cluster characterized by three large, distinct subclumps of galaxies. 667 The core of the cluster is compact. Is A667 a pre-cD cluster? A defect on the E-plate of the POSS which looks like a b-galaxy is located in a field near the center of the cluster. 668 Leir's (1976) R_c is too large because part of A663 is included in the circle of radius R_c centered on A668. 670 The cluster is compact. 671 The cluster membership is about half spiral galaxies, half S0 + E galaxies. 673 Two foreground spiral galaxies are superimposed on the cluster. 674 The cluster is sparse. 675 The southern subcluster is possibly closer than the northern subcluster. 679 The cluster is elongated. A foreground group of galaxies is superimposed on the cluster. 680 The galaxy which we identify as the most luminous member of the cluster (#1) has a curious elongated shape. 683 Two foreground galaxies (S + E/S0) are superimposed on the cluster. 684 One foreground Sc galaxy is superimposed on the cluster. 685 Two foreground spiral galaxies are superimposed on the cluster. 688 It is difficult to separate populations of galaxies. 690 Two foreground galaxies (Sb + E/S0) are superimposed on the cluster. 691 A foreground group of spiral galaxies is superimposed on the cluster. 693 R_c is restrictive. 694 The rectangular coordinates of the cluster as registered on plates of the POSS are X = 250 mm, Y = 313 mm. Galaxies in the western part of A694 are part of A695. 695 A foreground group of galaxies is superimposed on northern and eastern regions of the cluster. 699 The galaxy which we identify as the most luminous member of the cluster (#1) is a spiral galaxy with two satellite galaxies. Leir (1976) notes that a bright object is located in the foreground of a southern region of the cluster. 700 The distance class of the cluster is D=7. 701 The cluster is very faint. 702 Several probable foreground spiral galaxies are located in the field of A702 defined as the circle of radius R_c centered on the cluster. 703 Subclusters of galaxies are elongated and approximately parallel to each other. 705 Is A705 a cD cluster in the making? 708 Two foreground galaxies are superimposed on the northwestern part of the cluster. 709 The galaxy which we identify as the most luminous member of the cluster (#1) is located at the center of the cluster. 711 Several foreground galaxies are superimposed on the eastern and southern parts of the cluster. 713 A foreground Sc galaxy is superimposed on the cluster. 714 The cluster is rich in spiral galaxies. Four foreground spiral or S/S0 galaxies are superimposed on a northern region of the cluster. 718 Is the cluster more distant than is indicated by distance class 5? Four foreground spiral galaxies are superimposed on the cluster. 719 The cluster is compact. 720 Two foreground galaxies (E + S) are superimposed on the eastern part of the cluster. 721 Clumps of galaxies are elongated and approximately parallel to each other. 723 Two foreground spiral galaxies are superimposed on the cluster. 724 Two foreground galaxies (E + S) are superimposed on the cluster. The locational surface distribution of galaxies in the cluster has a position angle of major axis similar to the position angle of the line connecting the components of the two brightest members of the B cluster. 725X This cluster is the nearer of two clusters with the locational coordinates specified by Abell (1958). Is A725X a foreground group of galaxies superimposed on A725?. 726 Two foreground spiral galaxies are superimposed on the cluster. 727 Two bright foreground galaxies (bp + Scd) are superimposed on the cluster. A foreground group of spiral and S0 galaxies overlaps the cluster. 728 A possible foreground group of galaxies is located in the field of A728 defined as the circle of radius R_c centered on the cluster. A728 looks closer than is indicated by distance class 6. 730 The cluster is very elongated in the approximately north-south direction. 732 A foreground S0 galaxy is superimposed on the southwestern part of the cluster. The b-galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 733 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 734 Faint galaxies are distributed possibly in a "spiral" pattern around the cD galaxy. The cluster is possibly closer than is indicated by distance class 6. 735 The cluster is very open. 736 R_c is restrictive. 737 A foreground group of several spiral galaxies is superimposed on the cluster. 738 The cluster is compact. Several subclusters of faint galaxies are located in the cluster. 739 The cluster is elongated and contains subclusters of galaxies. Leir (1976) notes that A739 is possibly connected to a cluster to its northwest. 740 A foreground SBc galaxy is superimposed on the cluster. 741 A foreground Scd galaxy is superimposed on a region near the center of the cluster. 743 This cluster is a good example of an F cluster with three subclusters of galaxies. 744 The RS type of the cluster is probably C9 because the galaxy which we first identified as the most luminous member of the cluster (#1) is actually a foreground galaxy superimposed on the cluster (Kurtz, M. J., Huchra, J. P., Beers, T. C., Geller, M. J., Gioia, I., Maccacaro, T., Schild, R., and Stauffer, J. R. 1985, A. J., 90,1665). The galaxy which we identify as the second most luminous member (#2) has several companion galaxies. 746 A faint and diffuse foreground galaxy (morphological type IB) is superimposed on the northern part of the cluster. 748 The cluster is possibly elongated with a position angle of major axis similar to that of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). 750 The locational surface distribution of galaxies in the cluster has a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. 752 Several foreground galaxies are superimposed on a region near the periphery of the cluster. 755 A chain of galaxies is located in the cluster. 756 The cluster is sparse. The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 757 One foreground spiral galaxy is superimposed on the cluster. 762 Two foreground galaxies (S0 + SBc) are superimposed on the cluster. 763 Three foreground spiral galaxies are superimposed on a southern region of the cluster. 764 A possible foreground group of galaxies is located in the field of A764 defined as the circle of radius R_c centered on the cluster. Is A764 closer than is indicated by distance class 6? 765 A large foreground Sc galaxy is superimposed on the cluster. 766 One foreground spiral galaxy is superimposed on the cluster. 770 The cluster is sparse. A foreground b-galaxy is superimposed southwest of A770 defined as the circle of radius R_c centered on the cluster. 771 The cluster is very sparse. 772 The cluster is faint. 773 The cluster is dense and compact. 774 A possible foreground S/S0 galaxy is located in the field of A774 defined as the circle of radius R_c centered on the cluster. 775 The RS type of the cluster is possibly cD. 776 The cluster is elongated in the approximately east-west direction. The shape of the cluster is very regular. 780 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) (which constitute the two brightest members of the B cluster) are connected to each other by a bridge of galaxies. 783 The cluster is elongated. 784 Three foreground galaxies are superimposed around the periphery of the cluster. 790 The galaxy which we identify as the second most luminous member of the cluster (#2) is connected by tails of luminosity to companion galaxies. A small foreground group of galaxies is superimposed on the western part of the cluster. 792 A possible more distant group of galaxies is located in the field of A792 defined as the circle of radius R_c centered on the cluster. 793 The cluster is very sparse. Two foreground spiral galaxies are superimposed on the cluster. 796 A possible subgroup of galaxies is located in the northeastern part of the cluster. A796 looks closer than is indicated by distance class 6. Two foreground galaxies (SB + S0) are superimposed on the cluster. 797 The galaxy which we identify as the most luminous member of the cluster (#1) has luminous "tails". One foreground spiral galaxy is superimposed on the cluster. 799 Two foreground galaxies are superimposed on the western part of the cluster. 800 Foreground galaxies are superimposed on the northern part of the cluster. 802 The cluster is elongated. A foreground P-galaxy is superimposed on the cluster. 803 The cluster is very sparse. Two foreground S/S0 galaxies are superimposed on the cluster. 804 A foreground group of galaxies is superimposed on the eastern part of the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is not the galaxy which Leir (1976) assumes is the most luminous member of the cluster. 805 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. Foreground galaxies are superimposed on the southern subcluster of galaxies. 807 The cluster is elongated in the approximately north-south direction. 809 A foreground spiral galaxy is superimposed on the cluster. 812 The envelope of luminosity on the cD galaxy contains a "hole" or gap; it has a curious appearance. 814 The locational surface distribution of galaxies in the cluster has a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. One possible foreground spiral galaxy is located in the field of A814 defined as the circle of radius R_c centered on the cluster. 816 The cluster contains several radially directed chains of galaxies. 818 One foreground SBc galaxy is superimposed on the cluster. 819 Is the cluster closer than is indicated by distance class 5? 820 This cluster is connected to A827. 821 Two populations of galaxies are located in the field of A821 defined as the circle of radius R_c centered on the cluster; it is difficult to separate these populations. 822 The cD galaxy has a faint, elongated envelope of luminosity. 823 The cluster is very faint. A foreground group of galaxies is superimposed on the eastern part of the cluster. 825 The distance class of the cluster is D=7. Possible foreground galaxies are located in the field of A825 defined as the circle of radius R_c centered on the cluster. 826 R_c' is restrictive. 827 This cluster is connected to A820 and A831. 828 The cluster is very sparse. A possible more distant cluster is located in the southern part of the cluster. 829 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 831 This cluster is connected to A827. 832 The photographic plate is foggy; the cluster is very sparse or very distant (distance class 6). 835 Several spiral galaxies are located in the cluster. 836 A foreground group of galaxies overlaps the cluster. 837 The cluster is elongated. 838 V 116 is to the northeast and a bright group is to the northwest of the cluster. The Abell cluster is probably the superposition of two clusters located at different distances along the line-of-sight. 839 The RS type of the cluster is possibly I_s. A foreground b-galaxy and several spiral galaxies are superimposed on the cluster. 840 One subcluster of galaxies contains four b-galaxies. Probable foreground galaxies are located in the field of A840 defined as the circle of radius R_c centered on the cluster. 841 It is difficult to separate foreground galaxies from members of the cluster. 842 It is difficult to separate foreground galaxies from members of the cluster. 843 A secondary maximum is present in the radial distribution of surface number density of observed galaxies in the cluster. 845 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 846 The galaxy which we identify as the most luminous member of the cluster (#1) has several companion galaxies. 847 The cluster is elongated in the approximately east-west direction. 849 A foreground group of five spiral galaxies is superimposed on the cluster. 850 A foreground group of galaxies is superimposed on the western part of the cluster. 851 The distance class of the cluster is D=7. 854 The cluster is faint and compact. R_c is restrictive if the cluster to the northeast of the field of A854 (defined circle of radius R_c centered on the cluster) is actually a part of A854. Two foreground galaxies are superimposed on the eastern part of the cluster. 855 A foreground group of galaxies is superimposed on the western part of the cluster. A secondary maximum is evident in the radial distribution of surface number density of observed galaxies in the cluster. 859 A probable background C10 cluster is located in the center of the field of A859 defined as the circle of radius R_c centered on the cluster. 861 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. 862 A foreground irregular galaxy is superimposed on the northeastern part of the cluster. An S0 galaxy is located in the southern part of the cluster. 864 The cluster is very faint. Several defects on the E-plate of the POSS are located in the field of A864 defined as the circle of radius R_c centered on the cluster. 865 A probable background cluster is located in a southern field of A865. 872 A foreground group of galaxies is superimposed on the cluster. A872 looks closer than is indicated by distance class 6. 873 Is the cluster closer than is indicated by distance class 6? 877 Is the cluster closer than is indicated by distance class 6? 878 The galaxy which we identify as the most luminous member of the cluster (#1) has a luminous jet. The cluster contains several S/S0 galaxies. 880 The galaxies which we identify as the first and second most luminous member of the cluster (#1 and #2) each have large envelopes of luminosity. A foreground group of galaxies is superimposed on the western part of the cluster. 881 R_c is restrictive. 883 A possible background B cluster is located in a northwestern field of A883. 884 Two foreground spiral galaxies are superimposed on the cluster. 885 The cluster is compact. The galaxy which we identify as the third most luminous member of the cluster (#3) has a faint companion galaxy. R_c is possibly restrictive because possible subclusters of galaxies are located to the southwest and northwest of the circle of radius R_c centered on A885. 887 The cluster is sparse. Foreground galaxies are superimposed on the southern part of the cluster. 888 Several foreground galaxies are superimposed on the eastern part of the cluster. 892 One foreground spiral galaxy is superimposed on the cluster. 893 Leir (1976) notes that the cluster is characterized by two subclumps of galaxies connected to each other by a bridge of galaxies. Four foreground galaxies (Sbc + E + 2 S) are superimposed on the cluster. A893 is connected to A894. 894 A foreground group of galaxies is superimposed on the western part of the cluster. A894 is connected to A893. 895 This cluster is possibly connected to A898. 896 The cluster is characterized by very tight subclusters of galaxies. A foreground group of galaxies is superimposed on the cluster. The cluster is possibly closer than is indicated by distance class 5. 897 The RS type of the cluster is possibly F (C4+I). 898 This cluster is possibly connected to A895. 901 The cluster is sparse. A901 is possibly connected to A902. 902 The cluster is sparse. A902 is connected to A901. 904 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 906 A foreground b-galaxy is superimposed on the cluster. 908 The distance class of the cluster is D=7. A908 is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 909 Several foreground galaxies overlap the cluster. 912 A possible foreground lenticular galaxy is located in the field of A912 defined as the radius R_c centered on the cluster. 914 This cluster is connected to A922. 915 One foreground spiral galaxy is superimposed on the cluster. 916 A foreground group of galaxies overlaps the cluster. 917 Two foreground galaxies are superimposed on the southeastern part of the cluster. 919 The locational surface distribution of most galaxies in the cluster has a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. 920 Three foreground spiral galaxies are superimposed on the cluster. 922 This cluster is connected to A914. 923 The galaxy which we identify as the most luminous member of the cluster (#1) has many companion galaxies. 924 A defect on the E-plate of the POSS is located in a northern field of A924. 925 The cluster is characterized by three main clumps of bright galaxies. 926 R_c is restrictive because many other subclusters of galaxies are located out to a radius of 20 mm from the cluster center. 927 A chain of galaxies is located in the northern part of the cluster. 928 One foreground spiral galaxy is superimposed on the cluster. 930 A possible foreground Sc galaxy is located in the field of A930 defined as the circle of radius R_c centered on the cluster. A930 is closer than is indicated by distance class 5. 931 The cluster is compact. The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. 933 A possible foreground group of galaxies is located in a southern field of the cluster. 935 One foreground spiral galaxy is superimposed on the cluster. 937 Two foreground spiral galaxies are superimposed on a northeastern region of the cluster. 938 Two foreground Sc galaxies are superimposed on the cluster. 940 The cluster is sparse. Foreground galaxies are superimposed on the cluster. A large foreground Sc galaxy is superimposed on the eastern part of the cluster. A crowded star field is superimposed on the cluster. 941 One foreground spiral galaxy is superimposed on the cluster. 