Apparent size 0.7 by 0.7 arcmin.

Apparent size 0.7 by 0.3 arcmin.

Per Dreyer, NGC 1002 (Stephan list XII (#21), 1860 RA 02 30 25, NPD 55 59.2) is "very faint, very small, irregularly round, brighter middle and nucleus". The position precesses to RA 02 38 55.1, Dec +34 37 19, right on the galaxy, so the identification is certain. (See NGC 983 for a discussion of the double listing.) Apparent size 1.2 by 0.9 arcmin.

Apparent size 4.7 by 1.3 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SAB(s:)d.

Apparent size 1.4 by 1.2 arcmin.

Apparent size 1.0 by 0.8 arcmin.

Per Dreyer, NGC 1006 (Swift list V (#30), 1860 RA 02 30 38, NPD 101 38.4) is "most extremely faint, pretty small, round, a little brighter middle". The position precesses to RA 02 37 24.9, Dec -11 01 48, but the nearest galaxy of note (NGC 1010) lies about 10s of time to the east. The interesting thing (per Corwin) is that Swift's observation of "NGC 1006" is the same one involved in his corroboration of Stephan's discovery of NGC 1010. The difference is that in assigning a position to NGC 1010 (and for that matter, NGC 1011), Dreyer combined Stephan and Swift's observations with those by Ormond Stone, obtaining "averaged" positions that were very close to the correct ones; but for some unknown reason, in the case of NGC 1006 he used only Swift's position, and since its right ascension was 10s of time too small, ended up with two entries for the same observation. (Given the equivalence of NGC 1006 and 1010, see the latter entry for anything other than historical information.)

Apparent size 0.6 by 0.2 arcmin. (Listed as a peculiar galaxy in several databases, but it looks like a perfectly normal lenticular or spiral galaxy in the images below.)

Apparent size 0.8 by 0.6 arcmin. (for now, see the wide-field image of NGC 1007)

Apparent size 1.4 by 0.2 arcmin.

Per Dreyer, NGC 1010 (GC 5262 = Stephan list VIII (#6), Swift list V (#30), 1860 RA 02 30 49, NPD 101 38.1) is "extremely faint, small, round". The position precesses to RA 02 37 35.9, Dec -11 01 31, right on the galaxy, so the identification is certain. As noted in the NGC entry, Stephan observed this (and NGC 1011 first, and Swift independently discovered the objects (not being aware of Stephan's observations) later. The odd thing is that Swift's single observation of NGC 1010 led to his also being credited with a separate discovery, the duplicate entry NGC 1006 (which see for a historical discussion). Apparent size 0.8 by 0.8 arcmin.

Per Dreyer, NGC 1011 (GC 5263 = Stephan list VIII (#7), Swift list V, 1860 RA 02 30 52, NPD 101 36.9) is "extremely faint, small, round, a little brighter middle". The position precesses to RA 02 37 38.9, Dec -11 00 19, right on the galaxy, so the identification is certain. Apparent size 0.6 by 0.6 arcmin.

Apparent size 2.5 by 1.1 arcmin.

Apparent size 0.8 by 0.6 arcmin.

Per Dreyer, NGC 1014 (Muller list II (#342), 1860 RA 02 31 02, NPD 100 07.9) is "extremely faint, extremely small, irregularly round, preceding (westernmost) of 2", the other being NGC 1018. The position precesses to RA 02 37 52.0, Dec -09 31 21, but there is nothing there. Per Corwin, the key to the identification of NGC 1014 is Muller's statement of its relationship to NGC 1018, which he lists as being 0.2m east and 1' north of NGC 1014. The only thing that Muller could possibly have seen near that position is the double star 9.4s west and 1.8' south of NGC 1018, whose position is the one listed for this entry; so the identification is essentially certain (or as Corwin puts it, the double star is "positively identified" as the object in question). (Given the proximity of the two objects, see the wide-field image of NGC 1018.)

Apparent size 2.0 by 1.7 arcmin.

Apparent size 2.0 by 2.0 arcmin.

Per Dreyer, NGC 1017 (Swift list V (#33), Ormond Stone list I, 1860 RA 02 31 06, NPD 101 35.9) is "most extremely faint, very small, round, very difficult". The position precesses to RA 02 37 52.9, Dec -10 59 21, about 1.4 arcmin northeast of the appropriate galaxy, but since it is one of three nebulae observed on the same night, and all three (NGC 1010, 1011 and 1017) are in about their correct relative places, the identification is certain. Apparent size 0.7 by 0.6 arcmin.

