Historical Identification: Per Dreyer, NGC 1550 (= GC 835, d'Arrest, 1860 RA 04 12 21, NPD 87 56.2) is "very faint, small, round, 13th magnitude star near". The position precesses to RA 04 19 37.8, Dec +02 24 19, well inside the galaxy, so the identification is certain.
Physical Information: Based on a recessional velocity of 3715 km/sec, NGC 1550 is about 175 million light years away. Given that and its apparent size of 1.8 by 1.7 arcmin, it is about 90 thousand light years across.

Historical Identification: Per Dreyer, NGC 1551 (= GC 836 = WH II 464, 1860 RA 04 12 23, NPD 88 55.6) is "faint, very small, round, probably = (GC) 835", GC 835 being NGC 1550, so it was suspected that the two listings referred to the same object at the time of the original publication of the NGC. The problem was the NPD of GC 836, which apparently includes a 1 degree recording error by Herschel. Per Corwin, when d'Arrest observed what became NGC 1550 he could not find Herschel's GC 836, but subsequently realized that if Herschel made a 1 degree error in that object's NPD, then the positions of the two nebulae would be essentially identical. Since the NGC follows the format of the GC, Dreyer had already included a space for both nebulae, so he entered each as if separate; but agreeing with d'Arrest, he noted the presumed equivalence as 'probable' in the original NGC entry, and later adopted the identity as 'definitive'.
Physical Information: Given the duplicate entry, see NGC 1550 for anything else.

Historical Identification: Per Dreyer, NGC 1552 (= GC 837 = JH 313 = WH III 490, 1860 RA 04 13 10, NPD 91 02.3) is "considerably faint, pretty small, a little extended, very gradually brighter middle, 11th magnitude star to southwest".
Physical Information: Apparent size 1.5 by 1.1 arcmin.

Historical Identification: Per Dreyer, NGC 1553 (= GC 838 = JH 2630, (Dunlop #320), 1860 RA 04 13 11, NPD 146 07.8) is "very bright, pretty small, round, gradually much brighter middle, among 3 stars".
Physical Information: Based on a recessional velocity of 1080 km/sec, NGC 1553 is about 50 million light years away, in good agreement with widely varying redshift-independent distance estimates of 25 to 75 million light years. Given that and its apparent size of 6.8 by 5.2 arcmin, it is about 100 thousand light years across. The galaxy is a member of the NGC 1566 group. It is part of a possibly gravitationally bound pair with NGC 1549, which is a little over 11 arcminutes away in the sky, and if at a common distance of about 55 million light years may be separated by as little as 175 thousand light years. HST images of the core of NGC 1553 show clouds of gas and dust presumably related to a gravitational interaction with NGC 1549 (perhaps the strongest evidence that they are a pair). Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SA(rl)0⁺.

Historical Identification: Per Dreyer, NGC 1554 (= GC 5339, Otto Struve, d'Arrest, 1860 RA 04 13 33, NPD 70 49.0) is a "a magnificent or otherwise interesting object, variable, small, round, with a northern nucleus equivalent to a 13th magnitude star". The first IC adds a note for NGC 1554 that actually applies to NGC 1555, and is posted there. The second IC adds a note applying to both objects, of which these portions apply to NGC 1554: "...Barnard in February and March 1895 found (with the 36-inch refractor) that T Tauri was not, as in 1890, the nucleus of a pretty bright, small nebula; the star was perfectly stellar but involved in a very faint, diffuse nebulous glow; Struve's nebula was not seen, though there was a slight haziness there (MN, lv, pp 442-452, where the whole history of the object is given, to which may be added a reference to a diagram by Otto Struve in 1862, MN xxii, p 242)... Keeler on two photos taken in December 1899 found three very faint, irregular patches, connected by still fainter nebulosity, southwest and west of T Tauri, but clear of the star; no trace of Struve's nebula (ibid, lx p425). Not visible to Burnham around 1907.0 (AN 4209)."
Physical Information: As related in the IC note, NGC 1554 and 1555 have been associated with each other and T Tauri since their discovery. They are undoubtedly variations in the lighting of clouds of gas and dust surrounding T Tauri caused by the movement of denser clouds very close to the star, casting shadows on or allowing shafts of light to reach the surrounding nebulae. The resulting variability in their appearance is the reason that NGC 1555 is called "Hind's Variable Nebula", and the fact that there have been no observations of NGC 1554 since those of Struve and d'Arrest in 1868 makes its "Lost" name equally appropriate. The position given by Dreyer precesses to the one given above, but since nothing has been seen there in nearly a century and a half, NGC 1554 is more a historical curiosity than anything else.

