Per Dreyer, IC 1 (= Bigourdan 103, 1860 RA 00 01 15, NPD 63 04) is a "double star, magnitudes 13 and 13, one with nebulosity". The position precesses to 0.4 arcmin below the pair of stars identified as IC 1, so there is little doubt of the identification. The position listed above is halfway between the stars. The image below shows a 12 arcmin wide region centered on the pair.

Per Dreyer, IC 2 (= Javelle 1, 1860 RA 00 03 52, NPD 103 36.2) is "faint, small, brighter middle". The position precesses to the correct position, so there is no doubt of the identification. Based on recessional velocity of 6775 km/sec, about 300 million light years away. Given that and apparent size of 0.7 by 0.15 arcmins, about 60 thousand light years in diameter.

Per Dreyer, IC 3 (= Javelle 2, 1860 RA 00 04 56, NPD 91 12.1) is "faint, very small, irregular figure, mottled but not resolved". The position precesses to less than half an arcminute south of the galaxy, so there is no doubt of the identification. Based on recessional velocity of 5435 km/sec, about 245 million light years away. Given that and apparent size of 1.0 by 0.6 arcmin, about 70 thousand light years across.

Per Dreyer, IC 4 (= Pechüle 3259, 1860 RA 00 06 15, NPD 73 20.6) is "very faint, very small, round". The position precesses to the correct position, so there is no doubt of the identification. Based on recessional velocity of 5005 km/sec, about 225 million light years away. Given that and apparent size of 1.0 by 0.9 arcmin, about 65 thousand light years across.

Per Dreyer, IC 5 (= Javelle 3, 1860 RA 00 10 27, NPD 100 19.1) is "faint, nebula, 13th-magnitude star". The position precesses to within 0.2 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 6720 km/sec, about 300 million light years away. Given that and apparent size of 1.0 by 0.7 arcmin, about 85 thousand light years across.

Per Dreyer, IC 6 (= Javelle 4, 1860 RA 00 11 46, NPD 94 03.2) is "faint, very small, round, much brighter middle equivalent to 14th-magnitude star". The position precesses to the correct position, so there is no doubt of the identification. Based on recessional velocity of 6185 km/sec, about 275 million light years away. Given that and apparent size of 1.0 by 1.0 arcmin, about 80 thousand light years across.

Per Dreyer, IC 7 (= Javelle 506, 1860 RA 00 11 51, NPD 80 13.8) is "faint, very small, round, 12.5 magnitude star close by". The position precesses to 10 sec east and 3 arcmin south of the galaxy's position. However, given the description (especially the nearby star), the identification seems certain. Based on recessional velocity of 5365 km/sec, about 240 million light years away. Given that and apparent size of 0.65 by 0.6 arcmin, about 45 thousand light years across.

Per Dreyer, IC 8 (= Safford 89 and Javelle 5, 1860 RA 00 11 54, NPD 93 59.9), is "very faint, very small, irregularly extended, slightly brighter middle". The position precesses to the correct position, so there is no doubt of the identification. Based on recessional velocity of 6000 km/sec, about 265 million light years away. Given that and apparent size of 0.7 by 0.35 arcmin, about 55 thousand light years across.

Per Dreyer, IC 9 (= Javelle 6, 1860 RA 00 12 37, NPD 104 54.1) is "very faint, pretty large, round". The position precesses to within 0.1 arcmin of the correct position, so there is no doubt of the identification. A Seyfert galaxy (type Sy2). Based on recessional velocity of 12555 km/sec, about 560 million light years away. Given that and apparent size of 0.4 by 0.3 arcmin, about 65 thousand light years across.

Per Dreyer, IC 10 (= Swift list VII (#1), 1860 RA 00 12 44, NPD 31 28) is a "faint star involved in extremely faint, very large nebula". The position precesses to within half an arc minute of the current catalog position, which is less than ten percent of the apparent size of the galaxy, so there is no doubt of the identification. Dwarf galaxy IC10 is a member of the Local Group. Given its proximity, its recessional velocity should be a poor indicator of its distance, and in fact, it has a negative radial velocity (-350 km/sec), meaning that it is getting closer to us, not further away, so its distance can only be determined by redshift-independent methods. Those yield distance estimates of 2 to 3 million light years, about the same as the Andromeda Galaxy. Given the uncertainty in its distance, its 7 by 6 arcmin apparent size implies that it is 4 to 6 thousand light years across. The galaxy is considerably dimmed by intervening clouds of gas and dust in the plane of our own galaxy, the Milky Way. IC10 is the closest example of a "starburst" galaxy, in which numerous hot, bright, massive stars have recently formed (the false-color reddish glow in the NOAO image represents radiation emitted by clouds of hydrogen heated by nearby stars). One such star raced through its life, and after dying in a supernova explosion, became the most massive stellar black hole currently known -- between 24 and 33 times the mass of the Sun. The black hole was detected by X-radiation emitted when mass ejected by its companion, a Wolf-Rayet star destined to become a future supernova, was pulled into the black hole's accretion disk.

