Types for seventy-six clusters are given in Table 2. Column (1) gives a running number; column (2), the Abell number, with asterisks used in the sense defined by Abell (1958), i.e., the cluster does not meet the requirements for inclusion in the statistical sample; columns (3) and (4), distance and richness classes from Abell; and column (5), the type as determined from paper prints and the glass second-negative copy of the National Geographic Society - Palomar Observatory Sky Survey at the Yerkes Observatory. The final two entries (Hya A and Cyg A) were classified from photographs reproduced in Matthews, Morgan, and Schmidt (1964) and the Notes to Table 1 of that paper.
Table 2 is divided into three sections. The first section gives clusters of distance classes less than 4, for which fairly good types could be derived from the second negatives of the Sky Survey plates. Five clusters with uncertain types (followed by a colon) have been included because of features of special interest. The second section lists the nine richest clusters in Abell's catalog, together with A2029 and A2670, which are good examples of Class I (and which are illustrated in Matthews et al. 1964). The last section of the table consists of two entries, the clusters containing the radio galaxies Hya A and Cyg A.
| No. | Abell Cluster | D | R | Type | No. | Abell Cluster | D | R | Type |
| 1 | Abell 0014* | 3 | 0 | III: | 41 | Abell 1736* | 2 | 0 | III |
| 2 | Abell 0102* | 3 | 0 | II-III | 42 | Abell 1781* | 3 | 0 | III |
| 3 | Abell 0119 | 3 | 1 | II-III | 43 | Abell 1800 | 3 | 0 | I-II |
| 4 | Abell 0147* | 3 | 0 | III | 44 | Abell 1831 | 3 | 1 | II-III |
| 5 | Abell 0151 | 3 | 1 | II | 45 | Abell 1904 | 3 | 2 | II |
| 6 | Abell 0154 | 3 | 1 | I-II | 46 | Abell 1983 | 3 | 1 | III |
| 7 | Abell 0168 | 3 | 2 | III | 47 | Abell 2022 | 3 | 1 | III |
| 8 | Abell 0179* | 3 | 0 | III | 48 | Abell 2052 | 3 | 0 | Note |
| 9 | Abell 0194* | 1 | 0 | II | 49 | Abell 2063 | 3 | 1 | II-III |
| 10 | Abell 0240* | 3 | 0 | II-III | 50 | Abell 2065 | 3 | 2 | III |
| 11 | Abell 0262* | 1 | 0 | III | 51 | Abell 2079 | 3 | 1 | III |
| 12 | Abell 0347* | 1 | 0 | II-III | 52 | Abell 2124 | 3 | 1 | I |
| 13 | Abell 0397* | 3 | 0 | III | 53 | Abell 2151 | 1 | 2 | III |
| 14 | Abell 0399 | 3 | 1 | I-II | 54 | Abell 2152 | 1 | 1 | III |
| 15 | Abell 0400 | 1 | 1 | II-III | 55 | Abell 2197 | 1 | 1 | II |
| 16 | Abell 0401 | 3 | 2 | I | 56 | Abell 2199 | 1 | 2 | I |
| 17 | Abell 0426* | 0 | 2 | II-III | 57 | Abell 2247* | 3 | 0 | III |
| 18 | Abell 0539* | 2 | 1 | III | 58 | Abell 2255 | 3 | 2 | II-III |
| 19 | Abell 0548* | 1 | 1 | III | 59 | Abell 2256 | 3 | 2 | III |
| 20 | Abell 0576 | 2 | 1 | III | 60 | Abell 2399 | 3 | 1 | III |
| 21 | Abell 0595* | 3 | 0 | III: | 61 | Abell 2589* | 3 | 0 | I |
| 22 | Abell 0634* | 3 | 0 | III | 62 | Abell 2634* | 1 | 1 | I-II: |
| 23 | Abell 0671* | 3 | 0 | II | 63 | Abell 2657 | 3 | 1 | II-III |
| 24 | Abell 0757* | 3 | 0 | III | - - | - - - | - | - | - - |
| 25 | Abell 0779* | 1 | 0 | II | 64 | Abell 0545* | 5 | 4 | III |
| 65 | Abell 0665 | 6 | 5 | II-III | |||||
| 26 | Abell 0838* | 3 | 0 | III | |||||
| 27 | Abell 0993* | 3 | 0 | III | 66 | Abell 0777 | 6 | 4 | II-III |
| 28 | Abell 1035 | 3 | 2 | III | 67 | Abell 0910 | 6 | 4 | II |
| 29 | Abell 1060* | 0 | 1 | III | 68 | Abell 1146* | 5 | 4 | I |
| 30 | Abell 1069* | 3 | 0 | III | 69 | Abell 1689 | 6 | 4 | I-II |
| 70 | Abell 2029 | 4 | 2 | I | |||||
| 31 | Abell 1142* | 3 | 0 | II-III: | |||||
| 32 | Abell 1213 | 2 | 1 | III | 71 | Abell 2125 | 6 | 4 | II or II-III |
| 33 | Abell 1225* | 3 | 0 | III | 72 | Abell 2218 | 6 | 4 | II-III |
| 34 | Abell 1228 | 1 | 1 | III | 73 | Abell 2645 | 6 | 4 | (I or II)?? |
| 35 | Abell 1257* | 3 | 0 | III | 74 | Abell 2670 | 4 | 3 | I |
| -- | - - - | - | - | - - | |||||
| 36 | Abell 1291 | 3 | 1 | III | 75 | Hya A | I | ||
| 37 | Abell 1367 | 1 | 2 | II-III | 76 | Cyg A | I | ||
| 38 | Abell 1436 | 3 | 1 | III | |||||
| 39 | Abell 1656 | 1 | 2 | II | |||||
| 40 | Abell 1691 | 3 | 1 | II-III | |||||
| Notes to Table 2 | |||||||||
| No. 1. II-III? Red [D] galaxy centrally located.
