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NGC 2818
Emission nebula
Planetary nebula
	Hubble Space Telescope image of NGC 2818; (red: nitrogen, green: hydrogen, blue: oxygen)
Observation data: J2000.0 epoch
Right ascension	09h 16m 01.656s
Declination	−36° 37′ 38.76″
Distance	10,400 ly
Apparent dimensions (V)	2'
Constellation	Pyxis
Physical characteristics
Radius	3.25 ly
Designations	NGC 2818, PLN 261+8.1 ESO 372-PN13
	See also: Lists of nebulae

NGC 2818 is a planetary nebula located in the southern constellation Pyxis (The Compass). It consists largely of glowing gases from the star's outer layers ejected during the final stages of its life when it had run out of the fuel necessary to sustain its core fusion processes. The remnants of its core will remain as a white dwarf.^[3] The mass of the nebula is estimated at about 0.6 solar masses, while the progenitor star was likely about 2.3 times the mass of the Sun.^[4]

NGC 2818 presents a complex morphology, and overall has bipolar structure, making it a bipolar nebula. The two lobes are somewhat broken and irregular. There are also filamentary structures radiating from the center, and near the center of the nebula, several cometary knots.^[4]

It is often cited as a member of the open cluster NGC 2818A framing it, however, radial velocity differences between the planetary nebula and open cluster suggest a chance alignment.^[5]^[6] The case is an example of a superimposed pair, similar to NGC 2438 and M46.^[7]

Partly because of their small total mass, open clusters have relatively poor gravitational cohesion. Consequently, open clusters tend to disperse after a relatively short time, typically some 10 million years, because of external gravitational influences amid other factors. Under exceptional conditions, open clusters can remain intact for up to 100 million years.

Theoretical models predict that planetary nebulae can form from main-sequence stars of between 8 and 1 solar masses, which puts their age at 40 million years and older. Although there are a few hundred known open clusters within that age range, a variety of reasons limit the chances of finding a member of an open cluster in a planetary nebula phase. One such reason is that the planetary nebula phase for more massive stars belonging to younger clusters is on the order of thousands of years - a blink of the eye in cosmic terms. Only one association has been established between open clusters and nearby nebulae, the extremely distant nebula PHR 1315-6555.^[8]