Historical Identification: Per Dreyer, NGC 1555 (= GC 839, Hind, 1860 RA 04 13 48, NPD 70 48.8) is "a magnificent or otherwise interesting object, very faint, small, variable (Auwers 20)", the final reference being to a list of nebulae compiled by Arthur von Auwers. The first IC adds a note for NGC 1554 that actually applies to NGC 1555: "Hind's variable nebula, 2 degrees preceding and 40 arcsec south of the variable star T Tauri. Barnard in 1890 found an extremely faint nebula in position 185 degrees, 3/4 arcmin distant from T, which agrees well with Hind's and d'Arrest's observations. Barnard and Burnham also saw T Tauri within a very small condensed nebula (often seen by Tempel). Bigourdan's #144 (a 13th-magnitude nebulous star?) in RA 04 13 56, NPD 70 52, was apparently not seen at the Lick Observatory." The second IC added "Hind's variable nebula. Barnard in February and March 1895 found (with the 36-inch refractor) that T Tauri was not, as in 1890, the nucleus of a pretty bright, small nebula; the star was perfectly stellar but involved in a very faint, diffuse nebulous glow; Struve's nebula was not seen, though there was a slight haziness there (MN, lv, pp 442-452, where the whole history of the object is given, to which may be added a reference to a diagram by Otto Struve in 1862, MN xxii, p 242). In September 1895, on three nights, no trace of Hind's nebula was seen with the 36-inch (ibid, lvi, p 66). Keeler on two photos taken in December 1899 found three very faint, irregular patches, connected by still fainter nebulosity, southwest and west of T Tauri, but clear of the star; no trace of Struve's nebula (ibid, lx p425). Not visible to Burnham around 1907.0 (AN 4209)." As made clear by such extended notes, NGC 1555 and 1554 have been associated with each other and T Tauri since their discovery. They are undoubtedly variations in the lighting of clouds of gas and dust surrounding T Tauri caused by the movement of denser clouds very close to the star, casting shadows on or allowing shafts of light to reach the surrounding nebulae. The resulting variability in their appearance is the reason that NGC 1555 is called "Hind's Variable Nebula". As it happens, the brightness and variation of this and similar nebulae were greatest around the time of their discovery; the IC notes indicate that they were less obvious later on, and they are even less obvious now. Still, observers of such phenomena can always hope to see new activity. NGC 1555 is the brightest part of the reflection nebula just west of T Tauri, and the closest part of a much larger region of nebulosity surrounding the star. Dreyer's position precesses to RA 04 21 57.6, Dec +19 31 22, which is on the southern edge of that brightest part, and that and decades of avid observation following its discovery make the identity certain.
Physical Information: The star and surrounding nebula are about 460 light years away. Given that and its 0.5 arcmin apparent size, NGC 1555 is about .07 light years or 4000 AU across; but this is only the size of the brightest and most historically variable part of the nebula, specifically referred to by the NGC listing. As seen in the wide-field images below, surrounding nebular regions extend tens of times further, and the overall size of the nebulosity is much greater. (Note: It may seem odd that an object obviously not a galaxy should have a PGC listing, but there are numerous examples of such listings in the additions to the original PGC. Given the large number of additional objects, some sort of automated system must have been used to identify objects, and entries were created before being checked by a trained observer. At least the catalog entry notes that it is not a galaxy, but a nebula.)

Historical Identification: Per Dreyer, NGC 1556 (= GC 840 = JH 2631, 1860 RA 04 13 57, NPD 140 30.2) is "considerably faint, small, round, very gradually a little brighter middle". The second IC adds (per Delisle Stewart) "Not round, but extended 165 degrees".
Physical Information: Based on a recessional velocity of 990 km/sec, NGC 1556 is about 45 million light years away, in good agreement with redshift-independent distance estimates of 44 to 64 million light years. Given that and its apparent size of 1.4 by 0.5 arcmin, it is about 20 thousand light years across.