942 Two possible foreground spiral galaxies are located in the field of A942 defined as the circle of radius R_c centered on the cluster. 944 One foreground SBab galaxy is superimposed on the cluster. 945 A foreground Sbc galaxy is superimposed on the cluster. 951 The cluster is sparse but elongated with a position angle of major axis similar to that of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). 953 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. 954 The cluster is closer than is indiated by distance class 5. 958 The cluster is very faint. The galaxy which we identify as the most luminous member of the cluster (#1) is located at center of the cluster. Two foreground galaxies are superimposed on the northern part of the cluster. 960 Two foreground spiral galaxies are superimposed on the cluster. A960 is more distant than is indicated by distance class 5. 962 The cluster is closer than is indicated by distance class 5. 963 One probable foreground spiral galaxy is located in the field of A963 defined as the circle of radius R_c centered on the cluster. 964 Three foreground spiral galaxies are superimposed on the cluster. 965 This cluster is a good, uncluttered example of an I_c cluster. A965 looks closer than is indicated by distance class 6. 967 Two foreground spiral galaxies are superimposed on the cluster. 968 A foreground group of galaxies is superimposed on the southern part of the cluster. 975 Two foreground spiral galaxies are superimposed on the cluster. 976 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy's asymmetric envelope of luminosity. 978 A spiral pattern of galaxies is around the cD galaxy. 980 The cluster looks closer than is indicated by distance class 6. 981 The cluster is elongated. A981 overlaps A998. 982 The cluster is elongated with a position angle of major axis similar to the position angle of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). 983 Two bright foreground galaxies overlap the cluster. 984 The seven most luminous galaxies in the cluster all have roughly the same magnitude; it is difficult to identify the first, second, and third most luminous members of the cluster (#1, #2, and #3). A defect on the E-plate of the POSS is located in the southern field of A984. 985 A chain of galaxies is located in a southern region of the cluster. 986 The cluster contains three main concentrations of galaxies. A possible defect on the E-plate of the POSS is located in a western clump of the cluster. 988 The cluster is faint. 989 Two foreground spiral galaxies are superimposed on the cluster. 992 Three foreground galaxies are superimposed on the western part of the cluster. 994 Foreground galaxies are superimposed on the cluster; it is difficult to separate populations. A994 looks nearer than is indicated by distance class 6. 995 This cluster is connected to A997. One foreground spiral galaxy is superimposed on the cluster. 997 Three foreground galaxies (E + 2 Sbc) are superimposed on the cluster. 998 The galaxy which we identify as the most luminous member of the cluster (#1) has an S0 companion galaxy. R_c is too large because it includes parts of A981 and A1005. 1000 If the Abell cluster a single cluster, then it is very elongated in the approximately east-west direction and is possibly connected to A1002. 1001 A1001 overlaps A993, a cluster of distance class D=3. 1002 This cluster is possibly connected to A1000. 1003 The B_b cluster is the more distant of the two clusters with the locational coordinates specified by Abell (1958); the I_s cluster is closer than is indicated by distance class 5. 1009 This cluster overlaps A1013. 1010 A possible background cluster is located in the field of A1010 defined as the circle of radius R_c centered on the cluster. 1011 The cluster is faint and compact. 1012 The cluster is sparse, but it is a good example of an I_c cluster. 1013 Foreground galaxies are superimposed on the northern and western parts of the cluster. 1016 The cluster contains many lenticular galaxies. 1017 A foreground b-galaxy is superimposed on the northwestern part of the cluster. The cluster is sparse and faint. 1018 R_c is restrictive. A large foreground Sbc galaxy, b-galaxy, and several spiral galaxies are superimposed on the cluster. 1019 The cluster is sparse, but nevertheless, it is a good example of an I_c cluster. Leir (1976) notes that the cluster has three concentrations of galaxies. 1021 A probable foreground spiral galaxy is located in the field of A1021 defined as the circle of radius R_c centered on the cluster. 1022 One foreground spiral galaxy is superimposed on the cluster. 1024 The RS type of the cluster is possibly L7. One foreground spiral galaxy is superimposed on the cluster. 1026 The galaxy which we identify as the most luminous member of the cluster (#1) has several companion galaxies. Leir (1976) notes that A1026 overlaps the distance class 3 cluster A1035. 1027C The RS type of the cluster is possibly L5. 1028 Is the cluster closer than is indicated by distance class 5? 1034 R_c is probably restrictive because a probable subcluster of galaxies is located to the southwest of the circle of radius R_c centered on A1034. 1035 The RS type of the cluster is F because it contains "two adjacent clumps of core galaxies" (Rood and Sastry 1971). 1036 Several foreground galaxies are superimposed on the western part of the cluster. 1037 The cluster is sparse. 1038 The cD galaxy has an asymmetric envelope of luminosity. 1039 The cluster is sparse. A bright foreground Sp galaxy is superimposed on a region near the center of A1039. 1040 A foreground elliptical galaxy is superimposed on the cluster. 1041 The RS type of the cluster is possibly I_c. A foreground elliptical galaxy is superimposed on the cluster. 1042 A foreground group of galaxies is superimposed on a northern region of the cluster. 1043 A foreground S/S0 galaxy is superimposed on the cluster. A northwestern region of A1043 overlaps a nearer cluster. 1044 R_c is restrictive because apparent members of A1044 are located to the south of the circle of radius R_c centered on the cluster. Two foreground galaxies (S0 + diffuse S:) are superimposed on the cluster. 1048 A foreground group of galaxies is superimposed on a northwestern region of A1048. 1049 Is the cluster possibly a subcluster of A1046? 1050 The cD_np galaxy may represent an early stage of a cD galaxy in the making. Four foreground spiral galaxies are superimposed on the cluster. 1051 Several foreground galaxies are superimposed on a region at the periphery of the cluster. 1052 The cluster is sparse. 1053 One foreground spiral galaxy is superimposed on the cluster. 1054 One foreground SBc galaxy is superimposed on the cluster. 1055 A large foreground spiral galaxy is superimposed on the cluster. 1056 A large foreground SBcd galaxy is superimposed on the cluster. 1057 Two foreground spiral galaxies are superimposed on the cluster. 1060 Hydra I cluster. 1061 Jets of luminosity radiate 30 degrees apart from the galaxy which we identify as the third most luminous member of the cluster (#3). The major axes of the two L clusters are parallel. 1062 One probable foreground spiral galaxy is located in the field of A1062 defined as the circle of radius R_c centered on the cluster. 1063 The Abell cluster is probably the superposition of two clusters located at different distances along the line-of-sight. Several foreground spiral galaxies are superimposed on the cluster. 1066 The cluster is closer than is indicated by distance class 5. 1068 Two foreground spiral galaxies are superimposed on the cluster. The cD galaxy has several satellite galaxies. 1074 The cluster is elongated in the approximately east-west direction. A1074 is connected to A1077. 1076 One foreground E/S0 galaxy is superimposed on the cluster. 1077 The galaxy which we identify as the most luminous member of the cluster (#1) is located near center of the cluster. A1077 is connected to A1074. 1078 A possible foreground SBc glaxy is located in the field of A1078 defined as the circle of radius R_c centered on the cluster. 1079 One foreground spiral galaxy is superimposed on the cluster. 1082 The cluster is sparse. 1083 The cluster is very sparse. 1084 Two foreground spiral galaxies are superimposed on the cluster, one on an eastern region and one on a northern region. 1085 One foreground SBc galaxy is superimposed on the cluster. 1086 A large foreground SBc galaxy with a companion galaxy is superimposed on the western part of the cluster. 1089 Foreground galaxies are superimposed on the southern part of the cluster. 1091 A foreground spiral galaxy is superimposed on the southwestern part of the cluster. 1092 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. A1092 looks like a distance class 5 cluster. 1093 Six galaxies have similar luminosities; therefore it is difficult to identify the first, second, and third most luminous members of the cluster (#1, #2, and #3). 1094 The galaxy which we identify as the most luminous member of the cluster (#1) is located in the northern part of the cluster. 1097 The cluster is characterized by three collinear clumps of galaxies, each of type B_b. 1099 A foreground SBc galaxy is superimposed on the cluster. 1100 Possible foreground spiral galaxies are located in the field of A1100 defined as the circle of radius R_c centered on the cluster. 1101 The galaxy which we identify as the most luminous member of the cluster (#1) is connected by a bridge of luminosity to each of two faint companion galaxies. R_c is too large because A1101 overlaps A1106. 1104 It is probable that a foreground group of galaxies is located south of the cluster. 1106 Leir (1976) identified the cluster incorrectly; the rectangular coordinates of the cluster as registered on plates of the POSS which he adopts for A1106 are actually the rectangular coordinates for A1101; the BM type and radius R_c derived by Leir (1976) for A1106 are probably incorrect; we estimate that the cluster is BM type III with radius R_c = 10 mm. 1107 Leir (1976) does not note that the galaxy which he identifies as the most luminous member of the cluster is a b-galaxy. 1108 The cluster is closer than is indicated by distance class 5. 1109 Four foreground galaxies (3 S + P) are superimposed on the cluster. 1111 The galaxy which we identify as the most luminous member of the cluster (#1) has three faint, close companion galaxies. 1112 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. A large foreground spiral galaxy is superimposed on a region near the center of the cluster. A chain of eight galaxies is located in the southern part of the cluster. 1113 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. 1114 Two foreground spiral galaxies are superimposed on the cluster. 1115 This cluster is connected to A1121. 1116 One foreground spiral galaxy is superimposed on the cluster. 1118 A foreground group of galaxies is superimposed on the cluster. A1118 is connected to A1122. 1119 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. A1119 looks closer than is indicated by distance class 6. 1121 The cluster is very elongated in the approximately east-west direction. A1121 is connected to A1115. 1122 This cluster is connected to A1118. A foreground group of galaxies is superimposed on the cluster. 1124 A foreground group of galaxies is superimposed on the cluster. 1125 The cluster is elongated. 1126 Two large foreground galaxies (S + Ir) are superimposed on the cluster. 1128 Two foreground spiral galaxies are superimposed on the cluster. 1130 Several tight subclusters of galaxies characterize the cluster. 1131 Two foreground spiral galaxies are superimposed on the cluster. 1132 The galaxy which we identify as the most luminous member of the cluster (#1) is separated from a satellite galaxy by 0.20 mm on plates of the POSS. Two foreground galaxies (S + P) are superimposed on the cluster. A probable foreground group is located in a southeastern field of the cluster. 1133 The cluster is compact. A foreground group of galaxies is superimposed on the eastern part of the cluster. 1136 A defect on the E-plate of the POSS is located near the center of the cluster. 1137 Two foreground galaxies (S + E/S0) are superimposed on the cluster. 1138 A foreground b-galaxy and spiral galaxy are superimposed on the southwestern part of the cluster. 1139 The cluster is rich in spiral galaxies. 1140 A foreground galaxy is superimposed on a region near the center of the cluster. 1141 Two foreground galaxies (Sc + E) are superimposed on the cluster. 1142 The cluster is not type B as listed by Rood and Sastry (1971) because other galaxies are as bright as (and one is brighter than) the b-galaxy which Rood and Sastry (1971) assumed to be the two brightest members of a B cluster. 1143 An "arm" of galaxies is located in a northern region of the cluster. 1144 Two foreground spiral galaxies are superimposed on the cluster. 1145 Four foreground lenticular galaxies are superimposed on the cluster. 1146 The locational surface distribution of galaxies in the cluster is slightly elongated. 1147 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. 1148 R_c is restrictive. Several foreground spiral galaxies are superimposed on the cluster. 1149 The cD galaxy is a nest of two b-galaxies in a common envelope of luminosity (four distinct galaxies); the components of the b-galaxies are separated on plates of the POSS by 0.15 mm and 0.13 mm, respectively, and the b-galaxies themselves are separated by 0.25 mm. 1150 A foreground S/S0 galaxy is superimposed on the cluster. 1151 This cluster is a good example of an I_c cluster. A1151 looks closer than is indicated by distance class 6. 1153 Three foreground galaxies are superimposed on the western part of the cluster. 1154 R_c is restrictive because a subcluster of galaxies is located to the northwest of the circle of radius R_c centered on the cluster. 1155 Three foreground spiral galaxies are superimposed on the cluster. 1156 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the elongated cluster. 1161 Several probable foreground galaxies are located north and east of the cluster. 1163 A possible foreground group of galaxies is located in the field of A1163 defined as the circle of radius R_c centered on the cluster. 1164 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1166 The six b-galaxies are located in a southern region of the cluster. 1168 A foreground spiral galaxy is superimposed on the cluster. 1169 The cluster is closer than is indicated by distance class 5. 1170 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. 1175 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. 1176 Two foreground galaxies and a foreground diffuse object are superimposed on the western part of the cluster. 1178 A foreground group of galaxies overlaps the southern part of the cluster. 1183 The galaxy which we identify as the most luminous member of the cluster (#1) is separated from a faint companion galaxy by 0.17 mm on plates of the POSS. A foreground Sc galaxy is superimposed on the cluster. 1184 The cluster is very faint. 1185 Leo A cluster. There is a possible circumferential alignment of galaxies with respect to the center of the cluster. 1189 A foreground spiral galaxy is superimposed on the cluster. 1191 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster and is connected by a bridge of luminosity to each of two faint companion galaxies. 1192 The cluster contains many bright spiral galaxies; it is difficult to identify the first, second, and third most luminous members of the cluster (#1, #2, and #3). Foreground galaxies are superimposed on the eastern and northeastern parts of the cluster. 1193 A possible background cluster is located in a field near the center of A1193. 1194 The cluster looks closer than is indicated by distance class 6. The galaxy which we identify as the second most luminous member of the cluster (#2) is connected by a bridge of luminosity to each of two companion galaxies. A1194 is connected to A1198. 1195 R_c is restrictive. A foreground S/S0 galaxy is superimposed on the cluster. A more distant cluster is superimposed on the northeastern part of A1195. 1197 The cluster is closer than is indicated by distance class 5. 1198 This cluster is connected to A1194. A foreground group of galaxies is superimposed on A1195. 1202 Three foreground galaxies (S + 2 E) are superimposed on the cluster. 1204 A foreground group of galaxies is superimposed on the southern part of the cluster. 1206 It is difficult to separate a foreground group of galaxies from the population of galaxies in the southern part of the cluster. 1208 A large foreground galaxy is superimposed on the southwestern part of the cluster. 1209 A large foreground S0 galaxy is superimposed on the cluster. 1210 A foreground spiral galaxy is superimposed on a region near the center of the cluster. 1211 The galaxy which we identify as the most luminous member of the cluster (#1) is surrounded by many faint galaxies, has an envelope of luminosity, and is possibly a cD galaxy. 1213 Leo B cluster. Several foreground galaxies with a redshift z=0.028 (Hintzen 1980, Astron. J, 85, 626) are superimposed on the cluster. 1214 A foreground group of galaxies is superimposed on the cluster. 1215 Two foreground spiral galaxies are superimposed on the cluster. A possible background cluster is located in a southern field of A1215. 