NGC Objects: NGC 7350 - 7399 (original) (raw)

QuickLinks:
7350, 7351, 7352, 7353, 7354, 7355, 7356, 7357, 7358, 7359, 7360, 7361, 7362, 7363, 7364, 7365, 7366,
7367, 7368, 7369, 7370, 7371, 7372, 7373, 7374, 7375, 7376, 7377, 7378, 7379, 7380, 7381, 7382, 7383,
7384, 7385, 7386, 7387, 7388, 7389, 7390, 7391, 7392, 7393, 7394, 7395, 7396, 7397, 7398, 7399

Page last updated Sep 12, 2024 (Working on complete update of page, completed all Carnegie-Irvine Galaxy Survey images)
NEXT: Deal with all problem entries, check discoverers/observers databases for any incomplete references
NEXT: Consider all relevant comments by Gottlieb & Corwin
NEXT: Take care of Physical Information/etc for objects without problems
WORKING (7362 companions, 7369comp, 7386-89, 7390+) If ID in the previous step was certain, assessing physical information & adding images If an entry was marked as ID PROBLEM, DATA PROBLEM, etc, putting off until done with all certain IDs
Checked all NGC entries for typos, precessed positions, checked IDs
Finished checking NGC Notes, IC1 & IC2 corrections for all entries on this page
Updated all Corwin positions, Steinicke magnitudes/positions/IDs, LEDA & NED IDs/data

PROBLEM ID
NGC 7350
Recorded (Aug "7", 1864) by Albert Marth
Probably a lost object in Pegasus "near" RA 22 41 03.8, Dec +11 57 47
Formerly thought to be NGC 7350 but now considered unlikely: a triplet of stars at RA 22 40 47.6, Dec +12 00 17
Recently suggested but almost certainly not NGC 7350: a duplicate observation of NGC 7346

NOTE TO SELF: Although Corwin now believes the triplet is not 7350, and suggests 7346 as the best guess, he uses two question marks for the position, which almost always means that the identification is more of a stab in the dark than anything else; so need to very carefully justify my conclusion that 7350 is lost or nonexistent (e.g., point out that whether or not 7350 is 7346 makes no difference in identifying and discussing 7346, so trying to justify that ID for 7350 without any really good reason is probably a waste of time and effort).

Note About Marth's Date: Marth recorded the date of his observations as the year, plus the fraction of a year rounded to two decimal places, starting with Jan 0 (which is Dec 31 of the previous year). Many observers did or still do that; but to specify the exact date, you need three decimal places. Observations recorded as 1874.60 (which applies to 24 of Marth's observations) could have been made between midnight and dawn on August 6, and dusk to midnight on August 9 (Corwin notes that the date could have been Aug 8 plus or minus a day), but tradition has made Aug 7 the listed date for all of Marth's observations dated 1874.60. In most cases, the date chosen for one of his hundreds of observations isn't a great concern; but in this case, it may be important.
Historical Identification: Per Dreyer, NGC 7350 (= GC 6077, Marth #492, 1860 RA 22 34 07, NPD 78 46) is "very faint." The position precesses to RA 22 41 03.8, Dec +11 57 47 (whence the "lost" position shown above), but there are no nebulae there except a galaxy (NGC 7348) supposedly discovered by Marth on the same night (or the night before or after), about 7.5 arcmin to the southwest. On the night or nights in question, he would have observed a part of the sky as it moved westward, so larger right ascensions would have been observed after smaller ones. Presuming that the 24 observations made on 1874.60 were made in multiple sweeps on successive nights, most of the ones further west were probably observed on one of the earlier dates, and those further east were probably observed on one of the later dates, so objects with very different right ascensions were probably observed on different nights, while objects with similar right ascensions were probably observed on the same night. This means that NGC 7346 (Marth #490), NGC 7348 (Marth #491), 7350 (Marth #492), 7353 (Marth #493), and 7366 (Marth #495) were probably observed on the same night. It is unlikely that Marth would have recorded any of these twice on the same night at a very different position (particularly at a very different declination), so NGC 7350 should not be a duplicate observation of any of the others just listed. Aside from that, although NGC 7350 was described only as "very faint", NGC 7348 was described as "very faint, pretty large, irregularly round," which is sufficiently different to make it unlikely that NGC 7350 was a duplicate observation of 7348.
WORKING HERE
Aside from this, many of Marth's faint "nebulae" that are described as small or whose size wasn't mentioned were actually faint stars or pairs of stars, so the earliest modern identification of NGC 7350 (by the RNGC) was "lost". In the first "successful" effort to identify NGC 7350, Harold Corwin suggested that it was probably the small group of stars listed above, which are about 4.6 arcmin to the northwest of the NGC position. And until now (2024), many (if not all) databases (including mine) accepted that identification as sufficiently conclusive.
LEDA: the small group of stars listed above = "PGC 5067663"; NED: the small group of stars, nothing else
(Mis)identification Notes: In a 2016 reassessment of his earlier work, Corwin noted that Marth discovered numerous objects on the night in question (or nights, since 24 of his observations were listed as being made on 1864.60, which translates to Aug 8, 1864, plus or minus a day), and listed positions within about an arcmin of the current identification for 21 of those observations. In other words, only three of Marth's observations (NGC 7350, 7353 and 7283) had poor positions. In an effort to identify those three, Corwin decided (as described in detail in the entry for NGC 7353) that 7350 and 7353 were probably NGC 7346 and 7347. However, as noted in the entry for 7353, despite "rejecting" the group of stars that he had previously thought were NGC 7350, Corwin ended up putting two question marks on his new suggestion. In general, when Corwin lists a position with a single question mark (as he formerly did for the small group of stars), that means that the identification is uncertain, and when he uses two or more question marks, he's merely grasping at straws; and as he states near the end of his 2016 reassessment, he is not truly satisfied with the "duplicate entry" solution (though he apparently intends to cling to it, since there is no other possible ID). So although his reassessment supposedly changes the identification from the small group of stars to a duplicate observation of NGC 7346, all it really does is make "lost" the most reasonable identification of NGC 7350.
Lost? or Nonexistent?: As stated in the first paragraph of this entry, the RNGC listed NGC 7350 as "nonexistent", meaning that Marth might have thought that he saw something, but there was actually nothing there. However, there are a number of stars, pairs and groups of stars in the region, many of which could have been mistaken by Marth for a nebulous object (and as also noted above, that is a mistake that he often made). So although it is possible that what he thought he saw didn't really exist, his tendency to mistake stellar objects as faint nebulae makes it far more likely that he did see something, but we won't ever know what it was. With some other observers (e.g., Guillaume Bigourdan, the possibility of an entry for a nonexistent object (or as he called it, one of his "fausse images") would be far greater, and I would have written "lost or nonexistent" at the start of this entry; but for Marth, just "lost" is more appropriate.

Above, a 15 arcmin wide SDSS image centered on the NGC position for NGC 7350
Also shown are Corwin's first identification of NGC 7350, and NGC 7346, his new (but no more likely) candidate

NGC 7351 (= PGC 69489 = MCG -01-57-022)
Discovered (Sep 19, 1873) by �douard Stephan
Also observed (Nov 18, 1884) by Lewis Swift
Also observed (July 1898 to June 1899) by Herbert Howe
A magnitude 12.9 lenticular galaxy (type SB0) in Aquarius (RA 22 41 26.9, Dec -04 26 40.6)

Historical Identification: Per Dreyer, NGC 7351 (Stephan list IX (#30), Swift list II (#92), 1860 RA 22 34 12, NPD 95 10.5) is "pretty faint, pretty small, round, brighter middle, mottled but not resolved." The second IC notes "is not round but much extended 180 degrees (Howe)". The position precesses to RA 22 41 27.8, Dec -04 26 42, less than 0.2 arcmin due east of the center of the galaxy listed above and barely outside its bright central region, the description (and Howe's correction of that) is a perfect fit and there is nothing else nearby, so the identification is certain.
Discovery Notes: Stephan's extremely precise micrometric measurement is even more accurate than the rounded-off NGC position, but Swift's position is about 5 arcmin west-northwest of the galaxy. That's reasonably close for one of Swift's measurements, and since there is nothing else in the region, his independent discovery is just as certain.
Traditionally, Stephan's discovery date for this object is given as Oct 3, 1878. However, that is the date that Stephan reduced his micrometric position, as subsequently published in his list IV. Per his logbooks, he first observed the galaxy on the date shown in the description line (this is typical of his published work; objects that he only observed once rarely ended up in the NGC/IC).
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 530 km/sec (and H0 = 70 km/sec/Mpc), NGC 7351 is about 25 million light-years away. Given that and its apparent size of about 1.6 by 0.9 arcmin (from the images below), the galaxy is about 10 to 12 thousand light-years across.

Above, a 12 arcmin wide SDSS image centered on NGC 7351
Below, a 2 arcmin wide SDSS image of the galaxy

MINOR PROBLEM ID
NGC 7352
Recorded (Sep 24, 1829) by John Herschel
Probably a group of stars in Cepheus (RA 22 39 45.8, Dec +57 23 17)

Historical Identification: Per Dreyer, NGC 7352 (= GC 4826 = JH 2177, 1860 RA 22 34 15, NPD 33 20.0) is "a cluster, very large, pretty rich, very little compressed." Herschel's original description may be of importance here. It reads "A star 9-10 magnitude, the chief of a pretty rich, very large, very coarse cluster. The position precesses to RA 22 39 43.1, Dec +57 23 44, about 0.5 arcmin northwest of magnitude 8.4 star HD 214833, so that is presumably Herschel's "chief" star in the cluster (and its position is the one I used for the cluster); but it is located in a relatively rich part of the Milky Way, and if Herschel's "pretty large" (greater than 20 arcmin wide) cluster is the scattering of stars barely brighter than the background, it is very coarse, and the general opinion seems to be that it is hard to believe that such a "cluster" would have seemed worth Herschel's mentioning. Still, though there is another possible identification (as discussed in the next paragraph), the one centered on HD 214833 must be the first choice for NGC 7352.
Discovery Notes: WORKING HERE: QUOTE GOTTLIEB, CORWIN
Physical Information: Probably a random scattering of stars. LEDA lists it as an open cluster at a position slightly southwest of the central star, and gives it the pointless (and unsearchable) designation "PGC 5067716". NED says "no cluster at this position".

Above, a 30 arcmin wide DSS image centered on HD 214833 (NGC 7352 is presumbly the inner 20 to 25 arcmin)

PROBLEM ID
NGC 7353 (= PGC 85285)
Discovered (Aug "7", 1864) by Albert Marth
A magnitude 15.1 spiral galaxy (type S??) in Pegasus (RA 22 42 12.5, Dec +11 52 38)
Recently suggested but not likely to be a duplicate observation of NGC 7347

Historical Identification: Per Dreyer, NGC 7353 (= GC 6078, Marth #493, 1860 RA 22 34 27, NPD 78 48) is "extremely faint". The position precesses to RA 22 41 23.9, Dec +11 55 48, but there is nothing there nor near there.
Note About Marth's Dates: Since Marth used a decimal date (in this case, 1864.60), any of the observations made on "that" date could have been made between midnight and dawn on Aug 6, and dusk and midnight on Aug 9; but Aug 7 is always used as the putative date of those observations.
LEDA PGC 85285; Sc, 3K Vr 11117 km/sec; NED PGC 85285, spiral, 3K Vr 6968 km/sec (right ID, but wrong Vr; that Vr belongs to SIMBAD's 7353, which is the mistaken RNGC identity. SIMBAD agrees with LEDA's Vr for PGC 85285. Need to have a note about the error(s) in the NED and SIMBAD listings.
SIMBAD (RNGC mistaken identity) UGC 12134, PGC 69429, CGCG 429-018, MCG +02-57-008, 3K Vr 7349 km/sec, V 13.5
SIMBAD PGC 85285 helio Vr 11486
Corwin had KUG 2213+116 as the ID for his now rejected galaxy, but it was really KUG 2239+116, as shown in LEDA and NED, and he has corrected that error in his notes about the galaxy.
Physical Information: Apparent size 0.6 by 0.5? arcmin.

