Historical Identification: Per Dreyer, NGC 7250 (= GC 4778 = WH III 864, 1860 RA 22 12 29, NPD 50 08.2) is "very faint, small, much extended 165 ." The position precesses to RA 22 18 29.6, Dec +40 33 47, about 2.2 arcmin (12 seconds of time) east of the galaxy listed above, but the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 865 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7250 is about 40 million light-years away, in almost inevitable agreement with widely varying redshift-independent distance estimates of about 30 to 100 million light-years (the HST press release uses a distance of about 45 million light-years, so 40 to 45 million light-years would appear to be a reasonable estimate of the galaxy's actual distance). Given that and its apparent size of about 2.0 by 0.9 arcmin (from the images below), the galaxy is about 25 thousand light-years across.
 In the second image below, NGC 7250 is the galaxy at the center. The group of three bright blue knots above center is listed as a quarter arcmin wide galaxy (PGC 214816) in LEDA and as a result, NED lists NGC 7250 as part of a pair; but the HST image shows that the supposed companion is a gigantic star-forming region in NGC 7250 (as a result of which, it is listed as a starburst galaxy).

Historical Identification: Per Dreyer, NGC 7251 (= GC 4779 = JH 2158 = WH III 933, 1860 RA 22 12 53, NPD 106 27.8) is "faint, pretty small, round, gradually pretty much brighter middle." The position precesses to RA 22 20 26.9, Dec -15 45 42, about 0.7 arcmin north-northwest of the galaxy listed above and barely outside its northern outline, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4535 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7251 is about 210 to 215 million light-years away. Given that and its apparent size of about 1.35 by 1.1 arcmin for the central galaxy and about 2.1 arcmin for the outer arms (from the images below), the central galaxy is about 80 to 85 thousand light-years across, and its outer arms are about 130 thousand light-years in diameter.

Historical Identification: Per Dreyer, NGC 7252 (= GC 4780 = JH 3934 = WH III 458, 1860 RA 22 12 58, NPD 115 22.7) is "faint, small, round, extremely mottled but not resolved." The position precesses to RA 22 20 46.3, Dec -24 40 35, only 0.3 arcmin from the center of the galaxy listed above and well within its bright central portion, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: NGC 7252 is a pair of colliding galaxies well on the way to becoming a single galaxy, which displays a complex structure of stellar filaments surrounding the central core, and flung far into intergalactic space (this gives the galaxy an appearance similar to the diagram of an atom used as part of President Eisenhower's "Atoms for Peace" program's logo, and led to the galaxy's nickname). Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4485 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7252 is about 205 to 210 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 185 to 195 million light-years. Given that and its apparent size of about 2.3 by 2.1 arcmin for the central galaxy and its bright surroundings and about 8.5 by 3.2 arcmin for its far-flung extensions (from the images below), the central galaxy is about 140 thousand light-years across, while its extensions span more than 500 thousand light-years.
 NGC 7252 contains over 500 very bright, unusually blue globular clusters, whose hot young stars have Main Sequence lifetimes between 50 and 500 million years. The globular clusters in most galaxies are 12 to 13 billion years old, and contain only relatively faint, cool Main Sequence stars such as the Sun, and still fainter, cooler stars. The young globulars in NGC 7252 must be a by-product of a collision less than a billion years ago which is turning two spiral galaxies into a larger elliptical (although at the moment the core of the galaxy still looks more like a spiral than anything else). The idea that large elliptical galaxies form from such collisions has been around for a while, but galaxies that have had recent collisions have far more globular clusters than would be expected from the combination of the smaller galaxies which formed them. NGC 7252 and NGC 7257 show that this anomaly can be explained by the formation of new globulars during the collision.
Use By The Arp Atlas: NGC 7252 is used by the Arp Atlas of Peculiar Galaxies as an example of a galaxy with amorphous spiral arms, with the note "Loops, filaments at various angles."

Historical Identification: Per Dreyer, NGC 7253 (= GC 6037, Marth #471, 1860 RA 22 13 01, NPD 61 19) is "very faint, pretty extended." The position precesses to RA 22 19 25.9, Dec +29 23 03, about 0.8 arcmin south-southwest of the brighter member of the pair of galaxies listed above, and about 0.6 arcmin west-southwest of the average position of the two galaxies, the description fits (though it is not as clear as needed to solve one problem) and there is nothing nearby except the pair, so the identification is certain, except for one thing. Namely, should NGC 7253 be both members of the pair, or only the brighter one? Since the two positional errors noted above are nearly the same, they can't be used to tell whether Marth saw the pair as a single nebulous object or only saw the brighter galaxy (namely, the northwestern one). Because of this, some sources consider NGC 7253 to be only the brighter galaxy, and others (such as this entry) treat both galaxies as part of NGC 7253.
Physical Information: NGC 7253 is a pair of interacting spiral galaxies, which means that they must be at the same distance from us. Based on PGC 68572's recessional velocity relative to the Cosmic Microwave Background radiation of 4235 km/sec and PGC 68573's recessional velocity of 4165 km/sec, their average recessional velocity is about 4200 km/sec, which (using H₀ = 70 km/sec/Mpc), yields a Hubble Flow distance of about 195 million light-years for the pair, in good agreement with redshift-independent distance estimates of about 120 to 235 million light-years. Given that, PGC 68572's apparent size of about 1.65 by 0.7 arcmin including its western plume (from the images below) corresponds to a physical size of about 95 thousand light-years, while PGC 68573's apparent size of about 1.55 by 0.5 arcmin including its eastern and western plumes (also from the images below) corresponds to 85 to 90 thousand light-years, and the overall apparent size of the system of about 2.35 by 1.2 arcmin (also from the images below) corresponds to 130 to 135 thousand light-years.
Use By The Arp Atlas: NGC 7253 is used by the Arp Atlas of Peculiar Galaxies as an example of interacting galaxies, with the note "Position of large spiral. Bright long well defined arms, but, smooth, not patchy," position referring to the coordinates given in the table which specifies that Arp 278 is NGC 2753, and the description presumably referring to the appearance of the larger galaxy.

Historical Identification: Per Dreyer, NGC 7254 (Muller list II (#467), 1860 RA 22 14 20, NPD 112 26.0) is "very faint, very small, round, 11th magnitude star preceding (to west) 4.5 arcmin ." The position precesses to RA 22 22 02.9, Dec -21 43 46, and although there is nothing there, there is a galaxy which exactly fits the description (including the position of the star to its west) about 33 seconds of time to the east, and there is nothing else anywhere nearby, so the identification of that galaxy (namely, the one listed in the title for this entry) is certain. The second IC notes "7254 = 7256, NPD is 112 26.5, Howe," so the duplicate listing has been known for more than a century.
Identification Note: Dreyer only quoted part of Howe's statement in the IC2. It actually read "7254 and 7256. These are identical. The place of 7254 is wrong in right ascension, and the place of 7256 is 10 arcmin wrong in declination. I could find only one nebular object in this vicinity. Two of the three faint stars involved, and mentioned by Marth were seen; the third was suspected. The northernmost one was brightest, and was of magnitude 14. The 11 magnitude star which Muller saw 4.5 arcmin preceding the nebula was also observed." This detailed description makes the duplicate entry certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2385 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7254 is about 110 million light-years away, in reasonable agreement with a single redshift-independent distance estimate of about 90 million light-years. Given that and its apparent size of about 0.9 by 0.5 arcmin (from the images below), the galaxy is about 30 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7255 (Leavenworth list I (#249), 1860 RA 22 14 25, NPD 106 16.0) is "extremely faint, large, much extended 30 , suddenly brighter middle and nucleus." The position precesses to RA 22 21 58.2, Dec -15 33 46, but there is nothing there nor near there; however, there is a galaxy that fits the description (presuming that Leavenworth's 30&176; was measured clockwise, instead of the usual counter-clockwise direction) about 1.2 minutes of time to the east and 1.3 arcmin to the north of the NGC position, and since there is nothing else in the region it seems a reasonable candidate for what Leavenworth recorded, as errors of a minute or more in the right ascension are all too common in Leander McCormick Observatory positions. And as it happens, Corwin was able to confirm that the galaxy listed above is NGC 7255 using Leavenworth's sketch of the region, so the identification is absolutely certain.
Identification Note: Gottlieb notes that Bigourdan couldn't find the object because Leavenworth's position was worse than Bigourdan expected, and that the RNGC listed NGC 7255 as nonexistent, so the galaxy was not shown in the first edition of the Uranometria 2000.0 atlas.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4720 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7255 is about 220 million light-years away. Given that and its apparent size of about 1.15 by 0.25 arcmin (from the images below), the galaxy is about 70 to 75 thousand light-years across.
Classification Note: Since the galaxy is nearly edge-on (hence "sp" meaning "spindle") classification is difficult, but the type in the description line is probably close to what its face-on classification would be.