Per Dreyer, NGC 1018 (Muller list II (#343), 1860 RA 02 31 14, NPD 100 06.9) is "extremely faint, very small, extended 180°, following (easternmost) of 2", the other being NGC 1014. The position precesses to RA 02 38 04.0, Dec -09 30 22, but there is nothing there. There is, however, a suitable candidate for what Muller saw, both in brightness and orientation (180° corresponding to a north-south extension) less than 3 arcmin to the southeast, and there is no doubt that it is what Muller observed. This is supported by the fact (as discussed at the entry for NGC 1014) that there is a suitable candidate (albeit only a double star) to the southwest of NGC 1018 for the "preceding of 2", or NGC 1014. So despite the error in the individual positions of the two objects, their relative position and the description of NGC 1018 make their identifications certain. Apparent size 1.0 by 0.6 arcmin.

Apparent size 1.0 by 0.9 arcmin.

Apparent size 0.8 by 0.2 arcmin. (for images, see NGC 1021)

Apparent size 0.7 by 0.5 arcmin.

Apparent size 2.4 by 2.2 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type (R)SB(rs)a pec.

One of the nearest 'early-type' galaxies, with an almost unnoticeable low-surface brightness irregular companion on its eastern side, leading to its designation as Arp 135. Apparent size 7.4 by 2.5 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SB0^-.

Apparent size 1.3 by 0.7 arcmin. A very low-surface brightness companion of NGC 1023, which see for images.

Apparent size 3.9 by 1.5 arcmin.

Apparent size 0.9 by 0.5 arcmin.

Apparent size 1.7 by 1.3 arcmin.

Per Dreyer, NGC 1027 (GC 578 = WH III 66, 1860 RA 02 32 00, NPD 29 03.4) is a "cluster, large, scattered stars, one 10th magnitude", the "10th-magnitude star" actually being 7th-magnitude HD 16626. The position precesses to RA 02 42 46.4, Dec +61 32 46, a bit south of the center of the cluster but well within its boundary, so the identification is certain. (For a discussion of the double listing see IC 1824.) Apparent size 15 arcmin.

Apparent size 0.9 by 0.3 arcmin.

Apparent size 1.4 by 0.4 arcmin. (for now, see the wide-field image of NGC 1028)

Apparent size 1.9 by 0.6 arcmin.

Apparent size 2.1 by 1.0 arcmin.

Apparent size 3.4 by 1.1 arcmin.

Apparent size 1.2 by 1.0 arcmin.

Per Dreyer, NGC 1034 (Leavenworth list I (#55), 1860 RA 02 32 35, NPD 106 24.9) is "very faint, very small, a little extended, a little brighter middle, 2 bright stars 20" preceding (to the west)". The second Index Catalog lists a corrected RA (per Howe) of 02 31 37 and adds "the 2 stars to the west are of only 11th to 12th magnitude". The corrected position precesses to RA 02 38 13.4, Dec -15 48 24, right on the galaxy, so the identification is certain. Apparent size 0.8 by 0.7 arcmin.

Apparent size 2.2 by 0.6 arcmin.

Per Dreyer, NGC 1036 (GC 583 = JH 247 = WH III 475, 1860 RA 02 32 40, NPD 71 19.3) is "faint, small, round, a little brighter middle". The position precesses to RA 02 40 30.9, Dec +19 16 59, less than an arcmin to the southeast of the galaxy, so the identification is certain. Apparent size 1.5 by 1.1 arcmin.

Per Dreyer, NGC 1037 (Swift list 5 (#35), RA 02 32 52, NPD 92 20.3) is "most extremely faint, very small, much extended, very difficult". The position precesses to RA 02 39 58.1, Dec -01 44 00, as shown above, but there is nothing there. Per Corwin, Swift's original notes include the statement "(GC) 581 (= NGC 1032) in the field", which given the half-degree wide field of view for Swift's instrument would mean that NGC 1037 was well within 1/2 degree (and more likely within 1/4 degree) of NGC 1032; but there is nothing within that distance of NGC 1032 that Swift could have seen, and in any event, his position for NGC 1037 is nearly 3 degrees away from NGC 1032, so whatever object Swift thought was nearby was certainly not NGC 1032, and Corwin's original opinion was that NGC 1037 was lost. However, in a more recent post he mentions that others have suggested that perhaps PGC 9973, a couple of minutes west and not quite 7 arcmin to the south of Swift's position might be what Swift saw, and there is a faint galaxy off to its west (PGC 9936) that is close enough that Swift might have confused it with NGC 1032 (though only if he had no idea how much brighter that galaxy is than either of the PGC objects). Corwin considers that a reasonable possibility if one only considers the typical errors in Swift's positions, but cannot see how to reconcile any suggestion involving NGC 1032, whether that galaxy or an impostor, with the 3 degree difference between its position and the one Swift measured for NGC 1037. So he finally concludes that although other suggestions might have some merit, none of them are convincing enough to change his mind about the status of NGC 1037 as a "lost" object; and most of those who suggested other possibilities seem to have abandoned their positions and sided with Corwin, so although some places (such as Wikisky) still identify PGC 9973 as NGC 1037, they are in a very limited minority. Despite that, since there remain any suggestions that PGC 9936 might be NGC 1037, that object is discussed immediately following this entry.

