Historical Identification: Per Dreyer, NGC 7200 (= GC 4748 = JH 3917, 1860 RA 21 58 08, NPD 140 40.8) is "pretty faint, small, round, suddenly much brighter middle." The position precesses to RA 22 07 08.9, Dec -50 00 01, on the southern rim 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 Microwave Background radiation of 2705 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7200 is about 125 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 115 to 300 million light-years. Given that and its apparent size of about 1.1 by 0.85 arcmin (from the images below), the galaxy is about 40 thousand light-years across.
 NED lists a second recessional velocity of about 17250 km/sec, but this almost certainly belongs to a different object, as it would put the galaxy more than 700 million light-years away, so far beyond any other estimate of its distance that it is almost certainly wrong.
Classification Note: This galaxy is listed as just E or E+ in most references, but in the DSS2 "red" image it appears to have a short asymmetrical bar and bright lens (the "l" in parentheses) and a faint corona, and per Corwin, hence the classification provided by him. (AB means that the galaxy has an appearance in-between barred and unbarred, but with the bar more prominent than not.)

Historical Identification: Per Dreyer, NGC 7201 (= GC 4749 = JH 3918, 1860 RA 21 58 27, NPD 121 55.5) is "faint, round, gradually brighter middle, 1st of 4," the others being NGC 7202, 7203 and 7204. The position precesses to RA 22 06 33.7, Dec -31 14 44, just over an arcmin north-northeast 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 Microwave Background radiation of 4135 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7201 is about 190 to 195 million light-years away. Given that and its apparent size of about 1.4 by 0.5 arcmin (from the images below), the galaxy is about 75 to 80 thousand light-years across. NED lists NGC 7201 as a possible group member with NGC 7203, which see for more about this suggestion.

Historical Identification: Per Dreyer, NGC 7202 (= GC 4750 = JH 3920, 1860 RA 21 58 39, NPD 121 51.8) is "extremely faint, stellar, 2nd of 4," the others being NGC 7201, 7203 and 7204. The position precesses to RA 22 06 45.5, Dec -31 11 01, about 1.3 arcmin south-southeast of the galaxy now listed as NGC 7203, but the description "extremely faint, stellar" rules out that galaxy, and there is no other nebular object close to the position. However, in his Cape of Good Hope "results" (published in 1847), Herschel states that JH 3920 precedes (lies to the west of) JH 3921 (which is NGC 7203) exactly 1 second of time, and his listed declinations put 3920 exactly three arcmin to the south of its neighbor. In other words, NGC 7202 must be something "extremely faint" and "stellar" to the south-southwest of NGC 7203. Precessing the J2000 position of NGC 7203 (RA 22 06 43.9, Dec -31 09 45) to the equinox of 1830 (the one used in the Cape Catalogue's tables of nebulae and clusters) yields RA 21 56 52.6, Dec -31 59 10, which should place JH 3920 at (1830) RA 21 56 51.6, Dec -32 02 10, which precesses to (J2000) RA 22 06 43.0, Dec -31 12 45. That position lies only 0.3 arcmin north-northwest of the star listed above, and since it certainly fits the description of JH 3920, that star must be NGC 7202. (As a confirmation of this conclusion, Gottlieb notes that Baracchi carefully searched for the object with the Great Melbourne Telescope and also found only that star near Herschel's position.)
Note About PGC Designation: As is true for most NGC objects, HyperLEDA assigned a PGC designation to this object even though it isn't a galaxy. A search for NGC 7202 returns a result with that PGC designation and the fact that it is only a star, but a search of the database for the PGC designation returns no result, so it is shown in quotes.

Historical Identification: Per Dreyer, NGC 7203 (= GC 4751 = JH 3921, 1860 RA 21 58 40, NPD 121 49.7) is "considerably faint, round, stellar, 3rd of 4," the others being NGC 7201, 7202 and 7204. The position precesses to RA 22 06 46.4, Dec -31 08 55, just under an arcmin north-northeast of the galaxy listed above, and although the description seems a little misleading, there is nothing else nearby and as already noted in the entry for NGC 7202, all of Herschel's positions for the galaxies that he actually observed in this region are to the north-northeast of the actual objects, so the identification is certain.
Historical Misidentification: NED states that the CSRG misidentifies NGC 7203 as the star which is actually NGC 7202. Given the problems noted with the identification of NGC 7202, that mistake is hardly surprising, but it is still a mistake.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3785 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7203 is about 175 to 180 million light-years away, much further away from us than a single redshift-independent distance estimate of about 115 million light-years. Given that and its apparent size of about 1.6 by 0.8 arcmin (from the images below), the galaxy is about 80 to 85 thousand light-years across.
 NED lists this as a possible group member with NGC 7201, but the recessional velocity it shows (only 2210 km/sec) would make NGC 7203 a much closer foreground galaxy. However, HyperLEDA lists the 3K Vr of 3785 km/sec shown in the previous paragraph, and per Corwin the smaller 3K Vr is based on 21-cm measurements that appear to be precise but must be wrong, because a large number of other measurements of the recessional velocity are all close to the value shown in LEDA. This means that NGC 7201 and 7203 may be physical companions, since they could have peculiar velocities (random motions relative to their neighbors) as large as the difference in their recessional velocities.
Classification Note: The "type" shown in the description line is taken from NED, but the close-up image below suggests that this galaxy might actually be an early-type spiral; however, in the absence of better images it seems best to be cautious and use the listed type, instead of proposing one that might soon be proven wrong.

Historical Identification: Per Dreyer, NGC 7204 (= GC 4752 = JH 3922, 1860 RA 21 58 48, NPD 121 43.5) is "pretty bright, large, a little extended, gradually brighter middle, 4th of 4," the others being NGC 7201, 7202 and 7203. The position precesses to RA 22 06 54.1, Dec -31 02 42, only 0.3 arcmin due north of the pair of galaxies listed above, the description fits (and is better than the ones for the 2nd and 3rd objects in the list of 4) and there is nothing else nearby, so the identification is certain.
Discovery Note: Gottlieb writes that Herschel saw this "strongly interacting double system" as only a single object, and states that it was first observed as a close pair "in a Helwan Observatory photograph taken in 1914-16 with the 30" reflector and reported in the 1921 observations table" as "a curious double nebula." (Corwin also writes that since Herschel made no mention of any irregularity in his (single) observation of this nebula, we have to assume that the whole assemblage is his object.)
Note About PGC Designations: As is true for most NGC objects, HyperLEDA assigned a PGC designation to this pair. A search for NGC 7204 returns a result with that PGC designation and the fact that it is a double galaxy, but a search of the database for the PGC designation returns no result, so it is shown in quotes.
 An earlier version of this entry had the PGC designations for the individual galaxies reversed, due to their being taken from a now obsolete database. The current labels, in which the smaller PGC and MCG designations are applied to the northwestern component, is the result of correcting that error.
NED Search Note: A search of NED for the northwestern galaxy only recognizes PGC 68054 and MCG -05-52-028; it does not accept a search for PGC 68060 at all. Similarly, it only recognizes the southeastern galaxy as MCG -05-52-029.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2310 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7204 is about 105 to 110 million light-years away, in good agreement with a single redshift-independent distance estimate of about 110 million light-years. The more elongated southeastern Component 2 (PGC 68061) has an apparent size of about 1.0 by 0.25, and a faint western extension that makes the overall size of the galaxy about 1.55 arcmin (all sizes from the images below). Given that and its distance, that galaxy is about 30 to 35 thousand light-years across, and with its western extension, spans about 45 to 50 thousand light-years. The irregularly shaped northwestern Component 1 (PGC 68060) has a bright central region with an apparent size of about 0.4 by 0.3 arcmin, and fainter east-west extensions of about 0.9 by 0.5 arcmin (again, from the images below). Given that and its distance, its brighter portion is about 10 to 15 thousand light-years across, and the overall size of the galaxy is about 25 to 30 thousand light-years. Even in the images below it is obvious that the two galaxies are strongly interacting, and a really good image of the pair would undoubtedly be spectacular.
Classification Note: LEDA lists the northwestern component as SBab and the southeastern component as S0/a, but the interaction of the two galaxies makes any certain classification impossible. The classifications shown at the start of this entry were provided by Dr. Corwin, who has decades of experience dealing with such matters, and as shown by the numerous question marks, even he felt that an apparently certain "type" was out of the question (for 68061, "sp" stands for "spindle", meaning that the galaxy is seen edge-on). Fortunately, tentative types posted while waiting for his opinion were, within the uncertainty indicated by the question marks, in agreeement with his classifications; so apparently I've learned enough from him to let my types stand in simpler cases.

Historical Identification: Per Dreyer, NGC 7205 (= GC 4753 = JH 3919, 1860 RA 21 58 54, NPD 148 06.5) is "pretty bright, large, considerably extended, gradually then pretty suddenly a little brighter middle." The position precesses to RA 22 08 28.5, Dec -57 25 37, about 1.1 arcmin northwest of the center 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 Microwave Background radiation of 1535 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7205 is about 70 to 75 million light-years away, in good agreement with redshift-independent distance estimates of about 45 to 75 million light-years. Given that and its apparent size of about 4.2 by 2.0 arcmin (from the images below), the galaxy is about 85 to 90 thousand light-years across.
Use By The deVaucouleurs Atlas: NGC 7205 is used by The deVaucouleurs Atlas of Galaxies as an example of type SA(s)bc. The galaxy exhibits strong emission lines caused by heating of interstellar gases by young clusters of hot, bright stars, and is therefore classified as a LINER.

Warning About Non-Standard Designations: Since there are no standards for adding letters to NGC/IC designations, it is not uncommon for the same letters to be added to different galaxies, leading to the possibility that data belonging to one galaxy will be assigned to a completely different one. As a result, such non-standard designations should never be used, and I only use them in this catalog because they are used elsewhere, and I need a way to warn people about the dangers involved.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7080 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 68083 is about 330 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 320 million light-years away at the time the light by which we see it was emitted, about 325 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 1.15 by 1.1 arcmin (from the images below), the galaxy is about 105 to 110 thousand light-years across. (Note: Other than being in roughly the same direction, there is no relationship between "NGC 7205A" and NGC 7205, which is about 250 million light-years closer to us.)

