Based on a recessional velocity of 8380 km/sec, IC 1354 is about 390 million light years away. Given that and its apparent size of 0.6 by 0.4 arcmin it is about 70 thousand light years across.

Apparent size 0.5 by 0.2 arcmin.

Apparent size 0.3 by 0.1 arcmin.

Apparent size 0.3 by 0.2 arcmin.

(this entry will mostly consist of historical information; for anything else see IC 1350)

Apparent size 0.4 by 0.4 arcmin.

Apparent size 1.1 by 0.8 arcmin.

Apparent size 1.3 by 0.7 arcmin.

Apparent size 0.4 by 0.2 arcmin.

Apparent size 1.2 by 0.4 arcmin.

Apparent size 0.7 by 0.3 arcmin.

Apparent size 0.9 by 0.6 arcmin.

Apparent size 0.3 by 0.2 arcmin.

Apparent size 1.0 by 0.6 arcmin.

Apparent size 1.1 by 0.7 arcmin.

Apparent size 0.4 by 0.2 arcmin.

Apparent size 0.3 by 0.2 arcmin.

The second IC adds (per Howe "Not round but much extended 225°". Apparent size 1.2 by 0.4 arcmin.

Apparent size 5.0 arcmin.

Per Dreyer, IC 1370 (= Javelle 422, 1860 RA 21 08 08, NPD 88 23.7) is "very faint, 2 faint stars involved". The field contains a group of at least six galaxies and a star (presumably one of the '2 faint stars involved'). The brightest galaxy (the one whose data are listed here) is undoubtedly the primary object observed by Javelle, but as noted by Corwin some of the other galaxies could have contributed to the impression he had of the object (for one thing, it appears that one of them is what he thought was a second star), and in any event the whole group appears closely connected, so the IC listing is sometimes attributed to only the bright galaxy, and sometimes to the group. Based on a recessional velocity of 15160 km/sec, a straightforward calculation indicates that IC 1370 is about 700 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 IC 1370 was about 655 million light years away when the light by which we see it left it, about 680 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 1.6 by 0.5 arcmin, the brightest galaxy is about 300 thousand light years across.

Apparent size 0.9 by 0.7 arcmin.

Apparent size 0.8 by 0.4 arcmin.

Apparent size 0.3 by 0.3 arcmin.

Apparent size 0.3 by 0.2 arcmin.

Apparent size 1.0 by 0.7 arcmin.

Apparent size 0.8 by 0.7 arcmin.

Apparent size 0.3 by 0.3 arcmin.

Apparent size 0.3 by 0.3 arcmin.

Apparent size 0.8 by 0.5 arcmin.

(this entry will contain mostly historical information; for anything else see NGC 7056)

Apparent size 0.4 by 0.2 arcmin.

Apparent size 0.7 by 0.5 arcmin.

Apparent size 0.4 by 0.4 arcmin.

Apparent size 1.5 by 1.1 arcmin.

Apparent size 0.4 by 0.3 arcmin.

Apparent size 0.4 by 0.2 arcmin.

Apparent size 0.7 by 0.5 arcmin.

Apparent size 0.7 by 0.6 arcmin.

Apparent size 0.2 by 0.2 arcmin.

Apparent size 1.1 by 0.7 arcmin.

Apparent size 0.6 by 0.4 arcmin.

Apparent size 1.0 by 0.9 arcmin.

Apparent size 0.3 by 0.3 arcmin.

A nearly three degree wide (170 by 140 arcmin) emission nebula about 2500 light years from the Earth (and hence the best part of 150 light years across), IC 1396 fluoresces in the intense radiation of the 4th-magnitude variable star near its center, μ Cephei. Bordering the nebula and within it are numerous knots of cooler, denser gas and dust which are outlined by or silhouetted against the hot, glowing gas surrounding them. One of the more dramatic knots is the elongated structure to the west (right) of the nebula's center, called the Elephant Trunk Nebula (closeups of which are shown below in visible and infrared radiation). μ Cephei, also known as Herschel's Garnet Star, is the prototype of the μ-Cephei type variables. It is a red supergiant of irregular brightness, varying from about magnitude 3.5 to 5 over a period of two to two and a half years. Its mass is estimated at 15 times that of the Sun, and it is one of the largest stars known -- the best part of two billion miles across at maximum size -- meaning it would nearly fill the orbit of Saturn. It is a very cool star (only about 3700 Kelvins, or 6200 Fahrenheit), so most of its radiation is in the infrared. Its visible radiation is about 40 thousand times that of the Sun, and taking into account absorption of its light by interstellar dust and the large proportion of infrared radiation it must give off, its total luminosity must be nearly ten times greater, or about 350 thousand solar luminosities. The star is near the end of its life, having already begun to fuse helium into carbon in its core, and within a few million years (hardly any time on an astronomical time scale) will blow itself to bits in a supernova explosion, leaving behind nothing but (most likely) a black hole or (less likely) a neutron star.

Apparent size 14 by 2.0 arcmin. A region near the Elephant Trunk.

Apparent size 12 by 4.0 arcmin. A region to the west of the Elephant Trunk. See "IC 1396A" for a labeled view of the region.

Apparent size 0.7 by 0.3 arcmin.

Apparent size 0.9 by 0.4 arcmin.

Based on a recessional velocity of 11765 km/sec, a straightforward calculation indicates that IC 1399 is about 550 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 525 million light years away when the light by which we see it left it, about 535 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 0.75 by 0.6 arcmin, IC 1399 is about 115 thousand light years across.