[6] This nebula has been observed using telescopes with apertures as small as 80 mm (3.1 in), but a rich Milky Way background can make it difficult to find.

[8] NGC 6153 has a Peimbert type of I, indicating it is helium and nitrogen rich and the progenitor was a thin disk star.

[7] It was proposed that this discrepancy occurs due to cold, metal-rich, hydrogen deficient knots that have been included in the nebula.

[10] An analysis of Gaia data suggests that the central star may be a binary system.

[12] While on the cooling track, a white dwarf can undergo a final thermal pulse, causing the star to swell into a helium burning giant that follows nearly the same evolutionary track as the earlier star.