Historical Identification: Per Dreyer, NGC 1557 (= GC 841 = JH 2633, 1860 RA 04 14 01, NPD 160 46.4) is a "cluster, very little compressed, about 20 scattered stars".
Physical Information: Apparent size 10 arcmin, just south of 7th-magnitude HD 27346.

Historical Identification: Per Dreyer, NGC 1558 (= GC 842 = JH 2632, 1860 RA 04 14 56, NPD 135 22.0) is "pretty faint, small, extended, gradually brighter middle".
Physical Information: Based on a recessional velocity of 4530 km/sec, NGC 1558 is about 210 million light years away, in good agreement with redshift-independent distance estimates of 150 to 230 million light years. Given that and its apparent size of 3.0 by 0.9 arcmin, it is about 185 thousand light years across.

Historical Identification: Per Dreyer, NGC 1559 (= GC 843 = JH 2634, (Dunlop 264), 1860 RA 04 15 56, NPD 153 07.8) is "very bright, very large, much extended, very gradually pretty much brighter middle, 14th magnitude star attached on north".
Physical Information: Based on a recessional velocity of 1305 km/sec, NGC 1559 is about 60 million light years away, in good agreement with redshift-independent distance estimates of 40 to 70 million light years. Given that and its apparent size of 3.5 by 2.0 arcmin, it is about 60 thousand light years across. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SB(s)cd.

Historical Identification: Per Dreyer, NGC 1560 (Tempel list IX (#1), 1860 RA 04 16 03, NPD 18 25.0) is "very faint, large, extended, 9.3 magnitude star to southwest".
Physical Information: NGC 1560's negative radial velocity of -35 km/sec indicates that it is too close for the Universal expansion to affect its motion relative to us, or to provide any hint of its distance. Redshift-independent distance estimates range from 5 to 15 million light years, with 10 to 12 million light years being the best current estimate (very close galactically speaking, but definitely not part of the Local Group). Given that and its apparent size of 11.6 by 1.9 arcmin, the galaxy is about 35 thousand light years across. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type Sd/Sm sp.

Historical Identification: Per Dreyer, NGC 1561 (Leavenworth list I (#127), 1860 RA 04 16 38, NPD 106 11.3) is "very faint, very small, a little extended 170°, gradually a little brighter middle, 8th magnitude star 6 seconds to west". The second IC lists a corrected position (per Howe) of RA 04 16 29, NPD 106 10.5.
Physical Information: Apparent size 1.3 by 0.65 arcmin.

Historical Identification: Per Dreyer, NGC 1562 (Leavenworth list I (#128), 1860 RA 04 16 40±, NPD 106 06.3) is "very faint, extremely small, round, gradually a little brighter middle". The second IC lists a corrected position (per Howe) of RA 04 15 26, NPD 106 05.3.
Physical Information: Apparent size 0.45 by 0.45 arcmin.

Historical Identification: Per Dreyer, NGC 1563 (Leavenworth list I (#129), 1860 RA 04 16 40±, NPD 106 04.3) is "extremely faint, very small, round, a little brighter middle, a double nebula with NGC 1564. The second IC lists a corrected position (per Howe) of RA 04 16 32, NPD 106 03.7.
Physical Information: Based on a recessional velocity of 9350 km/sec, a straightforward calculation indicates that NGC 1563 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 420 million light years away at the time the light by which we see it was emitted, about 425 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 0.5 by 0.5 arcmin, the galaxy is about 60 thousand light years across.

Historical Identification: Per Dreyer, NGC 1564 (Leavenworth list I (#130), 1860 RA 04 16 40±, NPD 106 04.3) is "extremely faint, very small, round, a little brighter middle, a double nebula with NGC 1563. The second IC lists a corrected position (per Howe) of RA 04 16 39, NPD 106 04.1
Physical Information: Apparent size 0.65 by 0.45 arcmin.

Historical Identification: Per Dreyer, NGC 1565 (Leavenworth list I (#131), 1860 RA 04 16 40±, NPD 106 06.3) is "extremely faint, pretty small, a little extended". The second IC lists a corrected position (per Howe) of RA 04 17 02, NPD 106 04.4.
Physical Information: Based on a recessional velocity of 9195 km/sec, a straightforward calculation indicates that NGC 1565 is about 430 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 415 million light years away at the time the light by which we see it was emitted, about 420 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 0.95 by 0.85 arcmin, the galaxy is about 115 thousand light years across.