1217 The galaxy which we identify as the most luminous member of the more distant cluster (#1) is connected to a small chain of galaxies. 1217X This cluster is the nearer of two clusters with the locational coordinates specified by Abell(1958). The galaxy which we identify as the second most luminous member of the cluster (#2) is connected by a bridge of luminosity to a faint companion galaxy. 1219 R_c is restrictive. The RS type of the cluster is possibly F (C8 + C6) because two possible subclusters of galaxies are located the northeastern and southwestern parts of the cluster. The galaxies which we identify as the first and third most luminous members of the cluster (#1 and #3) have faint companion galaxies. 1220 This cluster is the more distant of two clusters with the locational coordinates specified by Abell (1958). Foreground galaxies are superimposed on the cluster. 1220X This cluster is the nearer of two clusters with the locational coordinates specified by Abell (1958). Is the distance class possibly D=5? 1223 Four foreground spiral galaxies are superimposed on the cluster. 1225 Three foreground galaxies and a possible background cluster are located in the field of A1225 defined as the circle of radius R_c centered on the cluster. 1226 A foreground spiral galaxy is superimposed on the cluster. 1228 A possible background cD cluster is located in the field of A1228 defined as the circle of radius R_c centered on the cluster. 1230 A foreground P galaxy is superimposed on the cluster. The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 192 mm, Y = 136 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1231 A foreground S0 galaxy is superimposed on the cluster. 1234 The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 183 mm, Y = 85 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). A1234 is connected to A1246. 1235 Two stars are superimposed on the cD galaxy. Is the cluster closer than is indicated by distance class 5? 1236 Is the cluster closer than is indicated by distance class 5? 1237 This cluster is connected to A1253. 1239 Foreground galaxies are superimposed on the southern and eastern parts of the cluster. 1241 Two foreground galaxies are superimposed on the northeastern part of the cluster. 1243 This cluster is a good example of an I_c cluster. Possible foreground galaxies are located in the field of A1243 defined as the circle of radius R_c centered on the cluster. 1244 Foreground galaxies are superimposed on the cluster. 1245 A foreground group of spiral galaxies is superimposed on the cluster. 1246 The cluster is elongated. A1246 is connected to A1234. The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 164 mm, Y = 89 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1247 A foreground group of galaxies is superimposed on an eastern region of the cluster. 1252 A background cluster and large foreground SBc galaxy are superimposed on A1252. 1253 This cluster is connected to A1237. The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) have faint companion galaxies. 1255 One foreground spiral galaxy is superimposed on the cluster, as noted previously by Leir (1976). 1257 Are possible foreground groups superimposed on the cluster? 1258 The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 140 mm, Y = 302 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1260 A foreground group of spiral galaxies is superimposed on the western part of the cluster. 1262 Foreground galaxies are superimposed on the cluster; it difficult to separate populations. 1264 Two foreground groups of galaxies are superimposed on a southern region of the cluster. 1265 The cluster is faint. Two foreground galaxies are superimposed on the eastern part of A1265. 1266 Three foreground spiral galaxies are superimposed on the cluster. 1268 The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 110 mm, Y = 218 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1269 A foreground group of galaxies is superimposed on the northeastern part of the cluster. A possible foreground group of galaxies is superimposed on the cluster. 1271 R_c is restrictive. 1272 Each of two brightest members of the B_b cluster is separated from a companion galaxy by 0.1 mm on plates of the POSS. The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 97 mm, Y = 215 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1274 Four foreground galaxies (3 S + S0) are superimposed on the cluster. 1275 A possible foreground Sbp galaxy is located in the field of A1275 defined as the circle of radius R_c centered on the cluster. 1276 A foreground group of galaxies is superimposed on the eastern and southern parts of the cluster. 1277 The cluster is very faint. The b-galaxy is very bright and may be a possible foreground galaxy located in the field of A1277 defined as the circle of radius R_c centered on the cluster. 1278 The cluster is very elongated. The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 86 mm, Y = 37 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1279 Three foreground spiral galaxies are superimposed on the cluster. 1280 This cluster is connected to A1284. 1282 Possible foreground galaxies are located in the field of A1282 defined as the circle of radius R_c centered on the cluster. 1283 This cluster is very close to A1289 causing possible confusion in determining the membership of both clusters. 1284 Possible foreground galaxies are located in the field of A1284 defined as the circle of radius R_c centered on the cluster. A1284 is connected to A1280. 1285 Each of the two brightest members of the B cluster has a companion galaxy. One foreground Sc galaxy is superimposed on the cluster. 1286 The cluster is elongated. Three foreground galaxies are superimposed on the western part of the cluster. The rectangular coordinates of the cluster as registered on plate E1353 of the POSS are X = 80 mm, Y = 139 mm because the plate center is incorrectly listed in the information booklet National Geographic Society and Palomar Observatory Sky Survey Catalogue of Plates 1960 which is provided with the print collection and contains basic information about the POSS; the equatorial coordinates of the correct E1353 plate center are RA = 11h20.6m, DEC = 23d17.8' (epoch 1950). 1288 The cluster is elongated in the approximately north-south direction. 1289 This cluster is a companion of A1283. A foreground SBc galaxy is superimposed on A1289. 1290 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1291 The cluster is rich in S/Ir galaxies and contains several peculiar galaxies. 1292 This cluster is connected to A1304. Several foreground galaxies are superimposed on A1292. 1293 The cluster is a possible cD cluster. A1293 is elongated with a position angle of major axis similar to that of the envelope of luminosity on the galaxy which we identify as the most luminous member of the cluster. A large foreground SBc galaxy is superimposed on the eastern part of the cluster. 1294 A small subcluster of galaxies is located in the southwestern part of the cluster. There is some overlap of A1294 with the distance class 3 cluster A1270. 1303 Subclusters of galaxies in the cluster are elongated in the approximately north-south direction. Several foreground spiral galaxies are superimposed on the northern part of the cluster. A1303 is very faint. 1304 This cluster is connected to A1292. A foreground Sp galaxy is superimposed on the northwestern part of the cluster. A large Sb galaxy is superimposed on the southwestern part of the cluster. 1305 One foreground Sp galaxy is superimposed on the cluster. 1306 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1312 Subclusters of galaxies are elongated in the approximately east-west direction. The galaxy which Leir (1976) assumes is the most luminous member of the cluster is a probable foreground galaxy located in the field of A1312 defined as the circle of radius R_c centered on the cluster. The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) have companion galaxies. 1313 A possible more distant L cluster is located in a field near the center of A1313. 1316 The cluster is sparse. Is A1316 closer than is indicated by distance class 6? 1318 Three possible foreground galaxies are located in the field of A1318 defined as the circle of radius R_c centered on the cluster; therefore, the galaxies which we identify as the three most luminous members of the cluster have uncertain separations (r_ij where ij=12,13,23, respectively). 1319 The cluster is elongated. A1319 is connected to A1326. 1320 The cluster is sparse. Foreground galaxies are superimposed on the eastern and northeastern parts of A1320. 1322 Four foreground spiral galaxies are superimposed on the cluster. 1324 A foreground S0/a is superimposed on the cluster. 1326 This cluster is connected to A1319. 1327 The cluster is sparse. R_c is probably restrictive because a probable subcluster of galaxies is located to the northwest of the circle of radius R_c centered on A1327. 1328 A foreground b-galaxy is superimposed on the cluster. 1330 A faint chain of galaxies is located in the southern part of the cluster. 1331 The C6 subcluster of galaxies is compact and elongated in the approximately east-west direction. The E-plate of the POSS which registers A1331 is poorly focused. 1332 Several foreground galaxies (S + E) are superimposed on the cluster. 1335 Two foreground Sp galaxies are superimposed on the cluster. 1336 Two possible foreground galaxies (S + SBbc) are located in the field of A1336 defined as the circle of radius R_c centered on the cluster. 1337 Two foreground spiral galaxies are superimposed on the cluster. 1339 The cluster is sparse. Two bright foreground spiral galaxies with faint companion galaxies are superimposed on the cluster. It is difficult to separate populations of galaxies. 1340 One foreground S/S0 galaxy is superimposed on the cluster. 1341 The cluster looks closer than is indicated by distance class 6. There is possible confusion of A1341 with A1342, A1345, and A1351. 1343 A foreground group of galaxies is superimposed on a western region of the cluster. 1344 A foreground S0 galaxy is superimposed on an eastern region of the cluster. 1350 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. Two foreground spiral galaxies are superimposed on the northern part of the cluster. 1351 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1353 A possible foreground b-galaxy is located in the field of A1353 defined as the circle of radius R_c centered on the cluster. A peculiar star-like object with a jet of luminosity is located in a southeastern field of the cluster. 1354 A foreground group of spiral galaxies is superimposed on a northern region of the cluster. 1355 A foreground group of galaxies is superimposed on the southern part of the cluster. 1356 A foreground group of E/S0 galaxies is superimposed on the cluster. 1359 Four foreground spiral galaxies are superimposed on the cluster. 1361 The cD galaxy has an asymmetric envelope of luminosity. 1364 Two foreground galaxies (E + SBb) are superimposed on the cluster. 1366 A foreground S0/a galaxy is superimposed on the cluster. 1369 Possible foreground galaxies are located in a field of A1369 defined as the circle of radius R_c centered on the cluster. 1370 Both subclusters of galaxies are sparse. 1371 The major axis of the locational surface distribution of many galaxies in the cluster has a position angle similar to that of the line connecting the two brightest members of the B_b cluster. 1373 A foreground group of galaxies is superimposed on a western region of the cluster. 1374 The cluster is sparse. A foreground spiral galaxy is superimposed on the southern part of the cluster. 1375 The cluster is possibly closer than is indicated by distance class 5. 1376 The galaxy which we identify as the most luminous member of the cluster (#1) is possibly a b-galaxy. 1377 Three probable foreground spiral galaxies are located in the field of A1377 defined as the circle of radius R_c centered on the cluster. 1378 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the C subcluster and is possibly a cD galaxy. 1383 Two foreground galaxies (Sp + P) are superimposed on the cluster. 1386 A foreground Sc galaxy is superimposed on the cluster. A1386 contains a chain of four b-galaxies. 1387 Three foreground spiral galaxies are superimposed on a southeastern region of the cluster. 1388 The cluster is compact and rich in spiral galaxies. A1388 is connected to A1384 [Leir (1976) states that A1384, A1388, and a cluster connected to the northwest of A1384 are all one cluster]. 1389 A foreground group of galaxies overlaps the cluster. 1391 Two foreground galaxies are superimposed on the eastern part of the cluster. 1393 Three foreground galaxies are superimposed on the eastern part of the cluster. 1394 The cluster is elongated with the position angle of major axis similar to that of the line connecting the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2). A foreground group of galaxies is superimposed on the southwestern part of the cluster. 1395 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1396 It is difficult to separate the population of galaxies in the cluster from that in a possible foreground group of galaxies located in the field of A1396 defined as the circle of radius R_c centered on the cluster. 1398 R_c is restrictive. 1399 MKW-3 cluster. Two foreground galaxies (SBb + E/S0) are superimposed on the cluster. 1400 There is probable contamination of the assumed membership of A1400 by members of a group of galaxies superimposed on a western part the cluster. 1402 A large foreground SB(r) galaxy is superimposed on the cluster. 1403 The cluster is faint. 1404 One foreground spiral galaxy is superimposed on the cluster. 1405 The cluster is sparse. The galaxy which we identify as the third most luminous member of the cluster (#3) is possibly a b-galaxy. A foreground SB galaxy is superimposed on the eastern part of the cluster. 1406 A foreground P galaxy is superimposed on the cluster. The RS type of the cluster is possibly C5 if the galaxy which we identify as the most luminous member of the cluster (#1) is a gS0 galaxy. 1408 One foreground spiral galaxy is superimposed on the cluster. 1412 The cluster is probably more distant than is indicated by distance class 4. 1413 The galaxy which we assume is the most luminous member of the cluster (#1), a cD galaxy, has several companion galaxies. The locational surface distribution of galaxies in the cluster has a position angle of major axis similar to that of the cD galaxy. 1415 Several chains of faint galaxies characterize the cluster. Two foreground galaxies (S + IB) are superimposed on the cluster. 1416 A foreground group of galaxies overlaps the cluster. 1417 A foreground group of galaxies is superimposed on the western part of the cluster. 1423 A possible background cluster is located in a western field of A1423. 1425 One foreground spiral galaxy is superimposed on the cluster. 1426 A foreground S0/a galaxy is superimposed on the cluster. 1427 Several foreground spiral galaxies and an S0 galaxy are superimposed on the cluster. 1428 Foreground galaxies are superimposed on the cluster. 1429 A foreground group of galaxies is superimposed on the western part of the cluster. 1430 Foreground galaxies are superimposed on the cluster. 1431 A foreground Sc galaxy is superimposed on the cluster. 1432 The cluster is sparse. 1433 One foreground S0 galaxy is superimposed on the cluster. 1435 The cluster is closer than is indicated by distance class 5. One foreground spiral galaxy is superimposed on the cluster. 1437 One foreground spiral galaxy is superimposed on the cluster. 1438 Possible foreground galaxies are located in the field of A1438 defined as the circle of radius R_c centered on the cluster. A1438 is connected to A1444. 1439 Two foreground galaxies (S + E/S0) are superimposed on the cluster. 1443 Two foreground spiral galaxies are superimposed on the cluster. 1444 This cluster is connected to A1438. 1445 A foreground group of galaxies is superimposed on the western part of the cluster. 1446 Two foreground galaxies (b + Sc) are superimposed on the cluster. 1447 Several possible foreground spiral galaxies and a compact peculiar galaxy are superimposed on the cluster. 1449 This cluster overlaps A1455. 1450 The galaxy which we identify as the third most luminous member of the cluster (#3) is surrounded by most of the faint galaxies (Do these galaxies constitute a possible background cluster superimposed on A1450?). 1451 The cluster is elongated in the approximately north-south direction. 1453 The cluster is sparse. 1454 Several foreground spiral galaxies are superimposed on the cluster. 1455 This cluster overlaps A1449. 1456 Two foreground spiral galaxies are superimposed on the cluster. 1457 Two foreground galaxies (I + S) are superimposed on the cluster. 1458 Foreground galaxies are superimposed on the cluster. 1459 One foreground spiral galaxy is superimposed on the cluster. 1460 The cluster is very faint. 1461 The cluster is closer than is indicated by distance class 5. A background L cluster is superimposed on a southern region of A1461. 1463 A foreground spiral galaxy is superimposed on the cluster. 1464 The cluster is very faint. The galaxy which we identify as the most luminous member of the cluster (#1) is a diffuse object and possibly may be a foreground galaxy superimposed on the cluster. 