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We studied a sample of stars associated with the Sh 2-296 nebula, part of thereflection nebulae complex in the region of Canis Major (CMa R1). Our samplecorresponds to optical counterparts of X-ray sources detected from observationswith the XMM-Newton satellite, which revealed dozens of possible low-mass youngstars not yet known in this region.  A sample of 58 young star candidates were selected based on optical spectralfeatures, mainly H{\alpha} and lithium lines, observed with multi-objectsspectroscopy performed by the Gemini South telescope. Among the candidates, wefind 41 confirmed T Tauri and 15 very likely young stars. Based on theH{\alpha} emission, the T Tauri stars were distinguished between classical(17%) and weak-lined (83%), but no significant difference was found in the ageand mass distribution of these two classes.  The characterization of the sample was complemented by near- and mid-infrareddata, providing an estimate of ages and masses from the comparison withpre-main-sequence evolutionary models. While half of the young stars have anage of 1-2 Myrs or less, only a small fraction (~25%) shows evidence of IRexcess revealing the presence of circumstellar discs. This low fraction isquite rare compared to most young star-forming regions, suggesting that someexternal factor has accelerated the disc dissipation.

Spectroscopic characterization of X-ray emitting young stars associated with the Sh 2-296 nebula