Per Dreyer, IC 11 (= Barnard, 1860 RA 00 13 00, NPD 34 11) is "very faint, large, triple star on northwest corner". As shown in the image below, there are no nebular objects near the position recorded by Dreyer (precessed above, to the equinox of 2000). However, Corwin says that the mention of a triple star suggests that this was a rediscovery of an object observed by Barnard in 1881 (and later listed as NGC 281), with a half-hour error by Barnard in transcribing the right ascension of the later observation, which would put it within the outer reaches of that nebula; hence the tentative identification above.

Above, a 12 arcmin wide region centered on the position recorded by Barnard; the "bright" star is 7th-magnitude HD 1598. Per Corwin's suggestion, also see NGC 281.

Per Dreyer, IC 12 (= Javelle 7, 1860 RA 00 13 06, NPD 93 26.2) is "pretty faint, small, extended north and south". The position precesses to within 0.3 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 6045 km/sec, about 270 million light years away. Given that and apparent size of 0.7 by 0.25 arcmin, about 55 thousand light years across.

Per Dreyer, IC 13 (= Javelle 507, 1860 RA 00 13 08, NPD 83 04.9) is "very faint, pretty large, extended north and south, diffuse". The position precesses to within 0.3 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 5710 km/sec, about 255 million light years away, in reasonable agreement with redshift-independent distance estimates of 195 to 245 million light years. Given that and apparent size of 1.4 by 0.5 arcmin, about 100 thousand light years across.

Per Dreyer, IC 14 (= Bigourdan 104, 1860 RA 00 15 22, NPD 80 18) is a "suspected nebula". The position precesses to RA 00 22 35, Dec +10 28 37, which is an empty area to the southeast of the position noted above, and according to Thomson, Bigourdan was unable to find his object on two subsequent occasions, so his "observation" was probably the result of trying to see more than could be seen. However, Thomson's precession of Bigourdan's measurement is RA 00 22 32, Dec +10 28 49, which is more nearly below the double star, and Corwin suggests that the pair may be what Bigourdan saw, hence the tentative identification above. Thomson disagrees, saying that if the double star were the object, Bigourdan should have easily found it again, since the pair is directly to the east of a fairly bright nebula (NGC 95) which Bigourdan also observed. So although the double star may be Bigourdan's object, it is just as likely (or even more likely) that IC 14 does not exist.

Above, a 12 arcmin wide region centered on the double star which may or may not be IC 14. The small + sign more or less below the star is Bigourdan's position per Thomson, while the larger + sign to the left of that is the position recorded by Dreyer, updated to the 2000 equinox with the NED precession engine. NGC 95 is also shown, to the west.

Per Dreyer, IC 15 (= Javelle 8, 1860 RA 00 20 48, NPD 90 50.7) is "very faint, very small, irregular figure, suddenly brighter middle". The position precesses to within 0.5 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 13805 km/sec, about 600 million light years away. Given that and apparent size of 0.45 by 0.4 arcmins, about 80 thousand light years in diameter.

Per Dreyer, IC 16 (= Javelle 9, 1860 RA 00 21 02, NPD 103 52.6) is "pretty bright, round, brighter middle". The position precesses to within 0.5 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 4845 km/sec, about 215 million light years away. Given that and apparent size of 0.5 by 0.3 arcmins, about 30 thousand light years in diameter.

Per Dreyer, IC 17 (= Javelle 10, 1860 RA 00 21 18, NPD 88 07.8) is "pretty bright, very small, round, stellar". The position precesses to within 0.2 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 4315 km/sec, about 190 million light years away. Given that and apparent size of 0.4 by 0.3 arcmins, about 20 thousand light years in diameter.

Per Dreyer, IC 18 (= Javelle 11, 1860 RA 00 21 29, NPD 102 21.6) is "pretty faint, small, irregular figure, gradually brighter middle". The position precesses to within 0.1 arcmin of the correct position, so there is no doubt of the identification. Also referred to as Arp 100, with a long tail extending to the north, and a shorter antitail to the south, presumably due to gravitational interaction with IC 19, which see. Based on recessional velocity of 6070 km/sec, about 270 million light years away. Given that and apparent size of 0.6 by 0.4 arcmins, about 45 thousand light years in diameter. However, with the northern tail (and fainter southern antitail), the outer limits of the galaxy extend an additional 100 thousand light years.