1466 The cluster is farther than is indicated by distance class 5. One foreground spiral galaxy is superimposed on the cluster. 1467 The cluster is sparse. Foreground galaxies are superimposed on the cluster; it is difficult to separate populations. 1468 Possible foreground spiral galaxies are located in the field of A1468 defined as the circle of radius R_c centered on the cluster. 1471 A cE galaxy is located near the center of the cluster. A bright foreground Sc galaxy is superimposed on the northwestern part of the cluster. 1472 This cluster is probably connected to A1473 and A1478. Several foreground spiral galaxies and a diffuse object are superimposed on the cluster. 1475 Five foreground spiral galaxies are superimposed on the cluster. 1476 The cluster is very elongated in the approximately east-west direction. Is the RS type of the cluster possibly L9? Foreground galaxies are superimposed on the southern part of the cluster. 1477 Foreground galaxies are superimposed on the western part of the cluster. 1478 R_c is restrictive, but probable foreground galaxies are located in the field of A1478 defined as the circle of radius R_c centered on the cluster. A1478 is probably connected to A1472 and A1473. 1479 Several foreground spiral galaxies are superimposed on the cluster. 1480 Two foreground galaxies (S + S0) are superimposed on the cluster. 1481 Two foreground galaxies (Sc + SB) are superimposed on the cluster. 1483 Is the cluster closer than is indicated by distance class 6? 1484 The galaxy which Leir (1976) assumes is the most luminous member of the cluster may be a foreground galaxy superimposed on the cluster. 1486 A foreground elliptical galaxy is superimposed on the cluster. 1487 The galaxy which we identify as the most luminous member of the cluster (#1) is located near center of the cluster. 1490 Three foreground E/S0 galaxies are superimposed on the southern part of the cluster. 1492 A foreground group of galaxies is superimposed on a northeastern region of the cluster. 1495 A foreground group of galaxies is superimposed on a western region of the cluster. 1496 A probable foreground SBc galaxy is located in the field of A1496 defined as the circle of radius R_c centered on the cluster. 1497 R_c is restrictive. A1497 looks closer than is indicated by distance class 6. 1498 This cluster is connected to A1506. 1499 Two foreground spiral galaxies are superimposed on the cluster. 1500 The RS type of the cluster is NOT cD as listed by Rood and Sastry (1971). Two foreground spiral galaxies are superimposed on the cluster. The members of the cluster look fainter than is usual for clusters in distance class 3. 1501 The cluster is T-shaped. 1502 A possible background cluster is located in a southern field of A1502. 1503 Three foreground spiral galaxies are superimposed on the cluster. 1504 A large foreground spiral galaxy is superimposed on the southeastern part of the cluster. 1506 The cluster is sparse. A1506 is connected to A1498. 1508 Four foreground spiral galaxies are superimposed on the cluster. 1510 The four b-galaxies are very faint. Foreground galaxies are superimposed on the eastern part of the cluster. 1513 One foreground spiral galaxy is superimposed on the cluster. 1514 Three foreground S/S0 galaxies are superimposed on the cluster. A foreground group of galaxies is superimposed on the northern part of the cluster. 1515 A foreground group of galaxies is superimposed on the northern part of the cluster. 1516 A large foreground spiral galaxy is superimposed on the cluster. 1519 Probable foreground galaxies are located in the field of A1519 defined as the circle of radius R_c centered on the cluster. 1520 One foreground spiral galaxy is superimposed on the cluster. 1521 Is the cluster closer than is indicated by distance class 5? A spiral pattern of galaxies surrounds the cD galaxy. 1522 The cluster is very faint. 1525 The core of the cluster is very compact. 1527 One foreground spiral galaxy is superimposed on the cluster. 1528 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1529 The cluster is compact. 1531 Foreground galaxies are superimposed on the western part of the cluster. 1532 A probable foreground group of galaxies is located in an eastern field of the cluster. 1536 The galaxy which we identify as the third most luminous member of the cluster (#3) may be a b-galaxy. One foreground spiral galaxy is superimposed on the cluster. 1538 The cluster is very faint. 1539 A foreground Sbc galaxy is superimposed on the cluster. 1540 Three bright foreground galaxies are superimposed on the cluster. 1543 Two foreground spiral galaxies are superimposed on the cluster. 1544 Leir(1976) notes that the cluster contains two concentrations of galaxies. 1545 This cluster is connected to A1550. 1546 Foreground galaxies are superimposed on the cluster. 1547 One foreground SB0 galaxy is superimposed on the cluster. 1548 The cluster is a possible cD cluster. Bright foreground galaxies are superimposed on the western and eastern parts of the cluster. 1549 Three foreground galaxies (S + b + E) are superimposed on the cluster. 1550 Two foreground galaxies are superimposed on the eastern part of the cluster. A1550 is possibly connected to A1545. 1553 The cluster looks closer than is indicated by distance class 6. 1555 The two apparent subclusters of galaxies are possibly located at different distances. 1557 The cluster is characterized by two main concentrations of galaxies. 1558 The galaxy which we identify as the most luminous member of the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. 1560 The distance class of the cluster is D=7. The galaxy which we identify as the second most luminous member of the cluster (#2) has faint companion galaxies. A foreground diffuse IB galaxy and b-galaxy are superimposed on the cluster. 1561 R_c is restrictive. The cluster looks closer than is indicated by distance class 6. 1562 Possible foreground galaxies are superimposed on the cluster. A1562 is connected to A1565. 1564 The galaxy which we identify as the second most luminous member of the cluster (#2) is separated from a companion galaxy by 0.36 mm on plates of the POSS. 1565 This cluster is connected to A1562. A peculiar diffuse spiral galaxy is located southwest of the cluster. 1566 This cluster is the more distant of two clusters with the locational coordinates specified by Abell (1958). Leir (1976) suggests that the locational coordinate of the cluster X = 47 mm; however, we believe that the original coordinates are correct. 1566X This cluster is the nearer of two clusters with the locational coordinates specified by Abell (1958). Leir (1976) may have misidentified A1566X for A1566 because he asks 'Is the distance class 6?'. 1567 A foreground group of five galaxies is superimposed on the cluster. 1570 The cluster is sparse and looks less rich than is indicated by richness class 1. 1572 A bright foreground spiral galaxy is superimposed on the eastern part of the cluster; a P galaxy is superimposed on the northern part of the cluster. A1572 is connected to A1573. 1573 This cluster is connected to A1572. 1575 Three foreground galaxies (E + cE + S/Sa) are superimposed on the cluster. 1576 A foreground group of galaxies is superimposed on the southern part of the cluster. 1577 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster and has faint companion galaxies. 1579 Possible foreground galaxies are located in the field of A1579 defined as the circle of radius R_c centered on the cluster. 1580 The cD subcluster of galaxies is a possible foreground group located in the field of A1580 defined as the circle of radius R_c centered on the cluster. 1581 Two foreground galaxies [S(r) + S0] are superimposed on the cluster. 1586 A bright SBc galaxy is located in the northern part of the cluster. 1587 Four foreground galaxies (2 P + 2 S0) are superimposed on the cluster. A1587 is connected to A1594. 1588 The galaxy which we identify as the most luminous member of the cluster (#1) has a luminous jet. One foreground spiral galaxy is superimposed on the cluster. 1591 Three foreground spiral galaxies are superimposed on the northwestern part of the cluster; one foreground spiral galaxy is superimposed on the southern part of the cluster. 1592 Two foreground galaxies (S + b) are superimposed on the cluster. 1593 One foreground spiral galaxy is superimposed on the cluster. 1594 This cluster is connected to A1587. 1595 The cluster is sparse. R_c is restrictive because a subcluster of galaxies is located to the northeast of the circle of radius R_c centered on A1595. 1596 The L subcluster of galaxies is possibly more distant than is the C subcluster. 1597 The cD galaxy has a very faint envelope of luminosity. The cluster is sparse. R_A' = 15 mm (Abell 1979) compared to R_c = 6 mm (Leir and van den Bergh 1977) on plates of the POSS. 1598 A bright star is superimposed on a region near the center of the cluster. Two galaxies (S + SB) are superimposed on the cluster. 1599 Two foreground galaxies (an elliptical and its companion galaxy) are superimposed on the cluster. 1601 Two foreground S0 galaxies are superimposed on an eastern region of the cluster. 1602 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy. The cD galaxy has a bright nucleus. A foreground diffuse P galaxy is superimposed on the cluster. 1605 A foreground SB galaxy is superimposed on the cluster. 1607 Two foreground galaxies (S0 + S) are superimposed on the cluster. 1609 A foreground E/S0 galaxy is superimposed on the cluster. 1610 Two foreground spiral galaxies are superimposed on the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. 1612 Foreground and background galaxies are superimposed on the cluster. A diffuse object is possibly a background cluster superimposed on the cluster. 1613 A foreground elliptical galaxy and a b-galaxy are superimposed on the eastern part of the cluster. 1614 Foreground spiral and S0 galaxies are superimposed on the cluster. 1618 Foreground galaxies are superimposed on the cluster. 1623 The cluster is sparse. Several bright foreground galaxies are superimposed on the northern and western parts of the cluster. 1624 The C5 subcluster is possibly the nearer of the two subclusters. 1625 One foreground spiral galaxy is superimposed on the cluster. 1626 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster and is possibly a cD galaxy. A foreground group of galaxies is superimposed on the northern part of the cluster. 1628 Six foreground galaxies (4 S + 2 E) are superimposed on the northern part of the cluster. 1629 Leir (1976) asks 'Is the Abell cluster two close clusters?'. 1630 The cluster is closer than is indicated by distance class 5. 1631 The cluster looks like a cD cluster, but the apparently most luminous galaxy is in the foreground of the cluster (Dressler 1981, private communication). 1632 Two foreground S/S0 galaxies are superimposed on the cluster. 1633 The C subcluster of galaxies is compact. 1634 Foreground galaxies are superimposed on the western part of the cluster. 1635 The cluster is very sparse. Several galaxies may be outliers of a group located in a western region of the cluster. 1636 The three subclusters of galaxies are collinear. The cluster looks closer than is indicated by distance class 6. A1636 is connected to A1640. 1637 The locational surface distribution of galaxies in the cluster has a position angle of major axis similar to the position angle of the line connecting the two brightest members of the B cluster. Two possible foreground galaxies (SB + S) are located in the field of A1637 defined as the circle of radius R_c centered on the cluster. 1640 This cluster is connected to A1636. 1641 Several foreground spiral galaxies are superimposed on the cluster. A foreground group of galaxies is superimposed on the eastern part of the cluster. 1642 Several foreground galaxies are superimposed on the eastern part of the cluster. 1643 The b-galaxy identified as the first brightest member of the cluster (#1) is located on the northwestern edge of the cluster. 1646 A foreground S/S0 galaxy is superimposed on the cluster. 1649 Four foreground spiral galaxies are superimposed on the cluster. 1650 The locational surface distribution of galaxies in the cluster is very elongated and has a position angle of major axis similar to that of the cD galaxy. Two foreground S/S0 galaxies are superimposed on the cluster. 1652 It is difficult to identify the three most luminous galaxies in the cluster, because there are many bright galaxies within and outside of subclusters. 1653 R_c is restrictive because subclusters lie outside the field of A1653 defined as the circle of radius R_c centered on the cluster; we estimate R_c = 15 mm on plates of the POSS. 1654 The cluster is sparse. 1655 The two brightest members of the B cluster are connected to each other by a long bridge of luminosity. 1656 Coma cluster. NGC 4889 has one bright lenticular galaxy and two fainter galaxies within its envelope of luminosity. There is a possible circumfrential alignment of galaxies around NGC 4874. 1659 Possible foreground galaxies are located in the field of A1659 defined as the circle of radius R_c centered on the cluster. 1660 A foreground group of galaxies is superimposed on a northern part of the cluster. 1661 In its southern part, the cluster overlaps the Coma cluster. 1663 The envelope of luminosity on the cD galaxy is "tear-drop"-shaped and points to a satellite galaxy. 1664 Three foreground spiral galaxies are superimposed on the northwestern part of the cluster. 1665 Two foreground elliptical galaxies in the Coma cluster are superimposed on A1665. A faint chain of galaxies is located in the southern part of the cluster. 1666 Several possible foreground Sc galaxies are located in the field of the A1666 defined as the circle of radius R_c centered on the cluster. 1667 The Abell cluster is probably the superposition of more than one cluster located at different distances along the line-of-sight, because the field defined by the circle of radius R_c centered on A1667 contains galaxies with several differing redshifts. 1669 The cluster is very faint. 1670 A foreground group of galaxies is superimposed on the southwestern part of the cluster; a b-galaxy is superimposed on the western part of the cluster. 1672 Four foreground spiral galaxies are superimposed on the cluster. 1675 The galaxy which we identify as the most luminous member of the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. We believe that this latter galaxy is in the foreground of the cluster. 1676 Three foreground spiral galaxies are superimposed on the southern part of the cluster; one foreground spiral galaxy is superimposed on the eastern part of the cluster. 1677 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) are a t-galaxy in a common envelope of luminosity. Is this t-galaxy a pre-cD galaxy? A foreground b-galaxy is superimposed on the cluster. 1679 The cluster is elongated. 1682 Foreground galaxies are superimposed on the eastern and southern parts of the cluster. 1683 A possible foreground b-galaxy is located in the field of A1683 defined as the circle of radius R_c centered on the cluster. 1685 A foreground group of galaxies is superimposed on the cluster. R_c is restrictive; our revised estimate is R_c ~~ 13 mm on plates of the POSS. 1686C The alternate line of data refers to only the I_s subcluster. 1688 Three foreground spiral galaxies are superimposed on the northern part of the cluster. 1689 The cluster is compact. The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) might be a t-galaxy. 1692 The rectangular coordinates of A1692 as registered on plates of the POSS are X = 268 mm and Y = 156 mm (The Y-coordinate listed by Sastry and Rood (1971) is incorrect). 1693 A possible foreground chain of galaxies is located in a western field of the cluster. 1694 One foreground spiral galaxy is superimposed on the cluster. 1696 Three foreground galaxies are superimposed on the northern part of the cluster. 1697 A foreground diffuse object (possibly an Ip galaxy) is superimposed on a region near the center of the cluster; a foreground Sbc galaxy is superimposed southwest of the cluster. 1699 A peculiar (comet shaped) object is located near the center of the cluster. 1701 Two foreground spiral galaxies are superimposed on the cluster. 1702 Possible foreground galaxies are located in the southern and eastern parts of the cluster. 1703 The cluster is `V' shaped. Several faint b-galaxies are superimposed on the cluster. 1704 The cluster is elongated. The galaxy which we identify as the most luminous member of the cluster (#1) may be a t-galaxy, and possibly a pre-cD galaxy. 1705 Several foreground galaxies are superimposed on the periphery of A1705. The cluster is very faint. 1706 Two foreground spiral galaxies are superimposed on the cluster. Leir (1976) notes that two clumps of galaxies characterize the cluster. 1707 The cluster overlaps the distance class 5 foreground cluster A1713. R_c is restrictive. 1710 One foreground E/S0 galaxy is superimposed on the cluster. 1712 A foreground spiral galaxy is superimposed on the northern part of the cluster. 1714 A foreground group of galaxies is superimposed on the southern part of the cluster. 1715 A background cluster is superimposed on a southwestern region of A1715. 