NGC 7354 (= P-K 107+02.1 = "PGC 3517826")
Discovered (Nov 3, 1787) by William Herschel
Also observed (Oct 9, 1829) by John Herschel
Also observed (Sep 20, 1851) by Bindon Stoney
Spectroscopically observed (1865) by Sir William Huggins
Photographically observed (1918) by Heber Curtis
A magnitude 12.2 planetary nebula in Cepheus (RA 22 40 19.9, Dec +61 17 09)

Historical Identification: Per Dreyer, NGC 7354 (= GC 4827 = JH 2178 = WH II 705, 1860 RA 22 35 08, NPD 29 26.7) is "a planetary nebula, bright, small, round, pretty gradually a very little brighter middle". The position precesses to RA 22 40 20.1, Dec +61 17 05, less than 0.1 arcmin nearly due south of the center of the nebula, and well within its outline, the description fits and there is nothing comparable nearby, so the identification is certain.
Discovery Notes: Gottlieb has a detailed historical commentary. He quotes William Herschel's "pretty bright, irregularly round, easily resolvable, almost of an equal light throughout", and John Herschel's "bright enough to be noticed and caught in sweeping in full moonlight, with the moon or meridian; pretty gradually brighter middle; round, no nucleus seen." He also notes that it was the most northerly object ever observed with Lord Rosse's 72-inch telescope, that Huggins was the first to spectrocopically observe that it had a single emisssion line (typical of gases), instead of a broad spectrum (typical of stars, clusters of stars and galaxies), and that based on a photograph taken with the Crossley telescope at Lick Observatory, Curtis gave a detailed description that rivals the best modern observations.
PGC Designation Note: As usual for NGC objects, HyperLEDA assigned a PGC designation for this object, even though it isn't a galaxy; however, a search of the database for that designation returns no result, so it is shown quotes.
Physical Information: Per the HST Picture of the Week, NGC 7354 is about 4200 light-years away (Wikidata lists the distance as about 1700 parsecs, or roughly 5540 light-years), has a circular outer shell and elliptical inner shell, a collection of bright knots roughly concentrated in the middle and two symmetrical jets shooting out from either side. It is thought that the jets are caused by an interaction of the central star that ejected the nebula (a former red giant now collapsing toward white dwarf status, with a current surface temperature of about 100 thousand Kelvins [despite its high temperature it is about magnitude 16.5, partly because there are about 3.5 magnitudes of dimming by interstellar dust lying between it and us, and partly because the vast majority of its radiation is in the far ultraviolet and can't be seen by human eyes], and a still red-giant companion of that star [the existence of such a companion has not been proven, but GAIA data suggest there is one]). The outer part of the nebula and the reddish knots are expanding faster than the inner part, and the outer part is larger partly because of its higher velocity (neither velocity is very large, being measured in only tens of km/sec, whereas some planetary nebulae have ejection speeds of more than a thousand km/sec), and partly because it is older (the time since ejection is estimated at about 2500 years for the outer shell and 1600 years for the inner one if the distance is 4200 km/sec; if they are further away, the ages would be proportionately longer). The outer shell has an apparent size of about 33 by 30 arcsec, while the inner one is about 20 by 30 arcsec (all values from the images below), which would make their physical sizes about 0.65 to 0.7 light-years diameter for the outer shell and about 0.6 light-years for the inner one if it is about 4200 light-years away, or about 0.85 to 0.9 light-years in diameter for the outer shell and 0.8 light-years for the inner one if it is 5540 light-years away.

Above, a 12 arcmin wide NOAO/DSS composite image centered on NGC 7354
(Image Credit Adam Block/NOAO/AURA/NSF (used by permission), superimposed on a DSS background)
Below, a 0.75 arcmin wide NOAO image of the planetary nebula (NOAO Image Credit as above)

Below, a 0.6 arcmin wide HST image of the nebula (Image Credit ESA/Hubble & NASA)

NGC 7355 (= PGC 69587 = PGC 631654 = ESO 406-006)
Discovered (Sep 1, 1834) by John Herschel
A magnitude 14.3 spiral galaxy (type SAB(rs)b?) in Grus (RA 22 43 30.6, Dec -36 51 55)

Historical Identification: Per Dreyer, NGC 7355 (= GC 4828 = JH 3952, 1860 RA 22 35 26, NPD 128 36.5) is "most extremely faint, small, round, double star following 40 seconds of time (to east)." The position precesses to RA 22 43 27.1, Dec -37 52 35, but there is nothing there nor near there. However, Corwin noticed that the galaxy listed above, exactly 1 degree to the north of the Cape of Good Hope position (which was faithfully copied into the GC and NGC), perfectly matches Herschel's description, including the bright double star just over 40 seconds of time to the east, so it appears that there was a single-digit error in Herschel's notes, and the identification of NGC 7355 as the galaxy listed above is considered certain.
Missed Identification: The RNGC, published decades before Corwin discovered the probable error in Herschel's declination, lists NGC 7355 as nonexistent.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 11480 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7355 is about 435 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 510 million light-years away at the time the light by which we see it was emitted, about 520 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 1.22 by 0.48 arcmin (from the images below), the galaxy is about 180 to 185 thousand light-years across.
Possible Companion: Corwin lists the (lenticular?) galaxy (2MASS22432913-3651560) running more or less north-south on the western rim of NGC 7355 as a possible companion. But other than its apparent size of about 0.3 by 0.1 arcmin (from the images below), there is nothing available about it, so whether it is an actual companion or a background galaxy isn't known.

Above, a 12 arcmin wide DSS image centered on NGC 7355
Below, a 12 arcmin wide image centered between NGC 7355 and the double star that makes the identification reasonably certain

Below, a 2 arcmin wide DSS image of the galaxy is too blurry to say much about it

Below, a 1.4 arcmin wide monochrome DESI Legacy image of the galaxy gives a far better idea of its appearance
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 image by Courtney Seligman, using AladinLite)

NGC 7356 (= PGC 69530 = UGC 12159 = CGCG 495-014 = MCG +05-53-010)
Probably discovered (Aug 31, 1867) by �douard Stephan
A magnitude 14.0 spiral galaxy (type (R?)Sbc?) in Pegasus (RA 22 42 02.5, Dec +30 42 31)

Historical Identification: Per Dreyer, NGC 7356 (Stephan list XIII (#94), 1860 RA 22 35 30, NPD 60 01.4) is "extremely faint, pretty small, round, gradually a little brighter middle, star attached." The position precesses to RA 22 42 02.3, Dec +30 42 28, less than 0.1 arcmin south of the center of the galaxy listed above and on the edge of the nucleus, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Traditionally, Stephan's discovery date for this object is given as Oct 4, 1883. However, that is the date that Stephan reduced his micrometric position, as subsequently published in his list XIII. Per his logbooks, he probably first observed this galaxy and/or NGC 7357 on the date shown in the description line, but his rough position from that date is about halfway between NGC 7356 and 7357, so which of the two was observed by Stephan in 1867 isn't clear, and it is possible that the date of his micrometric position is the actual original observation. Still, although the date of his first observation isn't certain he was certainly the first to observe this galaxy.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 6950 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7356 is about 320 to 325 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 315 to 490 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 315 million light-years away at the time the light by which we see it was emitted, about 320 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 0.55 arcmin (from the images below), the galaxy is about 105 thousand light-years across.

Above, a 12 arcmin wide SDSS image centered on NGC 7356
Below, a 1.5 arcmin wide SDSS image of the galaxy

Below, a 1.5 arcmin wide PanSTARRS image of the galaxy

NGC 7357 (= PGC 69544 = UGC 12162 = CGCG 495-016 = MCG +05-53-011)
Discovered (Aug 31, 1867) by �douard Stephan
A magnitude 14.0 spiral galaxy (type (R)S(r?)bc? pec) in Pegasus (RA 22 42 23.9, Dec +30 10 17)

Historical Identification: Per Dreyer, NGC 7357 (Stephan list XIII (#95), 1860 RA 22 35 51, NPD 60 33.6) is "very faint, very small, very faint star involved." The position precesses to RA 22 42 24.3, Dec +30 10 17, less than 0.1 arcmin from the center of the galaxy listed above and within its bright core, the description is reasonable and there is nothing else nearby, so the identification is certain.
Discovery Note: Stephan's discovery date for this object is usually given as Sep 26, 1883. However, that is the date that Stephan reduced his micrometric position, as subsequently published in his list XIII. Per his logbooks, he probably first observed this galaxy and/or NGC 7356 on the date shown in the description line, but his rough position from that date is about halfway between NGC 7356 and 7357, so which of the two was observed by Stephan in 1867 isn't clear, and it is possible that the date of his micrometric position is the actual original observation. Still, although the date of his first observation isn't certain he was certainly the first to observe this galaxy.
Physical Information: NGC 7357 has an outer ring with several star-forming regions, and a smaller, brighter central region of indeterminate nature (hence the several question marks in its "type"). Based on a recessional velocity relative to the Cosmic Background Radiation of 6965 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7357 is about 325 million light-years away, in good agreement with redshift-independent distance estimates of about 250 to 345 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 slightly over 315 million light-years away at the time the light by which we see it was emitted, about 320 to 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 0.5 by 0.3 arcmin for the central region and about 1.05 by 0.55 arcmin for the outer ring (from the images below), the central part of the galaxy is about 45 thousand light-years across, and the outer ring spans a little over 95 thousand light-years.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7357 (glare to northeast is from magnitude 2.9 Eta (η) Pegasi)
Below, a 1.25 arcmin wide PanSTARRS image of the galaxy

NGC 7358 (= PGC 69664 = ESO 109-018)
Supposedly but not observed (Sep 5, 1826) by James Dunlop
Discovered (Jul 20, 1835) by John Herschel
Photographically observed (1898 - 1901) by DeLisle Stewart
A magnitude 12.8 lenticular galaxy (type SAB0?) in Tucana (RA 22 45 36.5, Dec -65 07 18)

Historical Identification: Per Dreyer, NGC 7358 (= GC 4829 = JH 3953, Dunlop 255?, 1860 RA 22 36 10, NPD 155 51.3) is "faint, small, round, brighter middle." The second IC adds "Stellar nucleus with wisps at 175 degrees, DeLisle Stewart." The position precesses to RA 22 45 39.1, Dec -65 07 17, less than 0.3 arcmin nearly due east of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Notes: Gottlieb notes that although Herschel's position was accurate, he missed IC 5250, a much brighter interacting pair of galaxies less than 12 arcmin to the northeast, "and probably found earlier by Dunlop (D 255)".
Dunlop's Observation: Dunlop #255 is described in his published catalog as (1827) 22 36 04, SPD 24 01 (= Dec -65 59), "A small round nebula bright at the centre,10" diameter". The position precesses to RA 22 47 45.4, Dec -65 04 31, which is nowhere near NGC 7358. But since Herschel missed the nebula that became IC 5250, Dunlop's published description fit Herschel's description for what became NGC 7358, and Dunlop's positions were known to be hit and miss, Dreyer supposed (as indicated by "Dunlop 255?") that it might be Herschel's nebula. However, as noted in the entry for IC 5250 that was wrong, and Dunlop had actually discovered a "nova", or previously unknown object.
Warning About Erroneous Press Release: A 2014 NASA press release about a Herschel telescope image of NGC 7538 mistakenly called it NGC 7358 in several paragraphs, so a search for NGC 7358 may turn up that nebula, instead of the galaxy shown here.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3225 km/sec (and H0 = 70 km/sec/Mpc), NGC 7358 is about 150 million light-years away. Given that and its apparent size of about 2.25 by 0.8 arcmin (from the images below), the galaxy has a major axis of about 95 to 100 thousand light-years.

Above, a 12 arcmin wide DSS image centered on NGC 7358
Below, a 2.5 arcmin wide DESI Legacy image of the galaxy
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 image by Courtney Seligman, using AladinLite)

WORKING HERE: CONVERT STONE DATE TO MONTH, DAY, YEAR
NGC 7359 (= PGC 69638 = PGC 798209 = ESO 534-022 = MCG -04-53-034)
Photographically discovered (Jul 14, 1885) by Francis Leavenworth
Also observed (1888.899?) by Ormond Stone
Also observed (Jul 1898 - Jun 1899) by Herbert Howe
A magnitude 12.5 lenticular galaxy (type SAB0? sp) in Aquarius (RA 22 44 48.0, Dec -23 41 17)

Historical Identification: Per Dreyer, NGC 7359 (Leavenworth list I (#256), 1860 RA 22 36 20, NPD 114 26.4) is "pretty faint, very small, pretty much extended, brighter middle and nucleus." The first IC gives a corrected RA (per Ormond Stone [#852 with the seconds of time transposed?]) of 22 38 01. The second IC has a lengthy note: "Howe gives RA 22 37 10, NPD 114 25.3, while Ormond Stone has RA 22 38 01, NPD 114 26.6. Stone's comparison star is said to be CD 17171 and 3 anonymous stars following. None of these seem to be in the Cordoba DM. But if he used CD 17165, his first anonymous star, 51 seconds east and 2 arcmin south, would be CD 17171, and his result would agree with Howe's". (In other words, Dreyer suggests that Howe's position is correct, and Stone's differs because of an error in identifying the comparison star.) Precessing Howe's position yields RA 22 44 48.5, Dec -23 41 16.7, less than 0.1 arcmin east-southeast of the center of the galaxy listed above and well within its bright central region the description fits and there is nothing else nearby, so the identification is certain.
Discovery Notes: As noted by Gottlieb, Leavenworth's position was a minute of time too far to the west (a common error at the Leander McCormick Observatory), but his description was excellent. Stone's micrometric measurement should have been more accurate, but as noted in the second IC, he used the wrong comparison star, so the position wasn't accurately measured until Howe observed the "nebula" (it wasn't until the 1920's that astronomers began to seriously consider the possibility that most "nebulae" were actually objects comparable to the Milky Way Galaxy, but so incredibly far away that they just looked relatively insignificant).
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2950 km/sec (and H0 = 70 km/sec/Mpc), NGC 7359 is about 135 to 140 million light-years away. Given that and its apparent size of about 2.0 by 0.5 arcmin (from the images below), the galaxy is about 80 thousand light-years across.
Classification Note: "sp" for "spindle" means that the galaxy appears to be edge-on to our line of sight.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7359, also showing its probable companion, PGC 134459
Below, a 2.25 arcmin wide PanSTARRS image of the galaxy

PGC 134459
Not an NGC object but listed here as a probable companion of NGC 7359
A magnitude 15.5(?) lenticular galaxy (type S0/a?) in Aquarius (RA 22 44 57.8, Dec -23 42 30)

Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 3005 km/sec (and H0 = 70 km/sec/Mpc), PGC 134459 is about 140 million light-years away. Given that and its apparent size of about 0.45 by 0.4 arcmin (from the image below), the galaxy is about 15 to 20 thousand light-years across. (The image is pretty fuzzy, so the actual size and type are obviously uncertain.)
Possible Companionship: The difference between the recessional velocities of NGC 7359 and PGC 134459 is small compared to typical "peculiar velocities", or random motions of galaxies relative to their neighbors; so there is a good chance that they are a physical pair.