Historical Identification: Per Dreyer, NGC 7256 (= GC 6038, Marth #472, 1860 RA 22 14 55, NPD 112 36) is "3 faint stars in a faint nebula." The position precesses to RA 22 22 38.0, Dec -21 53 43, but there is nothing there; however, there is a suitable candidate just under 10 arcmin nearly due north, and as a result the second IC notes "7254 = 7256, NPD is 112 26.5, Howe," so the identification as the galaxy listed above and the duplicate listing have been known for more than a century.
Identification Note: Dreyer only quoted part of Howe's statement. It actually read "7254 and 7256. These are identical. The place of 7254 is wrong in right ascension, and the place of 7256 is 10 arcmin wrong in declination. I could find only one nebular object in this vicinity. Two of the three faint stars involved, and mentioned by Marth were seen; the third was suspected. The northernmost one was brightest, and was of magnitude 14. The 11 magnitude star which Muller saw 4.5 arcmin preceding the nebula was also observed." This detailed description makes the duplicate entry certain.
Physical Information: Given the duplicate entry, see NGC 7254 for anything else.

Historical Identification: Per Dreyer, NGC 7257 (= GC 6039, Marth #473, 1860 RA 22 14 56, NPD 94 44) is "faint, very small, a little extended." The position precesses to RA 22 22 12.4, Dec -04 01 44, but there is nothing there; however, there is a suitable candidate about 8 arcmin to the southeast and Marth made a similar error with NGC 7266, which he found on the same night, suggesting an error in the position of his comparison star, so the identification is considered to be certain.
Discovery Notes: Earlier references list a later discovery date by Stephan, based on his publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above. Gottlieb and Corwin note that in Swift's 4th list he reported his #83 as new, but he retracted the claim in an addendum to his 6th paper, stating that it was the same as GC 6040 (= NGC 7260), and since NGC 7257 was (much) later recognized to be the same object as NGC 7260, Swift's "nova" was also the same as GC 6039.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4550 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7257/60 is about 210 to 215 million light-years away, in good agreement with redshift-independent distance estimates of about 200 to 255 million light-years. Given that and its apparent size of about 2.1 by 1.2 arcmin (from the images below), the galaxy is about 130 thousand light-years across. As in the case of NGC 7252, there are numerous relatively young globular clusters in the central part of the galaxy, suggesting that their formation was a result of a collision between two smaller galaxies less than a billion years ago.

Historical Identification: Per Dreyer, NGC 7258 (= GC 4781 = JH 3935, 1860 RA 22 15 07, NPD 119 03.4) is "very faint, small, extended, gradually a little brighter middle, binuclear?" The position precesses to RA 22 23 01.0, Dec -28 21 05, less than 0.8 arcmin southeast of the center of the galaxy listed above and barely outside its southeastern outline, the description is reasonable (it isn't binuclear, but since that was questionable, it isn't a problem) and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3545 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7258 is about 165 million light-years away, in good agreement with redshift-independent distance estimates of about 140 to 170 million light-years. Given that and its apparent size of about 1.3 by 0.7 arcmin (from the images below), the galaxy is about 60 to 65 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7259 (= GC 4782 = JH 3936, 1860 RA 22 15 10, NPD 119 39.3) is "extremely faint, pretty large, round, very little brighter middle." The position precesses to RA 22 23 05.0, Dec -28 56 59, only 0.3 arcmin north-northwest of the center of the galaxy listed above and on its northwestern rim, the description fits and there is nothing comparable nearby, so the identification is certain.
Physical Information: NED lists this as a physical pair with PGC 68726, which means that we should use the average of their distance estimates to determine their distance. For NGC 7259 the recessional velocity relative to the Cosmic Microwave Background radiation is 1490 km/sec, and for PGC 68726 the value is 1515 km/sec, yielding an average of about 1500 to 1505 km/sec, and (using H₀ = 70 km/sec/Mpc), a Hubble Flow distance of about 70 million light-years, in good agreement with redshift-independent distance estimates of about 50 to 75 million light-years. Given that and its apparent size of about 1.1 by 0.85 arcmin (from the images below), the galaxy is 20 to 25 thousand light-years across.
Note About PGC Designations: Although NED lists the pair as "LEDA 4614489", a search of HyperLEDA for that designation returns no result. A search for [MK2011]NGC7259 does return a result, but with the designation "PGC 5066369", and a search for that designation also returns no result, hence the quotes around both PGC designations.

Physical Information: NED lists this as a physical pair with NGC 7259. As a result, the best estimate of the distance of the pair is based on the average of their individual distance estimates. As shown in the entry for NGC 7259, that yields a Hubble Flow distance of about 70 million light-years. Given that and its apparent size of about 3.0 by 0.28 arcmin (from the image below), PGC 68726 is about 60 thousand light-years across.
Note About PGC Designations: Although NED lists the pair as "LEDA 4614489", a search of HyperLEDA for that designation returns no result. A search for [MK2011]NGC7259 does return a result, but with the designation "PGC 5066369", and a search for that designation also returns no result, hence the quotes around both PGC designations.
Classification Note: Since PGC 68726 is almost exactly edge-on (hence "sp" for "spindle"), it is difficult to determine its type. NED lists the galaxy as Scd? edge-on and as Sdm? edge-on; based on that and the image below, I have used the average of those classifications in the description line above.

Physical Information: There appears to be no way to determine the distance of this galaxy, so although its apparent size (about 0.28 by 0.14 arcmin, from the image below) and type can be determined, there is no way to know its physical size and whether it is a companion of NGC 7259, or merely in nearly the same direction (that is, an optical double).

Relation to NGC 7259: As shown below, PGC 735575 is about 650 million light-years further from us than NGC 7259, so they are only an optical double.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 17245 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 735575 is about 800 to 805 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 720 million light-years away at the time the light by which we see it was emitted, about 770 to 775 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.2 by 0.15 arcmin (from the image below), the galaxy is 40 to 45 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7260 (= GC 6040, Stephan list VIII (#13), 1860 RA 22 15 21, NPD 94 49.5) is "extremely faint, pretty small, irregularly round." The position precesses to RA 22 22 37.5, Dec -04 07 12, less than 0.3 arcmin east-northeast of the center of the galaxy listed above and well within its outline, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above. Gottlieb notes that in Swift's 4th list he reported his #83 as new, but he retracted the claim in an addendum to his 6th paper, noting that it was the same as GC 6040 (= NGC 7260).
Physical Information: Although Stephan's position is accurate, and Marth's was so far off that the duplicate entry was only noted much later, it is standard practice to use the earlier numerical designation unless the later one has been used so often that it would be confusing to change it. As a result, see NGC 7257 for anything else.