Historical Identification: Per Dreyer, NGC 7206 (= GC 6022, Marth #462, 1860 RA 21 58 56, NPD 73 54) is "faint, small, a little extended, brighter middle." The position precesses to RA 22 05 39.2, Dec +16 46 44, just over half an arcminute southwest of the galaxy listed above, the description fits and and other than NGC 7207, discovered by Marth on the same night, there is nothing comparable nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 9090 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7206 is about 420 to 425 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 405 to 410 million light-years away at the time the light by which we see it was emitted, about 415 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 1.7 by 1.45 arcmin (from the images below), the galaxy is about 200 thousand light-years across.
 Given their recessional velocities, NGC 7206 and 7207 may be a physical pair; but although their peculiar velocities (random motions relative to their neighbors) may be large enough to explain the difference in their recessional velocities, it is just as likely that NGC 7207 is simply a foreground galaxy; and even if they are currently close companions, their relative velocity is probably large enough that any connection between them is only a temporary one (like ships passing in the night).

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4395 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68011 is about 205 million light-years away. Given that and its apparent size of about 0.75 by 0.15 arcmin (from the images below), the galaxy is about 45 thousand light-years across.
 Although listed here as an apparent companion of NGC 7206, PGC 68011 is much closer to us than either NGC 7206 or 7207, and has no relationship to either of them other than being in the same part of the sky.

Historical Identification: Per Dreyer, NGC 7207 (= GC 6023, Marth #463, 1860 RA 21 59 00, NPD 73 55) is "very faint, small." The position precesses to RA 22 05 43.2, Dec +16 45 45, less than 0.7 arcmin west-southwest of the galaxy listed above, the description fits and other than NGC 7206, discovered by Marth on the same night, there is nothing comparable nearby, so the identification is certain.
Designation Note: Gottlieb writes that neither UGC nor CGCG list this galaxy as NGC 7207, but that per Malcolm Thomson it corresponds to CGCG 451-007, as shown above.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 8440 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7207 is about 390 to 395 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 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 its apparent size of about 0.75 by 0.25 arcmin (from the images below), the galaxy is about 80 to 85 thousand light-years across.
 Given their recessional velocities, NGC 7206 and 7207 may be a physical pair; but although their peculiar velocities (random motions relative to their neighbors) may be large enough to explain the difference in their recessional velocities, it is just as likely that NGC 7207 is simply a foreground galaxy; and even if they are currently close companions, their relative velocity is probably large enough that any connection between them is only a temporary one (like ships passing in the night).

Historical Identification: Per Dreyer, NGC 7208 (= GC 4754 = JH 3923, 1860 RA 21 59 25, NPD 119 44.0) is "very faint, very small, round, almost a planetary nebula." The second IC lists a corrected RA (per Howe) of 22 00 23. The NGC position precesses to RA 22 07 26.6, Dec -29 03 09, but there is nothing there; there is, however, a galaxy that perfectly fits the description about a minute of time to the east and since visual observers often made single-digit errors of a minute of time, there is no doubt that the galaxy listed above is what Herschel observed. Howe's corrected position precesses to RA 22 08 24.2, Dec -29 03 03, well within the northwestern outline of the galaxy listed above, confirming that his measurement was essentially perfect.
Designation Note: Gottlieb writes that although this is MCG -05-52-032, MCG fails to list it as NGC 7208.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2370 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7208 is about 110 million light-years away. Given that and its apparent size of about 0.85 by 0.55 arcmin (from the images below), the galaxy is about 25 to 30 thousand light-years across.
Classification Note: Based on older images, NGC 7208 has traditionally been described (and still is, in LEDA and NED) as a lenticular galaxy; but as the PanSTARRS image shows, it is actually a peculiar spiral galaxy or irregular galaxy (Corwin lists it as I0 pec, whence the type shown above).

Historical Identification: Per Dreyer, NGC 7209 (= GC 4755 = JH 2147 = WH VII 53, 1860 RA 21 59 42, NPD 44 11.6) is "a cluster, large, considerably rich, pretty compressed, stars from 9th to 12th magnitude." The position precesses to RA 22 05 16.8, Dec +46 29 09, almost dead center on the brightest star in the cluster listed above and well within its outline, and the description fits so the identification is certain.
Note About PGC Designation: As usual, HyperLEDA has a page for NGC 7209 (which shows that it is an open cluster) and assigned a PGC designation to the cluster, even though it isn't a galaxy; but also as usual, a search of the database for that designation returns no result, so it is shown in quotes.
Physical Information: Based on the image below, the scattering of bright stars that probably make up Herschel's cluster is about 19 by 14 arcmin in size, with most of its members lying within a region about 2 to 3 arcmin smaller than that. The cluster is thought to be about 3800 light-years from us, in which case its apparent size corresponds to a physical size of about 15 by 20 light-years.

Historical Identification: Per Dreyer, NGC 7210 (= GC 4756 = JH 2148, 1860 RA 21 59 58, NPD 63 34.3) is "extremely faint, round, brighter middle, very faint double star to northwest." The position precesses to RA 22 06 22.2, Dec +27 06 31, but there is nothing there nor anywhere near there, so until recently the object was thought to be lost or nonexistent. However, in April 2016 Corwin took a look at the record of Herschel's sweep, and found that Herschel made a one hour error in recording the right ascension (which was too small), and a one degree error in the NPD (which was too large). Correcting for that, the position becomes 1860 RA 22 59 58, NPD 62 34.3, which precesses to RA 23 06 44.2, Dec 28 11 03, about 1.4 arcmin west northwest of the galaxy listed above, the description fits, and there is nothing else nearby, so the identification is certain.
NGC Note: In the notes at the end of the NGC Dreyer states "Not seen by (3rd) Lord Rosse (three observations), not looked for by d'Arrest." Given the huge errors in Herschel's position, it is hardly surprising that Lord Rosse failed to find this object.
Discovery Notes: Herschel's GC entry (and a GC note about it) showed that he was very uncertain about the position of the object, and Corwin stated in his original discussion of the observation (when it appeared to be of a lost or nonexistent object) that the NPD in Herschel's original record differed from that in the GC by a degree, but that he was unable to find anything at either declination (as it turned out, due to the unrecognized error in the right ascension). Reviewing Herschel's reduction of the NPD shows that the original record was correct and Herschel and Dreyer's usage of the incorrect NPD in the GC led to a one degree error in the declination. The error in the right ascension is not as obvious, but as discussed in detail by Corwin in his current notes, the only right ascension recorded in the sweep has a position differing from the clock entry by an hour. Presuming the clock entry was correct produces a one hour change in the right ascension and reasonably accurate positions for all three objects observed in the sweep (two double stars and JH 2148), thereby confirming the accuracy of the present identification of NGC 7210 as a prior observation of NGC 7487.
Note About PGC/NED Listings: HyperLEDA has a page for NGC 7210, which lists the object as unknown (in other words, it fails to note Corwin's recent discovery that it is NGC 7487), but it still assigned a PGC designation to the entry. As usual in such cases, a search of the database for that designation fails to return an entry, so it is shown in quotes. The other designations are for NGC 7487, and are shown here because the two entries are for the same object. NED also has a page for NGC 7210, which also fails to note the identity with NGC 7487, and contains nothing of any interest or value.
Physical Information: As implied by the previous paragraph, becaue of the relatively recent discovery of the duplicate entry, NGC 7210 is still listed as lost or nonexistent almost everywhere; so see NGC 7487 for anything else.

Historical Identification: Per Dreyer, NGC 7211 (= GC 6024, Marth #464, 1860 RA 21 59 58, NPD 98 47) is "extremely faint, small, stellar." The position precesses to RA 22 07 21.8, Dec -08 06 07, but there is nothing there. However, as noted by Corwin, there is a galaxy that perfectly fits the description exactly one minute of time to the west of Marth's position, so Marth almost certainly made an unfortunately common single-digit error in the right ascension, and between its description and position, the identification of NGC 7211 as the galaxy listed above is essentially certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7895 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7211 is about 365 to 370 million light-years away, in reasonable agreement with redshift-independent distances of about 315 to 335 million light-years. 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 to 360 million light-years away at the time the light by which we see it was emitted, about 360 to 365 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 0.55 arcmin (from the images below), the galaxy is about 75 to 80 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7212 (Swift list V (#93), 1860 RA 22 00 06, NPD 80 26.6) is "extremely faint, very small, a little extended." The position precesses to RA 22 07 00.4, Dec +10 14 16, less than half an arcminute west-northwest of the center of the pair of galaxies listed above, the description fits and there is nothing comparable nearby, so the identification is certain.
Observational and Designation Notes: Per Gottlieb this is an interacting pair with tidal plumes. Corwin provided the position for the pair, and the individual components. Given the NGC description and the appearance of the system, NGC 7212 must be considered to be the entire system (both components and their scattered debris), but the southwestern member of the pair is listed as 7212 in SIMBAD, and the northern member of the pair is listed as UZC J220702.3+101414 in SIMBAD and LEDA. As in many other cases, a search of HyperLEDA for the PGC designation assigned to the northern component returns no result, so it is shown in quotes, but for simplicity's sake I have used that designation to label the middle image below, instead of the UZC designation.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7630 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7212 is about 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 345 million light-years away at the time the light by which we see it was emitted, about 350 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). The main body of the southern component has an apparent size of about 1.05 by 0.45 arcmin, that of the northern component of about 0.65 by 0.3 arcmin, and the broadly scattered debris from their collision has an apparent size of about 1.85 by 1.3 arcmin (all apparent sizes from the images below). This and the probable distance would make the southern component about 105 thousand light-years across, the northern component about 65 thousand light-years across, and their scattered remains about 185 thousand light-years across.
Classification Notes: The brighter southern component is usually listed as type Sb or Sab (plus a very big "peculiar"), and is a Seyfert galaxy (type Sy1 or 2, depending on the reference consulted). The fainter northern component is not classified in any reference I can find, but is obviously a very disturbed spiral; a private communication by Corwin suggests Sa? pec, and that seems reasonable to me, as shown in the description line for the galaxy. Many references list this as a triplet, including the 2MASS object to the southwest, so that galaxy is discussed in the following entry.

Physical Information: Although there appear to be absolutely no measurements revealing the distance of this galaxy, its appearance in the images below suggests that it may be undergoing some kind of interaction with its apparent neighbors (aside from its disturbed dust lanes, which can be found in even "normal" galaxies, there are pretty convincing distortions at the northeastern and southwestern ends of the disk, which make it seem more likely than not that the apparent interaction is a real one). If so, then it must also be about 345 million light-years from us, and given its apparent size of about 0.4 by 0.08 arcmin (from the images below), it would be about 40 thousand light-years across.
Classification Note: Since the galaxy appears to be essentially edge-on (indicated by "sp" for "spindle"), its classification is uncertain. Corwin agrees with my educated guess that this might be a peculiar Sc galaxy, but notes that even taking foreground extinction into account it is redder than a typical Sc, and suggests that its nuclear bulge might justify type Sb, so I have used the intermediate "bc" and added a question mark.