Above, a 0.75 arcmin wide PanSTARRS image of PGC 134459 (see NGC 7359 for a wide-field image)

NGC 7360 (= PGC 69591 = UGC 12167 = CGCG 404-036 = CGCG 405-002 - MCG +01-58-001)
Discovered (Aug 29, 1864) by Albert Marth
A magnitude 13.7 lenticular galaxy (type S0(nr?)/a) in Pegasus (RA 22 43 34.0, Dec +04 09 04)

Historical Identification: Per Dreyer, NGC 7360 (= GC 6079, Marth #494, 1860 RA 22 36 26, NPD 86 34) is "extremely faint, very small." The position precesses to RA 22 43 32.0, Dec +04 09 57, just under 1 arcmin north-northwest of the galaxy listed above, the description is a reasonable fit 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 4315 km/sec (and H0 = 70 km/sec/Mpc), NGC 7360 is about 200 million light-years away. Given that and its apparent size of about 0.9 by 0.5 arcmin (from the images below), the galaxy is about 50 to 55 thousand light-years across.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7360
Below, a 1.0 arcmin wide PanSTARRS image of the galaxy

NGC 7361 (= IC 5237) (= PGC 69539 = PGC 722021 = UGCA 434 = ESO 468-023 = MCG -05-53-027)
Discovered (Sep 28, 1834) by John Herschel (and later listed as NGC 7361)
Discovered (Jul 19, 1897) by Lewis Swift (and later listed as IC 5237)
A magnitude 12.3 spiral galaxy (type (R)SBc? sp) in Piscis Austrinus (RA 22 42 18.2, Dec -30 03 30)

Historical Identification: Per Dreyer, NGC 7361 (= GC 4830 = JH 3954, 1860 RA 22 36 31, NPD 120 47.1) is "faint, pretty large, very much extended 0�, very gradually a very little brighter middle." The position precesses to RA 22 44 18.7, Dec -30 03 07, but there is nothing there nor near there. However, Corwin noticed that the galaxy listed above would be a perfect fit for Herschel's observation if he simply made a one-digit error in the right ascension (a not uncommon error). If Herschel's RA is reduced by exactly 2 minutes of time, to (1860) RA 22 34 31, NPD 120 47.1, the position precesses to RA 22 42 19.6, Dec -30 03 15, which is less than 0.4 arcmin northeast of the center of the galaxy listed above and barely outside its bright central region, the description (as pointed out by Corwin) is a perfect fit and there is nothing else nearby, so the identification is considered certain.
Note About Duplicate Observation: Sixty-some years later Swift made a similar error (2.4 minutes of time), but in the opposite direction, so although NGC 7361 and IC 5237 are more than 4 minutes of time apart in the NGC/IC, they are undoubtedly the same galaxy (see IC 5237 for more about Swift's mistake).
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 955 km/sec (and H0 = 70 km/sec/Mpc), NGC 7361 is about 45 million light-years away, in good agreement with redshift-independent distance estimates of about 40 to 75 million light-years. Given that and its apparent size of about 4.1 by 1.0 arcmin (from the images below), the galaxy is about 50 to 55 thousand light-years in diameter.
Classification Note: The galaxy is seen nearly edge-on (as indicated by "sp" for "spindle"), making classification difficult. In addition, it appears to have a relatively "messy" structure ("complex" might sound more "scientific", but I feel like calling a spade a spade), making it even harder. Still, the "type" shown in the description line isn't terribly different from the ones shown in major databases, and considering the lack of better images, probably as good as can be more or less confidently stated.

Above, a 12 arcmin wide DSS image centered on NGC 7361
Below, a 4 arcmin wide DSS image of the galaxy (Image Credit AladinLite processing by Courtney Seligman)

Below, a 4.0 by 4.3 arcmin wide Carnegie-Irvine image of the galaxy
(Image Credit & © Carnegie-Irvine Galaxy Survey (contrast increased by Courtney Seligman); used by permission)

NGC 7362 (= PGC 69602 = UGC 12171 = CGCG 405-003 = MCG +01-58-002)
Discovered (Sep 2, 1886) by Lewis Swift
A magnitude 12.6 elliptical galaxy (type E2) in Pegasus (RA 22 43 49.3, Dec +08 42 19)

Historical Identification: Per Dreyer, NGC 7362 (Swift list IV (#85), 1860 RA 22 36 45, NPD 82 01.8) is "very faint, small, round, a little brighter middle." The position precesses to RA 22 43 17.8, Dec +34 00 15, less than 0.3 arcmin north-northwest of the center of the galaxy above and not far outside its "brighter middle", the description fits and there is nothing else nearby, so the identification is certain.
Discussion of Data Problems: For unknown reasons, most of the galaxies apparently near NGC 7362 (and NGC 7362 itself) have published values for their recessional velocities which differ from other values for the same galaxy by hundreds of km/sec. I have decided that for NGC 7362's apparent neighbors I will only mention the range of values and the choices I made based on them, but for NGC 7362 this section of its entry discusses all of the data in detail, as an example of how choices are made when there are problems with the data.
SIMBAD currently lists a heliocentric recessional velocity for NGC 7362 of about 7640 km/sec, based on a 2002 paper comparing former SIMBAD and HyperLEDA values. HyperLEDA itself lists four values, two from papers published in 1983 and 1999, and two from 2011 and 2012 (both based on the 2MASS database). As should be expected, the papers based on the 2MASS database agree with each other, and the 1983 paper, even though based on an independent survey, has the same value for the heliocentric recessional velocity of 7645 km/sec. The 1999 paper, based on an update of the Zwicky Catalog, lists a different but nearly identical recessional velocity of 7630 km/sec.
The NED lists 8 values for NGC 7362's "redshift", four of which involve the same references as HyperLEDA, and therefore have the recessional velocities shown above. There are also two other values based on an independent survey of the sky, which naturally have the same value, but of 7448 km/sec, and two other papers, also based on independent surveys, list the 7645 km/sec value found in most of the HyperLEDA sources. The most "odd-man-out" value is in a 2014 paper based on the 2MASS database, which lists two different values: the same 7645 km/sec as most of the other references, but also a value of 6640 km/sec, which must be due to some sort of blunder. Throwing out that value, we are left with half a dozen values of 7645 km/sec, and two of 7448 km/sec. With so many values at or near 7645 km/sec, that feels like the "best" one to me, but for unknown reasons NED chose the 7448 km/sec heliocentric radial velocity for its calculations, resulting in a recessional velocity relative to the Cosmic Microwave Background radiation of about 7080 km/sec. In the discussion below I have chosen to use the 7645 km/sec heliocentric recessional velocity, which changes the CMB value to about 7275 km/sec. If the smaller value used in NED is correct, the galaxy would be about 10 million light-years closer to us, and its physical size would be very slightly smaller than the one shown below.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 7275 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7362 is about 335 to 340 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 suggests that the galaxy was about 330 million light-years away at the time the light by which we see it was emitted, about 335 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 1.35 by 1.10 arcmin (from the images below), the galaxy's major axis has a length of about 130 thousand light-years.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7362, also showing several possible "apparent companions"
Below, a 1.75 arcmin wide PanSTARRS image of the galaxy

Below, a 1.75 arcmin wide SDSS image of the galaxy

WORKING HERE

Possible companions of NGC 7362 (Vr 7645-7448), in order of increasing angular distance
**PGC 214861, PGC 214862, PGC 214860,**PGC 85294, PGC 1352986, PGC 69582

PGC 214861
Not an NGC object but listed here as an apparent companion of NGC 7362
A magnitude 16(?) lenticular galaxy (type S0 pec?) in Pegasus (RA 22 43 53.0, Dec +08 43 41)

Discussion of Possible Companionship: As in the case of NGC 7362, two papers based on the same (2MASS) database have different values for the recessional velocity of PGC 214861. SIMBAD's 2012 reference lists a heliocentric recessional velocity of 7795 km/sec, while NED's 2014 reference lists a value of 8228 km/sec, and a corresponding velocity relative to the Cosmic Microwave Background radiation of 7860 km/sec. Both heliocentric velocities are higher than any of those for NGC 7362 (by between 150 and 800 km/sec, depending on which value for one galaxy is compared to one of the values for the other one), so although close to NGC 7362 in the sky, PGC 214861 probably lies between 7 and 37 million light-years beyond it. If the smaller value is correct, the two might be an actual pair, and the difference in their velocities only a "peculiar velocity" (a random motion relative to neighboring galaxies), but if the larger one is correct PGC 214861 is relatively close to NGC 7362 in comparison to their huge distance from us, but too far beyond it to be anything but a background object. As a result, all that can be said with certainty is that the two are "apparent" companions; but for the discussion below I have used the recessional velocity that might justify thinking that the two are at least close to being gravitationally bound, but if the larger recessional velocity (and corresponding distance from us) is more accurate, then the distance and physical size derived below would have to be increased by about 5.5%.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7860 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214861 is a little over 365 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 355 million light-years away at the time the light by which we see it was emitted, about 360 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.52 by 0.2 arcmin (from the image below), the galaxy's major axis is about 50 to 55 thousand light-years.

Above, a 0.75 arcmin wide PanSTARRS image of PGC 214861 (see NGC 7362 for a wide-field image)

PGC 214862
Not an NGC object but listed here as a possible companion of NGC 7362
A magnitude 16.0(?) lenticular galaxy (type E/S0?) in Pegasus (RA 22 43 50.0, Dec +08 40 40)

Discussion of Possible Companionship: The two papers that are references for SIMBAD/LEDA and NED have extremely different recessional velocities. The 2MASS-based paper cited by NED has a heliocentric recessional velocity of 16095 km/sec, whereas a more recent paper that used various techniques for measuring recessional velocities lists a value of 7612 km/sec, which is close enough to the value for NGC 7362 that if correct, PGC 214862 is at least a possible companion of NGC 7362, as suggested above. However, as small as the galaxy appears, the much larger recessional velocity (and correspondingly much larger distance) may be correct, in which case PGC 214862 would be a very distant background galaxy, and the distance and physical size derived below would have to be more than doubled.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 7610 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214862 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 a little over 350 million light-years away at the time the light by which we see it was emitted, a little over 355 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 0.42 by 0.30 arcmin (from the images below), the galaxy's major axis is about 40 to 45 thousand light-years long.
Classification Note: The galaxy is too small and the images too grainy to clearly tell whether this is an elliptical or lenticular galaxy, so I have chosen a type on the dividing line between the two.

Above, a 0.75 arcmin wide PanSTARRS image of PGC 214862 (see NGC 7362 for a wide-field image)
Below, a 0.75 arcmin wide DESI Legacy image does a better job of showing the apparent size of the galaxy
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 image by Courtney Seligman, using AladinLite)

PGC 214860
Not an NGC object but listed here as an apparent companion of NGC 7362
A magnitude 16(?) spiral galaxy (type (R'?)SB(rs)b?) in Pegasus (RA 22 43 51.2, Dec +08 38 12)

Discussion of Possible Companionship: As in the case of all the other galaxies near NGC 7362 (and 7362 itself), SIMBAD, LEDA and NED have different recessional velocities, ranging from a low of 7395 km/sec heliocentric recessional velocity for SIMBAD to a high of more than 7945 km/sec for NED, each of the three databases citing only one reference, different from the references for both of the other databases. The NED heliocentric velocity corresponds to a recessional velocity of 7580 km/sec relative to the Cosmic Microwave Background radiation, while the SIMBAD CMB velocity would, like its heliocentric velocity, be 610 km/sec lower (or 6970 km/sec), which corresponds to a difference in the recessional velocity distance estimate of nearly 30 million light-years. Comparing these values to the 7275 km/sec adopted for NGC 7362's CMB recessional velocity, SIMBAD's value makes PGC 214860 closer to us than NGC 7362, while NED's value puts it well beyond the NGC object. In other words, there is no way to tell whether PGC 214860 is an actual companion of NGC 7362, or a foreground or background galaxy, so the only certain conclusion is that it is an "apparent" companion, as listed above.
Physical Information: Using the NED recessional velocity relative to the Cosmic Background Radiation of about 7580 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 214860 is about 350 to 355 million light-years away. However, for objects at such distances we should take into account the expansion of the Universe during the time it took their light to reach us. Doing that shows that the galaxy was about 340 to 345 million light-years away at the time the light by which we see it was emitted, about 345 to 350 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.68 by 0.55 arcmin (from the images below), the galaxy would be about 65 to 70 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on PGC 214860 also shows NGC 7362, PGC 214861, 214862 and 1349730
Below, a 0.9 arcmin wide SDSS image of the galaxy gives a good look at its structure