Per Dreyer, IC 19 (= Javelle 12, 1860 RA 00 21 33, NPD 102 24.9) is "round, small, stellar appearance equivalent to 14th-magnitude star". The position precesses to within half an arcmin or so of the correct position, so there is no doubt of the identification. Also referred to, in combination with the peculiar galaxy IC 18, as Arp 100, because their gravitational interaction is presumed responsible for the distorted appearance of the other galaxy. Based on recessional velocity of 6195 km/sec, about 275 million light years away, or essentially the same distance as IC 18. Given that and apparent size of 0.6 by 0.4 arcmins, about 45 thousand light years in diameter.

Per Dreyer, IC 20 (= Javelle 13, 1860 RA 00 21 35, NPD 103 47.5) is "pretty bright, round". The position precesses to within 0.4 arcmin of the correct position, and most of the error is due to an error in the position of Javelle's reference star, so there is no doubt of the identification. Based on recessional velocity of 7780 km/sec, about 350 million light years away. Given that and apparent size of 0.6 by 0.6 arcmins, about 60 thousand light years across.

Per Dreyer, IC 21 (= Javelle 14, 1860 RA 00 22 01, NPD 90 56.3) is "pretty bright, very small, irregular figure". The position precesses to within 0.3 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 18180 km/sec, about 810 million light years away (and as noted in the next entry, probably gravitationally bound to the smaller galaxy shown in the closeup image). Given that and apparent size of 0.5 by 0.45 arcmins, about 120 thousand light years across.

Based on recessional velocity of 18150 km/sec, about 810 million light years away, and probably gravitationally bound to IC 21, which see for images. Given that and apparent size of 0.25 by 0.2 arcmins, about 60 thousand light years across.

Per Dreyer, IC 22 (= Javelle 15, 1860 RA 00 22 27, NPD 99 51.5) is "faint, small, slightly brighter middle, mottled but not resolved". The position precesses to within 0.2 arcmin of the correct position, so there is no doubt of the identification. Based on recessional velocity of 6075 km/sec, about 270 million light years away. Given that and apparent size of 0.8 by 0.45 arcmins, about 65 thousand light years across.

Per Dreyer, IC 23 (= Javelle 16, 1860 RA 00 23 47, NPD 103 30.4) is "pretty bright, small, round, brighter middle". The position precesses to a point one second of time and 0.7 arcmin to the southeast of the correct position, but there is nothing near that position save for the galaxy currently identified as IC 23; so the identification seems certain. Based on recessional velocity of 6135 km/sec, about 275 million light years away. Given that and apparent size of 0.6 by 0.6 arcmins, about 50 thousand light years across.

Per Dreyer, IC 24 (= Bigourdan 105, 1860 RA 00 23 51, NPD 59 56) is "small, cluster, 30 to 40 seconds of arc, possible nebulosity". The cataloged position precesses to 3 seconds west of a double star, but Malcolm Thomson's precession of Bigourdan's position agrees almost exactly with the double, so the identification seems certain. Although the original listing was for a cluster with some nebulosity, Bigourdan often "saw" more in his plates than was actually there; and although he discovered many nebulae, he also recorded many stellar objects as having nebulosity which does not exist. (The pair is close to NGC 140, so the wide-field image for that galaxy is used here.)

Per Dreyer, IC 25 (= Javelle 17, 1860 RA 00 24 03, NPD 91 10.1) is "faint, very small, irregularly round, very slightly brighter middle, mottled but not resolved". The position precesses to 0.75 arcmin north of the correct position, but there is nothing near that position save for the galaxy currently identified as IC 25, so the identification seems certain. Based on recessional velocity of 5825 km/sec, about 260 million light years away. Given that and apparent size of 0.85 by 0.45 arcmin, about 65 thousand light years across.

Per Dreyer, IC 26 (= Javelle 18, 1860 RA 00 24 41, NPD 104 06.8) is "faint, small, round, gradually brighter middle". Javelle's position precesses to the correct value, but Leavenworth's position for NGC 135 was off by more than a minute of right ascension; hence the double listing by Dreyer. An observation a few years later by Herbert Howe showed that the two objects were actually the same.

Per Dreyer, IC 27 (= Javelle 19, 1860 RA 00 26 02, NPD 104 08.8) is "faint, very small, slightly extended east and west, brighter middle". The position precesses to within 0.1 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 7030 km/sec, about 315 million light years away. Given that and apparent size of 0.6 by 0.55 arcmin, about 55 thousand light years across.