Historical Identification: Per Dreyer, NGC 7213 (= GC 4757 = JH 3924, 1860 RA 22 00 29, NPD 137 50.6) is "very bright, pretty small, round, gradually brighter middle." The position precesses to RA 22 09 17.6, Dec -47 09 36, on the northeastern rim of the galaxy listed above, the description fits and there is nothing comparable nearby, so the identification is certain.
Modern Misidentification: A paper by Vedavathi and Doddamani appears to misidentify an image of NGC 4593 as one of NGC 7213, and although published in 2017, uses B1950 coordinates for the nine galaxies studied, which confuses the issue still further (when converted to J2000 coordinates, the position given for NGC 7213 is correct, but it is not one of the three galaxies whose images are shown in the paper). This sort of error is all too common in modern papers, and is one of the reasons that I undertook the creation of this historically accurate catalog.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 1545 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7213 is about 70 to 75 million light-years away, in perfect agreement with a single redshift-independent distance estimate of about 70 to 75 million light-years. Given that and its apparent size of about about 5.45 by 5.25 arcmin (from the images below), the galaxy is about 115 thousand light-years across.
Use By The deVaucouleurs Atlas: NGC 7213 is used by The deVaucouleurs Atlas of Galaxies as an example of type SA(rs)a, whence the classification shown in the description line above. Both LEDA and NED state that this is a Seyfert galaxy, but disagree on the classification, with LEDA listing type Sy3, and NED type Sy1.5. The galaxy is also listed as a LINER because of emission lines from interstellar gases heated by innumerable hot, bright young stars. As shown in the Carnegie-Irvine images below, a nucleus with multiple central rings and nearly circular spiral arms is surrounded by a much larger, fainter nearly circular disk with very faint and incomplete dust lanes.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 1585 km/sec (and H₀ = 70 km/sec/Mpc), PGC 130726 is about 70 to 75 million light-years away. That (and its recessional velocity) is essentially the same as the value for NGC 7213, so they are almost certainly physical companions. Given its distance and its apparent size of about 0.65 by 0.6 arcmin (from the images below), the galaxy is about 13 to 15 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7214 (= GC 4758 = JH 3926, 1860 RA 22 01 08, NPD 118 29.7) is "a globular cluster, pretty large, irregularly round, partially resolved (some stars seen)." The position precesses to RA 22 09 06.4, Dec -27 48 41, on the western rim of the galaxy listed above, the description is a reasonable fit and there is nothing comparable nearby, so the identification is certain.
Discovery Note: Howe stated that this did not appear to be a globular cluster, but a nebula with a nuclear condensation of magnitude 12, with surrounding nebulosity of indefinite extent. Per Gottlieb, in 1915 Knox-Show reported that it was not a globular cluster but an open spiral based on a photograph taken between 1912-13 at the Helwan Observatory (a more detailed description was later published based on images taken in 1914-16).
Physical Information: Since NGC 7214 is part of an interacting group of galaxies, the best way to estimate its (and the group's) distance is to take an average of all the information related to their individual distances. For NGC 7214 (HCG 91A), the recessional velocity relative to the Cosmic Microwave Background radiation is about 6860 km/sec, for HCG 91B that value is about 6975 km/sec, for HCG 91C that value is about 6895 km/sec, and for HCG 91D that value is about 7020 km/sec, yielding an average for the Compact Group of about 6935 to 6940 km/sec. Using that average (and H₀ = 70 km/sec/Mpc), HCG 91 is about 320 to 325 million light-years away from us, in fair agreement with redshift-independent distance estimates (only available for NGC 7214) of about 105 to 285 million light-years. Using the distance obtained from the average recessional velocity and its apparent size of about 1.7 by 1.0 arcmin for the main galaxy, and about 3.25 arcmin east-west and 1.7 arcmin north-south for its faint, extended arcs (all sizes from the images below), NGC 7214 is about 160 thousand light-years across and its extended arcs span more than 300 thousand light-years. Because of its brilliant nucleus, NGC 7214 is classified as a Seyfert Galaxy (type Sy1.2).

Physical Information: As discussed in the entry for NGC 7214, HCG 91 is about 320 to 325 million light-years away. Given that and its apparent size of about ? arcmin (from the images below), PGC 68155 is about ? thousand light-years across.

Physical Information: As discussed in the entry for NGC 7214, HCG 91 is about 320 to 325 million light-years away. Given that and its apparent size of about 0.9 by 0.75 arcmin (from the images below), PGC 68160 is about 85 thousand light-years across.

Physical Information: As discussed in the entry for NGC 7214, HCG 91 is about 320 to 325 million light-years away. Given that and its apparent size of about 1.15 by 0.2 arcmin (from the images below), PGC 68164 is about 105 to 110 thousand light-years across.
Classification Note: Since the galaxy is nearly edge-on (whence "sp" for "spindle" in its Type), the classification is uncertain.

Historical Identification: Per Dreyer, NGC 7215 (= GC 6025, Marth #465, 1860 RA 22 01 23, NPD 90 11) is "very faint, small, extended." The position precesses to RA 22 08 33.1, Dec +00 30 00, about 0.8 arcmin south-southwest 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 Microwave Background radiation of 3655 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7215 is about 170 million light-years away. Given that and its apparent size of about 0.9 by 0.35 arcmin (from the images below), the galaxy is about 45 thousand light-years across.
Classification Note: Since the galaxy is nearly edge-on classification is difficult, but it is definitely a spiral galaxy, and not lenticular, as currently classified by all major references. In reply to my note about that error (in which I proposed a "best guess" of SB(s)ab?), Corwin provided the type in the description line, based on his examination of SDSS and PanSTARRS images. He writes that although there is a bar it is very short and very weak (hence AB instead of just B), agrees that there are short spiral arms at the ends of the bar, but notes the presence of at least two central rings (hence rs instead of s), and assigns type "a: pec" to denote a smooth disk, but with various oddities that require a colon (to indicate uncertainty in the classification) and "pec" to correspond to the presence of those oddities.

Historical Identification: Per Dreyer, NGC 7216 (= GC 4759 = JH 3925, 1860 RA 22 01 31, NPD 159 20.8) is "pretty faint, small, round, gradually brighter middle." The position precesses to RA 22 12 32.0, Dec -68 39 35, only 0.3 arcmin west-northwest of the center of the galaxy listed above and barely outside its western boundary, 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 3440 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7216 is about 160 million light-years away, well beyond a single redshift-independent distance estimate of about 110 to 115 million light-years. Using its Hubble Flow distance and its apparent size of about 1.5 by 1.0 arcmin (from the images below), the galaxy is about 70 thousand light-years across.
Classification Note: Probably because of the "flocculent" appearance of its outer regions, some references list this as type S0/a; but without better images, whether that is more accurate than the usual E/S0 classification cannot be known. Either way, it would still be "lenticular", so all I have done is add a question mark to the usual classification.

Note About PGC Designation: Although listed in LEDA as a 2MASX object, and therefore assigned a PGC designation, there is nothing about the object on its page, and a search of the database for the PGC designation returns no result, so it is shown in quotes. (NED also has almost nothing about it, other than its position and magnitudes at various wavelengths, none of which are in the visual spectrum.)
Physical Information: There is no distance information for this galaxy, but odds are that it is simply a far more distant background galaxy, and not an actual companion of NGC 7216. Its magnitude is based on a conversion of its K-band magnitude (a little over 14) to a visual magnitude using typical differences for V-K. The galaxy has an apparent size of about 0.55 by 0.1 arcmin (from the images of NGC 7216, above), but without any distance information there is no way to tell its actual size.

Historical Identification: Per Dreyer, NGC 7217 (= GC 4760 = JH 2149 = WH II 207, 1860 RA 22 01 37, NPD 59 19.4) is "bright, pretty large, gradually brighter middle, extremely mottled but not resolved." The position precesses to RA 22 07 53.1, Dec +31 21 35, almost dead center on the galaxy listed above, the description fits and there is nothing comparable nearby, so the identification is certain.
Discovery Note: Gottlieb writes that Mitchell logged "there can hardly be a doubt that this neb(ula) is a Cl(uster); some stars near centre seen by (3rd) Lord R(osse)." That conclusion was incorrect, but presumably caused by (as noted by Gottlieb) "several faint stars involved or at the periphery." (Mitchell's reference to the Earl suggests that he was present on the night in question and also observed the object.)
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 625 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7217 is about 30 million light-years away, considerably closer than redshift-independent distance estimates of about 50 to 75 million light-years. If the recessional velocity and corresponding distance were considerably larger, it might be preferable to give more weight to the distance derived from that; but for small recessional velocities, peculiar velocities (random motions relative to neighboring galaxies) can substantially alter the measured recessional velocity, so the redshift-independent distance estimates need to be given more weight. I have therefore decided to use a distance of 50 plus or minus 20 million light-years for the following sentence. Given that and its apparent size of about 3.5 by 3.0 arcmin (from the images below, taking into account a very faint glow just outside its spectacular ring), NGC 7217 is about 50 thousand light-years (plus or minus 20 thousand light-years) across. The galaxy is classified as a Seyfert Galaxy (type Sy3) because of its brilliant center, and as a LINER because of strong emission lines by interstellar gases heated by clusters of hot, bright young stars. Detailed study of the galaxy at various wavelengths suggests that the central "disk" is actually a very thick "bulge", and includes an odd feature not seen in most galaxies — substantial numbers of stars moving around its center in the opposite direction from the rest of its stellar content, suggesting a merger with a smaller galaxy within the "recent" past (keep in mind that for galaxies, "recent" can mean within the last few billion years).
Use By The deVaucouleurs Atlas: NGC 7217 is used by The deVaucouleurs Atlas of Galaxies as an example of type (R)SA(r)ab. (Note: The Atlas page includes a discussion of the "detailed study" noted in the previous paragraph, but the suggestion involving a merger comes from an ESO paper.)