Historical Identification: Per Dreyer, NGC 7261 (= GC 4783 = JH 2159, 1860 RA 22 15 24, NPD 32 36.9) is "a cluster, large, pretty rich, a little compressed." The position precesses to RA 22 20 26.6, Dec +58 05 18, less than 0.2 arcmin northeast of the star that Herschel recorded as "The chief star of a coarse pretty rich cluster which fills the field. Stars 10th to 15th magnitude." The statement "fills the field" suggests that the cluster must be close to 15 arcmin in size, which is why Corwin uses the position shown in the description line as the position of the cluster; but as noted in the following paragraph the most obvious grouping consists of substantially brighter stars in a smaller region, which Corwin lists as the "core" of the cluster, even though it lies five arcminutes north-northeast of the larger group (at RA 22 20 13.0, Dec +58 06 54). For that reason, although it is certain that the field of view shown below must be what Herschel observed, and some part of it must be JH 2159 and therefore NGC 7261, it isn't obvious which part of the field of view is the NGC object, and whether any part of the "cluster" is actually a cluster, or simply a random group of stars superimposed on a stellar background.
A Matter of Some Debate: Gottlieb writes that he observed about 30 stars in a 7 by 3.5 arcmin group elongated north-south, with magnitude 9.6 HD 239927 on its eastern boundary. But Corwin writes that JH's cluster "is probably the scattered group of pretty bright stars stretching nearly north-south across an area 15 by 10 arcmin, about 20 seconds (of time) preceding (to the west of) his position for the bright star on its following (eastern) edge." He further states "There is a smaller core 7 by 5 arcmin of generally fainter stars about five arcminutes north-northeast of the center of the larger group" (Gottlieb's cluster), then wonders whether the smaller group is a background cluster, and whether the larger cluster is simply a random collection of moderately bright stars. He finishes by stating that to tell whether any part of the "cluster" or its "core" is actually a cluster we need parallaxes and proper motions for as many of the stars in the area as possible.

Historical Identification: Per Dreyer, NGC 7262 (= GC 4784 = JH 3937, 1860 RA 22 15 26, NPD 123 03.5) is "extremely faint, small, round, a little brighter middle." The position precesses to RA 22 23 27.3, Dec -32 21 09, about 0.7 arcmin north-northwest of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7880 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7262 is about 365 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 355 million light-years away at the time the light by which we see it was emitted, about 360 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.75 by 0.7 arcmin (from the images below), the galaxy is 75 to 80 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7263 (= GC 6041, Marth #474, 1860 RA 22 15 33, NPD 54 21) is "faint, small, round." The position precesses to RA 22 21 45.1, Dec +36 21 16, only a quarter of an arcmin north-northwest of the center of the galaxy listed above and on its northern outline, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5890 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7263 is about 275 million light-years away. Given that and its apparent size of about 0.75 by 0.55 arcmin for the central galaxy and about 1.8 by 1.6 arcmin for the outer shell/envelope (from the images below), the central galaxy is about 60 thousand light-years across, and its outer envelope spans about 140 to 145 thousand light-years.
About NGC 7263's "Companion": NGC 7263 appears to be accompanied by a magnitude 14.5 compact galaxy inside its northeastern outline, but GAIA measurements of its proper motion and parallax prove that the "companion" is actually a star in our own galaxy.
Classification Note: NGC 7263 has an unusual structure, so trying to fit it into a standard type is difficult. Its faint outer envelope could be called a shell or a ring, but "ring" suggests a structure outlining the central galaxy with a clear separation between them, whereas a shell can simply extend from and more or less merge with the central galaxy, so that seems a more appropriate classification. The central galaxy is also unusual, in that there appears to be a clear separation between the nucleus and the rest of the essentially lenticular structure, hence my use of (r) to describe that feature; but an expert in galaxy classification might treat both oddities in a slightly different way, hence the question mark after the basic type.

Historical Identification: Per Dreyer, NGC 7264 (= GC 6042, Marth #475, 1860 RA 22 16 02, NPD 54 19) is "very faint, pretty small, much extended." The position precesses to RA 22 22 14.3, Dec +36 23 19, almost dead center on the galaxy listed above (on the northeastern rim of its nucleus, but well within the outline of the galaxy), the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3955 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7264 is about 185 million light-years away, in good agreement with redshift-independent distance estimates of about 175 to 295 million light-years. Given that and its apparent size of about 2.15 by 0.35 arcmin (from the images below), the galaxy is about 115 thousand light-years across.
Classification Note: Since NGC 7264 is nearly edge-on (hence "sp" for "spindle") its type can only be determined from the size of its nucleus, which suggests either "ab" or "b" as its sub-type. LEDA and NED both use "Sb", albeit with a question mark in NED; so either of the choices in the previous sentence seem reasonable, and "b?" pretty much sums up the situation.

Historical Identification: Per Dreyer, NGC 7265 (= GC 6043, Stephan list VIII (#14), 1860 RA 22 16 15, NPD 54 29.5) is "faint, very small, round, much brighter middle." The position precesses to RA 22 22 27.8, Dec +36 12 50, less than a quarter arcmin north-northeast of the center of the galaxy listed above and well within its outline, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4680 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7265 is about 215 to 220 million light-years away. Given that and its apparent size of about 1.0 by 0.9 arcmin for the bright core and innermost shell and about 2.1 by 1.8 arcmin for the outermost shell (from the images below), the central galaxy is about 60 to 65 thousand light-years across, and its overall size is about 130 to 135 thousand light-years.
A Suggested Group: NED lists NGC 7265 as the brightest in a group of "at least 9" galaxies: Per Gottlieb they include a quartet of NGC 7265 with PGC 68690, PGC 214824 and PGC 214825; NGC 7273, 7274 and 7276 to the east-southeast; NGC 7263 and 7264 to the north-northwest; PGC 2075294 to the east-southeast, and PGC 68715 to the southeast. Which of these galaxies actually are part of a group can be estimated from their recessional velocities relative to the Cosmic Microwave Background radiation, which I have arranged in ascending order according to their recessional velocities: NGC 7264 (3953 km/sec), PGC 214825 (4183 km/sec), PGC 68690 (4512 km/sec), NGC 7265 (4678 km/sec), NGC 7273 (4753 km/sec), PGC 68715 (5096 km/sec), NGC 7274 (5629 km/sec), NGC 7276 (5662 km/sec), NGC 7263 (5889 km/sec), PGC 214824 (5998 km/sec), and PGC 2075294 (8369 km/sec). Based on these values, NGC 7265, NGC 7273 and PGC 68690 probably are companions, and PGC 68715 and PGC 214825 might be, but all the other galaxies appear to be foreground or background objects.
 Despite the above statement, per a private communication from Gottlieb it turns out that except for PGC 214825 and PGC 2075294, all the other galaxies probably are part of a loose group called USGC U813. The UZC-SSRS2 Group Catalog defines groups using a "friends-of-friends" algorithm that connects galaxies in one more or less certain group to galaxies in another more or less certain group, and through that group, to yet another one. The resulting group of groups could be thought of as being a very small "super-cluster", and although some of the galaxies identified as part of U813 are probably outliers and not actually part of any group, the peculiar velocities (random motions relative to neighboring galaxies or groups) of each group can make them appear to be unrelated to each other, even though they are in the same general region. That doesn't alter the conclusion in the previous paragraph that most of the galaxies in NED/Gottlieb's original list are not direct companions of NGC 7265, but does mean that many of them are members of other groups that appear to be connected to the one containing NGC 7265 and 7273.
Classification Note: Although listed as a more or less normal lenticular galaxy, NGC 7265 has at least two concentric shells outside its bright core, and even a ring-like and quasi-armlike structure between the core and the innermost shell, so it definitely deserves to be called peculiar.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4510 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68690 is about 210 million light-years away. Given that and its apparent size of about 1.2 by 1.05 arcmin (from the images below), the galaxy is about 70 to 75 thousand light-years across.
Classification Note: LEDA lists this as a spiral galaxy (NED merely says "star superposed"), but the images below show that it is a peculiar lenticular galaxy, with an extended envelope (perhaps a "shell") and a bright core (perhaps sufficiently brighter than the main galaxy to justify a "ringed" designation, whence "(r?)"). The tentative "B?" is based on the possibility that this is really a peculiar spiral galaxy, and probably deserves another question mark or to be deleted entirely.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5095 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68715 is about 235 to 240 million light-years away. Given that and its apparent size of about 0.8 by 0.25 arcmin (from the images below), the galaxy is about 55 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6000 km/sec (and H₀ = 70 km/sec/Mpc), PGC 214824 is about 280 million light-years away. Given that and its apparent size of about 0.6 by 0.2 arcmin (from the image below), the galaxy is about 45 to 50 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4185 km/sec (and H₀ = 70 km/sec/Mpc), 4185 is about 195 million light-years away. Given that and its apparent size of about 0.6 by 0.2 arcmin (from the image below), the galaxy is about 35 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7266 (= GC 6044, Marth #476, 1860 RA 22 16 18, NPD 94 41) is "faint, very small, round, almost stellar." The second IC lists a corrected position (per Bigourdan) of RA 22 16 42, NPD 94 47. The NGC position precesses to RA 22 23 34.3, Dec -03 58 37, but there is nothing there; however, there is a suitable candidate about 8.5 arcmin to the southeast (almost exactly the same error that Marth made for NGC 7257, which he found on the same night, suggesting a problem with his comparison star), and Bigourdan's position, which precesses to RA 22 23 58.4, Dec -04 04 35, lies on the southwest rim of that galaxy, so the identification of NGC 7266 as the galaxy listed above is considered certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4555 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7266 is about 210 to 215 million light-years away. Given that and its apparent size of about 0.65 by 0.4 arcmin (from the images below), the galaxy is about 40 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7267 (= GC 4785 = JH 3938, 1860 RA 22 16 21, NPD 124 24.0) is "considerably bright, pretty small, very little extended, gradually a little brighter middle, bright triple star south-preceding (to southwest)." The position precesses to RA 22 24 24.5, Dec -33 41 34, about half an arcminute east-northeast of the center of the galaxy listed above and within its eastern outline, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3080 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7267 is about 140 to 145 million light-years away, in fair agreement with redshift-independent distance estimates of about 60 to 115 million light-years. Given that and its apparent size of about 1.6 by 1.3 arcmin (from the images below), the galaxy is about 65 to 70 thousand light-years across.
Classification Note: The type shown above is taken from Crocker, Baugus and Buta's paper (and is also listed in NED), and seems a reasonable fit to the images below.