Below, a 0.9 arcmin wide DESI Legacy image, though overexposed, shows the overall size a little better
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC 4.0 processing by Courtney Seligman using AladinLite)

WORKING HERE
TEMP SKIP PGC 85294, PGC 1352986, PGC 69582
and PGC 85294 is just as deserving of consideration as a companion of NGC 7362
or, for that matter, PGC 1352986
(Just have to check 3K Vr for all of them, not an easy job since LEDA, NED and SIMBAD have different values for several of them)

NGC 7363 (= PGC 69580 = CGCG 514-102 = MCG +06-49-078)
Discovered (Aug 27, 1865) by Heinrich d'Arrest
A magnitude 13.8 spiral galaxy (type SABbc) in Pegasus (RA 22 43 18.4, Dec +33 59 57)

Historical Identification: Per Dreyer, NGC 7363 (= GC 6080, d'Arrest, 1860 RA 22 36 50, NPD 56 43.7) is "pretty faint, pretty large, extended, double star following (to east)." The position precesses to RA 22 43 17.8, Dec +34 00 15, about 0.25 arcmin nearly due north of the center of the galaxy listed above and within its outline, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 6400 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7363 is about 295 to 300 million light-years away, much further than a single redshift-independent distance estimate of only about 45 million light-years (that value undoubtedly belongs to a different galaxy and was assigned to this one through some sort of blunder). 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 290 million light-years away at the time the light by which we see it was emitted, about 295 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 1.0 by 0.90 arcmin (from the images below), the galaxy is about 85 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7363
Below, a 1.25 arcmin wide PanSTARRS image of the galaxy

NGC 7364 (= PGC 69630 = UGC 12174 = CGCG 379-002 = MCG +00-58-001)
Discovered (Oct 1, 1785) by William Herschel
Also observed (Sep 12, 1830) by John Herschel
A magnitude 12.6 spiral galaxy (type Sa?) in Aquarius (RA 22 44 24.4, Dec -00 09 44)

Historical Identification: Per Dreyer, NGC 7364 (= GC 4831 = JH 2179 = WH II 442, 1860 RA 22 37 14, NPD 90 53.7) is "faint, small, round, pretty suddenly brighter middle." The position precesses to RA 22 44 24.9, Dec -00 09 41, only 0.15 arcmin northeast of the center of the galaxy listed above and barely outside its "brighter middle", 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 about 4480 km/sec (and H0 = 70 km/sec/Mpc), NGC 7364 is about 205 to 210 million light-years away, in good agreement with redshift-independent distance estimates of about 155 to 360 million light-years. Given that and its apparent size of about 1.4 by 1.0 arcmin (from the images below), the galaxy is about 75 to 80 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7364
Below, a 1.75 arcmin wide PanSTARRS image of the galaxy

NGC 7365 (= PGC 69651 = ESO 603-010 = MCG -03-58-001)
Discovered (1886) by Francis Leavenworth
Also observed (Jul 1898 - Jun 1899) by Herbert Howe
A magnitude 12.9 lenticular galaxy (type E/S0?) in Aquarius (RA 22 45 10.0, Dec -19 57 07)

Historical Identification: Per Dreyer, NGC 7365 (Leavenworth list I (#257), 1860 RA 22 37 20, NPD 110 41.4) is "very faint, extremely small, round, gradually brighter middle and nucleus, 11th magnitude star 4' north-following (to northeast)." The second IC lists a corrected RA (per Howe) of 22 37 37. Howe's published position [(1900) RA 22 39 47, Dec -20 28.6] precesses to RA 22 45 24.0, Dec -29 57 20, about 0.15 arcmin east-northeast of the center of the galaxy listed above and barely outside its "bright middle", the description fits (including the star to the northeast) and there is nothing else nearby, so the identification is certain.
Correction Of An Old Error: An old version of this entry gave slight credence (with two question marks) to the idea that NGC 7481 might be a duplicate entry for NGC 7365. As discussed in the new entry for 7481, that was almost certainly wrong, and whether NGC 7481 is a duplicate listing of NGC 7365 has nothing to do with what 7365 is like, so deleting the former reference to 7481 is of no importance to this entry.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 2725 km/sec (and H0 = 70 km/sec/Mpc), NGC 7365 is about 125 to 130 million light-years away, in reasonable agreement with a single redshift-independent distance estimate of about 130 to 135 million light-years. Given that and its apparent size of about 1.3 by 0.9 arcmin (from the images below), the galaxy is about 50 thousand light-years across.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7365
Below, a 1.75 arcmin wide PanSTARRS image of the galaxy

NGC 7366 (= PGC 69629 = MCG +02-58-004)
Discovered (Aug "7" 1864) by Albert Marth
A magnitude 14.3 elliptical galaxy (type E2) in Pegasus (RA 22 44 26.6, Dec +10 46 53)

Historical Identification: Per Dreyer, NGC 7366 (= GC 6081, Marth #495, 1860 RA 22 37 26, NPD 79 56) is "extremely faint, small, stellar." The position precesses to RA 22 44 24.6, Dec +10 48 01, about 1.2 arcmin north-northwest of the galaxy above, the description is a good fit for a visual observation and there is nothing else in the region, so the identification is certain.
Note About Marth's Dates: Since Marth used a decimal date (in this case, 1864.60), any of the observations made on "that" date could have been made between midnight and dawn on Aug 6, and dusk and midnight on Aug 9; but Aug 7 is always used as the putative date of those observations.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 11265 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7366 is about 525 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 500 to 505 million light-years away at the time the light by which we see it was emitted, about 510 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 0.6 by 0.5 arcmin (from the images below), the galaxy is about 85 to 90 thousand light-years across.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7366
Below, a 1.0 arcmin wide PanSTARRS image of the galaxy

Below, a 1.0 arcmin wide DESI Legacy image of the galaxy shows that it is larger than it appears in the PanSTARRS image
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 image processed by Courtney Seligman using AladinLite)

WORKING HERE
NGC 7367 (= PGC 69633 = UGC 12175 = CGCG 379-003 = MCG +00-58-002)
Discovered (Aug 29, 1864) by Albert Marth
Discovered (Aug 30, 1865) by Heinrich d'Arrest
A magnitude 13.8 spiral galaxy (type Sab? sp) in Pegasus (RA 22 44 34.5, Dec +03 38 47)

Historical Identification: Per Dreyer, NGC 7367 (= GC 6082, d'Arrest, Marth #496, 1860 RA 22 37 29, NPD 87 04.7) is "very faint, pretty small, a little extended." The position precessses to RA 22 44 35.7, Dec +03 39 19, about 0.6 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 Background Radiation of about 6865 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7367 is about 320 million light-years away, somewhat further than redshift-independent distance estimates of about 240 to 255 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 310 million light-years away at the time the light by which we see it was emitted, about 315 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 1.6 by 0.4 arcmin (from the images below), the galaxy is about 145 thousand light-years in diameter.
Classification Note: Since the galaxy is seen nearly edge-on, I have added "sp" (= "spindle") to indicate that. Under such circumstances it is difficult to determine the type, which is why the "Sab?" (from both HyperLEDA and NED) requires a question mark.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7367
Below, a 1.75 arcmin wide PanSTARRS image of the galaxy

NGC 7368 (= PGC 69661 = ESO 345-049 = MCG -07-46=010)
Discovered (Oct 4, 1836) by John Herschel
A magnitude 12.0 spiral galaxy (type SBb? sp pec?) in Grus (RA 22 45 31.7, Dec -39 20 31)

Historical Identification: Per Dreyer, NGC 7368 (= GC 4832 = JH 3955, 1860 RA 22 37 31, NPD 130 04.6) is "faint, considerably small, a little extended, gradually a little brighter middle." The position precesses to RA 22 45 33.5, Dec -39 20 32, about 0.35 arcmin due east of the center of the galaxy listed above, the description is a good fit for a visual observation 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 about 2095 km/sec (and H0 = 70 km/sec/Mpc), NGC 7368 is about 95 to 100 million light-years away, in good agreement with redshift-independent distance estimates of about 80 to 125 million light-years. Given that and its apparent size of about 2.85 by 0.6 arcmin for the galaxy, and about 3.15 by 0.6 including a "wisp" extending from the northwestern end of the galaxy (both values from the images below), the galaxy is about 80 thousand light-years in diameter, and with the "wisp" spans about 90 thousand light-years.Classification Note: Since the galaxy is essentially edge-on (whence "sp" = "spindle"), the "type" is very uncertain, and requires a question mark.

Above, a 12 arcmin wide DSS image centered on NGC 7368
Below, a 2.75 arcmin wide DSS image of the galaxy (processing by Courtney Seligman using AladinLite)

Below, a 2.75 arcmin wide DESI Legacy image of the galaxy shows far more detail
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC 4.0 image by (unlisted?) author, additional processing by Courtney Seligman)

NGC 7369 (= PGC 69619 = CGCG 514-104 = CGCG 515-002 = MCG +06-49-080)
Discovered (Aug 29, 1865) by Heinrich d'Arrest
A magnitude 13.7 spiral galaxy (type SAB(rs)bc?) in Pegasus (RA 22 44 12.3, Dec +34 21 05)

Historical Identification: Per Dreyer, NGC 7369 (= GC 6083, d'Arrest, 1860 RA 22 37 43, NPD 56 23.2) is "pretty faint, between 2 faint stars." The position precesses to RA 22 44 10.7, Dec +34 20 49, about 0.4 arcmin southwest 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 Background Radiation of about 6270 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7369 is about 290 to 295 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 285 million light-years away at the time the light by which we see it was emitted, about 290 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 0.78 by 0.71 arcmin (from the images below), the galaxy is about 65 thousand light-years in diameter.
An Apparent Companion: Corwin lists an apparent companion (WISEA22441823+3419541), the faint "integral sign" galaxy about 1.7 arcmin southeast of NGC 7369; but whether it is a real or only apparent companion cannot be known at this time.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7369, also showing its apparent companion
Below, a 1.0 arcmin wide PanSTARRS image of the galaxy

WISEA22441823+3419541
Not an NGC object but listed here as an apparent companion of NGC 7369
A magnitude 16(?) spiral galaxy (type SB?(s?)d?) in Pegasus (RA 22 44 18.2, Dec +34 19 54)

Possible Companionship: Corwin lists this galaxy as a companion of NGC 7369, and was kind enough to provide the "type" shown above. There is almost nothing about it in any database, and since spiral galaxies (including such integral-sign spirals) come in a wide range of physical sizes, there is no way to know whether it is a relatively small galaxy at about the same distance as NGC 7369, or a larger spiral that lies well beyond the NGC object. So whether it is a probable, possible, or only apparent companion isn't known, and "apparent" companion is the only reasonable description.
Physical Information: The USNOA2 database lists the nucleus of this galaxy as a magnitude 16.4 star, but the "stellar" part of the galaxy doesn't include its entire luminosity, so although the outer regions are considerably fainter than the nucleus, the overall magnitude is probably a little closer to 16, as shown in the description line above, and the images below suggest an apparent size of about 0.65 by 0.25 arcmin; but since there is no information about its recessional velocity, the galaxy's approximate distance and physical size can't be known at this time.