1716 A very peculiar galaxy (containing jets of luminosity) is located in the northern part of the cluster. A possible foreground group of galaxies is located in the western field of the cluster. A1716 looks closer than is indicated by distance class 6. 1717 Two foreground galaxies (SB + Sb) are superimposed on the cluster. 1718 Probable foreground galaxies are located in the field of A1718 defined as the circle of radius R_c centered on the cluster. 1719 The cluster is very extensive. R_c' = 10 mm is restrictive. 1722 R_c is restrictive. Subclusters of galaxies are located in the western and southern parts of A1722 outside the circle of radius R_c centered on the cluster. The cluster is very faint. 1723 A foreground group of spiral galaxies is superimposed on an eastern region of the cluster. 1724 Several foreground spiral and S0 galaxies are superimposed on the cluster. 1725 Is the cluster closer than is indicated by distance class 6? A foreground group of spiral galaxies is superimposed on the northern part of the cluster. 1726 A possible background cluster is located in an eastern field of A1726. 1727 The cluster is sparse. 1728 Is the cluster closer than is indicated by distance class 6? The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. 1730 Several possible foreground galaxies are located in the field of A1730 defined as the circle of radius R_c centered on the cluster. 1731 One foreground spiral galaxy is superimposed on the cluster. 1732 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy, which has an asymmetric envelope of luminosity. 1733 The cluster is sparse. 1734 The cluster looks closer than is indicated by distance class 6. Foreground galaxies are superimposed on the northern part of the cluster. 1737 A foreground SB and elliptical galaxy are superimposed on the western part of the cluster. 1739 The cluster is sparse. A foreground Sc galaxy is superimposed on the northwestern part of the cluster. 1740 Two foreground galaxies are superimposed on a region near the center of the cluster. 1742 The cluster is sparse. Two foreground spiral galaxies are superimposed on A1742. 1744 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) each have small companion galaxies. One foreground Sab galaxy is superimposed on the cluster. 1745 The distance class of the cluster is D=7. 1750 Two bright foreground spiral galaxies are superimposed on the cluster. Leir (1976) notes that a possible subcluster of galaxies is located in a southern region of the cluster. 1751 The cluster is sparse. 1752 Two foreground spiral galaxies are superimposed on the cluster. 1753 Three foreground galaxies are superimposed on the southern part of the cluster. 1755 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1756 The cluster is sparse. Probable foreground galaxies are located in the field of A1756 defined as the circle of radius R_c centered on the cluster. 1757 A possible foreground b-galaxy is located in the field of A1757 defined as the circle of radius R_c centered on the cluster. 1758 This cluster is a good example of an F cluster. 1759 This cluster is a good example of an I_s cluster, but there are small subgroups around the main concentration of galaxies. A1759 is connected to the distance class 5 cluster A1760. 1760 It is difficult to classify the galaxies in the field of A1760 defined as the circle of radius R_c centered on the cluster. A1760 is confused with A1758 and A1759. 1761 A foreground galaxy is superimposed on a region near the center of the cluster. 1762 Leir (1976) notes that a foreground group of galaxies is superimposed on the eastern part of the cluster. 1763 Several spiral galaxies are located in the cluster. Two foreground galaxies are superimposed on the northern part of the cluster. 1764 The C6 cluster is the nearer of the two clusters; the I_s cluster is the more distant. 1765 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. A foreground SB galaxy is superimposed on the western part of the cluster. 1766 The cluster is compact. A foreground spiral galaxy is superimposed on the northern part of the cluster; a foreground b-galaxy is superimposed on the southern part of the cluster. 1767 The cD galaxy may be a very close binary, so the RS type of the cluster might be B_b. 1769 A foreground SB galaxy is superimposed on the cluster. 1771 A foreground SB(r) galaxy is superimposed on the cluster. 1774 The galaxy which we identify as the third most luminous member of the cluster (#3) has a faint companion galaxy. 1775 Hintzen (1979, Publ. Astron. Soc. Pac., 91, 478) argues that the cluster may be an optical double. 1776 A foreground SB galaxy is superimposed on the cluster. 1777 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 1778 Two foreground spiral galaxies are superimposed on the cluster. 1780 The cluster is closer than is indicated by distance class 5. 1781 A prominent line of spiral galaxies is located in an eastern part of the cluster. 1782 R_c is restrictive. Possible subclusters of galaxies are located in the western and southeastern parts of the cluster. 1783 Foreground spiral galaxies are superimposed on the cluster. 1784 The cD subcluster is sparse; the C6 subcluster is rich with galaxies. 1785 The cluster is T-shaped. 1786 R_c is restrictive because a subcluster of galaxies is located to the east of the circle of radius R_c centered on the cluster. 1787 R_c is restrictive because a subcluster of galaxies is located to the north of the circle of radius R_c centered on A1787. 1788 This cluster is connected to A1790. 1789 A foreground P galaxy is superimposed on the cluster. 1790 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. A1790 is connected to A1788. 1792 A foreground spiral galaxy is superimposed on the southewestern part of the cluster. 1797 Several possible foreground spiral galaxies are located in the field of A1797 defined as the circle of radius R_c centered on the cluster. 1798 Is the cluster closer than is indicated by distance class 6? Is the cluster richer than is indicated by richness class 0? Several foreground spiral galaxies are superimposed on the cluster. 1799 A chain of faint galaxies is located in the cluster. 1801 R_c is restrictive because other subclusters of galaxies are located outside the circle of radius R_c centered on A1801. 1801X A foreground group of galaxies is superimposed on the western part of the cluster. 1802 One foreground Sbc galaxy is superimposed on the cluster. 1803 This cluster is connected to A1811. 1805 Several foreground spiral galaxies are superimposed on the cluster; it is difficult to separate populations. 1807 The galaxy which we identify as the most luminous member of the cluster (#1) may have jets of luminosity. A foreground spiral galaxy is superimposed on the western part of the cluster. 1809 Three foreground galaxies are superimposed on the cluster. 1811 This cluster is connected to A1803. 1812 Probable foreground galaxies are located in the field of A1812 defined as the circle of radius R_c centered on the cluster. 1814 One foreground SB galaxy is superimposed on the cluster. 1815 The cluster is very elongated. The galaxy which we identify as the most luminous member of the cluster (#1) is a possible foreground galaxy located in the field of A1815 defined as the circle of radius R_c centered on the cluster. 1816 A crowded star field and a foreground group of galaxies are superimposed on the cluster. 1817 One foreground spiral galaxy is superimposed on the cluster. 1818 Two foreground galaxies (SBc + E/S0) are superimposed on the cluster. 1821 A foreground spiral galaxy is superimposed on the northwestern part of the cluster. 1822 The cluster is compact. 1824 Leir (1976) notes that the cluster has two concentrations of galaxies. 1826 A large foreground Sbc galaxy with several spiral companion galaxies is superimposed on a region near the center of the cluster. Foreground spiral galaxies are superimposed on the western part of the cluster. 1827 One foreground spiral galaxy is superimposed on the cluster. 1829 A foreground galaxy is superimposed on the southern part of the cluster. 1831 The cluster is rich in elliptical and S0 galaxies. 1834 One foreground E/S0 galaxy is superimposed on the cluster. 1835 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster and has many faint companion galaxies. Is this galaxy a pre-cD galaxy? A1835 looks like a richness class 1 or 2 cluster, rather than richness class 0. 1836 Three foreground galaxies (Sc, SB, E) are superimposed on the cluster. 1838 The cluster is very faint. 1839 The Bautz-Morgan type of the cluster is BM = III rather than BM = I, because the galaxy which Leir (1976) assumes is the most luminous member of the cluster is a probable foreground galaxy located in the field of A1839 defined as the circle of radius R_c centered on the cluster. 1841 A foreground galaxy is superimposed on a region near the center of the cluster. 1843 The cluster is sparse. 1846 Two bright foreground S0 galaxies are superimposed on the cluster. 1847 The L subclusters are approximately parallel to each other. 1849 One foreground spiral galaxy is superimposed on the cluster. 1850 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. Foreground spiral galaxies are superimposed on the southern and northwestern parts of the cluster. 1852 Three foreground spiral galaxies are superimposed on the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) has a close companion galaxy. 1853 A foreground galaxy is superimposed on the northern part of the cluster. 1854 Two foreground spiral galaxies are superimposed on the cluster. 1855 A foreground group of galaxies is superimposed on the northeastern part of the cluster. 1856 A possible background chain of galaxies is located in a western field of A1856. 1861 One foreground spiral galaxy is superimposed on the cluster. 1863 A foreground spiral galaxy is superimposed on the cluster. 1864 The galaxy which we identify as the most luminous member of the cluster (#1) has two companion galaxies. 1865 A possible background cluster is located in a field near the center of A1865. R_c is restrictive because the cluster is observed to extend to a radial distance from its center which is possibly as large as 18 mm on plates of the POSS. 1869 The cluster is a possible I_c cluster; it contains a few subclusters of galaxies. 1874 Two foreground galaxies (S + b) are superimposed on the cluster. 1875 The galaxy which we identify as the most luminous member of the cluster (#1) is connected by faint bridges of luminosity to companions galaxies. A1875 looks closer than is indicated by distance class 6. 1876 The galaxy which Leir (1976) identifies as the most luminous member of the cluster is a probable foreground galaxy located in the field of A1876 defined as the circle of radius R_c centered on the cluster. 1878 Two foreground spiral galaxies are superimposed on the cluster. 1882 Three foreground spiral galaxies are superimposed on the cluster. 1883 Two foreground spiral galaxies are superimposed on the cluster. 1884 It is difficult to identify the three most luminous members of the cluster because many galaxies have similar apparent magnitudes. R_c' is restrictive because the cluster is observed to extend to a radial distance from its center which may be as large as 15 mm on plates of the POSS. 1886 The L5 subcluster of galaxies may be part of another cluster to the northwest of A1886. 1887 Four foreground spiral galaxies are superimposed on the cluster. 1889 Three foreground spiral galaxies are superimposed on the eastern part of the cluster. 1890 A bright foreground spiral galaxy is superimposed on a northwestern part of the cluster. 1891 Two foreground spiral galaxies are superimposed on a western region of the cluster. 1892 Is the cluster more distant than is indicated by distance class 5? Three foreground spiral galaxies are superimposed on an eastern region of the cluster. 1895 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. 1897 Is the RS type of the cluster possibly cD? 1898 A possible background I galaxy is located in the field of A1898 defined as the circle of radius R_c centered on the cluster. 1900 Two foreground spiral galaxies are superimposed on the cluster. 1901 Is the cluster closer than is indicated by distance class 5? Several probable foreground spiral galaxies are located in the field of A1901 defined as the circle of radius R_c centered on the cluster. 1903 Three foreground spiral galaxies are superimposed on the cluster. 1905 Foreground galaxies are superimposed on the cluster. 1906 Two foreground spiral galaxies are superimposed on the cluster. 1907 One foreground S/S0 galaxy is superimposed on the cluster. 1908 The galaxy which we identify as the third most luminous member of the cluster (#3) has many companion galaxies. 1909 Is the cluster closer than is indicated by distance class 5? Two foreground spiral galaxies are superimposed on the cluster. 1910 A b-galaxy is located near the supergiant binary galaxy (the two brightest members) at the center of the B_b cluster. In the southern part of the cluster, A1910 overlaps A1909. 1913 Two possible foreground E/S0 galaxies are located in the field of A1913 defined as the circle of radius R_c centered on the cluster. 1914 The locational surface distribution of fainter galaxies in the cluster has a position angle of major axis similar to the position angle of the line of galaxies which characterizes the cluster. 1917 The cluster is faint. 1918 The cluster is elongated with a position angle of major axis similar to that of the envelope of luminosity on the cD galaxy. 1919 The RS type of the cluster is possibly cD. A1919 looks richer than is indicated by richness class 0. The galaxy which we identify as the most luminous member of the cluster (#1) has three faint companion galaxies. 1920 The locational surface distribution of most galaxies in the cluster has a position angle of major axis similar to that of the cD galaxy. 1921 The C10 cluster is the nearer of the two clusters; the cDp cluster is the more distant. 1922 A bright foreground Sc galaxy is superimposed on the northwestern part of the cluster. A foreground spiral galaxy is superimposed on a region near the center of the cluster. A possible background cluster is located in a western field of A1922. Is R_c restrictive? The Abell cluster is possibly a superposition of several clusters located at different distances along the line-of-sight. 1927 The cluster is structurally similar to A1149. 1928 R_c is restrictive. Possible foreground galaxies are located in the field of A1928 defined as the circle of radius R_c centered on the cluster. 1929 Several spiral galaxies are located in the cluster. 1933 Foreground elliptical galaxies are superimposed on the western part of the cluster. 1934 A bright foreground E/S0 galaxy is superimposed on a region near the center of the cluster. 1935 The cluster is sparse. 1938 Two foreground spiral galaxies are superimposed on the cluster. 1939 One foreground spiral galaxy is superimposed on the cluster. 1940 One foreground spiral galaxy is superimposed on the cluster. 1941 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate the populations. A foreground b_p-galaxy is super- imposed on the eastern part of the cluster. A1941 is connected to A1943. 1942 The galaxy which we identify as the most luminous member of the cluster (#1) has two companion galaxies on opposite sides. Several bright foreground spiral galaxies are superimposed on the southern part of the cluster. 1943 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. A1943 is connected to A1941. Foreground galaxies are superimposed on the cluster. 1944 Two foreground galaxies (S/S0 + b) are superimposed on the cluster. 1945 The rectangular coordinates of the cluster as registered on plates of the POSS are listed incorrectly by Sastry and Rood (1971); for agreement with the position of the cluster listed by Abell (1958), the rectangular coordinates are X = 310 mm, Y = 292 mm. 1947 Leir (1976) notes that the cluster contains two concentrations of galaxies, one with BM = II and the other with BM = II-III. A foreground spiral galaxy is superimposed on the southern part of the cluster. 1948 One foreground spiral galaxy is superimposed on the cluster. 1951 The cluster is very faint. Two foreground galaxies are superimposed on a region near the center of the cluster. 1952 This cluster is connected to A1954. 1954 This cluster is connected to A1952. 1956 Foreground galaxies are superimposed on the cluster. A1956 is connected to A1957. 1957 The locational coordinates of the cluster specified by Abell (1958) are correct, contrary to Leir's (1976) claim. A1957 is connected to A1956 and A1958. Foreground galaxies are superimposed on the cluster. 1958 This cluster is connected to A1957. A diffuse foreground SB/I galaxy is superimposed on the western part of A1958. A1958 looks poorer than is indicated by richness class 2. 1959 Several foreground spiral galaxies are superimposed on the cluster. 1960 A foreground group of galaxies is superimposed on northern and eastern regions of the cluster. 1961 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. A1961 is connected to A1963. 1963 This cluster is connected to A1961. 1967 The cluster is very elongated. A foreground group of galaxies is superimposed on the southern part of the cluster. 1968 Four foreground spiral galaxies are superimposed on the cluster. Is R_c restrictive? 