As discussed at the entry for NGC 1037, PGC 9973 is sometimes (almost certainly incorrectly) identified as NGC 1037. Apparent size 1.7 by 0.9 arcmin.

Apparent size 1.2 by 0.4 arcmin.

Per Dreyer, NGC 1039 (= Messier 34, 1860 RA 02 33 02, NPD 47 49.4) is a "cluster, bright, very large, slightly compressed, scattered 9th-magnitude stars". (Note: See the discussion of Hodierna for an explanation of why he was not credited with the discovery of this object.) The position precesses to RA 02 42 01.0, Dec +42 46 45, about 2 arcmin southwest of the center of the cluster, but essentially dead center in comparison to its apparent size of 30 or so arcmin, so the identification is certain. M34 consists of a hundred or so stars formed at the same time, about 200 million years ago. At its distance of about 1400 light years, its apparent size corresponds to a 15 light year diameter . An easy object to observe with binoculars or a small telescope, M34 will gradually disintegrate as it moves around the galaxy due to the gravitational effects of passing stars and star clusters. More massive clusters can survive such interactions for long periods of time, but small ones like M34 don't remain a cluster for more than a few hundred million years. However, even after the cluster's stars have been completely scattered, they will continue to live out their lives, unaffected by the loss of their siblings.

Per Dreyer, NGC 1040 (GC 5271 = Stephan list III (#18), 1860 RA 02 33 18, NPD 49 06.0) is "faint, small, brighter middle". The position precesses to RA 02 42 12.3, Dec +41 30 08, but there is nothing there. There is, however, a suitable candidate (= NGC 1053, which see for anything other than historical information) exactly 1m of time to the east, which (per Corwin) was suggested by Reinmuth as being the object Stephan observed. As Corwin notes, it is ironic that Stephan, who usually made very accurate measurements, was in this case outdone by Swift, who often made poor measurements; but an examination of Stephan's original notes shows that he made at least one careless error in recording the observation (misidentifying the comparison star by a single digit), so a similar error in the right ascension (namely, the 1m of time) would not be at all surprising. As a result, although Stephan's error led to a double listing and to Swift's observation taking precedence, the equivalence of the two listings is certain. Note: This object was initially known only as NGC 1053, because NGC 1040 appeared to be "lost" (as discussed above); but since Reinmuth noted the equivalence of the two entries nearly a century ago, it is now referred to as NGC 1040 almost as often as NGC 1053.

Apparent size 1.7 by 1.3 arcmin.

Apparent size 6.0 by 4.3 arcmin. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SAB(s)c.

Apparent size 0.9 by 0.2 arcmin.

Part of a physical pair with PGC 3080165, and probably associated with NGC 1046. Vr 6235 km/sec. Apparent size 1.1 by 0.8 arcmin.

Vr 6415 km/sec. Apparent size 0.4 by 0.3 arcmin. Part of a physical pair with NGC 1044, which see for images.

Apparent size 1.6 by 1.2 arcmin.

Vr = 6045 km/sec. Apparent size 0.9 by 0.9 arcmin. Probably a companion of NGC 1044.

Per Dreyer, NGC 1047 (Swift list III (#18), 1860 RA 02 33 47, NPD 98 46.0) is "most extremely faint, pretty small, round, very difficult". The position precesses to RA 02 40 39.6, Dec -08 09 48, about 2 arcmin southeast of the 14th-magnitude galaxy which is presumed to be his discovery, as there is nothing else near, and the identification seems certain. Apparent size 1.3 by 0.6 arcmin.

Per Dreyer, NGC 1048 (Swift list III (#19), 1860 RA 02 33 47, NPD 99 08.9) is "most extremely faint, pretty small, round, southeastern of 2", the other one being NGC 1042. The position precesses to RA 02 40 38.8, Dec -08 32 42, almost exactly on the pair of faint galaxies. Odds are that what Swift saw was the combined light of the pair, rather than either of them individually; so it seems most appropriate to treat the pair as the NGC object and each of the galaxies as individual components of the pair, and that has been the usual practice (though it seems to be fairly common to list NGC 1048B as simply NGC 1048). The apparent size of PGC 10137 is 0.7 by 0.4 arcmin; of PGC 10140, 1.0 by 0.3 arcmin.

Apparent size 1.2 arcmin. NGC 1049 is the brightest of six globular clusters in the Fornax dwarf galaxy, a satellite of our Milky Way galaxy, and as noted above was discovered in 1835, whereas the galaxy itself was not noticed until 1938, more than a century later.