Historical Identification: Per Dreyer, NGC 7218 (= GC 4761 = JH 2150 = WH II 897, 1860 RA 22 02 35, NPD 107 20.2) is "pretty bright, a little extended, mottled but not resolved." The position precesses to RA 22 10 12.5, Dec -16 39 03, well within the northern outline 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 Microwave Background radiation of 1330 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7218 is about 60 to 65 million light-years away, in good agreement with redshift-independent distance estimates of about 55 to 95 million light-years. Given that and its apparent size of about 3.25 by 1.4 arcmin (from the images below), the galaxy is about 55 to 60 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7219 (= GC 4762 = JH 3927, 1860 RA 22 02 47, NPD 155 32.1) is "pretty bright, small, round, 2 stars near." The position precesses to RA 22 13 07.4, Dec -64 50 48, well within the northwestern outline of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Observational Note: Gottlieb writes that this galaxy was photographed by Stewart between the dates listed above and noted as an "Ellipse of uniform nebulosity, B(right) stellar nucleus, E(xtended) at 55°."
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2845 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7219 is about 130 to 135 million light-years away, in good agreement with redshift-independent distance estimates of about 120 to 145 million light-years. Given that and its apparent size of about 1.6 by 1.1 arcmin (from the images below), the galaxy is about 60 to 65 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7220 (Muller list II (#466), 1860 RA 22 02 50, NPD 113 40.7) is "extremely faint, very small, very little extended, gradually brighter middle, 10th magnitude star 3' to north." The second IC lists a corrected position (per Howe) of RA 22 03 43, NPD 113 38.2. The original position precesses to RA 22 10 38.6, Dec -22 59 31, but there is nothing there; there is, however, a small galaxy that perfectly fits the description just under a minute of time to the east, and Howe's position, which precesses to RA 22 11 31.2, Dec -22 56 56, lies on that galaxy's northern rim, so the galaxy listed above is certainly what Howe observed, almost as certainly what Muller observed (since only a single-digit error of a minute of time in his right ascension would make that conclusion certain), and is universally considered to be NGC 7220.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4985 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7220 is about 230 to 235 million light-years away, somewhat closer than a single redshift-independent distance estimate of about 290 to 295 million light-years. Given that and its apparent size of about 0.65 by 0.55 arcmin (from the images below), the galaxy is about 40 to 45 thousand light-years across.
Classification Note: Standard references list this as a barred lenticular, or as a lenticular with signs of spiral structure; but neither of those classifications fit its images. In fact, it looks more like an elliptical galaxy than anything else; but since the standard references agree on the lenticular type, I have chosen the simplest type between an elliptical and a lenticular galaxy, and added a question mark to indicate the uncertainty about how the galaxy should be classified.

Historical Identification: Per Dreyer, NGC 7221 (= GC 4763 = JH 3928, 1860 RA 22 03 14, NPD 121 14.4) is "faint, small, round, gradually brighter middle, mottled but not resolved, 2 very small (faint) stars near." The position precesses to RA 22 11 17.2, Dec -30 33 10, on the northeastern rim 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 Microwave Background radiation of 4075 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7221 is about 190 million light-years away, in good agreement with redshift-independent distance estimates of about 165 to 215 million light-years. Given that and its apparent size of about 2.5 by 1.7 arcmin (from the images below), the galaxy is about 135 to 140 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7222 (= GC 6026, Marth #466, 1860 RA 22 03 45, NPD 88 35) is "very faint, small." The position precesses to RA 22 10 52.6, Dec +02 06 14, on the southeastern rim 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 11995 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7222 is about 555 to 560 million light-years away, in good agreement with a single redshift-independent distance estimate of about 565 to 570 million light-years. 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 to 535 million light-years away at the time the light by which we see it was emitted, about 540 to 545 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 1.0 arcmin (from the images below), the galaxy is about 160 to 165 thousand light-years across. As noted in the following entry, the galaxy about 4 1/2 arcmin to its east, PGC 68229, is a probable physical companion.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 11900 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 68229 is about 555 million light-years away (and since it has nearly the same recessional velocity as NGC 7222, is probably a physical companion of that galaxy, which might help explain the unusual structure of the two galaxies). 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), though the very small difference between these numbers and those for NGC 7222 is as likely to be due to their peculiar velocities (random motions relative to their neighbors) as to any difference in their real distance from us. Given that and its apparent size of about 0.6 by 0.5 arcmin for the main galaxy, and about 1.4 by 1.1 arcmin for its asymmetrical outer ring (from the images below), the main galaxy is about 90 to 95 thousand light-years across, and its outer ring spans about 215 thousand light-years.
Note: The magnitude 17.5 spiral galaxy (J2211064+020534) to the southwest of PGC 68229 is about 110 million light-years further from us, and is therefore not a companion of either PGC 68229 or NGC 7222.
Classification Note: There is a "faint outer ring" (or as Corwin prefers, a "faint outer envelope") shown in the SDSS image below, but how it is related to the central galaxy is unclear. In the PanSTARRS image it looks like it might be an extension of the southern arm of the central galaxy that wraps around the southeast and east, then almost all the way around the galaxy. Whether that should be indicated with an (R) or (R') or something completely different depends on one's confidence about what kind of structure it is, and what the most appropriate classification is will certainly require better images. Given the lack of such images, I chose to simply add "pec?" to Corwin's suggestion for the type shown in the description line.

Note About Lack Of Companionship: As stated in the entry for PGC 68229, this object looks like an apparent companion of that galaxy, which is almost certainly a physical companion of NGC 7222. However, as stated there and shown in the next paragraph, it is about 110 million light-years further from us, and is therefore only a background galaxy, and not a companion of either NGC 7222 or PGC 68229.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 14545 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that [DD2013] W4-1+1 71254 is about 675 to 680 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 640 million light-years away at the time the light by which we see it was emitted, about 655 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 0.4 by 0.25 arcmin (from the images below), the galaxy is about 75 thousand light-years across.
Additional Notes: The visual magnitude is an estimate (hence the question mark) based on the "g" magnitude shown in SIMBAD. The type shown in the description line is courtesy of Harold Corwin, but as shown by the question mark and colon, is also somewhat uncertain. Finally, although I have listed both designations shown in SIMBAD, neither LEDA nor NED returns a result for a search for either designation; so what you see here appears to be all that there is see about this object anywhere. But since this is only a background galaxy not related to anything else in the catalog, perhaps that's more notice than it deserves in the first place.

Historical Identification: Per Dreyer, NGC 7223 (= GC 4764 = JH 2151 = WH III 862, 1860 RA 22 04 16, NPD 49 40.8) is "extremely faint, pretty small, a little extended, mottled but not resolved, among 3 stars." The position precesses to RA 22 10 10.4, Dec +41 00 25, less than 0.7 arcmin south-southeast of the center of the galaxy listed above and on its southeastern rim, 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 4385 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7223 is about 205 million light-years away. Given that and its apparent size of about 1.7 by 1.6 arcmin for the brightest part of the galaxy and its multiple arms, and about 2.45 by 1.5 arcmin including its fainter southwestern extension (both sizes from the images below), the brighter regions are about 100 thousand light-years across, and the entire structure spans about 145 thousand light-years. As noted in the following entry, NGC 7223 is almost certainly interacting with the galaxy to its northwest (PGC 214803).

Historical Identification: As noted above, R. J. Mitchell observed, wrote about and made a sketch of this object, and of the bright arm just to the south of it (which he also thought was a companion of the larger galaxy); but Dreyer presumed that both of Mitchell's supposed companions of NGC 7223 were just part of that galaxy (which is almost certainly true for the southern one), so the real companion didn't make it into the NGC even though it was discovered more than 30 years earlier. (This and many other early discoveries that did not make it into the NGC can be found in Harold Corwin's "notngc" file.)
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4390 km/sec, PGC 214803 is almost certainly a physical companion of NGC 7223 (and given its unusual nucleus and the NGC object's peculiar structure, they are probably an interacting pair), so it is almost certainly at the same distance as its larger neighbor (namely, about 205 million miles from us). Given that and its apparent size of about 0.8 by 0.15 arcmin (from the image below), PGC 214803 is about 45 to 50 thousand light-years across.
Classification Note: Although this galaxy looks almost like a typical lenticular galaxy (whence "S0"), its nucleus is distended and tilted toward its larger neighbor, hence my addition of "B", "?", and "pec" to its otherwise unlisted classification.
Visual Magnitude Note: There appears to be no measurement of the brightness of this galaxy at any visible wavelength; as a result, the visual magnitude shown in the description line is based on its K-band magnitude, and a table of approximate average differences between V and K magnitudes for various types of galaxies provided by private communication from Corwin.

Historical Identification: Per Dreyer, NGC 7224 (= GC 6027, Marth #467, Stephan list II (#29), 1860 RA 22 05 07, NPD 64 49.5) is "faint, small, round." The position precesses to RA 22 11 35.5, Dec +25 51 50, within the southern outline of the nucleus 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: Based on a recessional velocity relative to the Cosmic Background Radiation of 11860 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7224 is about 550 to 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 525 to 530 million light-years away at the time the light by which we see it was emitted, about 535 to 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 of about 1.8 by 1.0 arcmin (from the images below), the galaxy is about 275 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7225 (= GC 4765 = JH 3929, 1860 RA 22 05 15, NPD 116 50.6) is "pretty faint, small, a little extended, brighter middle." The position precesses to RA 22 13 08.7, Dec -26 09 11, well within the southeastern outline 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 Microwave Background radiation of 4555 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7225 is about 210 to 215 million light-years away. Given that and its apparent size of about 1.9 by 1.0 arcmin (from the images below), the galaxy is about 115 to 120 thousand light-years across.
Classification Note: The type shown in the description line is a composite of LEDA and NED types, based on the appearance of the images below. The prominent dust lanes and slightly distorted shape of the galaxy are suggestive of a spiral galaxy, but there is no evidence of actual arms, and both references classify this as a lenticular galaxy, albeit with different details, all of which are partially but not completely supported by the images (hence the multiple question marks).

Historical Identification: Per Dreyer, NGC 7226 (Holden (#22), 1860 RA 22 05 28, NPD 35 17) is "pretty bright, large, in cluster." The position precesses to RA 22 10 32.6, Dec +55 24 18, near the eastern outline of the cluster listed above, and given the more detailed description below of what the cluster looks like, the identification is considered certain.
Discovery Note: Gottlieb quotes Holden's original description as a "pretty bright nebula connected with a small cluster of stars which radiate in two streams from the following (eastern) to preceding (western) side. Diam(eter) of Neb(ula) 5 arcmin, of Cl(uster) 15 arcmin. North-preceding (northwest) in p(osition angle) 315° is a small knot which may be nebulous." Gottlieb then notes that, as stated above, Holden's position is just off the eastern side of this small cluster. However, his visual examination of the cluster suggests that the actual cluster is only about 2 to 2.5 arcmin in diameter, and stars much beyond that region are probably just randomly scattered foreground and background stars. This appears to be confirmed by a list of open clusters which states that there are only about 25 stars in the cluster, which is about the same as the number seen by Gottlieb in his observations.
Note About PGC Designation: As usual for NGC objects, a search for NGC 7226 returns a page in HyperLEDA (which states that it is an open cluster) and assigns a PGC designation to that page; but also as usual, a search of the database for that designation returns no result, so it is shown in quotes.
Physical Information: The cluster is thought to be about 8500 light-years away, and if so, a 2 to 2.5 arcmin wide apparent size would correspond to about 5 to 8 light-years.