1969 R_c is restrictive because additional galaxies are located to the north of the circle of radius R_c centered on the cluster. The cluster is very faint. A foreground b-galaxy is superimposed on the eastern part of the cluster. 1970 Two foreground galaxies (S + P) are superimposed on the cluster. 1972 Two foreground spiral galaxies are superimposed on the cluster. 1973 Four galaxies (3 S0 + S) are superimposed on the northern part of the cluster. Three subclusters of galaxies in the cluster are elongated in the approximately east-west direction. 1975 Four foreground galaxies (3 S + S0) are superimposed on the cluster. 1977 One foreground spiral galaxy is superimposed on the cluster. 1980 The galaxy which we identify as the most luminous member of the cluster (#1) may be a pre-cD galaxy. 1982 Is the cluster closer than is indicated by distance class 5? 1983 The cluster is characterized by three distinct collinear clumpings of galaxies. 1986 One foreground Sa galaxy is superimposed on the cluster. 1987 The galaxies which we identify as the first, second, and third most luminous members of the cluster (#1, #2, and #3) may be a foreground group of galaxies superimposed on the cluster. 1988 One foreground spiral galaxy is superimposed on the cluster. 1990C The RS type of the cluster is possibly L8. 1991 The cluster is rich in spiral galaxies. 1992 A bright foreground Sp galaxy is superimposed on the cluster. Two possible foreground spiral galaxies are located in the field of A1992 defined as the circle of radius R_c centered on the cluster. 1993 A possible foreground P galaxy is located in an eastern field of the cluster. 1994 The cluster is elongated in the approximately east-west direction. 1995 The distance class of the cluster is D=7. A possible foreground galaxy is located in the northern field of the cluster. 1996 Is the richness class of the cluster R=1 (not R=0)? 1997 Three foreground spiral galaxies are superimposed on the cluster. 1998 A foreground group of galaxies is superimposed on the northeastern part of the cluster. 1999 The cluster is a good example of an I_s cluster. 2000 All three bright galaxies are peculiar. The galaxy which we identify as second most luminous member of the cluster (#2) has many nuclei and may be a pre-cD galaxy. 2001 Several edge-on S0 galaxies are located at each end of the line of galaxies which characterizes this L cluster. One foreground spiral galaxy is superimposed on the cluster. 2002 Foreground galaxies are superimposed on the western part of the cluster. A defect on the E-plate of the POSS looks like a b-galaxy in the western part of the cluster. 2003 One foreground S/S0 galaxy is superimposed on the cluster. 2004 One foreground spiral galaxy is superimposed on the cluster. 2005 Foreground lenticular galaxies are superimposed on the cluster. 2007 A possible background cluster is located in the field of A2007 defined as the circle of radius R_c centered on the cluster. 2008 This is a good example of a cluster with a secondary maximum in its radial distribution of surface number density of galaxies. Several foreground galaxies are superimposed on the southern part of the cluster. 2010 The cluster is sparse. Two foreground galaxies are superimposed on the eastern part of the cluster. 2011 Three foreground galaxies (E + S0 + S) are superimposed on the cluster. 2013 The galaxy which we identify as the third most luminous member of the cluster (#3) is connected by a tail of luminosity to a faint companion galaxy. Why did Leir (1976) decide that the Bautz-Morgan type of the cluster is possibly BM = I-II? 2014 The RS type of the cluster is possibly cD. The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. 2015 The cluster is characterized by compact subclusters of galaxies. A2015 is a good example of an I_c cluster. 2016 A foreground group of galaxies is superimposed on the southeastern part of the cluster. A bright Sb galaxy is located in the western part of the cluster. 2017 Two foreground Sc galaxies are superimposed on the cluster. 2018 One foreground spiral galaxy is superimposed on the cluster. 2019 Most clumps of galaxies are elongated in approximately the same direction. 2021 Probable foreground galaxies are located in the field of A2021 defined as the circle of radius R_c centered on the cluster. R_c is restrictive. 2024 R_c is restrictive. An L5 cluster with seven b-galaxies is located to the east of A2024 and is collinear with the C10 and I_s subclusters of A2024. Several foreground E/S0 and S/S0 galaxies are superimposed on the cluster. 2026 Two foreground elliptical galaxies are superimposed on an eastern region of the cluster. A defect on the E-plate of the POSS which looks like a b-galaxy is located in the field A2026. 2027 A foreground P galaxy is superimposed on the western part of the cluster. 2029 Two foreground spiral galaxies are superimposed on the cluster. 2030 The galaxy which we identify as the most luminous member of the cluster (#1) has several companion galaxies (Is this b-galaxy a pre-cD galaxy?). 2032 The galaxy which we identify as the most luminous member of the cluster (#1) may have two jets of luminosity. Two foreground galaxies are superimposed on the southern part of the cluster. 2035 R_c is very restrictive. A chain of galaxies is located in a northern region of the cluster. A possible background cluster is located in a northern field of the cluster. 2036 This is a good example of an I_c cluster. 2038 One foreground spiral galaxy is superimposed on the cluster. 2039 Two foreground spiral galaxies are superimposed on the cluster. 2042 The cluster is more distant than is indicated by distance class 5. 2043 A foreground P galaxy is superimposed on the cluster. 2045 The galaxies which we assume are the first and second most luminous members of the cluster (#1 and #2) have very diffuse envelopes of luminosity (Are #1 and #2 cD galaxies?). 2047 Three foreground galaxies are superimposed on the cluster. 2050 R_c is restrictive. 2051 The RS type of the cluster is possibly C6. A foreground group of galaxies is superimposed on the southern part of the cluster. A2051 overlaps A2053. 2053 The galaxy which we identify as the most luminous member of the cluster (#1) has a large, asymmetric envelope of luminosity. A2053 is connected to A2051. Foreground galaxies are superimposed on the southeastern part of the cluster. 2054 A foreground b-galaxy is superimposed on the southeastern part of the cluster. 2057 Two foreground spiral galaxies are superimposed on the cluster. 2058 The cluster is very faint. The galaxy which Leir (1976) assumes is the most luminous member of the cluster is a probable foreground galaxy. 2060 The galaxy which we identify as the second most luminous member of the cluster (#2) is isolated and a possible foreground galaxy superimposed on the cluster. 2062 Is the cluster closer than is indicated by distance class 5? 2063 Is A2063 an example of a cD cluster in the making? 2065 Corona Borealis cluster. 2066 R_c is very restrictive. 2067 A chain of lenticular galaxies is located in a northwestern region of the cD cluster. 2068 Possible foreground galaxies are located in the field of A2068 defined as the circle of radius R_c centered on the cluster. 2069 One foreground spiral galaxy is superimposed on the cluster. 2070 Several foreground spiral galaxies are superimposed on the periphery of the cluster. 2072 Two foreground galaxies (E + S) are superimposed on the cluster. 2073 Two foreground spiral galaxies are superimposed on the cluster. 2076 The cluster is faint. A foreground b-galaxy is superimposed on the western part of the cluster. 2078 The cluster is extensive and contains many subclusters of galaxies. R_c is very restrictive. 2082 A foreground elliptical galaxy is superimposed on the cluster. 2083 The locational surface distribution of faint galaxies in the cluster has a position angle of major axis similar to that of the cD galaxy. 2084 The cluster is elongated. The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 2085 The two b-galaxies are faint. Several bright foreground galaxies are superimposed on the southern and eastern parts of the cluster. 2086 The cluster looks poorer than is indicated by richness class 2. 2087 R_c is restrictive. 2088 R_c is very restrictive. 2090 Foreground galaxies are superimposed on the cluster. 2091 Several foreground spiral galaxies are superimposed on the northern part of the cluster. 2095 The cluster is sparse. Two foreground galaxies (S + b) are superimposed on the eastern part of the cluster. 2096 The galaxy which we identify as the most luminous member of the cluster (#1) has a luminous jet. 2097 The cluster is very faint. Foreground galaxies are superimposed on the cluster; it is difficult to separate populations. 2098 The cluster is sparse. Two foreground spiral galaxies are superimposed on the cluster, one on a northwestern region, and the other on a southwestern region. 2099 Leir (1976) suggests that four bright galaxies may be possible foreground galaxies in the field of A2099 defined as the circle of radius R_c centered on the cluster. Four b-galaxies are located in the southern part of the cluster. 2101 Two foreground galaxies (Sc + companion galaxy) are superimposed on the cluster. 2102 This cluster is connected to A2115. A defect on the E-plate of the POSS is superimposed on the southern part of the cluster. 2105 The cluster is very sparse (if extant at all). 2106 One foreground spiral galaxy is superimposed on the cluster. 2109 A foreground group of galaxies is superimposed on the southeastern part of the cluster. 2113 The cluster has a very compact core of galaxies. 2115 The cluster is sparse. A2115 is connected to A2102. A foreground b-galaxy is superimposed on the cluster. 2118 Three foreground spiral galaxies are superimposed on the cluster. 2120 The cluster is sparse. A foreground group of galaxies is superimposed on the cluster, mostly in its eastern part. 2121 Four very blue foreground galaxies are superimposed on the eastern part of the cluster. 2126 Two foreground galaxies are superimposed on the cluster. 2127 The cluster is sparse. 2130 The photographic images of the stars as registered on the E-plate of the POSS are elongated in the field of the cluster defined as the circle of radius R_c centered on the cluster. The cluster is characterized by three main clumps of galaxies each with one bright galaxy. 2133 R_c is restrictive because a subcluster of galaxies is located to the east of the circle of radius R_c centered on A2133. 2134 One foreground galaxy is superimposed on the eastern part of the cluster. 2135 The cluster is sparse and elongated. Three foreground galaxies (2S + E) are superimposed on the cluster. 2136 It is difficult to identify the three most luminous galaxies in the cluster because several of the brighter galaxies have the same apparent magnitude. A defect on the E-plate of the POSS is located in a field near the center of the cluster. A chain of galaxies is located in the southern part of the cluster. 2138 A foreground group of galaxies is superimposed on the western part of the cluster; it is difficult to separate populations. 2139 This cluster is a fairly uncluttered, good example of an I_c cluster. 2140 Foreground galaxies are superimposed on the eastern and western parts of the cluster. 2141 The photographic images of the stars as registered on the E-plate of the POSS are elongated in the field of A2141 defined as the circle of radius R_c centered on the cluster. 2142 Two probable foreground galaxies (S + E) are located in the field of A2142 defined as the circle of radius R_c centered on the cluster. 2146 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) have faint envelopes of luminosity. The cluster is elongated with a position angle of major axis similar to that of the line connecting #1 and #2. 2150 Foreground galaxies are superimposed on the cluster; it is difficult to separate the populations. 2151 Hercules cluster. Four b-galaxies are all at the southern edge of the cluster. 2153 Two foreground elliptical galaxies are superimposed on the cluster. 2154 The galaxy which we identify as the second most luminous member of the cluster (#2) has a faint companion galaxy. The galaxy which we identify as the third most luminous member of the cluster (#3) is located far from the main concentration of galaxies. 2157 The cluster is elongated in the approximately north-south direction. 2159 Two foreground Sp galaxies are superimposed on the cluster. 2160 The galaxies which we identify as the first, second, and third most luminous members of the cluster (#1, #2, and #3) are collinear and connected to each other by a bridge of luminosity. A foreground group of galaxies is superimposed on the southern and eastern parts of the cluster. 2161 The cluster is very faint. Foreground galaxies are superimposed on the cluster; it is difficult to separate the populations. 2164 Four foreground spiral galaxies are superimposed on the northern part of the cluster. A foreground elliptical galaxy is superimposed on a region near the center of the cluster. 2165 Foreground spiral galaxies are superimposed on the western, northern, and southeastern parts of the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is possibly a foreground galaxy located in the field of A2165 defined as the circle of radius R_c centered on the cluster. 2168 A foreground group of galaxies is superimposed on a western region of the cluster. 2170 A foreground lenticular galaxy is superimposed on an eastern region of the cluster. 2171 Foreground galaxies are superimposed on the cluster. 2172 A foreground bp-galaxy is superimposed on the cluster. 2175 A star may be superimposed on the cD galaxy. 2176 One foreground spiral galaxy is superimposed on the cluster. 2177 Foreground groups of galaxies are superimposed on the northern and eastern parts of A2177, perhaps at different distances along the line-of-sight. 2181 The cluster looks poorer than is indicated by richness class 1. 2182 A foreground group of galaxies is superimposed on the cluster. R_c' = 6.5 mm on plates of the POSS may be restrictive because other possible subclusters of galaxies are located to the southeast of the circle of radius R_c = 6.5 mm centered on the cluster; we have adopted R_c = 20 mm for the classification of A2182. 2185 R_c is restrictive because other subclusters of galaxies are located to the south of the circle of radius R_c centered on A2185. Leir (1976) notes that the cluster is possibly misidentified, the field is almost bare; however, we believe that Abell's (1958) identification is correct. 2187 Three foreground spiral galaxies are superimposed on a southern region of the cluster. 2190 A foreground spiral galaxy is superimposed on a region near the center of the cluster. An S0_p galaxy is located in the northern part of the cluster. 2191 The cluster is sparse. Foreground spiral galaxies are superimposed on the western and southeastern parts of the cluster. 2192 Four foreground elliptical galaxies are superimposed on the cluster. 2193 Five foreground galaxies (2 S + 3 S0) are superimposed on the cluster. 2194 Four foreground spiral galaxies are superimposed on the cluster. 2195 A foreground group of galaxies is superimposed on the cluster; it is difficult to separate populations. 2198 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the C subcluster. A foreground group of galaxies is superimposed on the northwestern part of the cluster. 2201 A foreground elliptical galaxy is superimposed on the cluster. 2202 A foreground group of spiral galaxies is superimposed on a western region of the cluster. 2203 Two foreground spiral galaxies are superimposed on the cluster. 2204 Two foreground spiral galaxies are superimposed on the cluster. 2206 The cluster is T-shaped. Two foreground spiral galaxies are superimposed on A2206, one on a region near the center of the cluster. 2209 The cluster is small and faint. Two foreground galaxies are superimposed on the western part of the cluster. 2211 Four b-galaxies are located in one subcluster of galaxies. A foreground SB galaxy is superimposed on the northern part of the cluster. 2212 A chain of galaxies is located at the center of the cluster. A foreground group of galaxies is superimposed on a western region of the cluster. 2214 Possible foreground galaxies are located in the field of A2214 defined as the circle of radius R_c centered on the cluster. 2216 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint envelope of luminosity. 2217 The RS type of the cluster is possibly L7. 2218 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. Two bright foreground galaxies (SBc + E) are superimposed on the cluster. 2219 Leir (1976) notes that a subcluster is located to the east of A2219. 2220 Two large galaxies with envelopes of luminosity and companion galaxies (possibly foreground b-galaxies) are located in the field of A2220 centered on the cluster. 2221 Two foreground spiral galaxies are superimposed on the cluster, one on a western region and one on a southwestern region. 2223 Most of the bright galaxies are edge-on with a position angle of major axis almost the same as that of the cluster. 2224 The cluster is compact. 2225 R_c is restrictive because a subcluster of galaxies is located to the northeast of the circle of radius R_c centered on A2225. 2226 Foreground galaxies are superimposed on the western part of the cluster. 2227 A foreground group of galaxies is superimposed on the cluster. 