Above, a 0.75 arcmin wide PanSTARRS image of this galaxy (see NGC 7369 for a wide-field image)
Below, a 0.75 arcmin wide DESI Legacy image of the galaxy gives a better idea of its size
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC 4.0 processing by Courtney Seligman using AladinLite)

NGC 7370 (= PGC 69662)
Discovered (Aug "7", 1864) by Albert Marth
A magnitude 15.3 spiral galaxy (type (R')SB(r?s)d? pec?) in Pegasus (RA 22 45 37.2, Dec +11 03 28)

Historical Identification: Per Dreyer, NGC 7370 (= GC 6084, Marth #497, 1860 RA 22 38 36, NPD 79 41) is "extremely faint, very small." The position precesses to RA 22 45 34.5, Dec +11 03 06, about 0.75 arcmin west-southwest of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Note About Marth's Dates: Since Marth used a decimal date (in this case, 1864.60), any of the observations made on "that" date could have been made between midnight and dawn on Aug 6, and dusk and midnight on Aug 9; but Aug 7 is always used as the putative date of those observations.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 8525 to 8530 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7370 is about 395 to 400 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 385 million light-years away at the time the light by which we see it was emitted, about 390 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 0.8 by 0.5 arcmin (from the images below), the galaxy (including its outer arms) is about 90 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7370, also showing NGC 7372
Below, a 0.8 arcmin wide PanSTARRS image of the galaxy

Below, a 1.0 arcmin wide DESI Legacy image of the galaxy does a better job of showing off its arms
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC 4.0 processing by Courtney Seligman using AladinLite)

NGC 7371 (= PGC 69677 = MCG -02-58-001)
Discovered (Nov 28, 1785) by William Herschel
Also observed (Sep 9, 1825) by John Herschel
A magnitude 11.5 spiral galaxy (type SAB(rs)ab?) in Aquarius (RA 22 46 03.7, Dec -11 00 04)

Historical Identification: Per Dreyer, NGC 7371 (= GC 4833 = JH 2180 = WH II 477, 1860 RA 22 38 40, NPD 101 44.5) is "very faint, pretty large, round, a little brighter middle." The position precesses to RA 22 46 02.8, Dec -11 00 23, less than 0.4 arcmin southwest of the center of the galaxy listed above and well within its outline, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 2335 km/sec (and H0 = 70 km/sec/Mpc), NGC 7371 is about 105 to 110 million light-years away, in reasonable agreement with redshift-independent distance estimates of about 95 to 100 million light-years. Given that and its apparent size of about 2.15 by 2.05 arcmin (from the images below), the galaxy is about 65 to 70 thousand light-years in diameter.
Classification Note: HyperLEDA and NED both list this as a lenticular galaxy, but the images below show that it is a spiral galaxy with a bright central bar and relatively low contrast spiral arms not easy to notice in low-resolution images.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7371
Below, a 2.25 arcmin wide PanSTARRS image of the galaxy (Brightness gradient altered by Courtney Seligman to better show outer regions)

Below, a 2.5 arcmin wide Carnegie-Irvine image of the galaxy
(Image Credit & © Carnegie-Irvine Galaxy Survey (slightly enhanced by Courtney Seligman); used by permission)

Below, a 2.15 arcmin wide Hubble Legacy Archive image of the galaxy
(Image Credit HST Archive/Flickr/Solomon Hendrix; CC 2.0 sizing & alignment by Courtney Seligman)

Below, the image above substantially brightened to better show the full extent of the galaxy (post-processing by Courtney Seligman))

NGC 7372 (= PGC 69670 = CGCG 430-004 = MCG +02-58-005)
Discovered (Aug "7", 1864) by Albert Marth
A magnitude 13.5 spiral galaxy (type Sbc) in Pegasus (RA 22 45 46.0, Dec +11 07 51)

Historical Identification: Per Dreyer, NGC 7372 (= GC 6085, Marth #498, 1860 RA 22 38 46, NPD 79 37) is "faint, small, irregularly round." The position precesses to RA 22 45 44.5, Dec +11 07 06, about 0.8 arcmin south-southwest of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Note About Marth's Dates: Since Marth used a decimal date (in this case, 1864.60), any of the observations made on "that" date could have been made between midnight and dawn on Aug 6, and dusk and midnight on Aug 9; but Aug 7 is always used as the putative date of those observations.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 11330 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7372 is about 525 to 530 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 505 million light-years away at the time the light by which we see it was emitted, about 515 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 0.8 by 0.7 arcmin (from the images below), the galaxy is about 115 to 120 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7372, also showing NGC 7370
Below, a 1.1 arcmin wide PanSTARRS image of the galaxy

NGC 7373 (= PGC 69688 = CGCG 379-004)
Discovered (Aug 11, 1864) by Albert Marth
Also observed (Aug 16, 1890) by Guillaume Bigourdan
A magnitude 13.6 lenticular galaxy (type SAB0?) in Pegasus (RA 22 46 19.4, Dec +03 12 36)

Historical Identification: Per Dreyer, NGC 7373 (= GC 6086, Marth #499, 1860 RA 22 39 00, NPD 87 31) is "faint, very small, brighter middle, stellar." The second IC lists a corrected RA (per Bigourdan) of 22 39 13. The corrected position precesses to RA 22 46 20.2, Dec +03 13 08, about 0.6 arcmin north-northeast of the center of the galaxy listed above, the description is reasonable for a visual observation and there is nothing else nearby, so the identification is certain.
Physical Information: Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4325 km/sec (and H0 = 70 km/sec/Mpc), NGC 7373 is about 200 million light-years away. Given that and its apparent size of about 0.95 by 0.5 arcmin (from the images below), the major axis of the galaxy is about 55 thousand light-years long.
Apparent size 1.3 by 0.5? arcmin.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7373
Below, a 1.5 arcmin wide PanSTARRS image of the galaxy

NGC 7374 (= PGC 69676 = CGCG 430-006 = MCG +02-58-007 = "NGC 7374A")
Discovered (Aug "7", 1864) by Albert Marth
A magnitude 13.8 spiral galaxy (type Sbc) in Pegasus (RA 22 46 01.0, Dec +10 51 13)

Historical Identification: Per Dreyer, NGC 7374 (= GC 6087, Marth #500, 1860 RA 22 39 02, NPD 79 52) is "very faint, pretty large, round." The position precesses to RA 22 46 00.8, Dec +10 52 07, about 0.9 arcmin nearly due north of the galaxy listed above, the description fits and the only nearby galaxy (IC 1452) is far too small to be called "pretty large", so the identification is certain.
Note About Marth's Dates: Since Marth used a decimal date (in this case, 1864.60), any of the observations made on "that" date could have been made between midnight and dawn on Aug 6, and dusk and midnight on Aug 9; but Aug 7 is always used as the putative date of those observations.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 6725 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7374 is about 310 to 315 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 305 million light-years away at the time the light by which we see it was emitted, nearly 310 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 0.53 arcmin (from the images below), the galaxy is about 65 to 70 thousand light-years in diameter.

Above, a 12 arcmin wide SDSS image centered on NGC 7374, also showing IC 1452
Below, a 0.9 arcmin wide SDSS image of the galaxy

Below, a 0.9 arcmin wide PanSTARRS image of the galaxy

IC 1452 ( = PGC 69675 = MCG +02-58-006 = "NGC 7374B")
Not an NGC object but listed here because sometimes called NGC 7374B
A magnitude 14.5 lenticular galaxy (type E/S0?) in Pegasus at (RA 22 45 59.2, Dec +10 52 03)

Warning About Non-Standard Designations: In general, the addition of letters to NGC/IC designations should be deprecated, because the same letter is often used for different galaxies, or different letters for the same galaxy, either of which can cause data for one galaxy to be mistakenly assigned to a different one. Aside from that, the usage of such non-standard designations is pointless when, as in this case, the galaxy already has a perfectly good IC designation.
Physical Information and Images: See NGC 7374 for an image of the region, and IC 1452 for anything else.

NGC 7375 (= PGC 69695 = CGCG 453-007 = MCG +03-58-003)
Discovered (Oct 1, 1866) by Truman Safford
Discovered (Sep 2, 1886) by Lewis Swift
Also observed (Oct 5, 1888) by Guillaume Bigourdan
A magnitude 13.7 lenticular galaxy (type (R)SB0(nr,r)/a) in Pegasus (RA 22 46 32.0, Dec +21 05 01)

Historical Identification: Per Dreyer, NGC 7375 (Swift list IV (#86), (Safford 57), 1860 RA 22 39 33, NPD 69 38.8) is "extremely faint, very small, round." (Swift's paper adds "forms equilateral triangle with 2 stars...") The second IC lists a corrected RA (per Bigourdan) of 22 39 44. The corrected position precesses to RA 22 46 31.0, Dec +21 05 22, less than 0.5 arcmin northwest of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Notes: Safford's observations weren't published until long after the fact, and Dreyer didn't become aware of them until he was in the last stages of preparing the NGC for publication. As a result they were only mentioned in an appendix, and none were included in the individual NGC entries (hence the credit here in parentheses).
300 Mly, 303 Myr
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 6615 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7375 is about 305 to 310 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 300 million light-years away at the time the light by which we see it was emitted, nearly 305 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 1.05 by 0.95 arcmin including the faint outer ring (from the images below), the galaxy is about 90 thousand light-years across.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7375
Below, a 1.4 arcmin wide PanSTARRS image of the galaxy

NGC 7376 (= PGC 69715 = CGCG 379-006)
Discovered (Aug 29, 1864) by Albert Marth
A magnitude 14.4 spiral galaxy (type (R'?)SB(r?s)b) in Pegasus (RA 22 47 17.4, Dec +03 38 44)

Historical Identification: Per Dreyer, NGC 7376 (= GC 6088, Marth #501, 1860 RA 22 40 11, NPD 87 07) is "extremely faint, very small, round." The position precesses to RA 22 47 17.8, Dec +03 37 12, about 1.5 arcmin nearly due south 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 8050 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7376 is about 375 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 360 to 365 million light-years away at the time the light by which we see it was emitted, about 365 to 370 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.6 by 0.4 arcmin (from the images below), the galaxy is about 60 to 65 thousand light-years across.

Above, a 12 arcmin PanSTARRS image centered on NGC 7376
Below, a 0.75 arcmin PanSTARRS image of the galaxy

NGC 7377 (= PGC 69733 = ESO 534-026 = MCG -04-53-038)
Discovered (Oct 13, 1786) by William Herschel
Also observed (Sep 16, 1830) by John Herschel
A magnitude 11.1 spiral galaxy (type (R)SA(rs)a pec) in Aquarius (RA 22 47 47.5, Dec -22 18 44)

Historical Identification: Per Dreyer, NGC 7377 (= GC 4834 = JH 2181 = WH II 598, 1860 RA 22 40 12, NPD 113 02.9) is "pretty bright, small, very little extended, very gradually much brighter middle, 12th magnitude star preceding (to west)." The position precesses to RA 22 47 47.8, Dec -22 18 40, almost dead center on 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 wrote "GC 4835-41 do not exist. The words "7 knots found" in P.T. 1861, p. 735, refer to the nebulae (JH) 2183-84, and not to (JH) 2181." Since NGC 7377 is (JH) 2181, this note is simply warning readers of the NGC that the nonexistent GC entries have nothing to do with NGC 7377.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 3025 km/sec (and H0 = 70 km/sec/Mpc), NGC 7377 is about 140 million light-years away. Given that and its apparent size of about 4.1 by 2.9 arcmin (from the images below), the galaxy is about 165 to 170 thousand light-years in diameter (a better image, not yet available, slightly changes these numbers).
Use By The de Vaucouleurs Atlas: NGC 7377 is used by the de Vaucouleurs Atlas of Galaxies as an example of galaxy type SA(s)0/a pec.
Classification Note: As shown in the preceding paragraph the de Vaucouleurs Atlas describes this as a lenticular galaxy, and although the Carnegie-Irvine image shows the presence of numerous faint dusty "arms", that "lenticular" classification could easily be accepted as part of the "pec" based on the images currently shown here. But a very "deep" image by Mark Hanson shows that it is actually a severely disturbed spiral galaxy (hence my different "type" in the description line, which is an understatement about its tortured appearance). If I receive permission to show part of his spectacular image, I will post it below; but since the image is copyrighted, the link to his website must suffice until I hear from him.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7377
Below, a 4 arcmin wide PanSTARRS image of the galaxy

Below, a 4.9 arcmin wide image of the galaxy (brightness slightly adjusted by Courtney Seligman)
(Image Credit & © Carnegie-Irvine Galaxy Survey; used by permission)

NGC 7378 (= PGC 69734 = PGC 193911 = PGC 3096699 = MCG -02-58-005)
Discovered (Sep 19, 1879) by Wilhelm Tempel
A magnitude 12.7 spiral galaxy (type (R'?)S(nr,rs?)ab? pec) in Aquarius (RA 22 47 47.7, Dec -11 49 00)

Historical Identification: Per Dreyer, NGC 7378 (Tempel list III (& list IV #10), 1860 RA 22 40 25, NPD 102 33.0) is "very faint, pretty large." The position precesses to RA 22 47 48.4, Dec -11 48 46, only about 0.25 arcmin northeast of the center of the galaxy listed above and on the edge of its bright central region, 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 about 2225 km/sec (and H0 = 70 km/sec/Mpc), NGC 7378 is about 100 to 105 million light-years away, in good agreement with redshift-independent distance estimates of about 80 to 120 million light-years. Given that and its apparent size of about 1.5 by 0.85 arcmin (from the images below), the galaxy is about 45 light-years in diameter. It is thought to be a Seyfert galaxy (type Sy2).

