This deep telescopic narrowband image shows a rarely photographed pair of planetary nebulae in the constellation of Vela. On the top right is NGC 2899 while on the top left is VBRC 2. 
NGC 2899 (aka RCW43) morphology strongly resembles a loose bipolar structure with conspicuous bright condensations. The advantage of long exposures taken under dark skies is revealing fainter extended structures that would not ordinarily be visible. A 28 arcminute long outflow associated with NGC 2899 can be seen clearly represented by two lobes of material to either side of the PN. The left one is much larger while the right component is quite small. This outflow was discovered by the professional astronomer Quentin Parker in 2005. 

VBRC 2, often referenced as RCW 44, is as an evolved planetary nebula by Van Den Bergh in 1973 and located approximately 3,900 light years away. The progenitor white dwarf, well visible in the middle of the nebula (the small central blue star) is one of the hottest and most evolved known for a planetary nebula. While the bright portion of the nebula spans a circular diameter of about 2.5′, looking closely a faint outer halo with a size to about 4′ can be glimpsed, which was discovered by the Galactic Planetary Nebula Halo Survey (GPNHS) team in August, 2014. 

On the bottom left shines N Velorum (N Vel), a 3rd-magnitude variable star sitting on the border between the Vela and Carina constellations. Showing an orange hue, this K-type giant star boasts twice the mass of our Sun and is positioned approximately 240 light years away. 

Completing this celestial tableau is the open cluster IC2488, originally discovered by Lacaille in the mid-18th century. Displaying a coarse appearance, this cluster, while estimated to harbor nearly 400 members, only reveals a few dozen through small telescopes, with brightness levels peaking at the 10th magnitude. (many thanks to Sakib Rasool for suggesting this elusive target and for providing inputs on the above description).

Takahashi CCA250 (250/f5) - ZWO 6200MM - Ha (1,170 min), OIII (480 min), B (90 min), G (90 min) and R (110 min) - AMT Observatory (A.Lau/M.Lorenzi/T.Tse), Río Hurtado, Chile.