No. 2. Wide double nucleus in common envelope. No. 4. Centrally placed [E3: + E:] in common envelope. No. 6. Two widely separated nuclei in common envelope. No. 9. 3C 040 [D + E] in common envelope. (Matthews, Morgan, and Schmidt 1964): "cD3 in D4 envelope. Brightest galaxy in cluster . . . secondary galaxy in edge of envelope." No. 10. Double nucleus in common envelope. No. 11. Centrally placed [D] with extended envelope. No. 12. 3C 066 No. 13. [D] galaxy with extended envelope. No. 15. 3C 075 [E: + E:] in common envelope. No. 17. 3C 083.1 Brightest galaxy [E2p]. Perseus Cluster. No. 21. Two [E:] galaxies in common envelope. No. 26. Two [E1:] galaxies in common envelope. No. 27. [D] galaxy with extended envelope. No. 28. Brightest galaxy [E:]. No. 31. Brightest [E? + E?] in common envelope. No. 36. [D] galaxy with extensive envelope. No. 38. Two [E?] galaxies in common envelope. No. 39. Coma Cluster. No. 47. [D] galaxy in central region. No. 48. 3C 317 Size, I-II; relative luminosity, II. (Matthews et al. 1964): "cD2 in D4 envelope. Three condensations in - or projected on - envelope. Outstandingly brightest galaxy in cluster." No. 50. Centrally placed [E1: + E2:] in common envelope. Corona Borealis Cluster. No. 51. Centrally placed [D:] with narrow extended envelope. No. 56. 3C 338 = NGC 6166. (Matthews et al. 1964): "Three secondary components in same envelope." No. 57. Chain of five [E] galaxies. No. 58. [D + D?] with extended envelope. No. 62. 3C 465 = NGC 7720. (Matthews et al. 1964): "Cluster ill-defined. [D2 in asymmetric D4 envelope]. Round, bright companion in same envelope." No. 64. Cluster in form of irregular closed loop with density minimum at center. No. 65. Refers to inner subclustering; brightest galaxy probably in elongated envelope. Thick outer arc of galaxies. Cluster very irregular. No. 66. Inner subclustering with [E? + E?] possibly in common envelope. Irregular cluster. No. 67. Like Coma, but richer. Two dominating galaxies: centrally located [D]; non-descript bright galaxy in southern part of cluster. Irregular; lumpy distribution of subclusterings. No. 68. [cD] in extended envelope located in densest part of clustering, which extends farthest toward south. No. 69. Three very bright [E?] possibly in common envelope. Cluster regular. No. 71. Irregular; very distant. Class would be II in subclustering containing brightest [E? + E?]. No. 72. [D] near center, with very large envelope. Cluster fairly regular. No. 73. Very distant. No. 75. 3C 218. The classification was made from two illustrations in Matthews et al. (1964), and from the following note from the same source: "[cD2], Double nucleus; not completely resolved. There is another galaxy in the outer envelope. In poor, faint cluster; very much brighter than any other cluster member." Also (Maltby, Matthews, and Moffet 1963): "The optical identification, first noted by Minkowski, is a very close pair of elliptical galaxies having a common envelope." (See also Dewhirst 1959.) No. 76. 3C 405. The classification was made from two illustrations in Matthews et al. (1964), and from the following note from the same source: "[cD3]. Double nucleus. Outstandingly brightest member of a cluster of richness 2." | |||||||||