Poster abstract details

Observation of NGC 2506 imposes strong external constraints on the models of its stellar population. The existence of stellar pulsators, in particular $\gamma$ Doradus (Dor) oscillators among its members makes it an excellent laboratory for asteroseismic studies.
We use the latest developed theoretical and computational tools: Frequency
Ratio Method (FRM) and Time Dependent Convection (TDC). These are specially adapted to analyse this type of pulsating stars. In particular the use of both techniques gives us the opportunity to construct a self-consistent interpretation procedure, allowing modes identification and improved modelling
of the $\gamma$ Dor members of the cluster.