Per Dreyer, NGC 250 (Swift list III (#2), 1860 RA 00 40 18, NPD 82 52.0) is "extremely faint, very small, round, among 3 stars". The position precesses to RA 00 47 33.0, Dec +07 53 55, a little over 4 arcmin east of the galaxy, but the position of the galaxy (near the center of a right triangle formed by three stars) so perfectly matches the description that the identification is certain. Apparent size 1.1 by 0.6 arcmin.

Apparent size 2.4 by 1.9 arcmin.

Per Dreyer, NGC 252 (GC 136 = GC 139, JH 59 = JH 60, WH II 609, 1860 RA 00 40 33, NPD 63 08.6) is "pretty bright, small, round, pretty much brighter middle, mottled but not resolved into stars, double star to the west". The position precesses to RA 00 48 01.8, Dec +27 37 18, almost dead center on the galaxy, so the identification is certain. Apparent size 2.1 by 1.5 arcmin.

Apparent size 25 by 5.5 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SAB(s)c.

Apparent size 2.6 by 1.7 arcmin.

Apparent size 3.1 by 2.7 arcmin.

Apparent size 0.6 arcmin.

Apparent size 1.9 by 1.3 arcmin.

Per Dreyer, NGC 258 (GC 137, 3rd Lord Rosse, 1860 RA 00 40 50, NPD 63 07) is "extremely faint, small, very faint star close". The position precesses to RA 00 48 18.9, Dec +27 38 54, about one and a half arcmin southeast of the galaxy, but there is nothing else nearby, and the nearby star makes the identification certain.

Apparent size 2.9 by 0.6 arcmin.

Per Dreyer, NGC 260 (GC 5118, d'Arrest, 1860 RA 00 41 08, NPD 63 04.8) is "extremely faint, pretty small, a little extended". The position precesses to RA 00 48 37.1, Dec +27 41 05, only about half an arcmin southeast of the galaxy, so the identification is certain. Apparent size 0.8 by 0.8 arcmin.

Apparent size 1.9 arcmin.

Per Dreyer, NGC 262 (Swift list II (#10), 1860 RA 00 41 29, NPD 58 48.4) is "extremely faint, very small, round, very difficult". The second Index Catalog lists a corrected RA (per Bigourdan) of 00 41 15. The corrected position precesses to RA 00 48 47.7, Dec +31 57 29, dead center on the galaxy, so the identification is certain. Apparent size 1.1 by 1.1 arcmin.

Apparent size 0.7 by 0.3 arcmin.

Apparent size 1.1 by 0.3 arcmin.

Apparent size 1.0 arcmin. About two hundred thousand light-years distant, in the Small Magellanic Cloud, are the 12th-magnitude open clusters NGC 265 and NGC 290. Each cluster spans about 65 light years, and contains hundreds or thousands of brilliant young stars. Most of the stars in these images are not cluster members, but lie in front of (in our own galaxy or the Small Magellanic Cloud) or behind (in the Small Magellanic Cloud) the clusters.

Apparent size 3.0 by 2.9 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SB(rs)ab.

Apparent size 2.5 arcmin.

Apparent size 1.6 by 1.1 arcmin.

Apparent size 0.6 arcmin.

Apparent size 1.7 by 1.2 arcmin.

Apparent size 2.2 by 1.7 arcmin.

Apparent size 5.0 arcmin.

Apparent size 2.1 by 0.6 arcmin.

Apparent size 1.4 by 1.2 arcmin.

Apparent size 1.5 by 1.2 arcmin. Paired with NGC 274, which see for images.

Per Dreyer, NGC 276 (Muller list II (#294), 1860 RA 00 44 01, NPD 113 27.9) is "extremely faint, pretty small, extended 265°, 11th-magnitude star 3' north". The second Index Catalog lists a corrected RA (per Howe) of 00 45 14, and adds "the star to the northeast is an 8th magnitude close double". The corrected position precesses to RA 00 52 07.5, Dec -22 42 10, about 1.3 arcmin south of the galaxy, but there is nothing else nearby, and the double star makes the identification certain. Apparent size 1.0 by 0.4 arcmin.

Apparent size 1.4 by 1.2 arcmin.

Apparent size 2.1 by 2.0 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SA(rs)b.

Apparent size 1.6 by 1.2 arcmin.

Apparent size 1.7 by 1.1 arcmin.

The nebula is about 10 thousand light years away, and based on its 40 arcmin apparent size, a little over 100 light years across. It is associated with open cluster OCL 313.

Apparent size 1.0 by 0.9 arcmin.

Per Dreyer, NGC 283 (Leavenworth list I (#14), 1860 RA 00 45 30, NPD 103 55.8) is "extremely faint, small, round, the 1st of 4", the others being NGC 284, 285 and 286, all of which have identical positions and descriptions in the original NGC. The second Index Catalog lists a corrected position (per Howe) of RA 00 46 14, NPD 103 55.5. That precesses to RA 00 53 14.6, Dec -13 09 49, right on the galaxy, so the identification is certain. Apparent size 1.6 by 1.0 arcmin.

Per Dreyer, NGC 284 (Leavenworth list I (#15), 1860 RA 00 45 30, NPD 103 55.8) is "extremely faint, small, round, the 2nd of 4", the others being NGC 283, 285 and 286, all of which have identical positions and descriptions in the original NGC. The second Index Catalog lists a corrected position (per Howe) of RA 00 46 25, NPD 103 55.2. That precesses to RA 00 53 25.5, Dec -13 09 32, right on the galaxy, so the identification is certain. Apparent size 0.6 by 0.5 arcmin.