Historical Identification: Per Dreyer, NGC 1566 (= GC 844 = JH 2635, Dunlop 338??, 1860 RA 04 16 52, NPD 145 16.6) is "bright, very large, very gradually then suddenly very much brighter middle, 15 seconds of time diameter in RA".
Physical Information: Based on a recessional velocity of 1505 km/sec, NGC 1566 is about 70 million light years away, at the upper range of redshift-independent distance measurements of 25 to 70 million light years. Given that and its apparent size of 8.4 by 8.1 arcmin, the galaxy is about 170 thousand light years across. It is a Seyfert galaxy (type Sy 1.5), and has an unusually high proportion of exceptionally hot, bright O-type stars (areas shown in white and pink in the bottom image are dominated by such stars). Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type (R₁')SAB(s)bc.

Apparent size 1.3 by 1.3 arcmin.

Swift would not have noticed PGC 15034, the fainter companion; but since they are physically interacting, NGC 1568 is considered to be the pair of galaxies. Based on an average recessional velocity of 4640 km/sec (there is only a difference of 30 km/sec between the separate values), NGC 1568 is about 215 million light years away. Given that, the 1.65 by 1.35 arcmin apparent size of PGC 15042 corresponds to about 100 thousand light years, while the 0.4 by 0.25 arcmin size of PGC 15034 corresponds to about 25 thousand light years. The 3.8 arcmin overall apparent size of the system, counting the extended tail caused by a recent collision or ongoing gravitational interaction, corresponds to about 240 thousand light years.

NGC 1569 is one of the nearest starburst irregular galaxies (it is a member of the IC 342/Maffei Group). It underwent a surge of star production about 25 million years ago, lasting for around 20 million years. The most massive stars produced during this time had very short lives, and almost immediately began a surge of supernova explosions that gives us an unusually detailed view of star birth and death. The galaxy's negative radial velocity (-105 km/sec) shows that it is too close for the Universal expansion to have an effect on its motion relative to us, so its distance cannot be determined from its 'recessional' velocity. Redshift-independent distance estimates range from 5 to 20 million light years, with 11 million light years being the current "best" estimate. Given that and its apparent size of 3.7 by 1.8 arcmin, the galaxy is about 12 thousand light years across. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type IB(s)m.

JH's declination for 1570 was off by 10 arcmin, hence the double listing. The description and RA confirm the identity of the two entries. (this entry to contain only historical information; for anything else see NGC 1571)

Apparent size 1.5 by 1.2 arcmin.

Based on a recessional velocity of 6110 km/sec, NGC 1572 is about 285 million light years away, a bit farther than redshift-independent distance estimates of 190 to 265 million light years. Given that and its apparent size of 2.8 by 1.2 arcmin, it is about 220 thousand light years across.

Apparent size 1.9 by 1.3 arcmin.

Based on a recessional velocity of 4500 km/sec, PGC 16052 is about 210 million light years away. Given that and its apparent size of 1.6 by 1.3 arcmin, it is about 100 thousand light years across. (Note: "in the general neighborhood of NGC 1573" is a bit of a stretch; as shown below, the two are nearly a degree apart.)

Based on a recessional velocity of 1040 km/sec, NGC 1574 is about 50 million light years away, in good agreement with redshift-independent distance estimates of 45 to 65 million light years. Given that and its apparent size of 4.0 by 3.6 arcmin, it is about 65 thousand light years across. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type SB0^-.

Swift's RA is nearly correct, but his declination is off. Muller's declination is OK, but his RA is too small. The two errors led to two entries, but the descriptions are sufficiently similar that Howe noted the identity of the two entries in a 1900 paper; hence Dreyer's second IC note (per Howe) that NGC 1575 is the same as NGC 1577; so the identity has been known for more than a century. Since both entries were "off", it seems appropriate to use the NGC number for the earlier discovery, and that is what happened. So this entry will deal only with historical information; for anything else see NGC 1577.

Apparent size 1.1 by 0.7 arcmin.

Based on a recessional velocity of 9335 km/sec, NGC 1577 is about 435 million light years away. Given that and its apparent size of 1.4 by 1.2 arcmin, it is about 175 thousand light years across.

Based on a recessional velocity of 6180 km/sec, NGC 1578 is about 290 million light years away (a second recessional velocity measurement of 6800 km/sec would suggest a distance of 315 million light years). Given that and its apparent size of 1.2 by 1.1 arcmin, it is about 100 to 110 thousand light years across.

