Speaker
Description
Aim:
The primary aim of this work is to derive the Galaxy Stellar Mass Function (GSMF) within the identified clusters with masses larger than 10^14 solar masses for redshifts lower than 0.4. We also investigate its variation as a function of galaxy properties (star-forming, quiescent) and of environment.
Method:
Establishing magnitude intervals, implementing a redshift limit, and applying a flux limit result in the formation of high-completeness subsamples. Subsequently, completeness is computed for each magnitude interval. To infer the optimal volume for stellar masses, a Richard curve is employed. Leveraging both completeness and volume, a robust galaxy stellar mass function is derived for each interval, addressing the characteristic upturn observed at intermediate
stellar masses using the Schechter function.