Per Dreyer, NGC 285 (Leavenworth list I (#16), 1860 RA 00 45 30, NPD 103 55.8) is "extremely faint, small, round, the 3rd of 4", the others being NGC 283, 284 and 286, all of which have identical positions and descriptions in the original NGC. The second Index Catalog lists a corrected position (per Howe) of RA 00 46 31, NPD 103 55.2. That precesses to RA 00 53 31.5, Dec -13 09 32, right on the galaxy, so the identification is certain. Apparent size 0.7 by 0.4 arcmin.

Per Dreyer, NGC 286 (Leavenworth list I (#17), 1860 RA 00 45 30, NPD 103 55.8) is "extremely faint, small, round, the 4th of 4", the others being NGC 283, 284 and 285, all of which have identical positions and descriptions in the original NGC. The second Index Catalog lists a corrected position (per Howe) of RA 00 46 31, NPD 103 52.4. That precesses to RA 00 53 31.5, Dec -13 06 44, right on the galaxy, so the identification is certain. Apparent size 1.3 by 0.9 arcmin.

Apparent size 0.8 by 0.4 arcmin.

Apparent size 13 arcmin.

The brighter portion of NGC 289 appears to be a more or less normal spiral galaxy about 3.1 by 2.5 arcmin across; but its wispy outer arms extend across a more than 9.5 by 7.5 arcmin wide region. A faint elliptically shaped area on one of the northern arms may be a large star-forming region, or an elliptical companion whose interaction with the larger galaxy is responsible for its appearance. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SB(rs)bc.

Apparent size 0.8 arcmin. About two hundred thousand light-years distant, in the Small Magellanic Cloud, are the 12th-magnitude open clusters NGC 265 and NGC 290. Each cluster spans about 65 light years, and contains hundreds or thousands of brilliant young stars. Most of the stars in these images are not cluster members, but lie in front of (in our own galaxy or the Small Magellanic Cloud) or behind (in the Small Magellanic Cloud) the clusters.

Apparent size 1.1 by 0.6 arcmin.

The Small Magellanic Cloud is a satellite or companion of our Milky Way Galaxy. Its recessional velocity of 158 km/sec is too small, in comparison to normal peculiar velocities (non-Hubble-redshift motions) to provide a reasonable estimate of distance. Redshift-independent distance estimates range from 160 to 250 thousand light years distance. At that distance, the SMC's apparent size of 315 by 235 arcmins implies a diameter of 18 thousand light years.

Apparent size 1.1 by 0.9 arcmin.

Apparent size 0.8 arcmin.

Per Dreyer, NGC 295 (GC 5123, Copeland using Lord Rosse's 6-foot reflector, 1860 RA 00 47 30, NPD 59 13.8) is "faint, small, round, star 10 arcsec north, II 214 northeast", II 214 being NGC 296. The position precesses to RA 00 55 05.4, Dec +31 31 49, whence the position listed above, but there is nothing there, save for NGC 296 (which must be there, since Copeland measured the position relative to what he thought was that nebula). As a result, NGC 295 has long been (and still is, in some places) thought to be the galaxy that should be listed as NGC 296, and that galaxy was thought to be lost, which is the exact opposite of the truth. Per Corwin, Copeland thought he was observing NGC 296 and another galaxy near it, but it is now clear that he must have been observing a different pair of galaxies, as his description (posted at the end of this entry) does not match anything in the field. To date, no one has found out which galaxies, but Copeland's notes may enable a future search for suitable candidates. For the presumed but incorrect NGC 296 he wrote: "faint, round, 10th-magnitude yellow star at position angle 29.6 degrees, 123.1 arcsec distant". For the "Nova" that became NGC 295 he wrote: "small, round, with a star or another nebula 10 arcsec north. Position angle from (the erroneous NGC 296) 242.0 degrees, 314.6 arcsec distant, or 21.6 seconds of time to the west and 147.6 arcsec south".

Above, a 12 arcmin wide view of spiral galaxy NGC 296 and Herschel and Copeland's positions for NGC 296 and 295 makes it appear that the galaxy should be Copeland's NGC 295, and not Herschel's NGC 296; and that was thought to be the case for a long time. But Copeland's description of the field does not match the galaxy, whereas Herschel's does; so it is now believed that the galaxy is NGC 296, and NGC 295 is lost or nonexistent.

Per Dreyer, NGC 296 (GC 167, WH II 214, 1860 RA 00 47 52, NPD 59 11.3) is "faint, a little extended, 10th magnitude star 2' to northeast" (note: in the copy of the NGC available to me 'a little extended', which should be lE, looks like lF, probably due to a damaged piece of type). The position precesses to RA 00 55 27.6, Dec +31 34 38, about 20s of time east-northeast of the correct position. That is close enough to the galaxy that it might have been easily identified as NGC 296 save for one thing, namely the 10th-magnitude star supposedly 2' to the northeast, which does not match the galaxy at all. Per Corwin, the problem is the entry for Copeland's NGC 295 (which see for more about the confounding of these entries), whose incorrect position is considerably closer to the correct NGC 296 than Herschel's position, leading to the presumption that NGC 295 was the galaxy now identified as NGC 296, and Herschel's object was lost or nonexistent. This incorrect identification was aided by Dreyer's description, which is not that of either William or John Herschel, but an amalgamation of their descriptions and the one for NGC 295 by Copeland (which as just noted was presumed to be "this" galaxy). The two Herschel's descriptions, though slightly different, agree that WH II 214 is "faint, extended, with a bright star to the east (and very near)". That is a perfect description of PGC 3260, and despite the error in Herschel's position, makes it certain that NGC 296 is the galaxy formerly identified as NGC 295. Apparent size 2.2 by 1.0 arcmin.

Apparent size 0.3 by 0.2 arcmin. Very close to NGC 298, which see for images.

Apparent size 1.7 by 0.4 arcmin.

Apparent size 0.7 arcmin.