Per Dreyer, IC 28 (= Javelle 20, 1860 RA 00 26 04, NPD 104 13.7) is "very faint, diffuse, very slightly brighter middle". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 6380 km/sec, about 285 million light years away. Given that and apparent size of 0.4 by 0.2 arcmin, about 35 thousand light years across.

Per Dreyer, IC 29 (= Javelle 21, 1860 RA 00 27 01, NPD 92 57.2) is "very faint, small, round, slightly brighter middle". The position precesses to within 0.3 arcmin of the correct position, so the identification is certain. Apparent size 0.6 by 0.6 arcmin; apparently nothing else available.

Per Dreyer, IC 30 (= Javelle 22, 1860 RA 00 27 05, NPD 92 51.5) is "very faint, small, round, slightly brighter middle". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 24600 km/sec, about 1.1 billion light years away. Given that and apparent size of 0.4 by 0.2 arcmin, about 130 thousand light years across.

Per Dreyer, IC 31 (= Javelle 508, 1860 RA 00 27 09, NPD 78 30.1) is "faint, extended east and west, diffuse". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 9520 km/sec, about 425 million light years away. Given that and apparent size of 1.6 by 0.3 arcmin, about 200 thousand light years across.

Per Dreyer, IC 32 (= Javelle 23, RA 00 27 52, NPD 92 55.2) is "very faint, very small, round, slightly brighter middle". The position precesses to within 0.4 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 16495 km/sec, about 735 million light years away. Given that and apparent size of 0.6 by 0.4 arcmin, about 130 thousand light years across. Given their nearly identical direction and distance, IC 32 and 33 may be a gravitationally bound pair.

Per Dreyer, IC 33 (= Javelle 24, 1860 RA 00 27 56, NPD 92 54.8) is "very faint, very small, round, slightly brighter middle". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 16680 km/sec, about 745 million light years away. Given that and apparent size of 0.8 by 0.6 arcmin, about 175 thousand light years across. Given their nearly identical direction and distance, IC 32 and 33 may be a gravitationally bound pair.

Per Dreyer, IC 34 (= Safford 97 and Swift list IX, 1860 RA 00 28 22, NPD 81 38.2) is "very faint, pretty small, slightly extended". The position precesses to within 0.5 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 5340 km/sec, about 240 million light years away, in good agreement with redshift-independent distance estimates of 245 to 265 million light years. Given that and apparent size of 2.8 by 1.0 arcmin, about 200 thousand light years across.

Per Dreyer, IC 35 (= Javelle 509, 1860 RA 00 30 26, NPD 80 24.8) is "very faint, small, diffuse, 9.5 magnitude star to northeast". The position precesses to within 0.3 arcmin of the correct position, and there is such a star to the northeast, so the identification is certain. Based on recessional velocity of 4585 km/sec, about 200 million light years away. Given that and apparent size of 1.0 by 0.8 arcmin, about 60 thousand light years across.

Per Dreyer, IC 36 (= Javelle 25, 1860 RA 00 30 47, NPD 106 12.6) is "faint, very small, round, diffuse". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 6960 km/sec, about 310 million light years away. Given that and apparent size of 0.55 by 0.5 arcmin, about 50 thousand light years across.

Per Dreyer, IC 37 (= Javelle 26, 1860 RA 00 31 32, NPD 106 08.1) is "extremely faint, very small, round, diffuse". The position precesses to within 0.3 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 16160 km/sec, about 720 million light years away. Given that and apparent size of 0.7 by 0.4 arcmin, about 150 thousand light years across. Since it has nearly the same direction and distance as IC 38, they may be a gravitationally bound pair.

Per Dreyer, IC 38 (= Javelle 27, 1860 RA 00 31 37, NPD 106 11.8) is "faint, small, round". The position precesses to within 0.4 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 16355 km/sec, about 730 million light years away. Given that and apparent size of 0.8 by 0.55 arcmin, about 170 thousand light years across. Since it has nearly the same direction and distance as IC 37, they may be a gravitationally bound pair (which might explain the apparent distortion in the structure of IC 38).

Per Dreyer, IC 39 (= Javelle 28, 1860 RA 00 32 05, NPD 104 56.4) is "pretty bright, pretty large, extended north and south, gradually brighter middle". Per Corwin: Javelle's position for IC 39 is accurate, but Stone's position for NGC 178 was off by a minute and a half of right ascension; hence the double listing by Dreyer. An observation a few years later by Howe corrected Stone's position, but the resulting identity with IC 39 "was not published until one of the Helwan observers noticed it". Corwin does not state who the Helwan observers are, but the reference is presumably to the Cairo observatory of that name.