2228 Galaxies are distributed with circular symmetry around the cD galaxy. 2229 A bright foreground SBc galaxy is superimposed on the southeastern part of the cluster. 2231 The two subclusters of galaxies are compact. 2232 The distance class of the cluster is D=7. A foreground b-galaxy is superimposed on the cluster. 2233 Foreground galaxies are superimposed on the cluster. 2234 The cluster is elongated in the approximately east-west direction with a position angle of major axis similar to that of the line connecting the two brightest members of the B cluster. Leir (1976) does not note that the most luminous galaxy in the cluster is a b-galaxy. A foreground S0 galaxy is superimposed on the northern part of the cluster. 2235 The two L subclusters of galaxies are parallel to each other. 2237 R_c is restrictive. 2240 The cluster is poorer than is indicated by richness class 3. Has the cluster possibly been misidentified? 2241 The Abell cluster may be two separate clusters superimposed along the line-of-sight (Spinrad & Bahcall 1976, Publ. Astron. Soc. Pac. 88, 660). 2246 R_c is restrictive. Three bright foreground S0 galaxies are superimposed on the cluster. 2251 Foreground spiral, S0, and elliptical galaxies are superimposed on the cluster. Leir (1976) notes that A2251 is possibly connected to a cluster to the southwest. 2252 A foreground E/S0 galaxy is superimposed on the southern part of the cluster. 2254 The cluster is elongated in the approximately east-west direction with a position angle of major axis approximately perpendicular to that of the b-galaxy which we identify as the most luminous member of the cluster. 2257 One foreground spiral galaxy is superimposed on the cluster. 2258 The cluster contains two faint lines of galaxies which intersect in a bent "t". 2261 The cluster is very circularly symmetric with a circularly symmmetric cD galaxy. 2262 The photographic images of the galaxies as registered on the E-plate of the POSS are faint and fuzzy in the field of A2262 defined as the circle of radius R_c centered on the cluster. Foreground spiral and S0 galaxies are superimposed on the southern part of the cluster, and two elliptical galaxies are superimposed on the western part of the cluster. 2264 A foreground galaxy is superimposed on the southwestern part of the cluster. 2265 The cluster is sparse. Foreground spiral galaxies are superimposed on the western and southern parts of the cluster. 2266 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) have several faint companion galaxies. 2267 The cluster is small and sparse. 2268 This cluster is connected to A2270. R_c is restrictive. A foreground Sb galaxy is superimposed on the western part of the cluster. A foreground b-galaxy is superimposed on a region near the center of the cluster. 2269 The cluster is faint and sparse (if extant at all). Possible foreground galaxies are located in the field of A2269 defined as the circle of radius R_c centered on the cluster. 2270 This cluster is possibly confused with and connected to A2268. 2272 The C10 is the nearer of the two clusters; the cD cluster is the more distant. 2273 Foreground galaxies are superimposed on the cluster; it is difficult to separate populations. 2276 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster and is surrounded by faint companion galaxies. A2276 looks closer than is indicated by distance class 6. 2277 A foreground group of galaxies is superimposed on the eastern part of the cluster. 2278 R_c is restrictive. Foreground galaxies are superimposed on the cluster. 2279 The RS type of the cluster is possibly C4. 2280 This B cluster is elongated with a position angle of major axis similar to that of the line connecting its two brightest members. A bright foreground spiral galaxy is superimposed on the northern part of the cluster. A foreground S0 galaxy is superimposed on a region near the galaxy which we identify as the most luminous member of the cluster (#1). 2281 The galaxy which we identify as the second most luminous member of the cluster (#2) has a close companion galaxy. Two foreground galaxies (S + S0/a) are superimposed on the western part of the cluster. 2282 A foreground group of galaxies is superimposed on the northern part of the cluster. Two spiral galaxies are located in the eastern part of the cluster. 2283 The brightest b-galaxies are parallel to the line of galaxies which characterizes the L cluster. 2285 Three foreground E/S0 galaxies are superimposed on the cluster. The galaxy which Leir (1976) assumes is the most luminous member of the cluster may be a foreground galaxy superimposed on the cluster. 2287 The cluster is faint. Three foreground spiral galaxies are superimposed on A2287. 2289 The cluster is sparse and looks poorer than is indicated by richness class 1. Two foreground S0 galaxies are superimposed on the western part of the cluster. 2291 R_c is restrictive. It is difficult to identify the three brightest galaxies because a bright star is located in the field of A2291 defined as the circle of radius R_c centered on the cluster. 2294 The cD galaxy has a large envelope of luminosity. The cluster is elongated. 2295 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. 2297 One foreground S/S0 galaxy is superimposed on the cluster. 2298 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 2299 Two foreground galaxies are superimposed on the western part of the cluster. 2303 One foreground spiral galaxy is superimposed on the cluster. 2306 One foreground spiral galaxy is superimposed on the cluster. 2307 The galaxy which we identify as the most luminous member of the cluster (#1) has a large circularly symmetric envelope of luminosity. A foreground elliptical galaxy is superimposed on the western part of the cluster. 2310 A foreground group of galaxies is superimposed on an eastern region of the cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is not the galaxy which Leir (1976) assumes is the most luminous member. 2313 The galaxy which we identify as the most luminous member of the cluster (#1) is compact. A foreground S0 galaxy is superimposed on the northeastern part of the cluster. 2314 A foreground group of galaxies is superimposed on northern and eastern regions of the cluster. 2316 The cluster is elongated in the approximately north-south direction. 2317 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) may be a t-galaxy. Foreground galaxies are superimposed on the western part of the cluster. 2318 A foreground group of galaxies is superimposed on a northwestern region of the cluster. 2321 A foreground galaxy is superimposed on the western part of the cluster. 2322 The cluster is sparse. The galaxy which we identify as the second most luminous member of the cluster (#2) has a faint companion galaxy. A large spiral galaxy is located in the southern part of the cluster. A foreground cP galaxy is superimposed on a region near the center of the cluster. 2323 The cluster may possibly be a foreground group of galaxies superimposed on a background group of galaxies. 2324 One foreground Sc galaxy is superimposed on the cluster. 2326 Several foreground galaxies are superimposed on the northeastern and southwestern parts of the cluster. 2327 Possible foreground galaxies are located in the field of A2327 defined as the circle of radius R_c centered on the cluster. 2329 The cluster is faint. 2332 Three foreground S0/a galaxies are superimposed on the eastern part of the cluster. 2334 A bright foreground galaxy is superimposed on the northeastern part of the cluster. 2337 The cluster is very elongated in the approximately east-west direction. Three bright foreground spiral galaxies are superimposed on the cluster. 2338 A large foreground spiral galaxy is superimposed on the cluster. 2340 A diffuse object (probably a foreground Ir galaxy) is located in the field of A2340 defined as the circle of radius R_c centered on the cluster. 2342 The cluster is very elongated in the approximately east-west direction. A2342 is connected to A2344 and possibly overlaps the distance class 5 cluster A2340. 2344 This cluster is connected to A2342. 2345 Two foreground spiral galaxies are superimposed on the cluster. 2350 Two foreground spiral galaxies are superimposed on the cluster. 2352 The cluster is faint and sparse. A foreground P galaxy is superimposed on the eastern part of the cluster; a foreground E/S0 galaxy is superimposed on the southwestern part of the cluster. Several smudges are located on the E-plate of the POSS. 2354 A foreground group of galaxies is superimposed on an eastern region of the cluster. 2355 Foreground spiral galaxies are superimposed on the western and southeastern parts of the cluster. 2356 A line of fainter galaxies is parallel to the line of brighter galaxies which determines the RS type of the cluster. 2358 One subcluster of galaxies located in the northern part of the cluster is "+" shaped. 2360 A foreground S/S0 galaxy is superimposed on the northeastern part of the cluster. 2361 This is a possible L10a cluster. 2364 R_A' = 4 mm (Abell 1979) compared to R_c = 17 mm (Leir and van den Bergh 1977) on plates of the POSS. 2365 A foreground group of galaxies overlaps the cluster. 2366 A possible foreground elliptical galaxy is located in the field of A2366 defined as the circle of radius R_c centered on the cluster. 2367 Two foreground E/S0 galaxies are superimposed on the cluster. The galaxy which we identify as the most luminous galaxy in the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. 2368 The cluster is very elongated in the approximately east-west direction. A foreground cluster is superimposed on the eastern part of the distance class 5 cluster A2368. 2372 Two foreground Sp galaxies are superimposed on the cluster. 2373 Several foreground galaxies are superimposed on the southeastern part of the cluster. 2374 Three foreground spiral galaxies are superimposed on the cluster. 2375 One foreground S0 galaxy is superimposed on the cluster. 2380 Three foreground E/S0 galaxies are superimposed on the western part of the cluster. 2384 The centers of the two subclusters of galaxies are separated by 9.9 mm on plates of the POSS. 2385 One foreground S0/Ep galaxy is superimposed on the cluster. 2386 A crowded star field is superimposed on the cluster. Foreground galaxies are superimposed on the northern, western, and southern parts of the cluster. 2391 Is the cluster closer than is indicated by distance class 5? 2392 The galaxies which we identify as the first and third most luminous members of the cluster (#1 and #3) are close such that together they constitute a possible a t-galaxy. The cluster is compact and sparse. A2392 looks like a cluster of richness class 0. 2393 The cluster is compact. 2396 A foreground spiral galaxy is superimposed on the northeastern part of the cluster. 2397 A foreground diffuse object (possibly an IB galaxy as indicated by visual inspection of the O-plate of the POSS) is superimposed on the southeastern part of the cluster. Two foreground spiral galaxies are superimposed on the eastern part of the cluster, and two galaxies with undetermined morphological type are superimposed on the northern part of the cluster. 2400 R_c is restrictive. 2402 Is the cluster closer than is indicated by distance class 5? 2404 A foreground spiral galaxy is superimposed on the eastern part of the cluster. 2405 A foreground group of galaxies is superimposed on an eastern region of the cluster. 2406 The cluster is faint. A foreground spiral galaxy is superimposed on the northeastern part of the cluster. 2408 Two foreground galaxies (E/S0 + S) are superimposed on the cluster. 2412 The cluster is sparse. 2413 A foreground Sa galaxy is superimposed on the northeastern part of the cluster. 2414 Is the cluster closer than is indicated by distance class 5? 2416 The rectangular coordinates of the cluster as registered on plates of the POSS are X = 277 mm, Y = 77 mm. Two foreground spiral galaxies are superimposed on the western part of the cluster. 2418 Three foreground elliptical galaxies are superimposed on the cluster, one on a southeastern region, one on a southwestern region, and one on a northwestern region. 2419 The cluster is very sparse. R_c is very restrictive. 2422 The galaxy which we identify as the most luminous member of the cluster (#1) has several close companion galaxies. The cluster has a compact core. 2423 Two foreground spiral galaxies are superimposed on the cluster, one on a northern region and one on a southern region. 2424 Two foreground spiral galaxies are superimposed on the western part of the cluster. 2426 One foreground S0 galaxy is superimposed on the cluster. 2428 Two foreground E/S0 galaxies are superimposed on the cluster. 2429 This cluster is connected to A2431. Two foreground spiral galaxies are superimposed on the southeastern part of the cluster. 2430 This cluster is a good example of an F (I_s + I_s) cluster of galaxies. Four foreground spiral galaxies are superimposed on the cluster, two in the northeastern and two in the northwestern parts of the cluster. 2431 The cluster is faint. A2431 is connected to A2429. Two foreground spiral galaxies are superimposed on the western part and two foreground spiral galaxies are superimposed on the southern part of the cluster. The photographic images of the stars on the E-plate of the POSS are elongated in the field of A2431 defined as the circle of radius R_c centered on the cluster. 2432 The galaxy which we identify as the most luminous member of the cluster (#1) is connected by a bridge of luminosity to a faint companion galaxy. Two foreground spiral galaxies are superimposed on the cluster, one on a northern region and one on a western region. 2434 One foreground spiral galaxy is superimposed on the cluster. 2435 This cluster is connected to A2431 and A2429. Two foreground E/S0 galaxies are superimposed on A2435, one on a region near the center of the cluster and one on its eastern part. 2436 The galaxies which we identify as the first, second, and third birightest members of the cluster (#1, #2, and #3) are all edge-on galaxies. #1 is different from the galaxy which Leir (1976) assumes is the most luminous member. Two foreground S0 galaxies are superimposed on the cluster. 2438 The Abell cluster is possibly the superposition of two clusters located at different distances along the line-of-sight. 2444 The cluster is faint. A foreground spiral galaxy is superimposed on the southern part of the cluster. 2446 Is the cluster more distant than is indicated by distance class 5? A foreground Sc galaxy is superimposed on the cluster. 2447 Three main clumps of galaxies characterize the cluster. 2451 The cluster is sparse. 2452 This cluster is connected to A2450. Two foreground spiral galaxies are superimposed on the eastern part of the cluster. A diffuse galaxy (Hubble type SB:) is located in the southeastern part of the cluster. 2454 Two foreground spiral galaxies are superimposed on the cluster. R_c is restrictive. 2456 Two foreground galaxies (E + SB) are superimposed on the cluster. 2458 One foreground Sc galaxy is superimposed on the cluster. 2460 R_c is restrictive. Two foreground spiral galaxies are superimposed on the cluster. 2463 Two foreground spiral galaxies are superimposed on the cluster. 2464 A foreground group of galaxies is superimposed on the southern part of the cluster. 2466 Two foreground spiral galaxies are superimposed on the northern part of the cluster. A foreground b-galaxy is superimposed on the eastern part of the cluster. 2468 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint envelope of luminosity. Two foreground galaxies are superimposed on the northern part of the cluster. Two foreground galaxies are superimposed on the cluster, a bright foreground SB galaxy on a southern region and an Sa galaxy on a northeastern region. 2469 R_c is restrictive. A foreground Sb galaxy is superimposed on the cluster. 2470 A foreground spiral galaxy is superimposed on the cluster. 2471 This cluster is connected to A2475. Several foreground spiral and S0 galaxies are superimposed on A2471. 2472 The cluster is faint. 2473 Two bright foreground S0 galaxies are superimposed on a region near the center of the cluster. A foreground group of galaxies is superimposed on the southwestern and eastern parts of the cluster; it is difficult to separate populations. 2475 The galaxy which we identify as the third most luminous galaxy in the cluster (#3) has jets of luminosity. A2475 is connected to A2471. 2476 A foreground group of galaxies is superimposed on the western part of the cluster. 2477 Two foreground spiral galaxies are superimposed on the cluster. 2478 The galaxy which we identify as the most luminous member of the cluster (#1) is located near center of the cluster. It is difficult to identify the third most luminous member of the cluster (#3). Two foreground galaxies are superimposed on the western part of the cluster. 2481 Two foreground galaxies are superimposed on the northwestern parts of the cluster. 2482 The galaxy which we identify as the third most luminous member of the cluster (#3) has one companion galaxy with a large envelope of luminosity. 2483 The cluster is elongated. It is difficult to identify the third most luminous member of the cluster (#3). 2484 R_c is restrictive. The cluster is very faint. A foreground group of galaxies overlaps the cluster. 