Historical Identification: Per Dreyer, NGC 7227 (= GC 6028, Stephan list IV (#8), 1860 RA 22 05 31, NPD 51 58.1) is "very faint, very small, round, a little brighter middle, north-preceding (northwestern) of 2," the other being NGC 7228. The position precesses to RA 22 11 32.0, Dec +38 43 15, well within the eastern outline of the galaxy listed above, the description fits and the only other galaxy of note in the region is Stephan's IV#9 (= NGC 7228), 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 6230 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7227 is about 290 million light-years away, in essentially perfect agreement with redshift-independent distance estimates of about 280 to 290 million light-years. (Since it has nearly the same recessional velocity as NGC 7228, the two galaxies are probably a pair. Based on that assumption, the recessional velocity shown above is the average of their individual velocities (6215 km/sec for NGC 7227, and 6245 km/sec for NGC 7228), although the redshift-independent distance measurements only apply to NGC 7228.) Given the estimated distance and its apparent size of about 1.1 by 0.55 arcmin (from the images below), NGC 7227 is about 90 to 95 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7228 (= GC 6029, Stephan list IV (#9), 1860 RA 22 05 48, NPD 51 59.5) is "faint, very small, round, a little brighter middle, south-following (southeastern) of 2," the other being NGC 7227. The position precesses to RA 22 11 49.3, Dec +38 41 52, well within the southeastern outline of the galaxy listed above, the description fits and the only other galaxy of note in the region is Stephan's IV#8 (NGC 7227), 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: As discussed in the entry for NGC 7227, which is almost certainly a physical pair with NGC 7228, the galaxy is about 290 million light-years away. Given that and its apparent size of about 1.9 by 1.2 arcmin (from the images below), the galaxy is about 160 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 14925 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214807 is about 695 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 655 million light-years away at the time the light by which we see it was emitted, about 670 to 675 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 0.15 arcmin (from the images below), the galaxy is about 95 thousand light-years across.
Additional Note: No visible-wavelength magnitudes are available for this object, so the magnitude shown in the description line is an educated guess based on typical differences between V and K magnitudes, and the question mark is fully justified.

Historical Identification: Per Dreyer, NGC 7229 (= GC 4766 = JH 3930, 1860 RA 22 06 05, NPD 120 04.1) is "faint, pretty large, round, very gradually a little brighter middle." The position precesses to RA 22 14 04.6, Dec -29 22 36, on the northeastern rim 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 Microwave Background radiation of 3995 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7229 is about 185 million light-years away. Given that and its apparent size of about 1.35 by 1.25 arcmin (from the images below), the galaxy is about 70 to 75 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7230 (= GC 4767 = JH 2152 = WH III 931, 1860 RA 22 06 37, NPD 107 45.7) is "very faint, small, round, brighter middle." The position precesses to RA 22 14 14.3, Dec -17 04 10, on the northeastern rim 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 Microwave Background radiation of 4065 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7230 is about 190 million light-years away. Given that and its apparent size of about 0.9 by 0.85 arcmin (from the images below), the galaxy is about 50 to 55 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7231 (= GC 4768 = JH 2153 = WH II 606, 1860 RA 22 06 43, NPD 45 20.9) is "extremely faint, small, extremely mottled but not resolved." The position precesses to RA 22 12 26.6, Dec +45 20 33, just over one arcmin 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 Microwave Background radiation of 795 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7231 is about 35 to 40 million light-years away, a little closer than redshift-independent distance estimates of about 45 to 50 million light-years. For galaxies at very large distances, the recessional velocity is primarily affected by the expansion of the space between us and the galaxy and can be a better indication of distance than anything else; but for galaxies only a few tens of millions of light-years away, peculiar velocities (random motions relative to neighboring galaxies) can substantially affect the recessional velocity, so the best way of determining the distance of NGC 7231 is probably to choose a value between the two ranges shown above, or about 40 to 45 million light-years. Given that and its apparent size of about 1.85 by 0.65 arcmin (from the images below), the galaxy is probably about 20 to 25 thousand light-years across.
Classification Note: Since the galaxy is nearly edge-on (as indicated by "sp" in the type), it is hard to tell what it would look like when seen face-on, which is the angle at which galaxies' types are most easily determined; so the question mark in the classification is undoubtedly appropriate.

Historical Identification: Per Dreyer, NGC 7232 (= GC 4769 = JH 3931, 1860 RA 22 06 57, NPD 136 32.5) is "pretty bright, small, pretty much extended, pretty suddenly brighter middle, preceding (western) of 2," the other being NGC 7233. The position precesses to RA 22 15 36.4, Dec -45 50 53, within the western portion of the bar of the galaxy listed above, the description fits and the only other galaxy of note in the region is Herschel's "following of 2," observed on the same night (namely, NGC 7233), so the identification is certain.
Physical Information: The recessional velocities of NGC 7232 and 7233 are so close that they are generally assumed to be a physical pair, and some references (e.g., the NOIRLab press release which provided the high-resolution image below) also treat PGC 68433, whose recessional velocity is close enough to those for the NGC objects that any difference in its recessional velocity could be explained by its peculiar velocity (random motion relative to its neighbors), as part of a triplet with the NGC objects. So there are two ways to use the galaxies' recessional velocities to estimate their distance: (1) treat the NGC objects as a pair, and ignore the PGC object, or (2) treat all three as members of a triplet.
If The NGC Objects Are A Pair: NGC 7232 has a recessional velocity relative to the Cosmic Microwave Background radiation of 1700 km/sec, and a single redshift-independent distance estimate of about 70 to 75 million light-years. NGC 7233 has a corresponding recessional velocity of 1625 km/sec, and a single redshift-independent distance estimate of about 75 million light-years. Based on their average recessional velocity of about 1662 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7232 and 7233 are about (77.5) 75 to 80 million light-years away, in good agreement with the two redshift-independent distance estimates.
If All Three Galaxies Are A Triplet: PGC 68433 has a recessional velocity to the Cosmic Microwave Background radiation of 1945 km/sec. Taking the average of its recessional velocity and those of the NGC objects yields a value of 1755 km/sec for the supposed triplet, which (using the same method as in the previous paragraph) corresponds to a distance of about 80 to 85 million light-years, which is the same as PGC 68433's single redshift-independent distance estimate, and not much further than the distances obtained for the pair. In other words, although it is perhaps a little more likely that PGC 68433 is not part of a triplet with NGC 7232 and 7233, it is almost as likely that it is part of a triplet, which undoubtedly explains why some references treat the NGC objects as a pair, and others as part of a triplet.
Summary Of Results For NGC 7232: NGC 7232 has an apparent size of about 2.15 by 0.6 arcmin (from the images below). If it is part of a pair about 70 to 75 million light-years away, that corresponds to a physical size of about 45 thousand light-years; but if it is part of a triplet about 80 to 85 million light-years away, it has a physical size of about 50 thousand light-years. Since the actual situation is uncertain, it is probably best to say that it is about 45 to 50 thousand light-years across.
Classification Note: NGC 7232 is seen almost exactly edge-on (hence "sp" for "spindle" in its classification), so determining its type is difficult. The NED classification of SB(rs)a? seems too detailed for even the NOIRLab image to justify, so I have used the tentative classification shown above (per a private communication by Corwin).

Warning About Non-Standard Designations: There are no standards for the use of letters added to NGC/IC designations, and as a result, assigning the same letter to two or more galaxies is all too common, which risks (and has definitely caused at least some) errors in assigning data that belong to one galaxy to a completely different one. For that reason, such designations should always be avoided, and they are only used here to provide that warning.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2190 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68329 is about 100 to 105 million light-years away. Given that and its apparent size of about 2.1 by 0.3 arcmin (from the images below), the galaxy is about 60 to 65 thousand light-years across.
Classification Note: As an edge-on galaxy (indicated by "sp" for "spindle"), the classification of PGC 68329 is more difficult than usual. NED lists "SB(rs)ab edge-on" as the type, but the details in that classification exceed what can be determined from the available images, and other classifications shown on a linked page include "S0/a", "S", and "foreshortened bar", so I have adopted a bare-bones type that is more in keeping with the quality of the images shown below.
Final Note: NED lists this as part of a pair without specifying its apparent companion, but presumably means with IC 5181 (which NED also lists as part of a pair, in the same vague way), which lies to its southwest. However, there is a substantial difference in their recessional velocities, so I doubt that they are actual companions.

Warning About Non-Standard Designations: There are no standards for the use of letters added to NGC/IC designations, and as a result, assigning the same letter to two or more galaxies is all too common, which risks (and has definitely caused at least some) errors in assigning data that belong to one galaxy to a completely different one. For that reason, such designations should always be avoided, and they are only used here to provide that warning.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 1945 km/sec (and H₀ = 70 km/sec/Mpc), PGC 68443 is about 90 million light-years away, in reasonable agreement with a single redshift-independent distance estimates of about 80 to 85 million light-years. Given the assumption that the Hubble Flow distance of 90 million light-years is correct and its apparent size of about 1.55 by 1.4 arcmin (from the images below), PGC 68443 is about 40 thousand light-years across.
 However, many references treat PGC 68443 as part of a triplet with NGC 7232 and 7233, and as discussed in the entry for NGC 7232, if it is part of such a triplet, then it is about 80 to 85 million light-years away (the same as its redshift-independent distance estimate), and its apparent size corresponds to about 35 to 40 thousand light-years, which (given how close that is to the Hubble Flow size) is probably the best estimate that can be given for its physical size regardless of its actual distance.
Classification Note: Various references list this as SBm, SB(s)m, and as an (R'₂)SB(s)dm LINER (the latter appellation meaning that it has strong emission lines presumably radiated by interstellar gases heated by clusters of hot, young, bright stars). The SB is obvious, the spiral arms extending from its bar certainly justify the (s), and for such a disorganized galaxy hardly anyone would quibble over whether dm or m is preferable. But whether the partial outer ring implied by the third classification is reasonable depends on the person doing the classification and the quality of the images they use. A tentative classification by Corwin agrees with my statement, so hopefully the type shown in the description line is appropriate.