Apparent size 12 by 8 arcmin.

Based on a recessional velocity of 4265 km/sec, NGC 1580 is about 200 million light years away. Given that and its apparent size of 1.05 by 0.9 arcmin, it is about 60 thousand light years across.

Apparent size 1.8 by 0.7 arcmin.

Apparent size 24 arcmin.

The second IC lists a corrected RA (per Howe) of 04 22 05. Apparent size of 0.7 by 0.7 arcmin.

The second IC lists a corrected RA (per Howe) of 04 21 54. Apparent size 0.6 by 0.6 arcmin.

Based on a recessional velocity of 4655 km/sec, NGC 1585 is about 215 million light years away. Given that and its apparent size of 1.2 by 0.7 arcmin, it is about 75 thousand light years across.

Based on a recessional velocity of 3570 km/sec, NGC 1586 is about 165 million light years away, in good agreement with redshift-independent distance estimates of 140 to 175 million light years. Given that and its apparent size of 1.7 by 0.9 arcmin, it is about 80 thousand light years across.

Apparent size 1.7 by 1.4 arcmin. Probably paired with NGC 1588.

Apparent size 1.1 by 0.6 arcmin. Probably paired with NGC 1587.

Based on a recessional velocity of 3795 km/sec, NGC 1589 is about 175 million light years away. Given that and its apparent size of 3.2 by 1.0 arcmin, it is about 165 thousand light years across.

Based on a recessional velocity of 3895 km/sec, NGC 1590 is about 180 million light years away. Given that and its apparent size of 0.9 by 0.7 arcmin, it is about 50 thousand light years across.

Based on a recessional velocity of 4115 km/sec, NGC 1591 is about 190 million light years away, in reasonable agreement with redshift-independent distance estimates of 140 to 180 million light years. Given that and its apparent size of 1.2 by 0.8 arcmin, it is about 65 thousand light years across.

Historical Identification: Per Dreyer, NGC 1592 (= GC 862 = JH 2645, 1860 RA 04 23 53, NPD 117 16.0) is "very faint, very small". The second IC adds "Only faint stars seen by Howe". The position precesses to RA 04 29 35.3, Dec -26 57 29, but there is nothing there, which is presumably why Howe saw only faint stars near Herschel's position. However, given the fact that it is listed by Herschel as being nearly due south of and fainter than GC 681 = NGC 1591, it seems appropriate to look for a somewhat fainter galaxy than NGC 1591 somewhere to its south; and the galaxy listed above fits the description, so despite being nearly half a degree further south its identification as NGC 1592 is considered reasonably certain (sufficiently so that although some references list NGC 1592 as nonexistent, most identify it as PGC 15292).
Additional Note: Presuming that NGC 1592 is the object listed above, Herschel would only have been able to see its brighter eastern part (PGC 15292), and as a result that is the usual identification for NGC 1592. However, the complex structure shown in the images below consists of PGC 15292 and PGC 15285, so I have chosen to include both of them not only in this discussion but also in the title and description for this entry.
Physical Information: Based on a recessional velocity of 945 km/sec, NGC 1592 is about 45 million light years away, in fair agreement with a single redshift-independent distance estimate of 30 million light years. Since both distances are uncertain (the Hubble distance due to the possible presence of "peculiar" or non-Hubble redshift motions of a few tens of km/sec (or more), and the redshift-independent distance due to inherent uncertainties in the method used to produce what is literally an "estimate" of the distance), it seems appropriate to assign an approximate distance of about 40 million light years to the system. Given that, the apparent size of the overall structure of about 1.6 by 0.55 arcmin corresponds to about 20 thousand light years, making it a relatively small galaxy. NGC 1592 might best be described as a single irregular galaxy, but it has been suggested that it is the result of the merger of at least two formerly independent galaxies, seen at a fairly late stage in their merger, in which case some of the brighter regions in the eastern part of the structure may represent the nuclei of the original galaxies, and the irregular appearance of the galaxy's halo is consistent with such a merger. However, the reddish blobs near the center of the structure are definitely large star-forming regions, and even the brighter regions to their east may simply be much more active star-forming regions, in which case the galaxy may not be the result of a recent merger, but simply a "late bloomer" in terms of its history of star formation (as appears to be the case for many "dwarf" irregular galaxies).