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7378
Below, a 1.8 arcmin wide PanSTARRS image of the galaxy

Below, a 1.8 arcmin wide DESI Legacy image of the galaxy
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 reprocessing by Courtney Seligman)

NGC 7379 (= PGC 69724 = UGC 12187 = CGCG 531-013 = MCG +07-46-018)
Discovered (Sep 19, 1876) by �douard Stephan
A magnitude 13.4 spiral galaxy (type SAB(rs)ab) in Lacerta (RA 22 47 32.9, Dec +40 14 20)

Historical Identification: Per Dreyer, NGC 7379 (= GC 6089, Stephan list VIII (#24), 1860 RA 22 41 13, NPD 50 30.0) is "extremely faint, small, round, a little brighter middle." The position precesses to RA 22 47 32.7, Dec +40 14 15, barely southwest of the center of the galaxy listed above and within its bright central region, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Traditionally, Stephan's discovery date for this object is given as Sep 22, 1876. However, that is the date that Stephan reduced his micrometric position, as subsequently published in his list VIII. Per his logbooks, he first observed the galaxy on the date shown in the description line (this is typical of his published work; objects that he only observed once rarely ended up in the NGC/IC).
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 5040 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7379 is about 235 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 230 million light-years away at the time the light by which we see it was emitted, a between 230 and 235 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 1.2 by 0.85 arcmin (from the images below), the galaxy is about 80 thousand light-years in diameter.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7379
Below, a 1.75 arcmin wide PanSTARRS image of the galaxy (to be cleaned up later)

NGC 7380 (= OCL 244 = "LBN 511" = "PGC 3518437")
Discovered (Aug 7, 1787) by Caroline Herschel
Also observed (Nov 1, 1788) by William Herschel
Also observed (Sep 24, 1829) by John Herschel
A magnitude 7.2 open cluster (type III3pn) in Cepheus (RA 22 47 15.0, Dec +58 08 00)

Historical Identification: Per Dreyer, NGC 7380 (= GC 4842 = JH 2182 = WH VIII 77, C (Herschel) II, 1860 RA 22 41 23, NPD 32 39.1) is "a cluster, pretty large, pretty rich, a little compressed, stars from 9th to 13th magnitude." The position precesses to RA 22 46 57.1, Dec +58 05 08, about 0.4 arcmin nearly due east of magnitude 8.2 star HD 215835. Such stars were often chosen by the Herschels to determine the position of a cluster, and although there are other stars (and double stars) of similar brightness, the position was (as noted below) meant to specify that one, so the identification is certain. (The position of that star does not agree with the one shown in the description line because that is an estimate of the approximate center of the cluster, without reference to any particular star. Different observers usually choose somewhat different positions for the "center" of a cluster, so other references may have a different position, but still be inside the open cluster defined above as NGC 7380.)
Discovery Notes: Caroline's description does not specify a size for the cluster, just that it is "a nebulous patch in a line from [stet] Epsilong (ε) Cephei continued through Delta (δ) towards 1st and 2nd Flamsteed Casseiopeia." [Her 4 inch telescope only showed the cluster as a fuzzy (therefore "nebulous") patch.] William described the object as "a cluster of coarsely scattered stars 7 or 8 arcmin diameter", and John (in his second sweep of the cluster) wrote "A double star, the chief of a fine, pretty rich, large cluster, 10 arcmin diameter; stars 9th to 13th magnitude." All of these descriptions indicate that the cluster was "large", and close to 10 arcmin in size, so Dreyer's "pretty large", which implies only a 1 arcmin diameter, is very misleading.
LBN Designation Note: The Herschels could not see the nebula lit up by the cluster, which was too faint to see in their telescopes, so NGC 7380 is only the open cluster; but in modern photographs the nebula (LBN 511, placed in quotes because it is not NGC 7380) looks far more spectacular, so NGC 7380 is sometimes mistakenly listed as both the cluster and the nebula, or even as only the nebula.
PGC Designation Note: As usual for NGC/IC objects, HyperLEDA assigned a PGC designation to this, even though it isn't a galaxy; but also as usual in such situations, a search of the database for that designation returns no result, hence the quotes placed around it.
Physical Information: Estimates of the cluster's size range from about 10 to 20 arcmin, but since the Herschels were apparently more impressed with the 8 to 10 arcmin concentration of stars near the center of more widely scattered stars I have used a 12 arcminute image to show the region corresponding to their observations. A catalog of open clusters states that there are about 40 stars in the cluster, at a distance of about 7250 light-years. That corresponds pretty closely to the number of reasonably bright stars in the 12 arcmin wide image below, and using the Herschels' 10 arcmin wide apparent size for the cluster and the distance just stated, that part of the cluster spans just over 20 light-years. If stars further out than that are counted as part of the cluster then the size would be proportionate; e.g., using a 20 arcmin size that includes more distantly scattered stars, the cluster would be twice as large, or a little over 40 light-years in diameter.
As noted by John Herschel and Gottlieb's visual observations, the cluster's western vertex is the star chosen by Herschel as the position of the cluster. Gottlieb writes that that star is a rare spectroscopic eclipsing binary consisting of massive stars of type O5.5 and O6.5, and is the main source of the ionizing (UV) radiation that lights up LBN 511.

Above, a 45 arcmin wide region centered on NGC 7380 and the surrounding emission nebula
Below, a 12 arcmin wide DSS image centered on the position shown in the description line

NGC 7381 (= PGC 69828 = ESO 603-017 = MCG -03-58-007A)
Discovered (Oct 9, 1885) by Francis Leavenworth
A magnitude 14.2 irregular galaxy (type Im?) in Aquarius (RA 22 50 08.2, Dec -19 43 30)

Historical Identification: Per Dreyer, NGC 7381 (Leavenworth list I (#258), 1860 RA 22 41 25, NPD 110 29.5) is "extremely faint, very small, round, gradually brighter middle." The position precesses to RA 22 48 57.3, Dec -19 45 12, but there is nothing there nor near there. However, as noted by Gottlieb, Leavenworth's positions were only given to the nearest minute of time and declination [in this case as (1890) RA 22 43, Dec -20 20], and experience with other Leander McCormick Observatory observations tells us that they were often "off" by 1 or 2 units in either value. So we need to look for something a minute or two of right ascension to the east or west, and a minute or two of declination to the north or south. Fortunately, there is almost nothing in that region that Leavenworth's photograph would have shown except the galaxy listed above, which is just over 1 minute of time to the west and 2 minutes of arc to the north of the NGC position. And since that galaxy's appearance fits Leavenworth's description, it is universally presumed that PGC 69828 is what Leavenworth observed, and Dreyer listed as NGC 7381. (As an example of how this works, if Leavenworth's published position had been (1890) 22 44, -20 18, it would have precessed to RA 22 49 54.9, Dec -19 43 06, which is only 3 arcmin due west of the galaxy listed above, and that is close enough that the identification would have been considered certain without having to consider possible errors in the published position.)
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 4180 km/sec (and H0 = 70 km/sec/Mpc), NGC 7381 is about 195 million light-years away. Given that and its apparent size of about 0.6 by 0.5 arcmin (from the images below), the galaxy is about 35 thousand light-years across. Despite its small size its unusually blue color indicates that it is undergoing a considerable amount of bright star formation; for that reason, it is classed as an HII source (meaning that it has lots of hot, bright, bluish stars which must have recently formed because they have very short lifetimes).
Classification Note: HyperLEDA and NED list this as a spiral galaxy of type (R)Sc or (R)Scd pec?, but the images below show no sign of spiral organization, so between that and its small size, I suspect that it would be better classed as type Im (as shown in the description line).
Image Note: The SDSS image database does a better job of showing the (lack of) structure of the galaxy, but doesn't cover the northern part of a 12 arcmin field of view, so I used PanSTARRS for the wide-field image.

Above, a 12 arcmin wide PanSTARRS image centered on NGC 7381
Below, a 0.75 arcmin wide SDSS image of the galaxy

NGC 7382 (= PGC 69840 = PGC 631761 = ESO 408-015 = MCG -06-50-005)
Discovered (Sep 1, 1834) by John Herschel
A magnitude 13.3 spiral galaxy (type (R'?)Sa? sp) in Grus (RA 22 50 24.0 Dec -36 51 26

Historical Identification: Per Dreyer, NGC 7382 (= GC 4843 = JH 3956, 1860 RA 22 42 23, NPD 127 34.9) is "extremely faint, very small, round, 12th magnitude star attached north-preceding (to northwest)." The position precesses to RA 22 50 18.2, Dec -36 50 31, about 1.5 arcmin northwest of the galaxy listed above, the description is a good fit (the position of the "attached" star clinches things) 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 about 11330 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7382 is about 525 to 530 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 505 million light-years away at the time the light by which we see it was emitted, about 515 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 0.35 arcmin (from the images below), the galaxy is about 130 to 135 thousand light-years in diameter.
Classification Note: The images below are too poor to tell whether this is a lenticular or spiral galaxy, but HyperLEDA lists it as type Sa, and NED as (R?)SAa? sp, "sp" standing for "spindle", or nearly edge-on. I feel doubtful about these classifications, but have used a compromise between them and more question marks for the "type" in the description line.

Above, a 12 arcmin wide DSS image centered on NGC 7381
Below, a 1.2 arcmin wide DSS image of the galaxy

Below, a 1.2 arcmin wide monochrome DESI Legacy image shows a smidgen more detail
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 reprocessing by Courtney Seligman using AladinLite)

WORKING HERE
NGC 7383 (= PGC 69809 = CGCG 430-012 = MCG +02-58-014)
Discovered (Nov 27, 1850) by Bindon Stoney
Discovered (Sep 19, 1862) by Heinrich d'Arrest
A magnitude 13.7 spiral galaxy (type (R')SB(s)b? pec) in Pegasus (RA 22 49 35.6, Dec +11 33 23)

Historical Identification: Per Dreyer, NGC 7383 (= GC 4844, 3rd Lord Rosse, d'Arrest, 1860 RA 22 42 38, NPD 79 11.1) is "very faint, very small, round, (WH) III 216 north-following (to northeast)," WH III 216 being NGC 7385. The position precesses to RA 22 49 36.6, Dec +11 33 16, only about 0.25 arcmin east-southeast of the center of the galaxy listed above, the description fits (including the position of NGC 7385) and there is nothing comparable nearby, so the identification is certain.
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case Bindon Stoney.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7565 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7383 is about 350 to 355 million light-years away, in almost inevitable agreement with widely varying redshift-independent distance estimates of about 260 to 585 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 340 to 345 million light-years away at the time the light by which we see it was emitted, about 345 to 350 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.75 by 0.75 arcmin (from the images below), the galaxy is about 75 thousand light-years in diameter.
Classification Note: Most references classify this as a lenticular galaxy of type SB0, but the arms extending from either end of its bar suggest that it is a spiral galaxy in the last stages of becoming a lenticular galaxy, hence the "type" I chose in the description line.

Above, a 12 arcmin wide SDSS image centered on NGC 7383
Also shown are the galaxy mistakenly listed as NGC 7384, NGC 7385, and several PGC objects
(Also shown are the two stars mentioned in the entry for NGC 7384)
Below, a 1.0 arcmin wide PanSTARRS/SDSS composite image of NGC 7383 (processing by Courtney Seligman)

WORKING HERE; several other PGC objects may be companions of one of the three NGC objects

Corwin lists an apparent companion (PGC 1395249) at 22 49 39.9, +11 32 50
LEDA G, B 18.2 => V 17.5(?), no Vr; NED & SIMBAD nil

WORKING HERE SEP 13, 2024: probably done, but need to re-read, to make sure clearly explained
NGC 7384
Observed (Nov 27, 1850) by Bindon Stoney
Basically a "lost" object somewhere to the southeast of NGC 7383
Usually listed as a magnitude 16 star ("PGC 5067082") in Pegasus (RA 22 49 42.6, Dec +11 29 15)
but possibly a magnitude 15.3 star at RA 22 49 51.1, Dec +11 29 53
or one of several other stars and double stars in their vicinity

Historical Identification: Per Dreyer, NGC 7384 (3rd Lord Rosse, 1860 RA 22 42 46, NPD 79 15) is "considerably faint, 5' north-following (northeast of) GC 4844", GC 4844 being NGC 7383. However, per Corwin and Gottlieb, Stoney's sketch of the region involved shows that the object is southeast of NGC 7383, so the NGC position is certainly wrong, and aside from that there is nothing to the northeast of NGC 7383 except stars too faint for Stoney to see, or too bright to be mistaken for nebulae. And as noted in the following paragraph, the NGC position must be a rough estimate by Dreyer of the distance from the star shown in Stoney's sketch, incorrectly stated as being northeast of NGC 7383, instead of (more or less) southeast of that galaxy.
Discovery Notes: Gottlieb notes that the RNGC, PGC and SIMBAD all misidentify the galaxy to the east of NGC 7383 (PGC 69819 as NGC 7384, and as a result, so do Wikisky and AladinLite (HyperLEDA, however, changed the PGC misidentification to the 16th magnitude star noted in the description line, based on the following discussion, whence the PGC designation [in quotes, since a search of the database for that designation returns no result] assigned to that star). Given the fact that between Stoney's sketch and Dreyer's incorrect interpretation of that sketch what Stoney observed was probably a star or double star about 5 or so arcmin more or less southeast of NGC 7383 (since Stoney didn't measure the star's position, Dreyer's estimate of its distance from NGC 7383 could be off by an arcmin or more, and in general, objects listed in the NGC as "southeast" of something else could be in any direction from east-southeast to south-southeast). Given that, Corwin tentatively identified NGC 7384 as the magnitude 16 star shown in the description line, which is about 4.5 arcmin south-southeast of NGC 7383; but he notes that there are several other stars in the region which might be what Stoney saw, including the magnitude 15.3 star listed above, which is exactly 5.0 arcmin exactly southeast of NGC 7383. PGC 69819 can be positively ruled out because it is only 2.5 arcmin almost due east of NGC 7383, which is only half of Dreyer's estimated distance from 7383, and couldn't be said to be even "more or less" southeast; so its _mis_identification is certain. But although one of the two stars listed above has a good chance of being what Stoney observed, which (if either) cannot be known with any certainty, so as shown at the start of this entry, NGC 7384 is basically "lost".
Discoverer Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case Bindon Stoney.

(See NGC 7383 for an image showing the region to the southeast of that galaxy)

PGC 69819 (not = NGC 7384)
Not an NGC object but listed here because misidentified as NGC 7384 in several databases
A magnitude 14.5(?) elliptical galaxy (type E2?) in Pegasus (RA 22 49 46.0, Dec +11 33 09)

Modern Misidentification: The RNGC, SIMBAD and the original PGC misidentified this galaxy as NGC 7384. HyperLEDA has corrected that error, but SIMBAD has not, and since the RNGC was a printed paper and not an online resource, it can't correct the mistake.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 6950 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 69819 is about 320 to 325 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 315 million light-years away at the time the light by which we see it was emitted, nearly 320 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 ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Possible Companionship: See NGC 7385 for a discussion of the possible relationship of the galaxies in this region.