Historical Identification: Per Dreyer, NGC 7233 (= GC 4770 = JH 3932, 1860 RA 22 07 08, NPD 136 32.3) is "faint, very small, round, 8th magnitude star following (to east), following (eastern) of 2," the other being NGC 7232. The position precesses to RA 22 15 47.3, Dec -45 50 40, within the northwestern outline of the galaxy listed above, the description is a perfect fit and the only other galaxy of note in the immediate vicinity is Herschel's "preceding of 2", observed on the same night (namely, NGC 7232), so the identification is certain.
Physical Information: See NGC 7232 for a discussion of the calculations that suggest that if only NGC 7232 and 7233 are a physical pair, they are about 75 to 80 million light-years away, but if they are part of a triplet with PGC 68433, the that triplet is about 80 to 85 million light years away. Given that and NGC 7233's apparent size of about 1.45 by 1.0 arcmin (from the image below), the galaxy is about 30 thousand light-years across if it is part of a pair, and about 35 thousand light-years across if it is part of a triplet. Since the actual situation is uncertain, it is probably best to say that it is about 30 to 35 thousand light-years across.
A Mysterious "Companion": The NOIRLab press release (which treats this as a triplet) says that there may be a "dark galaxy" (or more accurately, about 400 million solar masses of gas torn out of NGC 7233 due to its interaction with one of its companions) just to the north of (above) the foreground star to the east (left) of NGC 7233 in the wide-field NOIRLab image (for which see NGC 7232), but adds that if there are any stars in it, they are too few in number to be detected by their instruments.
Classification Note: Most published classifications are based on the DSS image shown below, and vary from SB0/a and SAB(s)0/a to SAB(r)a. The type shown in the description line is a "first-glance" look by Corwin, and given the unusual distribution of dust lanes wrapped around the central bar, "pec" is not only fully justified, but might represent some kind of complex polar ring structure. In addition, the lack of regions of rapid star formation in the amorphous arms half-surrounding the galaxy greatly contrasts with the far brighter central bar, and the "dark galaxy" discussed in the NOIRLab press release adds to the mystery.

Historical Identification: Per Dreyer, NGC 7234 (= GC 4771 = WH VIII 63, 1860 RA 22 07 08, NPD 33 42.9) is "a cluster, small, poor, a little compressed." The position precesses to RA 22 12 06.7, Dec +56 58 33, but there is nothing there, or at least nothing obvious. Various suggestions have been made over the years, assigning one or more small groups of stars (corresponding to "small, poor") to this NGC entry, but most modern catalogs listed it as lost or nonexistent. As it happens the problem with Herschel's observation was solved by Arthur von Auwers in an 1862 publication of observations and corrections for objects in Herschel's catalogs. On page 197 of that work he lists a corrected position for (WH) VIII 63 of (1830) RA 22 06 21, Dec +56 26, which precesses to RA 22 12 22.0, Dec +57 16 18, right on the cluster recorded by John Herschel as JH 2154. Unfortunately, although Auwers' publication specifically noted the equivalence of the two observations, the younger Herschel failed to notice Auwers' correction when compiling his General Catalog, as did Dreyer when compiling his New General Catalog. So even though Auwers discovered the equivalence of what became NGC 7234 and NGC 7235 two years before the publication of the GC and 26 years before the publication of the NGC, what the elder Herschel observed remained essentially unknown for well over a century.
Discovery Notes: As noted above John Herschel did not notice Auwers' correction when he compiled the GC, nor did Dreyer when he compiled the NGC; and though Dreyer's 1912 study of Herschel's papers revealed an error in the reduction of Herschel's position by his sister Caroline, Dreyer failed to realize that this meant that NGC 7234 = NGC 7235, and did not include "7234 = 7235" in his 1912 list of corrections to the NGC. As a result, for many years NGC 7234 was thought to be a completely different cluster, and was listed as such by Steinicke as recently as 2013; and since I used Steinicke's database when I entered the basic information for this page in 2012, NGC 7234 was also misidentified here until I received a private communication in early 2015. If I'd gotten back to this entry sooner I might have noticed that Corwin's 2004 update of his database included a reference to Auwers' paper and the resulting equality of the two NGC entries, but as those following my work on this catalog are aware, it is a long-term project, so other than entries that already include complete historical identifications there may be similar mistakes yet to be unearthed.
Note About PGC Designation: As usual for NGC objects, LEDA has a page for NGC 7234, with a PGC designation, which states that it is an open cluster; but a search of the database for the PGC designation returns no result, so it is shown in quotes.
Physical Information: Given the centuries-long ignorance of the erroneous NGC position for NGC 7234, see NGC 7235 for anything else.

Above, a 45 arcmin wide DSS image centered on Herschel's incorrect published position for his VIII 63, also showing the position of the cluster therefore long thought to be NGC 7234, the correct position for Herschel's VIII 63, and John Herschel's JH 2154 = NGC 7235

Historical Identification: As noted in the entry above, until recently many catalogs incorrectly listed this grouping as NGC 7234 (though as many or more catalogs simply listed that NGC object as lost or nonexistent).
Physical Information: Apparent size 3.5? arcmin.

Historical Identification: Per Dreyer, NGC 7235 (= GC 4772 = JH 2154, 1860 RA 22 07 35, NPD 33 25.2) is "a cluster, pretty compressed, has a ruby 10th magnitude star." The position precesses to RA 22 12 32.7, Dec +57 16 17, well within the bright cluster listed above and just south of JH's "ruby" star, so the identification is certain.
Discovery Notes: See NGC 7234 for a discussion of the duplicate listing.
Note About PGC Designation: As usual for NGC objects, LEDA has a page for NGC 7234 (which it equates with NGC 7235), with a PGC designation, which states that it is an open cluster; but a search of the database for the PGC designation returns no result, so it is shown in quotes.
Physical Information: NGC 7235 is thought to be between 9000 and 9500 light-years away, with roughly 30 stars scattered over a region about roughly 4 by 3 arcmin wide region (per Gottlieb, extended east-west). This implies a physical size of about 10 light-years. However, some references include the reddish star to the east of the main body of the cluster, in which case the cluster would be about 6 by 3 arcmin, and about 15 light-years across.

Historical Identification: Per Dreyer, NGC 7236 (= GC 6030, Marth #468, 1860 RA 22 07 56, NPD 76 52) is "very faint, small, stellar." The position precesses to RA 22 14 45.8, Dec +13 49 37, about 1.2 arcmin south-southeast of the galaxy listed above and 0.9 arcmin south-southwest of the galaxy to its southeast; but since the southeastern galaxy was observed by Marth on the same night and is his #469 (= NGC 7237), there is no doubt that (as it should be, given the NGC's being in order of right ascension) the western of the two galaxies is NGC 7236.
Designation Note: Although the NGC, PGC and MCG designations are different for NGC 7236 and 7237, the CGCG and UGC designations apply to the pair (in fact, the UGC designation even includes PGC 200377), not the individual galaxies (that's why they are followed by a colon, which indicates that the individual galaxies are only part of those designations), and CGCG fails to mention either NGC object. Also, because of the confusion in the UGC and CGCG designations, the original PGC mixed up the designations, so some references may state that NGC 7236 is PGC 68383, and NGC 7237 is PGC 68384; however, HypedLEDA fixed those errors, and the designations shown on this page are the correct ones.
Physical Information: NGC 7236 is undoubtedly interacting with NGC 7237, and must therefore be at the same distance. For that reason, the best estimate of their distance is one based on the average of both galaxies' data. For NGC 7236 the recessional velocity relative to the Cosmic Background Radiation is 7495 km/sec, while for NGC 7237 the corresponding value is a nearly identical 7500 km/sec, either of which corresponds (using H₀ = 70 km/sec/Mpc for all calculations) to a distance of about 350 million light-years, in reasonable agreement with redshift-independent distance estimates of 205 to 440 million light-years for NGC 7236 and 250 to 520 million light-years for NGC 7237. 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 335 to 340 million light-years away at the time the light by which we see them was emitted, about 340 to 345 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 the apparent size of about 0.55 by 0.4 arcmin for the central galaxy and about 1.45 by 0.9 for its extended envelope (from the images below), NGC 7236 is about 55 thousand light-years across, and its outer regions span about 140 to 145 thousand light-years.
Additional Note: A third galaxy in line with the pair, PGC 200377 (listed in NED as LEDA 200377), is often listed as part of a triplet with them (as shown below and in the title for this entry, there is no mention of a triplet in the Arp Atlas), but that galaxy is probably not physically connected with its apparent neighbors, as its recessional velocity is 700 km/sec smaller than theirs, which would either require it to have an exceptionally large peculiar velocity (a random motion relative to its neighbors), or to be more than 20 million light-years closer to us (which seems more likely). And in the unlikely event that it is currently near the NGC objects, its large relative speed means that it will not remain near them for long.
Use By The Arp Atlas: NGC 7236 and 7237 are used by the Arp Atlas of Peculiar Galaxies as an example of galaxies with diffuse counter-tails, with the note "Faint diffuse plumes coming away from two galaxies. 3C442."