Per Dreyer, IC 40 (= Javelle 510, 1860 RA 00 32 12, NPD 88 18.6) is "faint, small, round, gradually brighter middle with nucleus equivalent to 13.5 magnitude star". The position precesses to 0.5 arcmin east of the correct position, but there is nothing else nearby, so the identification is certain. Based on recessional velocity of 5415 km/sec, about 240 million light years away. Given that and apparent size of 1.1 by 0.5 arcmin, about 75 thousand light years across.

Per Dreyer, IC 41 (= Javelle 29, 1860 RA 00 32 38, NPD 104 56.6) is "very faint, small, diffuse". The position precesses to within 0.1 arcmin of the correct position, so the identification is certain. Per Malcolm Thomson: Several references (including HyperLeda and Wikisky) equate IC 41 with NGC 207, but this is wrong, as shown in the wide-field image below. Based on recessional velocity of 3960 km/sec, about 175 million light years away. Given that and apparent size of 0.7 by 0.5 arcmin, about 35 thousand light years across.

Per Dreyer, IC 42 (= Javelle 30, 1860 RA 00 34 04, NPD 106 11.8) is "small, irregular, very diffuse". The position precesses to within 0.1 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 16410 km/sec, about 730 million light years away. Given that and apparent size of 0.6 by 0.4 arcmin, about 130 thousand light years across.

Per Dreyer, IC 43 (= Bigourdan 106, 1860 RA 00 34 52, NPD 61 07) is "very faint, small, much brighter middle". The position precesses to 0.7 arcmin northwest of the correct position, but given the galaxy's size is within its border, and the bright core makes the identification certain. Based on a recessional velocity of 4855 km/sec, about 215 million light years away. Given that and apparent size of 1.6 by 1.4 arcmin, about 100 thousand light years across.

Per Dreyer, IC 44 (= Swift list X (#1), 1860 RA 00 35 08, NPD 89 53.5) is "extremely faint, small, round, between two stars". The precessed position for Bond's observation is within 0.4 arcmin of the correct position; but Swift's position is more than 2 arcmin to the north; this is presumably why Dreyer posted separate listings. But per Corwin, the descriptions of the objects (and the flanking stars) make it clear that they are one and the same.

Per Dreyer, IC 45 (= Bigourdan 107, 1860 RA 00 35 12, NPD 61 06) is a "suspected nebula". As in the case of IC 43, which lies directly to the west of IC 45, the position precesses to the north of the correct position, so it appears that Bigourdan's positions were "off" by about the same amount for the two objects. Several sources, including HyperLeda and Wikisky, identify galaxy PGC 2537 (which lies directly to the north of IC 43) as IC 45, but Malcolm Thomson gives a thorough explanation of why that cannot be correct. The wide-field image of IC 43 shows a correctly labeled view of the region.

Per Dreyer, IC 46 (= Javelle 511, 1860 RA 00 35 31, NPD 63 31.0) is "pretty bright, small, round, brighter middle". The position precesses to within 0.2 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 5285 km/sec, about 235 million light years away. Given that and apparent size of 0.6 by 0.5 arcmin, about 40 thousand light years across.

Per Dreyer, IC 47 (= Javelle 31, 1860 RA 00 35 53, NPD 104 30.8) is "extremely faint, extremely small, round, stellar appearance". The position precesses to within 0.3 arcmin of the correct position, so the identification is certain. Based on recessional velocity of 11040 km/sec, about 490 million light years away. Given that and apparent size of 0.7 by 0.35 arcmin, about 100 thousand light years across.

Per Dreyer, IC 48 (= Barnard 3097, 1860 RA 00 36 31, NPD 98 38.9) is "pretty faint, small, possibly variable brightness" (in the first IC correction, it was noted as "up to 1895 always faint"). Per Corwin: Barnard's 1888 position was correct, but in converting it to the 1860 Equinox, Dreyer reversed the sign of the precessional correction. Barnard's later observation was done at a different observatory, and had a one-minute error in right ascension. The combination of the two errors led to the double identification by Dreyer. Based on recessional velocity of 5960 km/sec, about 265 million light years away. Given that and apparent size of 1.0 by 0.8 arcmin, about 80 thousand light years across.

Per Dreyer, IC 49 = (Swift list X (#2), 1860 RA 00 36 43, NPD 88 54.6) is "most extremely faint, pretty small, round, extremely difficult". The position precesses to 0.6 arcmin northwest of the correct position, near the rim of the galaxy; so the identification is certain. Based on recessional velocity of 4560 km/sec, about 200 million light years away. Given that and apparent size of 1.5 by 1.3 arcmin, about 90 thousand light years across.