Historical Identification: Per Dreyer, NGC 7268 (= GC 4786 = JH 3939, 1860 RA 22 16 44, NPD 121 53.8) is "faint, considerably small, very little extended, preceding (western) of 2," the other being NGC 7277. The position precesses to RA 22 24 42.5, Dec -31 11 21, but there is nothing there; however, there is a reasonable candidate just under a minute of time to the east of the position, and both Gottlieb and Corwin note that Herschel's Cape position was good, but that the GC and NGC positions were a minute of time too far west (see the Identification Note). At any rate, since the description fits the pair of galaxies listed above, and a reasonable explanation of the error in the right ascension exists, the identification of NGC 7268 is essentially certain.
Identification Note: Corwin notes that Herschel's three Cape observations' right ascensions were given as "22 15 58.7", "60.5" and "64.6", and that the two values greater than 60 seconds should have been treated as being 22 16 00.5 and 22 16 04.6, but whoever did the computation for the GC must have treated them as being at 22 15 00.5 and 22 15 04.6, leading to the nearly one minute of error in the right ascension. Gottlieb also notes that the RNGC "clearly" misidentifies NGC 7268 as if it were 3 arcmin south of ESO 467-IG55, "clearly" meaning both that there is nothing at the RNGC position, and that it is an unexplainable 12 arcmin south and 20 seconds of time to the west of Herschel's Cape positions (which, since many of the RNGC positions make no sense, is not terribly surprising).
Note About PGC Designation: HyperLEDA assigns a PGC designation ("PGC 3168477") to the pair of galaxies, but a search of the database for that designation returns no result, so it is in quotes.
Physical Information: Since this is a pair of interacting galaxies, the best estimate of their distance is based on an average of their distance estimates. For PGC 68847 the recessional velocity relative to the Cosmic Background Radiation is 8210 km/sec, while for PGC 68848 it is 8520 km/sec. Using the average recessional velocity of 8365 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7268 is about 390 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the pair was about 375 to 380 million light-years away at the time the light by which we see it was emitted, about 380 to 385 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and an apparent size of 0.5 by 0.5 arcmin for the main part of PGC 68847, 0.4 by 0.3 arcmin for the main part of PGC 68848, and 1.45 by 0.9 arcmin for their envelope (all from the images below), PGC 68847 is about 55 thousand light-years across, PGC 68848 is about 40 to 45 thousand light-years across, and the overall structure including their envelope spans about 160 thousand light-years.

Historical Identification: Per Dreyer, NGC 7269 (Leavenworth list I (#250), 1860 RA 22 17 25, NPD 103 55.1) is "extremely faint, pretty small, round, gradually a little brighter middle." The second IC lists a corrected position (per Howe) of RA 22 18 19, NPD 103 52.6. The NGC position precesses to RA 22 24 54.2, Dec -13 12 37, but there is nothing there; however, there is a reasonable candidate just under a minute of time to the east and about 2.5 arcmin to the north, errors of a minute or two of time in Leander McCormick right ascensions are common, and Howe's position precesses to RA 22 25 47.9, Dec -13 10 02, barely to the east of the center of that galaxy and on its eastern outline. So the identification of NGC 7269 as the galaxy listed above is considered certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 9220 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7269 is about 430 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 415 million light-years away at the time the light by which we see it was emitted, about 420 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 1.05 by 0.65 arcmin (from the images below), the galaxy is about 125 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7270 (= GC 6045, Marth #477, 1860 RA 22 17 28, NPD 58 16) is "very faint, small, extended." The position precesses to RA 22 23 49.0, Dec +32 26 27, about 2.3 arcmin north-northeast of the galaxy listed above, the description fits and there is nothing nearby that isn't already assigned another NGC designation, and all of those objects are further from the position, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6335 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7270 is about 295 million light-years away, in good agreement with redshift-independent distance estimates of about 285 to 440 million light-years. Given that and its apparent size of about 0.95 by 0.6 arcmin (from the images below), the galaxy is about 80 to 85 thousand light-years across.
Probable Companion: Based on their similar recessional velocity and distance, NGC 7271 and NGC 7270 are probably companions.

Historical Identification: Per Dreyer, NGC 7271 (= GC 6046, Marth #478, 1860 RA 22 17 38, NPD 58 19) is "very faint, small, very little extended." The position precesses to RA 22 23 59.2, Dec +32 23 27, about 1.5 arcmin north-northeast of the galaxy listed above (an error similar to Marth's position error for NGC 7270, observed on the same night), the description fits and there is nothing comparable nearby that doesn't already have another NGC designation, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6280 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7271 is about 290 to 295 million light-years away. Given that and its apparent size of about 0.55 by 0.25 arcmin (from the images below), the galaxy is about 45 to 50 thousand light-years across.
Probable Companion: Based on their similar recessional velocity and distance, NGC 7270 and NGC 7271 are probably companions.

Historical Identification: Per Dreyer, NGC 7272 (= GC 6047, Marth #479, 1860 RA 22 17 43, NPD 74 07) is "very faint, small, irregularly round." The position precesses to RA 22 24 30.5, Dec +16 35 29, about 0.3 arcmin northwest of the center of the galaxy listed above and on its northwestern rim, the description fits and there is nothing comparable nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 9835 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7272 is about 455 to 460 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 440 million light-years away at the time the light by which we see it was emitted, about 445 to 450 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.9 by 0.8 arcmin (from the images below), the galaxy is about 115 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 8120 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214829 is about 375 to 380 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 365 million light-years away at the time the light by which we see it was emitted, about 370 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.3 by 0.15 arcmin (from the image below), the galaxy is about 30 to 35 thousand light-years across.
 Note that although PGC 214829 is not a companion of NGC 7272, but only a foreground galaxy, it does appear to be a companion of PGC 1511999.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 8075 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 1511999 is about 375 to 380 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 365 million light-years away at the time the light by which we see it was emitted, about 370 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.35 by 0.2 arcmin (from the image below), the galaxy is about 35 to 40 thousand light-years across.
 Note that although PGC 1511999 is not a companion of NGC 7272, but only a foreground galaxy, it does appear to be a companion of PGC 214829.