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7655 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214811 is about 355 to 360 million light-years away, much further away than a single redshift-independent distance estimate of about 115 to 120 million light-years.
 For such large recessional velocities, the Hubble Flow distance is probably a better indicator of their true distance than such a surprisingly low redshift-independent distance estimate, and if so, there is a possibility that PGC 214811 is a member of the same group of galaxies that includes NGC 7236 and NGC 7237. There is, of course, also the possibility that the recessional velocity is incorrect, but of the five values shown in the NED, four agree with the number shown above (the fifth is much higher, and probably represents a value for a different galaxy, mistakenly assigned to PGC 214811; it is the possibility of such errors that led to this discussion). Based on that agreement, it seems more likely that the redshift-independent distance estimate is the one that is wrong, and the rest of this paragraph therefore relies on the Hubble Flow distance. However, even making that assumption, 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 345 million light-years away at the time the light by which we see it was emitted, about 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 0.45 by 0.35 arcmin (from the images below), the galaxy is about 45 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7920 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 1442938 is about 365 to 370 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 to 360 million light-years away at the time the light by which we see it was emitted, about 360 to 365 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 0.25 by 0.15 arcmin (from the images below), the galaxy is about 25 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7237 (= GC 6031, Marth #469, 1860 RA 22 07 58, NPD 76 52) is "very faint, small, stellar." The position precesses to RA 22 14 47.8, Dec +13 49 37, about 0.9 arcmin south-southeast of the galaxy listed above, which as noted in the entry for NGC 7236, also observed by Marth on the same night, should be (since the NGC is supposed to be in order of right ascension and the galaxy above is the eastern member of a close pair) and certainly must be NGC 7237.
Designation Note: Although the NGC, PGC and MCG designations are different for NGC 7236 and 7237, the CGCG and UGC designations apply to the pair (in fact, the UGC designation even includes PGC 200377), not the individual galaxies (that's why they are followed by a colon, which indicates that the individual galaxies are only part of those designations), and CGCG fails to mention either NGC object. Also, because of the confusion in the UGC and CGCG catalog designations, the original PGC mixed up the designations, so some references may state that NGC 7236 is PGC 68383, and NGC 7237 is PGC 68384; however, HypedLEDA fixed those errors, and the designations shown on this page are the correct ones.
Physical Information: As discussed in the entry for NGC 7236 (which see for the gory details), since it and NGC 7237 are obviously interacting, they must have the same distance from us, or about 335 to 340 million light-years. Given that and its apparent size of about 0.4 by 0.35 arcmin for the main galaxy and 1.75 by 1.3 arcmin for its extended stellar plumes (from the images below), the galaxy is about 40 thousand light-years across, and its outer regions span about 170 to 175 thousand light-years. NGC 7237 is listed as having a radio jet, but of course that is not visible in optical images.
Use By The Arp Atlas: NGC 7236 and 7237 are used by the Arp Atlas of Peculiar Galaxies as an example of galaxies with diffuse counter-tails, with the note "Faint diffuse plumes coming away from two galaxies. 3C442."

Designation Note: UGC 11958 includes NGC 7236, NGC 7237 and PGC 20037; the colon after the designation indicates that it applies to more than just the galaxy in question.
Warning About Non-Standard Designations: There are no standards for the use of letters added to NGC/IC designations, and as a result, assigning the same letter to two or more galaxies is all too common, which risks (and has definitely caused at least some) errors in assigning data that belong to one galaxy to a completely different one. For that reason, such designations should always be avoided, and they are only used here to provide that warning.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6800 km/sec (and H₀ = 70 km/sec/Mpc), PGC 200377 is about 315 million light-years away. Given that and its apparent size of about 0.35 by 0.2 arcmin (from the images below), the galaxy is about 30 to 35 thousand light-years across.
Additional Note: PGC 200377 is often listed as part of a triplet with NGC 7236 and 7237, but is probably not physically connected with its apparent neighbors, as its recessional velocity is 700 km/sec smaller than theirs, which would either require it to have an exceptionally large peculiar velocity (a random motion relative to its neighbors), or to be more than 20 million light-years closer to us (which seems more likely). And in the unlikely event that it is currently near the NGC objects, its large relative speed means that it will not remain near them for long.

Historical Identification: Per Dreyer, NGC 7238 (Swift list IV (#82), 1860 RA 22 08 45, NPD 68 10.5) is "pretty faint, small, round, much brighter middle, 4 stars preceding (to west)." The position precesses to RA 22 15 20.7, Dec +22 31 11, but there is nothing there nor near there, let alone something that matches the description. (Swift's original paper gives a position of (1885) RA 22 09 55, Dec +21 56 53, which precesses to RA 22 15 20.1, Dec +22 31 10 [whence the position shown above].) Corwin states that he searched POSS1 plates for as much as an hour of right ascension east-west and 20 degrees of declination north-south without finding anything that matched Swift's description. I suppose that if four stars could be found that match Swift's original text ("4 stars in form of a square near preceding (to the west)"), then perhaps it might be possible to tell where he was looking, and try to find out whether any known comet happened to be in that region on the night in question; but barring that very remote possibility, NGC 7238 is well and truly lost, and certainly not any object permanently fixed in the sky.
Note About PGC Designation: As usual, HyperLEDA includes a page about NGC 7238, even though it lists it as "unknown", and as for all such pages, it assigns a PGC designation to the object; but also as usual in such cases, a search of the database for that designation returns no result, so it is shown in quotes.

Historical Identification: Per Dreyer, NGC 7239 (= GC 6032, Marth #470, 1860 RA 22 08 46, NPD 95 44) is "extremely faint, very small." The position precesses to RA 22 16 04.3, Dec -05 02 17, but there is nothing there; however, there is an object that fits Marth's description almost exactly a minute of time to the west, and since several of his observations have a single-digit error of a minute of time, it seems likely that the galaxy listed above is what Marth observed. As a check of that (generally accepted) possibility I precessed (1860) RA 22 07 46, NPD 95 44, obtaining RA 22 15 04.3, Dec -05 02 23, which falls only about an arcmin northwest of the galaxy listed above, and if that had been the result of precessing the original position the identification would be considered certain, which is undoubtedly why there is essentially universal agreement that PGC 68388 is indeed NGC 7239.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7450 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7239 is about 345 to 350 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 335 to 340 million light-years away at the time the light by which we see it was emitted, about 340 to 345 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 0.65 arcmin (from the images below), the galaxy is about 85 to 90 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7240 (= GC 6033, Stephan list V (#6), 1860 RA 22 09 16, NPD 53 25.1) is "extremely faint, extremely small, star attached on north, preceding (western) of 2," the other being NGC 7242. The second IC notes "Barnard, A.N. 4136, gives a sketch of six nebulae, three of which must be 7240, 7242, and Bigourdan 449, but it is difficult to identify these." The position precesses to RA 22 15 22.6, Dec +37 16 36, only about 0.2 arcmin south of the center of the galaxy listed above and within its outline despite its small size, the description fits and other than NGC 7242, which is far too large to fit the description, there is nothing else close enough to question the identity. However, as noted below, NGC 7240 has been misidentified as the galaxy listed as IC 1441, so I have placed a warning about that in the title for this entry.
Discovery Note: Gottlieb states that it is not clear whether Stephan discovered NGC 7240 on Sep 24 or Sep 16 of 1873; but since Sep 24 is the traditionally accepted date, I have used that in the discovery credits, and just added this note about the uncertainty.
Designation Errors: Gottlieb also states that MCG failed to label this galaxy as NGC 7240, and RNGcS and Dorothy Carlson incorrectly equated it with IC 1441, which as shown in the wide-field image below is the galaxy an arcmin to the north-northwest of NGC 7240 (the error is mentioned in Malcolm Thomson's unpublished "Catalogue Corrections").
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5670 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7240 is about 265 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 185 to 245 million light-years. Given that and its apparent size of about 0.7 by 0.7 arcmin (from the images below), the galaxy is about 50 to 55 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7241 (= GC 6034, Stephan list IV (#10), 1860 RA 22 09 24, NPD 71 27.9) is "pretty faint, a little extended, 10th magnitude star attached on south." The second IC lists a corrected RA (per Bigourdan) of 22 09 08. The original NGC position precesses to RA 22 16 05.4, Dec +19 13 51, about 16 seconds of time to the east of the galaxy listed above, but the description fits and there is nothing else nearby, so the identification is certain. (As it happens, Stephan's measurements were perfect, but he made a 16 second error in reducing them which wasn't discovered until Emmanuel Esmiol reduced Stephan's observations to the equinox of 1900 in 1916.) Bigourdan's position precesses to RA 22 15 49.4, Dec +19 13 49, just barely west of the center of the galaxy listed above and well within its western outline, making it a testament to the accuracy of his observations of NGC objects.
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 1135 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7241 is about 50 to 55 million light-years away, considerably closer than redshift-independent distance estimates of about 85 to 222 million light-years. Part of the difference between the two estimates might be due to a substantial peculiar velocity (that is, a random motion relative to its neighbors) making its recessional velocity lower than it should be, so it is possible that the galaxy is 60 to 70 million light-years away, instead of as close as its recessional velocity implies. Using the Hubble Flow distance and its apparent size of about 3.6 by 1.1 arcmin (from the images below), the galaxy would be about 55 thousand light-years across, but if it is closer to 65 million light-years away, it would be about 65 thousand light-years in diameter (in other words, it has a diameter in thousands of light-years nearly equal to its distance in millions of light-years).
Classification Note: The galaxy is nearly edge-on (hence the "sp" for "spindle"), making it harder to determine its type, but is seen in enough detail in the images below to perhaps justify the relatively detailed classification. The bluish more or less circular region nearly centered on the galaxy is presumably a gigantic starburst region created by some recent catastrophe, and fully justifies the "pec" classification (and perhaps even my exclamation point). Note that the closeup images show an even larger albeit fainter more or less circular region surrounding the more obvious one; so perhaps more than one interesting event was involved.

Historical Identification: Per Dreyer, NGC 7242 (= GC 6035, Stephan list V (#7), (Voigt 10), 1860 RA 22 09 33, NPD 53 24.1) is "very faint, small, a little brighter middle, following (eastern) of 2," the other being NGC 7240 (which see re an IC2 note). The position precesses to RA 22 15 39.8, Dec +37 17 38, well within the southern outline of the galaxy listed above, the description fits and there is nothing comparable nearby, so the identification is certain.
Discovery Notes: Voigt's discovery was one of ten nebulae he discovered between March and August of 1865; but they were only noted in his observing records and were not published until 1987 (though Gottlieb writes that Stephan might have had access to Voigt's logbook and been aware of the prior discovery), so Dreyer had no knowledge of his observation, hence his inclusion in the NGC entry only in parentheses.
Designation Note: CGCG and MCG treat NGC 7242 and IC 5195 as two components of their designations ("a" for the NGC object and "b" for the IC object, though neither catalog actually called the latter galaxy IC 5195). The colons in their designations indicate that the designation refers to more than one galaxy, and the same designations will be found in the entry for IC 5195, which see for more about this.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5475 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7242 is about 255 million light-years away, in good agreement with redshift-independent distance estimates of about 185 to 315 million light-years. Given that and an apparent size of about 2.4 by 1.7 arcmin for the main body of the galaxy and about 4.0 by 2.05 arcmin for the faint outer extensions especially visible to the northeast (both sizes from the images below), the main galaxy is about 175 to 180 thousand light-years across, and its fainter extensions span at least 300 thousand light-years, making it truly a giant.
Note About Physical Size: In doing research for this entry I have seen discussions that put NGC 7242's outer regions' size at as much as 600 thousand light-years, but the images here don't justify that, and the original references were not mentioned, so I don't know if that should be given any credence. LEDA and NED list sizes smaller than those determined from the images below, and Gottlieb lists the apparent size as 2.1 by 1.4 arcmin, so the references he used are also slightly smaller than those measured here.
Classification Notes: LEDA and NED list this galaxy as type E, E/S0?, E+ (which is the same as E/S0) and cD? (a term used to represent a giant elliptical galaxy with a diffuse structure, which is certainly a reasonable description of NGC 7242, which is why I chose that type out of the four possibilities). The images below show that it is a distorted type E or E/S0, with its main body considerably larger on the southwest than on the northeast, and with an extended field of scattered stars (particularly to the northeast), and I feel justifies adding the "pec".