Images to be added ASAP

NGC 7385 (= PGC 69824 = UGC 12207 = CGCG 430-015 = MCG +02-58-017)
Discovered (Oct 18, 1784) by William Herschel
Also observed (Oct 17, 1825) by John Herschel
A magnitude 12.0 elliptical galaxy (type E2? pec) in Pegasus (RA 22 49 54.6, Dec +11 36 31)

Historical Identification: Per Dreyer, NGC 7385 (= GC 4845 = JH 2183 = WH III 216, 1860 RA 22 42 55, NPD 79 07.9) is "considerably faint, small, round, gradually a little brighter middle, 11th magnitude star north-preceding (to northwest)." The position precesses to RA 22 49 53,6, Dec +11 36 29, about 0.2 arcmin nearly due west of the center of the galaxy listed above and on the rim of its bright central region, the description is a perfect fit and there is nothing nearby that isn't accounted for by another NGC object, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7480 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7385 is about 345 to 350 million light-years away, in inevitable agreement with widely differing redshift-independent distance estimates of about 195 to 920 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 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 1.65 by 1.4 arcmin (from the images below), the galaxy is about 160 to 165 thousand light-years across.
Classification Note: Although the "type" is shown here as an E with a number indicating its "ellipticity", such giant ellipticals are often just called cD galaxies.
Possible Companionship: NGC 7383, 7385, 7389 and the apparent companion of NGC 7387 (PGC 69835) all have recessional velocities relative to the Cosmic Microwave Background radiation of between 7390 and 7565 km/sec, and may well be a physical group. NGC 7386 and PGC 69819 (incorrectly identified as NGC 7384 by some databases) have velocities of 6950 km/sec, and 7387 has one of 6750 km/sec, so those four objects may be a somewhat closer group. NGC 7390 has the highest recessional velocity of any of these objects (7970 km/sec), and may be a slightly background galaxy. However, depending on their masses (and the gravitational fields associated with them) it is conceivable that all of these objects are a single group, with "peculiar velocities" (random motions relative to neighboring galaxies) of up to 600 km/sec. Such very large peculiar velocities are common in rich clusters of galaxies, but would be unusual in a smaller group, such as these galaxies seem to form; but the fact that they are all in such a small part of the sky (less than 12 arcmin across) makes it tempting to suppose that they might be a physical group.

Above, a 12 arcmin wide SDSS image showing NGC objects near NGC 7385: NGC 7383, 7386, 7387, 7388, 7389 and 7390
Also shown is the galaxy misidentified as NGC 7384 by the RNGC, SIMBAD and the original PGC, PGC 69819
(Finally, PGC 69835 is shown as an apparent companion of NGC 7387, and as discussed above, perhaps a physical companion)
Below, a 2.5 arcmin wide PanSTARRS image of NGC 7385

Below, a 2.25 arcmin wide HST image of the galaxy's core (Image Credit Hubble Legacy Archive, raw image cleaned up by unknown author)
(A missing part of the HLA image was removed by concentrating on the core and cloning nearby pixels)

Below, the image above with brightness curves adjusted (per CC0 license, by Courtney Seligman) to show the whole galaxy
(The missing part of the image, though invisible in the image above, faintly reappears as a diagonal streak)

WORKING HERE
NGC 7386 (= PGC 69825 = UGC 12209 = CGCG 430-016 = MCG +02-58-018)
Discovered (Oct 18, 1784) by William Herschel
Also observed (Oct 9, 1830) by John Herschel
A magnitude 12.3 lenticular galaxy (type E/S0?) in Pegasus (RA 22 50 02.1, Dec +11 41 55)

Historical Identification: Per Dreyer, NGC 7386 (= GC 4846 = JH 2184 = WH III 217, 1860 RA 22 43 04, NPD 79 02.5) is "considerably faint, small, round, pretty gradually brighter middle, following (eastern) of 2," the other being NGC 7385. The position precesses to RA 22 50 02.5, Dec +11 41 53, about 0.6 arcmin nearly due south of the center of the galaxy listed above and just outside its brighter center, the description is a perfect fit and there is nothing comparable nearby that isn't accounted for by another NGC object, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 6950 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7386 is about 320 to 325 million light-years away, in good agreement with redshift-independent distance estimates of about 195 to 340 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 315 million light-years away at the time the light by which we see it was emitted, about 320 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 1.1 arcmin (from the images below), the galaxy's major axis is about 165 thousand light-years long.

Above, a 12 arcmin wide SDSS image centered on NGC 7386, also showing NGC 7385, 7387 & 7388, PGC 69832 & 69835
Below, a 3 arcmin wide SDSS image of the galaxy

NGC 7387 (= PGC 69834 = CGCG 430-019 = MCG +02-58-022)
Discovered (Sep 9, 1856) by R. J. Mitchell
Observed (Sep 19, 1862) by Heinrich d'Arrest
A magnitude 14.0 lenticular galaxy (type E/S0?) in Pegasus (RA 22 50 17.7, Dec +11 38 12)

Historical Identification: Per Dreyer, NGC 7387 (= GC 4847, 3rd Lord Rosse, d'Arrest, 1860 RA 22 43 19, NPD 79 05.9) is "extremely faint, very small, round, two 11th magnitude stars to south." The position precesses to RA 22 50 17.6, Dec +11 38 30, about 0.25 arcmin due north of the center of the galaxy listed above and just outside its bright center, the description fits (though the two stars are to the southeast) and there is nothing comparable nearby, so the identification is certain.
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case R. J. Mitchell.
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 6750 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7387 is about 315 million light-years away, somewhat further than a single redshift-independent distance estimate of about 260 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 305 million light-years away at the time the light by which we see it was emitted, about 310 million years ago (the difference between the two numbers being due to the expansion of the intervening space during the light-travel time). Given that and its apparent size of about 0.85 by 0.45 arcmin (from the images below), the galaxy's major axis is about 75 thousand light-years long.

Above, a 12 arcmin wide SDSS image centered on NGC 7387, also showing NGC 7385, 7386, 7388 & 7389, PGC 69832 & 69835
Below, a 1.5 arcmin wide SDSS image of NGC 7387 and PGC 69835

WORKING HERE: Check "straightforward" & relativistic distances (something seems off); type??
PGC 69835 (= MCG +02-58-023)
Not an NGC object but listed here as an apparent companion of NGC 7387
A magnitude 16(?) ? galaxy (type ?) in Pegasus (RA 22 50 18.0, Dec +11 37 40)

Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 7390 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that PGC 69835 is about 345 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 million light-years away at the time the light by which we see it was emitted, nearly 340 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 ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
"Companionship" With NGC 7387: Since the recessional velocity of this galaxy is more than 600 km/sec larger than that of NGC 7387, it is almost certainly a background galaxy, and therefore only an "apparent" companion of its larger "neighbor".
Another "Apparent" Companion: Corwin lists the galaxy on the northwest rim of PGC 69835 (running north-northwest to south-southeast and centered at RA 22 50 17.9, Dec +11 37 41) as an apparent companion of PGC 69835. However, there is nothing about that object in any database, so whether it has anything to do with PGC 69835 or is merely an optical double can't be known at the present time. Given its appearance and the lack of any apparent interaction between the "pair", it is almost certainly a far more distant background galaxy; but that doesn't mean that it can't be listed as an apparent companion, hence its mention here.

Add image of this object
Above, a ? arcmin wide ? image of PGC 69835 (for wider-field images, see )
NGC 7388 (= "PGC 5067400")
Observed (Oct 11, 1873) by Lawrence Parsons, 4th Lord Rosse
A magnitude 16.0 star in Pegasus (RA 22 50 21.0, Dec +11 42 38)

Historical Identification: Per Dreyer, NGC 7388 (= GC 6090, 4th Lord Rosse, 1860 RA 22 43 21, NPD 79 01.3) is "very faint, 11th magnitude star following (to the east) 2.5 arcmin." The position precesses to RA 22 50 19.5, Dec +11 43 06, but there is nothing obvious there, and no 11th magnitude star nearby. However, per Gottlieb, Lord Rosse made careful micrometric measurements of the position of this object relative to NGC 7387 that point "precisely to a very faint star, whose position is" the one shown in the discovery line, above, and does have a star about 2.5 arcmin to its east-southeast (though it's magnitude 14, not 11). And although the description isn't perfectly accurate, the position is less than 0.6 arcmin northwest of the the star, so Dreyer's conversion of Lord Rosse's measurements to the NGC position wasn't far off, and if the object involved had been anything more noticeable, its identification would have been considered certain. As it is, there is nothing in the region that could be considered more certain, so there is relatively general agreement that this star is what Parsons observed (though see the note immediately below).
Discovery Notes: RNGC and SIMBAD misidentify the extremely faint galaxy (PGC 69832) about 1.4 arcmin nearly due north of the 16th magnitude star as NGC 7388 (and as a result, so do Wikisky and AladinLite), but that object is far too faint for 19th century observers to have seen, even using Lord Rosse's 72-inch "Leviathan", and although Gottlieb could easily see the star he couldn't see the galaxy to its north in his examination of the region, confirming the fact that the RNGC/SIMBAD ID must be wrong.
Additional Mistaken References: Aside from the RNGC and SIMBAD, although the NED correctly identifies NGC 7388 as the star listed above and gives the correct position for the star, it includes the ID for the galaxy that is not NGC 7388 in its list of identifications. So HyperLEDA appears to be the only major database to completely correctly identify NGC 7388 as the star.

Above, a 12 arcmin wide SDSS image centered on NGC 7388, also showing PGC 69832, the galaxy often misidentified as NGC 7388

PGC 69832
Not an NGC object but listed here because often misidentified as NGC 7388
A magnitude 17(?) spiral(?) galaxy (type S?) in Pegasus (RA 22 50 20.8, Dec +11 44 04)

Modern Misidentification: The RNGC chose this as the only galaxy near the position of NGC 7388, without taking into consideration the fact that it is far too faint for any 19th century observer to have seen. For a discussion of the mess this has created in modern databases, see the entry for NGC 7388.
Physical Information: Other than its apparent size and a rough estimate of its brightness (based on a HyperLEDA value for its B magnitude), no database appears to have any information about this object, so all that can be said (other than the description based on its images, which is as uncertain as those images are unsatisfactory) is that it is probably a very distant background galaxy, and that it has an apparent size (based on the images below) of about 0.32 by 0.25 arcmin.

Classification Note: The color and appearance of the galaxy suggests that it is either a spiral or irregular galaxy, and I have tentatively chosen spiral simply because the DESI Legacy image shows a bright central region more typical of a spiral galaxy than an irregular one; but if far better images were available I wouldn't be terribly surprised to find that it is an irregular galaxy with considerable star-forming activity, hence the question marks associated with "spiral" in the description line.

Above, a 0.5 arcmin wide PanSTARRS image of PGC 69832 (for a wide-field image see NGC 7388)
Below, a 0.5 arcmin wide DESI Legacy image of the galaxy
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC4.0 processing by Courtney Seligman using AladinLite)

POOR POSITION
INCLUDE DIAGRAM FROM ROSSE'S PAPER, SHOW PROPER CALCULATIONS
NGC 7389 (= PGC 69836 = CGCG 430-018 = MCG +02-58-019)
Discovered (Nov 27, 1850) by Bindon Stoney
Also observed (Oct 11, 1873) by John Dreyer
A magnitude 13.9 spiral galaxy (type S??) in Pegasus (RA 22 50 16.2, Dec +11 33 58)

Historical Identification: Per Dreyer, NGC 7389 (= GC 4848, 3rd Lord Rosse, 1860 RA 22 43 24, NPD 79 07.8) is "very faint, round." The position precesses to RA 22 50 22.6, Dec +11 36 37, but although there are numerous galaxies in the area, there is nothing close to that position. Per Gottlieb, the problem is that on the sketch he made of the area Stoney didn't label the object, and John Herschel, when compiling his General Catalogue (GC), apparently thought it was the object labeled Delta (Σ), which is NGC 7387, and of course that led to a poor position in the GC, and therefore in the NGC, despite the fact that Dreyer himself measured an offset and position angle from NGC 7390 to this object in 1873 (as shown above). (MORE TO FOLLOW IN FINAL ITERATION OF THIS PAGE)
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case Bindon Stoney.
LEDA SBa; NED SB0, 342 Mly
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of 7565 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7389 is about 350 to 355 million light-years away, considerably further away redshift-independent distance estimates of about 195 to 265 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 340 to 345 million light-years away at the time the light by which we see it was emitted, a little over 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 ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 1.4 by 0.9? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7389
Below, a ? arcmin wide ? image of the galaxy

POSITION ID
NGC 7390 (= PGC 69837 = CGCG 430-020 = MCG +02-58-020)
Discovered (Nov 27, 1850) by Bindon Stoney
Also observed (Oct 11, 1873) by John Dreyer
A magnitude 14.2 lenticular galaxy (type S0?) in Pegasus (RA 22 50 19.5, Dec +11 31 52)

