A closer look at the young stellar group around Sh 2-295

Context . Star formation is governed by multiple physical processes, making it inherently complicated. One excellent example is the Canis Major OB1/R1 association, whose complex history of star formation is related to different episodes. Three supernova (SN) events potentially altered the environment and impacted star formation and stellar evolution. Aims . Prior investigations revealed two stellar groups of different ages associated with GU CMa and Z CMa. This work focusses on identifying the low-mass young stellar population near FZ CMa, located between these two groups and spatially related to the H II region Sh 2-295. Our main goal is to verify whether this group is age-mixed and characterise its physical properties. Methods . We analysed multi-object spectroscopic data acquired with Gemini/GMOS to search for typical features of T Tauri stars (TTs) and to determine their spectral types. Lithium absorption line ( λ 6708 Å) was used as a youth indicator, while H α emission was investigated to probe accretion activity. We also derived ages based on optical photometry from Gaia DR3 and compared the projected spatial distribution to diffuse infrared emission. Results . We identified 29 TTs, including six new members of the association and three classical TTs. The equivalent width of the Li I absorption line suggests an age of 8.1 −3.8 +2.1 Myr, while optical photometric data indicate stellar ages ranging from ~1 to 14 Myr. Younger stars are concentrated around Sh 2-295, whereas the older ones are more widely dispersed. Conclusions . We increased the number of known TTs related to the CMa association. Our results support a scenario of multiple star formation episodes, including a younger group that may have been triggered by the expansion of Sh 2-295. The influence of SN events appears limited in this context.