Historical Identification: Per Dreyer, NGC 7273 (= GC 6048, Stephan list VIII (#15), 1860 RA 22 17 56, NPD 54 30.4) is "faint, very small, round, much brighter middle." The position precesses to RA 22 24 09.7, Dec +36 12 05, about 0.1 arcmin northeast of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Possible Companions: NGC 7273 is probably part of a small group with NGC 7265 (which see).
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4755 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7273 is about 220 million light-years away. Given that and its apparent size of about 0.85 by 0.6 arcmin (from the images below), the galaxy is about 55 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7274 (= GC 6049, Stephan list VIII (#16), 1860 RA 22 17 57, NPD 54 34.9) is "pretty faint, very small, much brighter middle." The position precesses to RA 22 24 10.9, Dec +36 07 35, almost dead center on the galaxy listed above, the description fits and there is nothing else nearby, so the identififcation is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5630 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7274 is about 260 to 265 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 275 to 365 million light-years. Given that and its apparent size of about 1.65 by 1.3 arcmin (from the images below), the galaxy is about 125 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7275 (= GC 6050, Marth #480, 1860 RA 22 17 58, NPD 58 14) is "extremely faint, small, much extended." The position precesses to RA 22 24 19.2, Dec +32 28 29, about 1.7 arcmin north-northeast of the galaxy listed above, the description fits and there is nothing else nearby that isn't already designated as another NGC object, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6200 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7275 is about 285 to 290 million light-years away, in good agreement with redshift-independent distance estimates of about 180 to 315 million light-years. Given that and its apparent size of about 0.95 by 0.2 arcmin (from the images below), the galaxy is about 80 thousand light-years across.
Classification Note: Since the galaxy is edge-on (hence "sp" for "spindle"), classification is more difficult than for more nearly face-on galaxies. The type shown above is based on NED and LEDA morphology data, taking into account the fact that the nucleus is not as large as is typical fror an Sa galaxy, and adding a question mark hecause of the edge-on presentation.

Historical Identification: Per Dreyer, NGC 7276 (= GC 6051, Stephan list VIII (#17), 1860 RA 22 18 01, NPD 54 37.2) is "very faint, very small, much brighter middle." The position precesses to RA 22 24 15.0, Dec +36 05 17, bare;u 0.1 arcmin east-northeast of the center of the galaxy listed above and well within its outline, the description fits and there is nothing nearby that doesn't have another NGC designation, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5660 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7276 is about 260 to 265 million light-years away. Given that and its apparent size of about 0.8 by 0.7 arcmin (from the images below), the galaxy is about 60 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7277 (= GC 4787 = JH 3940, 1860 RA 22 18 16, NPD 121 51.4) is "faint, considerably small, very little extended, following (eastern) of 2," the other being NGC 7268. The position precesses to RA 22 26 13.7, Dec -31 08 49, about 1.7 arcmin nearly due east of the center of the galaxy listed above and not far from its northeastern border, the description fits and there is nothing comparable nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3715 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7277 is about 170 to 175 million light-years away, in good agreement with redshift-independent distance estimates of about 165 to 185 million light-years. Given that and its apparent size of about 1.05 by 0.45 arcmin (from the images below), the galaxy is about 50 to 55 thousand light-years across.
Note About "Companions": As shown in the following two entries, it has been suggested that PGC 133404 and PGC 708158 may be companions of NGC 7277. However, the former is nearly twice as far from us as NGC 7277, and the latter is more than twice as far as that, so they are both much more distant background galaxies and have no connection with their apparently larger neighbor, or with each other.
Classification Note: The type in the description line is taken from NED, but given the poor quality of the available images, although it may be reasonable it can't be considered definitive, so the question mark may be the most significant part of the classification.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7590 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 133404 is about 350 to 355 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 340 to 345 million light-years away at the time the light by which we see it was emitted, about 345 to 350 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.5 by 0.25 arcmin (from the image below), the galaxy is about 50 thousand light-years across.
 Given the much greater distance of PGC 133404, it is not a companion of NGC 7277, but merely a background object.

Physical Information; Based on a recessional velocity relative to the Cosmic Background Radiation of 17585 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 708158 is about 815 to 820 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 765 million light-years away at the time the light by which we see it was emitted, about 785 to 790 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.3 by 0.3 arcmin (from the image below), the galaxy is about 65 to 70 thousand light-years across.
 Given the much greater distance of PGC 708158, it is not a companion of NGC 7277, but merely a background object.

Historical Identification: Per Dreyer, NGC 7278 (= GC 4788 = JH 3941, 1860 RA 22 18 57, NPD 150 52.9) is "most extremely faint, a little extended, very gradually a very little brighter middle, 3 stars south-following (to southeast)." The position precesses to RA 22 28 22.4, Dec -60 10 12, dead center on the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 12420 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7278 is about 575 to 580 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 550 million light-years away at the time the light by which we see it was emitted, about 560 to 565 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.85 by 0.55 arcmin (from the images below), the galaxy is about 135 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7279 (= GC 4789 = JH 3942, 1860 RA 22 19 07, NPD 125 51.3) is "very faint, pretty small, round, very gradually a very little brighter middle." The position precesses to RA 22 27 12.0, Dec -35 08 38, about 0.2 arcmin south-southwest of the center of the galaxy listed above (between its bright southern arm and the fainter arms outside that), the description is reasonable and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 8760 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7279 is about 405 to 410 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 395 million light-years away at the time the light by which we see it was emitted, about 400 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 1.05 by 0.9 arcmin (from the images below), the galaxy is about 120 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7280 (= GC 4790 = JH 2160 = WH II 248, 1860 RA 22 19 39, NPD 74 33.8) is "faint, considerably small, round, gradually brighter middle equivalent to a small (faint) star, 3 stars to north and north-following (northeast)." The position precesses to RA 22 26 27.6, Dec +16 08 51, almost dead center on the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 1490 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7280 is about 70 million light-years away, in good agreement with redshift-independent distance estimates of about 65 to 85 million light-years. Given that and its apparent size of about 1.8 by 1.15 arcmin (from the images below), the galaxy is about 35 to 40 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 1545 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68878 is about 70 to 75 million light-years away, in fair agreement with a single redshift-independent distance estimate of about 85 to 90 million light-years. Given that and its apparent size of about 0.85 by 0.45 arcmin (from the images below), the galaxy is about 15 to 20 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7281 (= GC 4791 = JH 2161, 1860 RA 22 19 39, NPD 32 52.4) is "a cluster, large, pretty rich, a little compressed, stars from 10th to 16th magnitude." The position precesses to RA 22 24 47.9, Dec +57 50 11, barely 0.1 arcmin southeast of magnitude 10.0 HD 239947, the star that Herschel used for the position, so the general position of the cluster is certain; however, exactly what part of the star field is what Herschel observed is not certain.
Possible Identificaions: (1) Herschel's use of the term "large" corresponds to a size of about 4 arcmin, which is the same size given by Gottlieb for a group of about 20 stars centered about 2 arcmin to the east of Herschel's star, and a list of open clusters also agrees with that description. Gottlieb's group consists of the most obvious collection of bright stars in the region, and like Herschel's observation is based on visual observations, so it is certainly a reasonable and perhaps the best definition of NGC 7281.
 (2) Corwin, on the other hand, writes that the cluster is about 15 arcmin east-west by 7 arcmin north-south, and places its center at RA 22 25 18, Dec +57 49.9, about 30 seconds of time to the east of Herschel's star; and since Gottlieb notes that "outliers greatly increase the diameter and total number of stars," it is also a reasonable, though perhaps not as obvious solution to the question of just what group of stars should be called NGC 7281.
 (3) SIMBAD lists a much larger region (namely, 16 by 16 arcmin), with the cluster's center closer to Herschel's star (at RA 22 25 02.2, Dec +57 52 08); but other than the brighter stars in Gottlieb's and Corwin's suggested solutions as to just what region is NGC 7128, most of what lies within SIMBAD's definition looks no different than the random background of stars found throughout the area, so depending on what the paper quoted in SIMBAD says about the region, it may be no more than a barely educated guess.
  Given Herschel's description and the three possibilities listed above, it appears that Gottlieb's group most closely agrees with JH 2161, but if the region actually contains a real cluster that is larger than Herschel's description, then either of the other definitions might fit that cluster better than what Herschel saw; but if, as suspected by Gottlieb, the stars may just be an asterism and not an actual cluster, then the other definitions of NGC 7128 would be wrong, so until additional data are added to the mix, the actual nature of NGC 7128 will remain more uncertain than not.
About "Working Here": Before removing "WORKING HERE" from this entry I will try to find the paper quoted by SIMBAD, and use GAIA to study the parallaxes and proper motions of the stars in the three regions defined above. If those data suggest that there is an actual cluster associated with NGC 7128 then I will note that and alter the image below; but if they do not, then I will define NGC 7128 as only the stars in the region observed by Gottlieb, and state that it is not actually a cluster, but just a random grouping of stars (that is, an "asterism").
Note About PGC Designation: As usual for NGC/IC objects, HyperLEDA assigned a PGC designation to this object, even though it isn't a galaxy; but as also usual in such cases, a search of the database for that designation returns no result, so it is in quotes.
Physical Information: SIMBAD's parallax puts its definition of the cluster about 7500 light-years from our Sun. Given that, the 4 arcmin size listed by Gottlieb corresponds to about 10 light-years, while the 16 arcmin size in SIMBAD corresponds to about 35 light-years, and Corwin's description would correspond to 30 to 35 light-years east-west and about half that north-south.