Historical Identification: Per Dreyer, NGC 7243 (= GC 4773 = JH 2155 = WH VIII 75, 1860 RA 22 09 41, NPD 40 48.9) is "a cluster, large, poor, a little compressed, stars very large (bright)." The position precesses to RA 22 15 12.1, Dec +49 52 49, well within the cluster listed above, so the identification is certain.
Note About PGC Designation: As usual, a search of HyperLEDA for the NGC object returns a page stating that this is an open cluster, and a PGC Designation for the page; however, also as usual, a search of the database for that designation returns no result, so it is shown in quotes.
Physical Information: NGC 7243 is thought to be about 2650 light-years from us, and per Gottlieb, contains the best part of 200 stars irregularly scattered across a region about 21 arcmin wide, with a number of bright stars, and "is a striking cluster at low power". Given its distance and apparent size, the cluster has a diameter of about 15 light-years.

Historical Identification: Per Dreyer, NGC 7244 (= GC 6036, Stephan list IV (#11), 1860 RA 22 09 41, NPD 74 13.5) is "extremely faint, extremely small, round, brighter middle." The position precesses to RA 22 16 27.0, Dec +16 28 16, essentially dead center on the galaxy listed above, the description fits and there's nothing else nearby, so the identity 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 Background Radiation of 7205 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7244 is about 335 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 325 million light-years away at the time the light by which we see it was emitted, about 330 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 0.45 arcmin (from the images below), the galaxy is about 70 to 75 thousand light-years in diameter.

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 11810 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 1508710 is about 550 million light-years away (since this is much further away than NGC 7244, PGC 1508710 is not an actual companion of that galaxy). 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 525 million light-years away at the time the light by which we see it was emitted, about 535 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 0.45 by 0.25 arcmin (from the images below), the galaxy is about 65 to 70 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7245 (= GC 4774 = JH 2157 = WH VI 29, 1860 RA 22 10 02, NPD 36 22.0) is "a cluster, compressed, stars extremely small (faint)." The position precesses to RA 22 15 16.1, Dec +54 19 44, right on the cluster listed above and the description fits, so the identification is certain.
Note About "Nearby" Clusters: As noted by Gottlieb and Corwin there are two stellar condensations just to the northeast of NGC 7245. The more significant is King 9, described by Gottlieb as a rich but very faint cluster (its brightest stars are only magnitude 16.5), which is discussed in the following entry. The more obvious, though it may not be a cluster at all, is a group of about a dozen or so magnitude 13.5 to 14 stars superimposed on the northern half of King 9. In a DSS image only the brighter group (which is probably just a random grouping of Milky Way stars) is obvious; but in the PanSTARRS image shown below (and in the image in the entry for King 9), the multitude of faint stars comprising King 9 is also visible. It is interesting that although what the Herschels observed is the most impressive cluster in the region, there are two other stellar condensations in nearly the same direction (of course King 9 would have been far too faint for them to see even a single star in that cluster).
Note About PGC Designation: As usual, a search of HyperLEDA for the NGC object returns a page stating that this is an open cluster, and a PGC Designation for the page; however, also as usual, a search of the database for that designation returns no result, so it is shown in quotes.
Physical Information: NGC 7245 is thought to be about 6800 to 6900 light-years away. Given that and its apparent size of about 5 arcmin (per Gottlieb), the cluster has a diameter of about 10 light-years. However, a study of its Hertzsprung-Russell Diagram suggests a much larger distance of about 12000 to 12500 light-years, in which case this "sparse" cluster (as it is described in that paper) would be about 16 to 20 light-years in diameter. The same study estimates an age for NGC 7245 of about 400 million years.

Identification Note: In his observation of NGC 7245 Gottlieb notes that King 9 is close northeast of that cluster. He states that this "rich, distant cluster" of stars fainter than magnitude 16.5 is just south of a group of magnitude 13.5 to 14 stars. Those stars are far easier to see with visual observations than the fainter stars in King 9, and as a result, they are sometimes mistakenly identified as King 9.
Physical Information: SIMBAD lists a parallax of 0.000129 arcsec, which would put King 9 a little over 25 thousand light-years away. The angular size is listed in SIMBAD as 2.5 arcmin, and if that is correct, the cluster has a diameter of about 15 to 20 light years. A study of its Hertzsprung-Russell Diagram suggests that although King 9 is probably "only" about 3 billion years old (relatively old for an open cluster), its stars have a low amount of "metals" (that is, anything other than hydrogen and helium) compared to stars like the Sun, which is backwards from what we would expect (younger stars usually have more "metals" than older ones, and the Sun is about 4.5 billion years old). The same paper states that the cluster's giant branch is bluer than expected, and suggests that there may be a "significant fraction of binary population including some blue stragglers." (Note: The paper quoted is the same one referred to in the entry for NGC 7245.)
Visual Magnitude Note: I have yet to find an estimate of how bright this cluster is, but since it appears to have about 100 or so stars of magnitude 16.5 or fainter, its total magnitude should be about 11.5 or fainter, whence my rough estimate of that value in the description line.

Historical Identification: Per Dreyer, NGC 7246 (= GC 4775 = JH 2156 = WH III 932, 1860 RA 22 10 09, NPD 106 15.7) is "very faint, small, very little extended, very gradually brighter middle, 13th magnitude star to north." The position precesses to RA 22 17 43.1, Dec -15 33 51, well within the northeastern outline of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain. (See IC 5198 for a discussion of the duplicate listing.)
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3795 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7246 is about 175 to 180 million light-years away, somewhat further than a single redshift-independent distance estimate of about 135 million light-years. Using the Hubble Flow distance and its apparent size of about 1.8 by 1.0 arcmin (from the images below), the galaxy is about 90 to 95 thousand light-years across, but if it is closer to 135 million light-years away, it would be about 70 thousand light-years in diameter.
Classification Note: In the PanSTARRS image there is a hint of some kind of oval well outside the main body of the galaxy, and NED lists this galaxy as (R)SA(r)a: (based on the image I have changed "a:" to "ab?" and "(r)" to "(rs)"); but there is no hint of an outer ring in DSS images, and PanSTARRS images are often full of various kinds of artifacts, so I have ignored the (R).

Historical Identification: Per Dreyer, NGC 7247 (Leavenworth list I (#248), 1860 RA 22 10 20, NPD 114 25.9) is "pretty faint, very small, round, a little brighter middle, bright double star 13 seconds of time preceding (to west)." The second IC lists a corrected RA (per Howe) of 22 09 53. The original position precesses to RA 22 18 07.5, Dec -23 44 01, about 26 seconds of time to the east of the galaxy listed above, but the description perfectly fits that object and its surroundings and there is nothing else nearby, so there is no doubt that it is what Leavenworth observed; and Howe's position precesses to RA 22 17 40.7, Dec -23 44 04, which lies within the southwestern outline of the galaxy, so the IC2 correction was essentially perfect.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2160 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7247 is about 100 million light-years away, in good agreement with redshift-independent distance estimates of about 90 to 140 million light-years. Given that and its apparent size of about 1.4 by 0.85 arcmin (from the images below), the galaxy is about 40 to 45 thousand light-years across.
Classification Note: NED and LEDA list this as a barred spiral, but at first glance the images below don't look a barred spiral at all; however, it could be said that the region between the southern end of the large arm on the east and the smaller arm on the north side of the nucleus vaguely resembles a bar. For that reason I have included a "B" in the type shown above, but with the A underlined to indicate that this looks more like a normal spiral to me than a barred one.

Historical Identification: Per Dreyer, NGC 7248 (= GC 4776 = WH III 863, 1860 RA 22 11 00, NPD 50 10.2) is "very faint, very small, much brighter middle." The position precesses to RA 22 16 59.8, Dec +40 31 39, about 1.9 arcmin northeast of the galaxy listed above, 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 3985 km/sec (and H₀ = 70 km/sec/Mpc), NGC 7248 is about 185 million light-years away. Given that and its apparent size of about 1.65 by 0.85 arcmin (from the images below), the galaxy is about 90 thousand light-years across.

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 5470 km/sec (and H₀ = 70 km/sec/Mpc), PGC 214813 is about 255 million light-years away (meaning that it is not a companion of NGC 7248, but only a background galaxy). Given that and its apparent size of about 0.45 by 0.3 arcmin (from the images below), the galaxy is about 30 to 35 thousand light-years across.

Historical Identification: Per Dreyer, NGC 7429 (= GC 4777 = JH 3933, 1860 RA 22 11 26, NPD 145 48.9) is "most extremely faint, round, doubtful object." The position precesses to RA 22 20 35.5, Dec -55 06 51, only 0.9 arcmin northeast of the galaxy listed above, and if what Herschel observed was "extremely faint" and "doubtful", it's "extremely" unlikely that he would have noticed one of the even fainter galaxies and not noticed the brightest one in the field; so the identification is considered certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 11775 km/sec (and H₀ = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7249 is about 545 to 550 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 520 to 525 million light-years away at the time the light by which we see it was emitted, about 530 to 535 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 0.5 arcmin (from the images below), the galaxy is about 115 thousand light-years across.
 Many of the galaxies in the vicinity of NGC 7249 are thought to be part of a rich cluster, of which NGC 7249 is the brightest member; but the only one listed as an apparent companion (in the following entry) has no measurement that indicates its distance, so whether it is also a member of that cluster or merely happens to be in the same direction cannot be known at this time.

Designation Note: NED does not recognize the PGC/HyperLEDA designation (even if expressed as LEDA 95401), so a search of that database requires the 2MASX designation shown above.
Physical Information: Based on the images below, PGC 95401 has an apparent size of about 0.35 by 0.1 arcmin; but there appears to be absolutely no information about its distance anywhere, so neither its actual size, nor whether it is a companion of NGC 7249 or merely a foreground or background object can be known at this time.
Classification Note: Both LEDA and NED list this as an S0/a; but its color seems far too blue for a lenticular galaxy, so it is probably an edge-on ("sp" = "spindle") spiral, most likely of type Sb or a little later. However, the image quality is too poor to be sure, hence the question mark.