The nebulae components of the system are not observable to the naked eye nor with amateur instruments, since they tend to be very weak. The main sequence of nebulae that compose it is located a few degrees northwest of the star Lambda Velorum, while some dark ramifications also extend south of it, reaching the central areas of the constellation.
The Vela Molecular Ridge appears as a sequence of bright and dark nebulae, located on the northwestern side of Vela. Observation Map of the Vela Molecular Ridge. Among these is the well-known NGC 2626 nebulae which belongs to the VMR D cloud and hosts some stars presenting Hα emission and the famous Herbig-Haro object HH 132. The brightest and warmest stars of the Vela R2 association illuminate some filaments of gas that shine with a bluish light, typical of reflection nebulae. Stellar formation activity is confirmed by the discovery of several associations of T Tauri stars, particularly in the VMR D cloud, as well as by the presence of several open clusters heavily obscured and deeply immersed in the gas observable at infrared wavelengths. Part of the gas in the clouds is ionized by the ultraviolet radiation of some of the most massive stars associated with the complex, constituting H II regions of great extent, as Gum 14 (RCW 27) and Gum 20 ( RCW 36). The most important clouds in the region are identified by the letters A, B, C and D, and in fact belong to two different complexes: the clouds A, C and D are located at an average distance of about 700-1000 parsecs (2300-3300 light years) and are related to the OB association Vela R2, while cloud B is located at a greater distance, up to 2000 parsecs (6500 light years) away, and is physically connected to the extended Vela OB1 association. This cloud complex lies on the sky in the direction of the Gum Nebula (foreground) and the Carina–Sagittarius Spiral Arm (background). Radio 12CO observations of the region showed the ridge to be composed of several clouds, each with masses 100,000–1,000,000 M ☉.
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