Per Dreyer, NGC 1593 (= Marth 97, 1860 RA 04 23 56, NPD 89 44) is "very faint". The position precesses to RA 04 31 07.5, Dec +00 34 22, but there is nothing there, and apparently no one realized that it might be the same as NGC 1608 before Corwin, so it was a "lost" object for the best part of a century. However, since the solution appears to be a simple one (Marth's RA was 1 minute too small, which is a not uncommon transcription error), the identity of the two listings seems reasonably certain.

Per Dreyer, NGC 1594 (= Swift list V (#61), 1860 RA 04 24 17, NPD 96 06.5) is "very faint, pretty small". Swift's RA is wrong, but the second IC lists a corrected RA (per Howe) of 04 23 59. The corrected position precesses to RA 04 30 51.3, Dec -05 48 07, which is well inside the galaxy, so the identification is certain. Based on a recessional velocity of 4330 km/sec, NGC 1594 is about 200 million light years away, in fair agreement with redshift-independent distance estimates of 220 to 250 million light years. Given that and its apparent size of 1.8 by 1.3 arcmin, the galaxy is about 110 thousand light years across.

The Carafe Group is a triplet of three galaxies that have similar recessional velocities (and are therefore presumably at comparable distances) in the same region of Caelum. It consists of PGC 15172, NGC 1595 and NGC 1598. Based on a recessional velocity of 4945 km/sec, PGC 15172 is about 230 million light years away. Similar calculations indicate a distance for NGC 1595 of about 225 million light years, and for NGC 1598 of about 240 million light years, suggesting a common distance (if the triplet really is a physical group) of about 230 million light years. Given that and its apparent size of 2.1 by 1.8 arcmin, PGC 15172 is about ? thousand light years across. A Seyfert galaxy (type Sy 2). Perhaps a polar ring galaxy (that is, one in which a ring circles the galaxy perpendicular to the plane of its disk).

The Carafe Group is a triplet of three galaxies that have similar recessional velocities (and are therefore presumably at comparable distances) in the same region of Caelum. It consists of the Carafe Galaxy (PGC 15172), NGC 1595 and NGC 1598. Based on a recessional velocity of 4810 km/sec, NGC 1595 is about 225 million light years away. Similar calculations indicate a distance for PGC 15172 of about 230 million light years, and for NGC 1598 of about 240 million light years, suggesting a common distance (if the triplet really is a physical group) of about 230 million light years. (This is far greater than redshift-independent distance estimates for NGC 1595 of only 92 to 108 million light years, and cannot be reconciled with them; and I have chosen to ignore the redshift-independent estimates, on the basis of the prevailing view that NGC 1595 is part of the Carafe Group.) Given that and its apparent size of 1.5 by 1.05 arcmin, NGC 1595 should be about 100 thousand light years across.

Based on a recessional velocity of 1510 km/sec, NGC 1596 is about 70 million light years away, a bit further than redshift-independent distance estimates of 44 to 58 million light years. Given that and its apparent size of 4.4 by 1.1 arcmin, it is about 90 thousand light years across. Used by the de Vaucouleurs Atlas of Galaxy Types as an example of galaxy type S0^- sp.

Apparent size 0.9 by 0.7 arcmin.

The Carafe Group is a triplet of three galaxies that have similar recessional velocities (and are therefore presumably at comparable distances) in the same region of Caelum. It consists of the Carafe Galaxy (PGC 15172), NGC 1595 and NGC 1598. Based on a recessional velocity of 5130 km/sec, NGC 1598 is about 240 million light years away, in fair agreement with redshift-independent distance estimates of 135 to 220 million light years. Similar calculations indicate a distance for PGC 15172 of about 230 million light years, and for NGC 1595 of about 225 million light years, suggesting a common distance (if the triplet really is a physical group) of about 230 million light years. Given that and its apparent size of 1.4 by 0.8 arcmin, NGC 1598 is about 95 thousand light years across. Like the Carafe Galaxy, NGC 1598 has an extended system of peculiar arms and jets (faintly visible in the images below) that cover half again the area of the main galaxy (about 2.1 by 1.5 arcmin), or about 140 thousand light years.

Based on a recessional velocity of 4055 km/sec, NGC 1599 is about 190 million light years away. Given that and its apparent size of 0.9 by 0.8 arcmin, it is about 50 thousand light years across.