Colour-magnitude diagram of the field observed by eROSITA. Large symbols indicate stars with eROSITA X-ray detections. Of these, members of NGC 2516 are displayed in orange, while non-members detected in X-rays are in black. NGC 2516 cluster members undetected with eROSITA are marked with small blue crosses, while field stars (undetected in X-rays) are shown with small grey dots. Potential (member) binaries from radial velocity (Bailey et al. 2018; Fritzewski et al. 2020), astrometry (Gaia RUWE), or photometry (above the main sequence in Gaia photometry) are additionally marked with squares. Certain stars on the cluster upper main sequence (clearly photometric members) are marked as non-members because they do not meet the formal (and restrictive) membership criteria set up for our predominantly cool star sample (see text). The few cluster members well above the cluster sequence are on it in other photometry, indicating an issue with their Gaia photometry.