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