Based on recessional velocity of 840 km/sec, about 38 million light years away, in reasonable agreement with redshift-independent distances of 40 to 70 million light years. Given that and apparent size of 6.2 by 0.6 arcmins, about 65 thousand light years in diameter. As shown in the images below, NGC 100 is an exceptionally elongated galaxy, even for a spiral, suggesting that it has a very small nucleus, in comparison to its overall size. Such galaxies are sometimes called "superthin" galaxies.

Based on recessional velocity of 3385 km/sec, about 150 million light years away. Given that and apparent size of 2.2 by 2.0 arcmins, about 95 thousand light years in diameter.

Based on recessional velocity of 7330 km/sec, about 330 million light years away. Given that and apparent size of 1.0 by 0.9 arcmins, about 95 thousand light years in diameter.

Because of its brightness, visible without optical aid in a dark sky, and therefore labeled as a starlike object, 47 Tucanae. It is the second largest and brightest globular cluster in our galaxy, exceeded only by Omega Centauri (NGC 5139). Even at a distance of 16 to 18 thousand light years, its 120 light-year diameter is as large as the full moon, and contains several million stars. Based on its Main Sequence turnoff point, its age is estimated at 10 billion years.
     NGC 104 was recently used to prove a theory of stellar mass sorting by globular clusters. More massive stars tend to settle to the center of the cluster, while less massive ones spread out over a larger region. To prove that, 130 thousand stars near the center of the cluster were studied for seven years, using techniques that allowed movements as small as 1/100th of an HST image pixel to be detected. "Blue stragglers", Main Sequence stars located well above the cluster's turnoff point, were shown to be moving more slowly than stars of more normal mass. (The "stragglers" are believed to be produced by collisions between normal mass stars, which are virtually impossible in normal regions of stellar space, but fairly common in the densely packed cores of globular clusters.)
     Directly below is a "normal" image of the entire cluster. Below that is an illustration of the region studied in detail by the HST, to measure the motions of stars in the cluster's core. Upper image, ESO

Lower image, ground-based image on the left, VLT, R. Kotak & H. Boffin, ESO; HST closeup, ESA, G. Meylan (Ecole Polytechnique Federale de Lausanne) NASA

Based on recessional velocity of 5290 km/sec, about 240 million light years away, in good agreement with redshift-independent distance estimates of 190 to 250 million light years. Given that and apparent size of 1.1 by 0.7 arcmins, about 75 thousand light years in diameter.

Based on recessional velocity of 6060 km/sec, about 270 million light years away. Given that and apparent size of 1.3 by 0.6 arcmins, about 100 thousand light years in diameter.

Based on recessional velocity of 6290 km/sec, about 280 million light years away. Given that and apparent size of 0.6 by 0.5 arcmins, about 50 thousand light years in diameter.

Based on recessional velocity of 4735 km/sec, about 210 million light years away. Given that and apparent size of 2.0 by 1.6 arcmins, about 120 thousand light years in diameter.

Based on recessional velocity of 5460 km/sec, about 240 million light years away. Given that and apparent size of 1.1 by 1.0 arcmins, about 80 thousand light years in diameter.

A loose collection of moderately bright stars surrounding a 9th-magnitude central star, this is as likely to be a random grouping of northern Milky Way stars, as an actual cluster or association. The "cluster" is represented by most of the brighter stars in the roughly half-degree wide image shown below, centered on the "central" star in the "group".

Based on recessional velocity of 6285 km/sec, about 280 million light years away, in reasonable agreement with redshift-independent distance estimates of 250 to 275 million light years. Given that and apparent size of 1.1 by 0.5 arcmins, about 90 thousand light years in diameter.

Based on recessional velocity of 4460 km/sec, about 200 million light years away. Given that and apparent size of 1.4 by 1.0 arcmins, about 80 thousand light years in diameter.

Based on recessional velocity of 4160 km/sec, about 185 million light years away. Given that and apparent size of 0.9 by 0.7 arcmins, about 50 thousand light years in diameter.

Based on recessional velocity of 1825 km/sec, about 80 million light years away, in good agreement with redshift-independent distance estimates of 77 to 130 million light years. Given that and apparent size of 1.9 by 0.9 arcmins, about 45 thousand light years in diameter.

The NGC identification is very uncertain, as there is no object at the originally recorded position. The galaxy thought to be NGC 116 has the same right ascension as the original observation, but is a quarter degree to the north. Several other galaxies lie within the region, but are thought to be too faint to be the recorded object. The following information applies to PGC 1671, and to NGC 116, if the current identification is correct. Based on recessional velocity of 7575 km/sec, about 340 million light years away. Given that and apparent size of 0.6 by 0.3 arcmins, about 60 thousand light years in diameter.

Based on recessional velocity of 5365 km/sec, about 240 million light years away. Given that and apparent size of 0.7 by 0.4 arcmins, about 50 thousand light years in diameter.

A possibly irregular galaxy, also listed as a Seyfert galaxy. Based on recessional velocity of 11250 km/sec, about 500 million light years away. Given that and apparent size of 0.7 by 0.5 arcmins, about 100 thousand light years in diameter.

Based on recessional velocity of 7430 km/sec, about 330 million light years away. Given that and apparent size of 1.0 by 1.0 arcmins, about 95 thousand light years in diameter.

Based on recessional velocity of 3985 km/sec, about 175 million light years away. Given that and apparent size of 1.5 by 0.6 arcmins, about 75 thousand light years in diameter.

NGC 121 is about 200 thousand light years distant, or about the same distance as the Small Magellanic Cloud, and is almost certainly associated with that galaxy. It is the oldest globular cluster in the SMC, with an estimated age of about 11 billion years old, making it about 2 billion years younger than Milky Way globulars of similar composition (percentage of heavy elements)

Per Corwin: Javelle's position for IC 26 was accurate, 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.

Based on recessional velocity of 1515 km/sec, about 70 million light years away, in reasonable agreement with a redshift-independent distance estimate of 60 million light years. Given that and its apparent size of 2.0 by 0.8 arcmins, about 40 thousand light years in diameter.

Based on recessional velocity of 4845 km/sec, about 220 million light years away. Given that and its apparent size of 1.2 by 0.7 arcmins, about 75 thousand light years in diameter.