This planetary nebula was discovered 1980 by A. J. Longmore and S. B. Tritton on photo plates made with the 1.2 m UK Schmidt Telescope in New South Wales, Australia. It was listed as fifth in a list of 11 newly discovered nebulae and is hence referred to as Longmore-Tritton 5 or short: LoTr 5. They described it as, "a very large and very faint non-uniform disk, slightly brighter towards the centre. Two members of a distant group or cluster of galaxies can be seen through the nebula."

LoTr 5 is located just 1.5° ways from the north galactic pole and therefore the planetary nebula with the highest galactic latitude. Modelling shows that is expanding asymmetrically and shows some form of bipolar structure with the axis inclined around 17° to the line of sight.The central star IN Comae Berenices (SAO 82570, HD 112313, BD +26°2405) has a visual magnitude of 8.88 mag and is a fast-rotating G5 giant of luminosity class III-IV with a rotational period of 5.9 days. A long-term brightness variation with a period of ~7.2 years results from an orbiting low mass M5 companion star. Gaia DR3 distance is 455 pc.

From Alba Aller Journal Article:

LoTr 5 is a planetary nebula with an unusual long-period binary central star. As far as we know, the pair consists of a rapidly rotating G-type star and a hot star, which is responsible for the ionization of the nebula. The rotation period of the G-type star is 5.95 d and the orbital period of the binary is now known to be ∼2700 d, one of the longest in central star of planetary nebulae. The spectrum of the G central star shows a complex H α double-peaked profile which varies with very short time-scales, also reported in other central stars of planetary nebulae and whose origin is still unknown. We present new radial velocity observations of the central star which allow us to confirm the orbital period for the long-period binary and discuss the possibility of a third component in the system at ∼129 d to the G star. This is complemented with the analysis of archival light curves from Super Wide Angle Search for Planets, All Sky Automated Survey, and Optical Monitoring Camera. From the spectral fitting of the G-type star, we obtain an effective temperature of Teff = 5410 ± 250 K and surface gravity of log g = 2.7 ± 0.5, consistent with both giant and subgiant stars. We also present a detailed analysis of the H α double-peaked profile and conclude that it does not present correlation with the rotation period and that the presence of an accretion disc via Roche lobe overflow is unlikely.