Historical Identification: Per Dreyer, NGC 7390 (3rd Lord Rosse, 1860 RA 22 43 24, NPD 79 09.5) is "extremely faint, south of GC 4848", GC 4848 being NGC 7389. The position precesses to RA 22 50 22.7, Dec +11 34 55, but as in the case of 7389, the position is wrong (Gottlieb says "as in the case of 7389, the offsets were wrong". Refer to his and Corwin's notes when correcting this entry).
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case Bindon Stoney.
LEDA G; NED S0?, 360 Mly
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of about 7970 km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that NGC 7390 is about 370 million light-years away, considerably further than a single redshift-independent distance estimate of about 260 to 265 million light-years. Ignoring that problem, 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. Using the recessional velocity implies that the galaxy was about 360 million light-years away at the time the light by which we see it was emitted, about 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 ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 1.0 by 0.7? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7390
Below, a ? arcmin wide ? image of the galaxy

NGC 7391 (= PGC 69847 = UGC 12211 = CGCG 379-008 = MCG +00-58-006)
Discovered (Oct 1, 1785) by William Herschel
Also observed (Sep 12, 1830) by John Herschel
A magnitude 11.9 elliptical galaxy (type E1) in Aquarius (RA 22 50 36.2, Dec -01 32 41)

Historical Identification: Per Dreyer, NGC 7391 (= GC 4849 = JH 2185 = WH II 443, 1860 RA 22 43 24, NPD 92 17.1) is "considerably faint, considerably small, round, suddenly brighter middle equal to a 13th magnitude star, star north-preceding (to the northwest)." The position precesses to RA 22 50 36.3, Dec -01 32 41, essentially dead center on the galaxy listed above, the description fits (except that the north-preceding star is more nearly due north) 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 about 2680 km/sec (and H0 = 70 km/sec/Mpc), NGC 7391 is about 125 million light-years away, considerably closer than redshift-independent distance estimates of about 175 to 320 million light-years. Using the recessional velocity distance and its apparent size of about 1.7 by 1.5 arcmin for the central galaxy and about 2.5 by 2.3 arcmin for its outer halo (from the images below), the galaxy is about 60 to 65 thousand light-years across, while its outer halo spans about 90 thousand light-years.

Above, a 12 arcmin wide SDSS image centered on NGC 7391
Below, a 3 arcmin wide SDSS image of the galaxy

Below, a 4 arcmin wide DESI Legacy image shows a huge halo surrounding the central galaxy
(Image Credit Legacy Surveys / D. Lang (Perimeter Institute); CC 4.0 image by Courtney Seligman using AladinLite)

NGC 7392 (= PGC 69887 = ESO 603-022 = MCG -04-53-040)
Discovered (Sep 11, 1787) by William Herschel
Also observed (Sep 16, 1830) by John Herschel
A magnitude 11.9 spiral galaxy (type SA(rs)ab?) in Aquarius (RA 22 51 48.8, Dec -20 36 29)

Historical Identification: Per Dreyer, NGC 7392 (= GC 4850 = JH 2186 = WH II 702, 1860 RA 22 44 16, NPD 111 21.0) is "pretty bright, pretty small, a little extended 120�, much brighter middle." The position precesses to RA 22 51 48.5, Dec -20 36 31, almost dead center on the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 2840 km/sec (and H0 = 70 km/sec/Mpc), NGC 7392 is about 130 to 135 million light-years away, in good agreement with redshift-independent distance estimates of about 100 to 165 million light-years. Given that and its apparent size of about 2.2 by 1.3 arcmin (from the images below), the galaxy is about 85 thousand light-years across.

Above, a 12 arcmin wide DSS image centered on NGC 7392
Below, a 2.4 arcmin wide DSS image of the galaxy

Below, a 2.4 arcmin wide Carnegie-Irvine image of the galaxy (Image Credit & © Carnegie-Irvine Galaxy Survey; used by permission)

Below, a 1.25 by 0.9 arcmin wide HST image of part of the galaxy (Image Credit Hubble Legacy Archive)

NGC 7393 (= Arp 15) (= PGC 69874 = MCG -01-58-002)
Discovered (Oct 5, 1785) by William Herschel
Also observed (Oct 4, 1828) by John Herschel
A magnitude 12.9 spiral galaxy (type SB(rs)c? pec) in Aquarius (RA 22 51 38.1, Dec -05 33 26)

Historical Identification: Per Dreyer, NGC 7393 (= GC 4851 = JH 2187 = WH II 453, 1860 RA 22 44 22, NPD 96 18.0) is "very faint, pretty large, a little extended, very gradually brighter middle, mottled but not resolved." The position precesses to RA 22 51 38.3, Dec -05 33 31, only 0.1 arcmin below the center of the galaxy listed above and inside the bright central region, the description fits and there is nothing else nearby, so the identification is certain.
LEDA SB(r)c; NED SB(rs)c pec, 158 Mly
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 3395 km/sec (and H0 = 70 km/sec/Mpc), NGC 7393 is about 155 to 160 million light-years away, in fair agreement with redshift-independent distance estimates of about 85 to 140 million light-years. Given that and its apparent size of about ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Based on a recessional velocity of 3765 km/sec, NGC 7393 is about 175 million light years away, in fair agreement with redshift-independent distance estimates of 130 to 140 million light years. Given that and its apparent size of 2.0 by 0.9 arcmin, it is about 100 thousand light years across.

Above, a 12 arcmin wide SDSS image centered on NGC 7393, also known as Arp 15
Below, a 2.4 arcmin wide SDSS image of the galaxy

POSITION ID
NGC 7394 (= "PGC 5067431")
Discovered (Sep 12, 1829) by John Herschel
A group of stars in Lacerta (RA 22 50 12.0, Dec +52 10 08)
Corwin's position is 22 50 08, +52 10.8, with a "core" at 22 50 21, +52 08.3

Historical Identification: Per Dreyer, NGC 7394 (= GC 4852 = JH 2188, 1860 RA 22 44 36, NPD 38 33.9) is "a cluster, very poor." The position precesses to RA 22 50 32.4, Dec +52 10 33, near a scattering of bright stars that might have stood out because the multitude of fainter stars in this part of the Milky Way wouldn't have been visible to Herschel. NEED TO CHECK CORWIN & GOTTLIEB BEFORE SAYING MORE
LEDA "open cluster"; NED "star cluster"
Physical Information: Apparent size 8 by 5? arcmin. Not listed as, but perhaps an open cluster; proper motions would be needed to decide.

RECONCILE LEDA/NED DATA
NGC 7395 (= PGC 69861 = UGC 12216 = CGCG 515-008 = MCG +06-50-006)
Discovered (Sep 4, 1872) by �douard Stephan
A magnitude 13.6 lenticular galaxy (type S0?) in Lacerta (RA 22 51 02.9, Dec +37 05 17)

Historical Identification: Per Dreyer, NGC 7395 (= GC 6091, Stephan list V (#8), 1860 RA 22 44 36, NPD 53 39.3) is "extremely faint, very small, round, brighter middle." The position precesses to RA 22 51 03.1, Dec +37 05 10, only 0.1 arcmin south-southeast of the center of the galaxy listed above and within its "brighter middle", the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: Traditionally, Stephan's discovery date for this object is given as Aug 21, 1873. However, that is the date that Stephan reduced his micrometric position, as subsequently published in his list V. Per his logbooks, he first observed the galaxy on the date shown in the description line (this is typical of his published work; objects that he only observed once rarely ended up in the NGC/IC).
LEDA S0, 3K Vr 5248 km/sec; NED S0?, 3K Vr 5354 km/sec, z 0.0178586 => 244 Mly, 246 Myr
Physical Information: Based on a recessional velocity relative to the Cosmic Background Radiation of ? km/sec (and H0 = 70 km/sec/Mpc), a straightforward calculation indicates that ? is about ? 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 ? million light-years away at the time the light by which we see it was emitted, about ? 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 ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 1.2 by 1.1? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7395
Below, a ? arcmin wide ? image of the galaxy

NGC 7396 (= PGC 69889 = PGC 194157 = UGC 12220 = CGCG 379-010 = MCG +00-58-007)
Discovered (Oct 12, 1827) by John Herschel
A magnitude 12.9 spiral galaxy (type Sa?) in Pisces (RA 22 52 22.6, Dec +01 05 33)

Historical Identification: Per Dreyer, NGC 7396 (= GC 4853 = JH 2189, 1860 RA 22 45 14, NPD 89 39.0) is "pretty faint, pretty small, round, gradually brighter middle." The position precesses to RA 22 52 23.6, Dec +01 05 32, about 0.2 arcmin nearly due east of the center of the galaxy listed above and within the "brighter middle", the description is a good fit for a visual observation and there is nothing else nearby, so the identification is certain.
LEDA Sa; NED Sa pec sp, 119 Mly
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 4560 km/sec (and H0 = 70 km/sec/Mpc), NGC 7396 is about 210 to 215 million light-years away, in good agreement with redshift-independent distance estimates of about 155 to 295 million light-years. Given that and its apparent size of about ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 2.4 by 1.6? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7396
Below, a ? arcmin wide ? image of the galaxy

NGC 7397 (= PGC 69904 = PGC 194217 = CGCG 379-011 = MCG +00-58-008)
Discovered (Oct 2, 1856) by R. J. Mitchell
A magnitude 14.2 lenticular galaxy (type SB0/a?) in Pisces (RA 22 52 46.7, Dec +01 07 58)

Historical Identification: Per Dreyer, NGC 7397 (= GC 4854, 3rd Lord Rosse, 1860 RA 22 45 36, NPD 89 36.7) is "extremely faint, very small." The position preesses to RA 22 52 45.5, Dec +01 07 51, about 0.3 arcmin west-southwest of the center of the galaxy listed above and barely outside its outline, the description fits and the closest other galaxy was also discovered by Mitchell on the same night, so it can be ruled out as a candidate for NGC 7397, and the identification is considered certain.
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case R. J. Mitchell.
LEDA SB0(r)/a; NED SB0(rs)/a
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 4350 km/sec (and H0 = 70 km/sec/Mpc), NGC 7397 is about 200 to 205 million light-years away. Given that and its apparent size of about ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 0.7 by 0.5? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7397
Below, a ? arcmin wide ? image of the galaxy

NGC 7398 (= PGC 69905 = PGC 194223 = UGC 12225 = CGCG 379-012 = MCG +00-58-009)
Discovered (Oct 2, 1856) by R. J. Mitchell
A magnitude 13.6 spiral galaxy (type Sa?) in Pisces (RA 22 52 49.3, Dec +01 12 04)

Historical Identification: Per Dreyer, NGC 7398 (= GC 4855, 3rd Lord Rosse, 1860 RA 22 45 38, NPD 89 32.5) is "very faint, pretty large." The position precesses to RA 22 52 47.5, Dec +01 12 04, about 0.4 arcmin due west of the center of the galaxy listed above, the description fits and the closest other galaxy was also discovered by Mitchell on the same night, so it can be ruled out as a candidate for NGC 7398, and the identification is considered certain.
Discovery Notes: Although Dreyer credits the discovery to William Parsons, 3rd Earl of Rosse, he notes that many of Rosse's nebular discoveries were actually made by one of his assistants, in this case R. J. Mitchell.
LEDA (R)SBa; NED SA(r)a?, roughly 203 Mly
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of about 4365 km/sec (and H0 = 70 km/sec/Mpc), NGC 7398 is about 200 to 205 million light-years away, somewhat closer than widely varying redshift-independent distance estimates of about 220 to 1155(!) million light-years. Given that and its apparent size of about ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 1.2 by 0.8? arcmin.

Above, a 12 arcmin wide ? image centered on NGC 7398
Below, a ? arcmin wide ? image of the galaxy

NGC 7399 (= PGC 69902 = MCG -02-58-006)
Discovered (Nov 15, 1884) by Lewis Swift
Also observed (Jul 1898 to Jun 1899) by Herbert Howe
A magnitude 13.7 lenticular galaxy (type S0/a?) in Aquarius (RA 22 52 39.2, Dec -09 16 04)

Historical Identification: Per Dreyer, NGC 7399 (Swift list II (#93), 1860 RA 22 45 42, NPD 99 59.4) is "extremely faint, pretty large." The second IC lists a corrected RA (per Howe) of 22 45 19. The corrected position precesses to RA 22 52 39.0, Dec -09 14 51, about 1.2 arcmin due north of the galaxy listed above, the description is a reasonable fit and there is nothing else nearby, so the identification is considered certain. (If Dreyer had used Swift's full position, the (1860) declination would have been changed to -10 0.6, and the precessed position would have been RA 22 52 39.1, Dec -09 16 03, nearly dead center on the galaxy.)
LEDA S0/a; NED Sab, S0/a HII
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 4100 km/sec (and H0 = 70 km/sec/Mpc), NGC 7399 is about 190 million light-years away. Given that and its apparent size of about ? arcmin (from the images below), the galaxy is about ? thousand light-years across.
Apparent size 0.9 by 0.4? arcmin.

Above, a 12 arcmin wide SDSS image centered on NGC 7399
Above, a 2.4 arcmin wide SDSS image of the galaxy