Historical Identification: Per Dreyer, NGC 7282 (Stephan list IX (#29), 1860 RA 22 19 49, NPD 50 23.7) is "extremely faint, pretty large, diffuse, between 3 stars." The position precesses to RA 22 25 54.8, Dec +40 18 56, less than 0.2 arcmin east-northeast of the center of the galaxy listed above and well within its eastern outline, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above. Gottlieb states that Stephan's 1869 position was unpublished and 8 arcmin too far to the east, but that he measured an accurate position on Oct 2, 1878 (which is the date usually listed, and is the basis of the NGC position).
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4235 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7282 is about 195 to 200 million light-years away, in good agreement with redshift-independent distance estimates of about 140 to 200 million light-years. Given that and its apparent size of about 2.9 by 1.3 arcmin (from the images below), the galaxy is about 165 to 170 thousand light-years across. Because of its bright center, NGC 7282 is listed as a Seyfert galaxy (type Sy2).

Historical Identification: Per Dreyer, NGC 7283 (= GC 6052, Marth #481, 1860 RA 22 20 51, NPD 73 17) is "very faint, very small, round." The position precesses to RA 22 27 38.0, Dec +17 25 45, but there is nothing there. However, the galaxy listed above is almost exactly 1 minute of time to the east, and could easily fit Marth's description, if it is supposed that Marth accidentally made a single-digit error in the right ascension. Assuming that is the problem, changing the 1860 RA to 22 21 51 yields a J2000 position of RA 22 28 38.2, Dec +17 25 50, which lies about 2.7 arcmin south-southeast of the galaxy in question. That is good enough that most references list that galaxy as NGC 7283, though sometimes with a note that what Marth actually saw might be the faint double star about 2.2 arcmin west-northwest of Marth's position, which is why the double star is also listed above, and shown in the second wide-field image below.
Discovery Note: Corwin suspects that the double star is more likely to be what Marth observed, since the error in the declination which would be required for the galaxy to be NGC 7283 is not typical of Marth's usually accurate positions; but he feels that the galaxy cannot be ruled out, and therefore lists both the galaxy and the pair of stars in his list of positions and his note about this NGC entry. Gottlieb treats the galaxy as the NGC object but states that the identification is very uncertain, and that as a result CGCG and MCG do not list the galaxy as NGC 7283, though LEDA, NED, RNGC and SIMBAD do.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6925 km/sec (and H₀ = 70 km/sec/Mpc), the galaxy listed above is about 320 to 325 million light-years away. Given that and its apparent size of about 0.8 by 0.3 arcmin (from the images below), the galaxy is about 75 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7284 (= GC 4792 = JH 3943 = WH II 469, 1860 RA 22 20 51, NPD 115 34.3) is "considerably faint, considerably small, a little extended, mottled but not resolved, double star involved." The second Index Catalog adds "Delete 'double star involved'. This and 4285 (a typographical error for NGC 7285) are two nebulous stars of magnitudes 12.5 and 13, position angle 60 , distance 40 arcsec, Howe." The position precesses to RA 22 28 36.9, Dec -24 51 31, about 0.9 arcmin south-southeast of the galaxy listed above, the descriptions fit, and there is nothing nearby except the other member of the pair, so the identification is certin.
Discovery Note 1: NGC 7284 is part of an interacting pair with NGC 7285, and Dreyer's NGC note and IC correction make it clear that Herschel observed the interacting pair of galaxies now called NGC 7284 and 7285 as a binuclear nebula, supposing the nuclei to be two stars. There is no indication of which listing corresponds to which galaxy, but since the NGC is arranged in order of right ascension, NGC 7284 must refer to the western member of the pair, and NGC 7285 to the eastern member.
Discovery Note 2: Dreyer's note in the second IC is partially based on an observation that Herschel made at the Cape of Good Hope (sweep 474, well before a third sweep on Sep 14, 1835). Howe's comments include "The description of 7285, discovered by Lassell, is "'Nebulous star 1 arcmin distant from 7284.' I judge 7285 to be simply one of the components of 7284... The brighter one is of magnitude 12.5. The other is of magnitude 13, and lies at position angle 60°, distant about 40 arcsec."
Physical Information: As members of an interacting pair of galaxies, the galaxies are grossly disturbed by their encounter, and extended streams of gas and stars are visible for some distance from their central structure. Based on a recessional velocity of 4370 km/sec relative to the Cosmic Microwave Background radiation (and H₀ = 70 km/sec/Mpc), NGC 7284 is about 200 to 205 million light-years away. However, it must be the same distance as its companion, whose radial velocity corresponds to only 185 to 190 million light-years, so I have adopted an average distance of about 195 million light-years for the pair. Given that and an apparent size of about 1.2 by 0.6 arcmin for the central part of NGC 7284, about 1.8 by 1.7 arcmin for the pair of galaxies, and about 5.4 by 2.75 arcmin including the extended plume of 7285 (from the images below), NGC 7284 is about 65 to 70 thousand light-years across, the pair of galaxies spans about 100 to 105 thousand light-years, and with the long plume, Arp 93 spans about 305 to 310 thousand light-years.
Use By The Arp Atlas: NGC 7284 and 7285 are used by The Arp Atlas of Peculiar Galaxies as an example of a spiral galaxy (NGC 7285) with an elliptical companion (NGC 7284), with the note "Long faint plume bifurcates from arm, E(lliptical) comp. in other arm. Suggested rotation of axis of spiral."