2487 A foreground E/S0 galaxy is superimposed on the northern part of the cluster. 2488 A foreground b-galaxy is superimposed on the southern part of the cluster; two foreground E/S0 galaxies are superimposed on the northern part of the cluster. 2489 The cluster is very faint and elongated. 2491 The cluster is compact. 2495 Is the cluster closer than is indicated by distance class 5? 2497 The cluster is sparse. Two foreground P galaxies (one with jets of luminosity?) are superimposed on the southern part of the cluster. A defect on the E-plate of the POSS is located in an eastern field of A2497. 2499 R_c is restrictive. A foreground group of galaxies is superimposed on a western region of the cluster. 2500 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) are located in chains of galaxies. 2501 Five foreground galaxies (4 S + b) are superimposed on the cluster. A foreground group of galaxies is superimposed on the western part of the cluster. 2502 One foreground spiral galaxy is superimposed on the cluster. 2503 Most clumps of galaxies are elongated in the same direction. A possible foreground SB(r) galaxy is located in the field of A2503 defined as the circle of radius R_c centered on the cluster. 2505 The galaxy which we identify as the most luminous member of the cluster (#1) is surrounded by six b-galaxies. Several bright edge-on galaxies are located in the southern part of the cluster. A foreground Sbc galaxy is superimposed on the eastern part of the cluster and a foreground Sc galaxy is located in the northern part of the cluster. A2505 looks like a cluster of distance class 5. 2506 A foreground spiral galaxy is superimposed on the cluster. 2507 The galaxy which we identify as the most luminous member of the cluster (#1) has an envelope of luminosity and two close companion galaxies. 2508 The galaxy which we identify as the most luminous member of the cluster (#1) has a close companion galaxy. A possible foreground spiral galaxy is located in a field near the center of the cluster. 2509 Three foreground spiral galaxies are superimposed on the cluster. A possible background B_b cluster is located in the field of A2509 defined as the circle of radius R_c centered on the cluster. 2510 R_c is restrictive. 2513 The cluster is very faint and elongated in the approximately east-west direction. Five foreground spiral galaxies are superimposed on the cluster. 2514 The cluster is characterized by two elongated subclusters of galaxies. A foreground b-galaxy is superimposed on the southwestern part of the cluster. 2515 The cluster is compact and elongated. A local minimum is visible in the radial distribution of surface number density of galaxies in the cluster. 2516 Three foreground S/S0 galaxies are superimposed on the cluster. 2517 The galaxy which we identify as the most luminous member of the cluster (#1) has a close companion galaxy. 2518 A foreground Sc galaxy is superimposed on the cluster. 2520 The cluster is elongated. Two foreground spiral galaxies are superimposed on the cluster, one on a northern region and one on a southeastern region. A2520 is connected to A2522. 2522 Two foreground spiral galaxies are superimposed on the eastern part of the cluster. A2522 is connected to A2520. 2523 Leir (1976) notes that the cluster is characterized by two concentrations of galaxies. The galaxy which we identify as the second most luminous member of the cluster (#2) contains a luminous jet. 2527 The cluster is elongated. A foreground E/S0 galaxy is superimposed on the northern part of the cluster. 2530 A foreground group of galaxies is superimposed on a northern region of the cluster. 2531 One foreground spiral galaxy is superimposed on the cluster. 2532 The galaxy which we identify as the second most luminous member of the cluster (#2) has two faint companion galaxies. 2534 This cluster is connected to A2536. A foreground group of galaxies is superimposed on the western part of the cluster. 2536 This cluster is connected to A2534. A foreground spiral galaxy is superimposed on the eastern part of the cluster. 2537 The cluster is very faint. 2540 Many galaxies are distributed in an annulus around the core of the cluster. 2541 Two foreground spiral galaxies are superimposed on the cluster. 2542 The rectangular coordinates of the cluster as registered on plates of the POSS are X = 100 mm, Y = 97 mm. 2543 The RS type of the cluster is possibly L4a. The cluster is sparse. 2545 The cluster is sparse. A foreground spiral galaxy is superimposed on the cluster. 2546 One foreground spiral galaxy is superimposed on the cluster. 2548 A chain of t-galaxies is located in the cluster. Two foreground S/S0 galaxies are superimposed on the cluster. 2549 Two foreground spiral galaxies are superimposed on the cluster. 2550 This cluster overlaps A2554 and A2556. 2551 A foreground group of galaxies is superimposed on the northern and southern parts of the cluster. 2552 Two foreground galaxies are superimposed on the western part of the cluster. One foreground spiral galaxy is superimposed on the eastern part of the cluster. 2553 The galaxy which we identify as the most luminous member of the cluster (#1) has an asymmetric envelope of luminosity. The galaxy which we identify as the third most luminous member of the cluster (#3) has two faint companion galaxies. The cluster is asymmetric and contains subclusters each with a membership of several spiral galaxies. 2558 Is the cluster closer than is indicated by distance class 5? 2560 A foreground spiral galaxy is superimposed on a region near the center of the cluster. 2562 The cluster is small and compact. 2563 The cluster is sparse. 2566 The galaxy which we identify as the most luminous member of the cluster (#1) is possibly a pre-cD galaxy. 2567 Foreground spiral and S0 galaxies are superimposed on the northern and southern parts of the cluster. 2568 Two foreground Sc galaxies are superimposed on the cluster. 2569 Is the cluster closer than is indicated by distance class 5? 2571 The galaxy which we identify as the most luminous member of the cluster (#1) has faint companion galaxies. A2571 is connected to A2573. A2571 looks closer than is indicated by distance class 6. 2573 This cluster is connected to A2571. 2573C The RS type of the cluster is possibly B. 2574 Leir (1976) notes that the cluster has possibly been mis-identified and is possibly part of a group of galaxies to the northeast of the cluster. 2575 The cluster is elongated. Foreground S/S0 galaxies are superimposed on the southeastern and eastern parts of the cluster. 2576 Two main subclusters of galaxies characterize the cluster. A foreground elliptical galaxy is superimposed on the southwestern part of the cluster. Leir (1976) does not note that the galaxy which he assumes is the most luminous member of the cluster is a b-galaxy. 2577 In its southeastern part, the cluster overlaps and is confused with the distance class 5 cluster A2580. 2578 Two bright foreground S0 galaxies are superimposed on the western part of the cluster. 2580 Two foreground S0 galaxies are superimposed on the cluster. 2581 The cluster is elongated. 2582 A foreground spiral galaxy is superimposed on the southern part of the cluster; a foreground peculiar galaxy is superimposed on the eastern part of the cluster. 2585 This is an open cluster. The rectangular coordinates of the cluster as registered on plates of the POSS are X = 263 mm, Y = 14 mm. 2586 A foreground S/S0 galaxy is superimposed on the cluster. 2587 R_c is very restrictive. 2588 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. A foreground spiral galaxy is superimposed on a region near the center of the cluster. Two foreground spiral galaxies are superimposed on the northern part of the cluster. 2590 Four foreground spiral galaxies are superimposed on the cluster. 2592 A foreground group of spiral galaxies is superimposed on an eastern region of the cluster. 2593 The cD galaxy is an outlying member of the cluster; possibly the Abell cluster is two separate clusters at different distances. A possible foreground group of spiral galaxies is located in the field of A2593 defined as the circle of radius R_c centered on the cluster. 2594 A foreground spiral galaxy is superimposed on the eastern part of the cluster. 2596 Two foreground spiral galaxies are superimposed on the cluster. 2601 Several edge-on spiral galaxies are located in the I_s subcluster; Two foreground spiral galaxies are superimposed on the southeastern part of the cluster. 2602 Are jets of luminosity located on the galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2)? A foreground spiral galaxy is superimposed on the northern part of the cluster. 2603 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) each have a faint envelope of luminosity. A foreground spiral galaxy is superimposed on the northern part of the cluster. 2604 A foreground S0 galaxy is superimposed on the cluster. 2606 Two foreground galaxies (S + E) are superimposed on the cluster. 2607 A large foreground S0 galaxy is superimposed on the northeastern part of the cluster. 2609 The cluster is very elongated. The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. The galaxies which we identify as the second and third most luminous members of the cluster (#2 and #3) are very close to each other; #2 + #3 is possibly a t-galaxy. Two foreground S/S0 galaxies are superimposed on the northeastern part of the cluster. 2611 The galaxy which we identify as the most luminous member of the cluster (#1) is different from the galaxy which Leir (1976) assumes is the most luminous member. 2612 The cluster is very faint. 2614 A foreground S/S0 galaxy is superimposed on the northern part of the cluster; two foreground E/S0 galaxies are superimposed on the cluster, one on a southern region and one on a southwestern region. 2615 Several lines of galaxies are located in the cluster. A foreground group of galaxies is superimposed on the northwestern part of the cluster; two foreground spiral galaxies are superimposed on the eastern part of the cluster. 2617 Two foreground spiral galaxies are superimposed on the cluster. 2619 Three foreground spiral galaxies are superimposed on the cluster. 2620 Leir (1976) notes that the Abell cluster is characterized by two concentrations of galaxies, possibly separate clusters. Four foreground spiral galaxies are located in the eastern part of the cluster; one foreground spiral galaxy is superimposed on a region near the center of the cluster. 2621 Foreground spiral galaxies are superimposed on the northern and western parts of the cluster. 2624 In its western part, the cluster overlaps the distance class 5 cluster A2623. Two foreground spiral galaxies are superimposed on the eastern part, and one spiral galaxy is superimposed on the southwestern part of the cluster. 2628 A foreground spiral galaxy is superimposed on the eastern part of the cluster; a foreground diffuse P galaxy is superimposed on the northern part of the cluster. 2629 R_c is restrictive. A foreground group of spiral galaxies is superimposed on the southern part of the cluster. One foreground spiral galaxy is superimposed on the northern part of the cluster. 2630 Two foreground galaxies (Ep + S0p) are superimposed on the cluster. 2631 The galaxy which we identify as the most luminous member of the cluster (#1) does not have an envelope of luminosity but is surrounded by companion galaxies. A bright Sbc galaxy is located in the northern part of the cluster. 2633 Four foreground galaxies are superimposed on the western part of the cluster; two foreground galaxies are superimposed on the southeastern part of the cluster. 2635 This cluster is elongated in the approximately east-west direction. 2635X The galaxies which we identify as the first and third most luminous members of the cluster (#1 and #3) have close companion galaxies. 2636 Leir (1976) notes the presence of subclusters of galaxies. Three foreground spiral galaxies are superimposed on the western part of the cluster. 2638 Several foreground spiral galaxies are superimposed on the cluster. 2639 The cluster looks closer than is indicated by distance class 6. 2641 The cluster is very faint. A2641 is characterized by two main clumps of galaxies, which are elongated and roughly parallel to each other. 2643 Leir (1976) notes that the cluster is characterized by two groups of galaxies. A bright foreground group of spiral galaxies is superimposd on the cluster. 2644 One foreground spiral galaxy is superimposed on the cluster. 2645 The galaxy which we identify as the most luminous member of the cluster (#1) is located near the center of the cluster. Two foreground galaxies are superimposed on the southern part of the cluster. 2646 R_c is restrictive. A foreground spiral galaxy and elliptical galaxy are superimposed on the southern part of the cluster. A foreground SBcp galaxy is superimposed on the northwestern part of the cluster. 2647 A possible foreground galaxy is located in the field of the cluster defined as the circle of radius R_c. 2648 Several bright spiral galaxies are located in the cluster. Three foreground spiral galaxies are superimposed on the northern part of the cluster. A foreground b-galaxy is superimposed on the northeastern part of the cluster. 2650 A chain of faint galaxies is located at the center of the cluster. 2652 A foreground E/S0 galaxy is superimposed on the eastern part of the cluster. 2653 A bright star is superimposed on the cluster near the galaxy which we identify as the third most luminous member of the cluster (#3). 2658 A foreground group of galaxies is superimposed on the northwestern part of the cluster. 2659 Two foreground spiral galaxies are superimposed on the cluster. 2661 The subclusters of galaxies are arranged in an approximately collinear configuration. 2662 Leir (1976) notes that many bright galaxies are located near the periphery of the cluster. Three foreground galaxies are superimposed on the eastern part of the cluster. 2663 R_c is restrictive. 2664 The cluster is elongated and possibly a cD cluster. The galaxy which we identify as the most luminous member of the cluster (#1) is located in a region near the center of the cluster. The photographic images of galaxies as registered on the E-plate of the POSS are poor. 2667 The cluster is very faint. Three foreground galaxies (2 E/S0 + b) are superimposed on the northern part of the cluster. 2668 Two foreground galaxies (S + E/S0) are superimposed on the cluster. 2669 The cluster is faint. The galaxy which we identify as the most luminous member of the cluster (#1) has a jet of luminosity or a close companion galaxy. 2670 This is a good example of a cD cluster. 2671 A foreground spiral galaxy is superimposed on a region near the center of the cluster. 2672 Three foreground galaxies (S + S0 + b) are superimposed on the cluster. 2676 Two foreground galaxies (S + S0) are superimposed on the cluster. 2678 A chain of galaxies is located in the field of A2678 defined as the circle of radius R_c centered on the cluster. One foreground spiral galaxy is superimposed on the cluster. 2679 The galaxy which we identify as the most luminous member of the cluster (#1) has a faint companion galaxy. The rectangular coordinates of the cluster as registered on plates of the POSS which were derived by Leir (1976) are X = 186 mm, Y = 329 mm. A2679 is connected to A2682. 2680 The L subcluster seems to point towards the C subcluster. Leir (1976) indicates that the Abell cluster could be the superposition of two clusters located at different distances along the line-of-sight. 2681 This cluster is connected to A2685. Two foreground E/S0 galaxies are superimposed on the northern part of the cluster. 2682 This cluster is connected to A2679. 2683 Two foreground spiral galaxies are superimposed on the cluster. 2684 Two foreground galaxies (S0 + b) are superimposed on the northern part of the cluster. 2685 The cluster is open. A2685 is connected to A2681. 2688 A foreground cE galaxy is superimposed on the northern part of the cluster. A foreground spiral galaxy is superimposed on the southwestern part of the cluster. 2689 A foreground group of galaxies is superimposed on the western part of the cluster. 2691 Three foreground spiral galaxies are superimposed on the cluster. 2695 Two bright foreground spiral galaxies are superimposed on the northern part of the cluster. 2696 A chain of galaxies points toward the cD galaxy. 2697 The galaxy which we identify as the most luminous member of the cluster (#1) has a companion galaxy. 2698 The cluster is elongated with a position angle of major axis similar to that of the cD galaxy. 2699 Two foreground galaxies are superimposed on the cluster, one on a northern region and one on a southern region. 2701 A foreground spiral galaxy is superimposed on the northeastern part of the cluster. 2702 A foreground SBc galaxy is superimposed on the cluster. 2703 A foreground SBc galaxy is superimposed on the cluster. 2704 The galaxies which we identify as the first and second most luminous members of the cluster (#1 and #2) are very close to each other. #1 has a faint companion galaxy. 2705 Two foreground galaxies (SBc + S) are superimposed on the cluster. 2708 The three b-galaxies are all in the northwestern part of the cluster. 2711 A bright spiral galaxy is located in the eastern part of the cluster. 2712 A foreground group of galaxies is superimposed on the western part