Historical Identification: Per Dreyer, NGC 7285 (= GC 5078, Lassell, 1860 RA 22 20 51 , NPD 115 34 ) is "a nebulous star 1 arcmin distant from h 3943," (JH) 3943 being NGC 7284. The position precesses to RA 22 28 36.9, Dec -24 51 13, about 0.8 arcmin south-southwest of the galaxy listed above, the descriptions fit and there is nothing nearby except the other member of the pair, so the identification is certain.
Discovery Note 1: As indicated by the signs in the 1860 position for NGC 7285, which member of the pair should receive which listing, and who should receive credit for discovering one or the other might be a matter of some debate in more obscure circumstances. But the question is not which galaxy did Herschel or Lassell see. They both saw both galaxies, but Herschel only noted the binuclear nature of the object in one of three sweeps, so that was not mentioned in the GC or NGC, while Lassell realized that the "two stars" were two nebulae. And the question of which galaxy is NGC 7284 or 7285 is easy to answer, since the NGC is arranged in order of right ascension, so NGC 7284 must be the western galaxy, and 7285 the eastern.
Discovery Note 2: Lassell did not publish his observation in Marth's catalogue, but mentioned the discovery to John Herschel in a note of Nov 1, 1862, so Dreyer added it to the GC supplement as GC 5078. Gottlieb notes that although both William and John Herschel reported a double nucleus or two stars involved for NGC 7284, neither used two catalogue numbers, as Dreyer did. See the Discovery Notes for NGC 7284 for an excerpt from Howe's paper.
Physical Information: As members of an interacting pair of galaxies, the galaxies are grossly disturbed by their encounter, and extended streams of gas and stars are visible for some distance from their central structure. Based on a recessional velocity of 4015 km/sec relative to the Cosmic Microwave Background radiation (and H₀ = 70 km/sec/Mpc), NGC 7284 is about 185 to 190 million light-years away. However, it must be the same distance as its companion, whose radial velocity corresponds to 200 to 205 million light-years, so I have adopted an average distance of about 195 million light-years for the pair. Given that and an apparent size of about 1.5 by 1.0 arcmin for the central part of NGC 7285, about 1.8 by 1.7 arcmin for the pair of galaxies, and about 5.4 by 2.75 arcmin including the extended plume of 7285 (see the images at NGC 7284), NGC 7285 is about 85 thousand light-years across, the pair of galaxies spans about 100 to 105 thousand light-years, and with the long plume, Arp 93 spans about 305 to 310 thousand light-years.
Use By The Arp Atlas: NGC 7284 and 7285 are used by The Arp Atlas of Peculiar Galaxies as an example of a spiral galaxy (NGC 7285) with an elliptical companion (NGC 7284), with the note "Long faint plume bifurcates from arm, E(lliptical) comp. in other arm. Suggested rotation of axis of spiral."

Historical Identification: Per Dreyer, NGC 7286 (= GC 4793 = JH 2162, 1860 RA 22 20 52, NPD 61 36.8) is "very faint, small, round, among stars." The second IC lists a corrected RA (per Bigourdan) of 22 21 21. The NGC position precesses to RA 22 27 20.6, Dec +29 05 56, but there is nothing there. However, there is a reasonable candidate exactly 30 seconds of time due east of that position, namely the galaxy listed above. Bigourdan's IC2 correction yields a J2000 position of RA 22 27 49.8, Dec +29 05 58, about a quarter of an arcmin northwest of the center of the galaxy and on its northern outline, the description is reasonable and there is nothing else in the region, so the identification is certain.
Discovery Note: Since Herschel's right ascension was exactly 30 seconds of time too small, it is thought that his position was probably "off" as a result of a digit error, rather than an incorrect measurement.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 675 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7286 is about 30 to 35 million light-years away, considerably closer than redshift-independent distance estimates of about 50 to 75 million light-years. However, for such a small recessional velocity, peculiar velocities (random motions relative to neighboring galaxies) can substantially affect the distance estimate, so odds are that the galaxy happens to be moving toward us relative to other galaxies in the same region, and that a distance somewhere between the Hubble Flow estimate and the redshift-independent estimates is probably closer to the correct value. For that reason I have adopted a distance of 40 to 45 million light-years. Given that and its apparent size of about 1.5 by 0.55 arcmin (from the images below), the galaxy is about 16 to 20 thousand light-years across.
Classification Note: In most respects the galaxy looks like a sparsely populated E/S0, but it is unusually blue for a lenticular galaxy, which is probably why LEDA and NED list it as the type S0/a shown in the description line.

Historical Identification: Per Dreyer, NGC 7287 (Muller list II (#468), 1860 RA 22 20 54, NPD 112 51.1) is "extremely faint, slightly nebulous double star." The position precesses to RA 22 28 35.6, Dec -22 08 18, but there is nothing there. The second IC confuses the situation by stating "Howe says that the RA is about 2 minutes too great, and that the object is only a faint double star, distance (separation) 6 arcsec. But he must have found a different object, as Burnham (Lick Obs., ii., p. 180), without noticing any great error in RA, gives position angle 60 degrees, distance 20 arcsec, and states that the preceding (western) one is undoubtedly a nebula, while the following (eastern) one may be a star". Corwin agrees with Dreyer that Burnham's object must be different from Howe's, but concludes that Howe's observation is probably of the same object seen by Muller, as their descriptions are essentially identical (namely a position angle equivalent to 150 degrees and a separation of about 6 arcsec, though Muller estimated the magnitude as 15 and Howe as 11) and a 1 or 2 minute of time error in the right ascension is fairly typical of observations at the Leander McCormick Observatory, where Muller worked. Unfortunately, there is nothing at Howe's position either (2 minutes of time to the west of the NGC position, thereby precessing to about RA 22 26 35, Dec -22 08 30), but there is an object between the NGC and Howe's positions that almost perfectly fits Muller and Howe's descriptions of the object, namely the triplet of stars listed above (although the total extent of the triplet is 12 arcsec, if seen as a pair of stars the separation would look more like 8 or so seconds of arc). So although the identification of the triplet with NGC 7287 cannot be considered certain, it is probably what Howe and Muller observed.
Discovery Note: Gottlieb's notes contain several comments about possible and improbable identifications and refers to Corwin's similar notes. This entry will not be complete until I have studied all these comments in detail. They note several possible candidates and even some egregious errors in one catalog or another.
Physical Information: Apparent size from one end of the triplet to the other about 12 arcsec. Apparent magnitude about 11.5 for each star, overall magnitude a little less than 11.

Historical Identification: As noted in the entry for NGC 7287, there was (and to a certain extent still is) considerable confusion about the identity of that object, and when Burnham observed the star and nebula listed in this entry, he presumed it was Muller's NGC 7287; but the orientation and separation of the star and galaxy are completely different from Muller's description of what he observed, so Burnham's object is certainly not the same thing, and therefore not the NGC object, either.
Physical Information: The supposed "double" consists of a magnitude 15(?) star about 20 arcsec east northeast of magnitude 15(?) galaxy PGC 68960, plus a magnitude 16(?) galaxy (PGC 68959) that would have contributed little or nothing to Burnham's impression of the pair. PGC 68960 has an apparent size of 0.4 by 0.15 arcmin, but its distance is unknown, so its actual size is also unknown. PGC 68959 has an apparent size of 0.2 by 0.15 arcmin, but its distance can be estimated, based on its recessional velocity of 11905 km/sec. A straightforward calculation (dividing the recessional velocity by the Hubble expansion "constant") indicates that PGC 68959 is about 555 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 530 million light-years away at the time the light by which we see it was emitted, about 540 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size, PGC 68959 is about 30 thousand light-years across.

Physical Information: Apparent size 0.3 by 0.2? arcmin

Historical Identification: Per Dreyer, NGC 7288 (= GC 6053, Marth #482, (Safford #84), 1860 RA 22 21 00, NPD 93 36) is "very faint, extremely small, stellar." The position precesses to RA 22 28 14.6, Dec -02 53 13, less than 0.2 arcmin south-southwest of the center of the galaxy listed above and on the rim of the nucleus, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Notes: Safford's observations were not published until long after the fact, and Dreyer was already in the last stages of publication of the NGC when he read about them, so he only noted them in an appendix and none of the individual NGC entries mention his observations; hence the inclusion of his name in parentheses.
Physical Information: Apparent size 2.3 by 1.5? arcmin

Historical Identification: Per Dreyer, NGC 7289 (= GC 4794 = JH 3944, 1860 RA 22 21 12, NPD 126 10.4) is "very faint, small, round, gradually brighter middle." The position precesses to RA 22 29 16.6, Dec -35 27 34, about 1 arcmin northwest of the galaxy listed above, the description fits and there is nothing comparable nearby, so the identification is certain.
Physical Information: Apparent size 1.3 by 1.0? arcmin

Historical Identification: Per Dreyer, NGC 7290 (= GC 6054, Marth #483, 1860 RA 22 21 40, NPD 73 34) is "pretty bright, small, pretty much extended." The position precesses to RA 22 28 27.6, Dec +17 08 49, less than 0.3 arcmin east of the center of the galaxy listed above and barely outside its nucleus, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Apparent size 1.6 by 1.0? arcmin

Historical Identification: Per Dreyer, NGC 7291 (= GC 6055, Stephan list VIII (#18), (Safford #56), 1860 RA 22 21 42, NPD 73 55.9) is "extremely faint, extremely small, round, suddenly much brighter middle." The position precesses to RA 22 28 30.1, Dec +16 46 55, less than 0.3 arcmin east-southeast of the center of the galaxy listed above and barely outside its nucleus, the description fits and there is nothing comparable nearby, so the identification is certain.
Discovery Note 1: Safford's observations were not published until long after the fact, and Dreyer was already in the last stages of publication of the NGC when he read about them, so he only noted them in an appendix and none of the individual NGC entries mention his observations; hence the inclusion of his name in parentheses.
Discovery Note 2: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Physical Information: Apparent size 1.8 by 1.7? arcmin

Historical Identification: Per Dreyer, NGC 7292 (= GC 6056, Stephan list IV (#12), 1860 RA 22 21 59, NPD 60 25.4) is "extremely faint, small, oval, faint star involved." The position precesses to RA 22 28 26.0, Dec +30 17 26, less than 0.1 arcmin south-southwest of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Earlier references list a later discovery date, based on Stephan's publication of a micrometrically measured position of this object; but studies of Stephan's original notes show that as in the case of many other discoveries, he had actually observed the "nova" on an earlier date, which is the one shown above.
Physical Information: Apparent size 2.1 by 1.6? arcmin

Historical Identification: Per Dreyer, NGC 7293 (= GC 4795, Harding (4), 1860 RA 22 22 06, NPD 111 33.0) is "a remarkable object, pretty faint, very large, extended or binuclear (Auwers 48)." The position precesses to RA 22 29 45.2, Dec -20 50 07, barely east of the center of the nebula listed above and well within its bright outline, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Notes: The discovery (and multiple rediscoveries) of this nebula involved "(Auwers 48)", which refers to the fact that John Herschel became aware of Harding's discovery as a result of its entry in Auwers' catalog, and added it to the GC despite never observing it himself. Gottlieb notes that Ernesto Capocci independently discovered the nebula in late 1824, but because his list wasn't checked until 1857 (by August Winnecke) and his position is over a degree to the west, so his "object" wasn't found or even known about by others even after that. Christian Peters reported his "discovery" in an 1856 paper, and Jermaine Porter also reported its "discovery" in 1884, although it had already been listed in the GC. (Gottlieb also makes several comments about 1912 to 1921 photographic observations.)
PGC Designation Note: For purposes of completeness, LEDA assigned a PGC designation for this object, even though it isn't a galaxy; however, a search of the database for that designation returns no result, so the designation is shown quotes.
Physical Information: At less than 500 light-years' distance, the Helix Nebula has the largest apparent size of any planetary nebula, its brighter central region covering nearly 20 arcmin, and its faint outer halo extending another 5 arcmin to the northeast. Because of its size, its light is spread out (and correspondingly faint), and it went unnoticed by both Herschels; but with modern telescopes and CCD cameras it is easy to detect, and is considered one of the finest objects for amateur observers.

Historical Identification: Per Dreyer, NGC 7294 (Leavenworth list I (#251), 1860 RA 22 22 20, NPD 116 08.2) is "very faint, very small, round." The second IC lists a corrected RA (per Howe) of 22 24 22. The NGC position precesses to RA 22 30 06.2, Dec -25 25 17, but there is nothing there nor anywhere near there. The nearest object that Leavenworth might have recorded is a galaxy that lies about 2 minutes of time to the east and 2 arcmin to the north of Leavenworth' position (and since Leander McCormick's right ascensions are notorious for 1 or 2 arcmin errors, would be a suitable candidate). Evidently that's what Howe thought, as his position precesses to RA 22 32 07.5, Dec -25 25 07, about 1.2 arcmin nearly due south of that galaxy, and since the description is a reasonable fit and there is nothing comparable anywhere in the region, that galaxy is listed here as NGC 7294, with essentially no doubt about the certainty of the identification. (See IC 5225 for a discussion of the duplicate entry.)
IC 5225: Per Dreyer, IC 5225 (Swift list XII #38, 1860 RA 22 23 47, NPD 116 04.9, is "most extremely faint, pretty small, round, between 2 stars." The position precesses to RA 22 31 32.6, Dec -25 21 52, (finish up here and move to IC 5225). IC 5226, which Swift discovered on the same night, (Swift list XII #39, 1860 RA 22 23 57, NPD 115 22.6) is "most extremely faint, pretty large, round." Its position precesses to RA 22 31 41.5, Dec -24 39 34, but the currently accepted position is RA 22 32 30.2, Dec -25 39 43, about 50 seconds of time to the east of Swift's position, and NGC 7294 lies about 36 seconds of time to the east of Swift's position, so it appears that IC 5225 is a duplicate observation of NGC 7294. NOTE: SIMBAD lists IC 5225 as the very faint galaxy (much fainter than IC 5226 or NGC 7294) about 25 seconds of time to the WEST of Swift's position, which seems very unlikely.
Physical Information: Apparent size 2.0 by 1.2? arcmin

Historical Identification: Per Dreyer, NGC 7295 (= GC 4796 = JH 2163, 1860 RA 22 22 21, NPD 37 53.4) is "a cluster, poor, a little compressed, stars from 12th to 13th magnitude."
Physical Information: Apparent size 4? arcmin
Gotttlieb describes this as an asterism of about 10 stars in an east-west string about 3 arcmin in length (an unimpressive random grouping). Gottlieb notes that JH called this "A Milky Way straggler, a poorish cluster of stars 12 to 13th magnitude". RNGC lists this as nonexistent, while Corwin suggests that if JH's declination was 30 arcmin too far north, 7295 = 7296 (JH listed his father's VII-1 (= 7296) as a "synonym" with a question mark, so he was uncertain as to whether his #2163 was actually a different object. Gottlieb's description presumes that JH's position was correct, and if 7295 is 7296, then the entry for that would be more appropriate.

Historical Identification: Per Dreyer, NGC 7296 (= GC 4797 = WH VII 41, 1860 RA 22 22 37, NPD 38 24.8) "a cluster, irregularly round, a little compressed, stars very small (faint)."
Physical Information: Given the duplicate entry, see NGC 7295 for anything else.
Gottlieb says this is roughtly 30 stars in a 3 x 2 arcmin area elongated north-south. "Not particularly distinctive as located in a rich star field." Gottlieb further states that JH's RA was 40 seconds too large. It appears that the identification of 7295 and 7296 are at least somewhat uncertain, pending a look at Corwin's notes.

Historical Identification: Per Dreyer, NGC 7297 (= GC 4798 = JH 3945, 1860 RA 22 22 59, 128 33.0) is "extremely faint, small, round, preceding (western) of 2," the other being NGC 7299.
Physical Information: Apparent size 0.9 by 0.6? arcmin

Historical Identification: Per Dreyer, NGC 7298 (= GC 6057, Marth #484, 1860 RA 22 23 18, NPD 104 54) is "very faint, pretty large, irregularly round."
Physical Information: Apparent size 1.3 by 1.1? arcmin

Historical Identification: Per Dreyer, NGC 7299 (= GC 4800 = JH 3946, 1860 RA 22 23 24, NPD 128 32.2) is "extremely faint, small, round, following (eastern) of 2," the other being NGC 7297.
Physical Information: Apparent size 0.7 by 0.7? arcmin