  We investigate the influence of effective nucleon mass on the equation of
state (EOS), which is constructed for simulations of core-collapse supernovae
and binary neutron-star mergers, within the relativistic mean-field (RMF)
framework. The study introduces a new RMF parameter set, TM1m, which is a
modification of the TM1e model with an adjusted effective mass, maintaining the
saturation properties of nuclear matter. The TM1m model, with a larger
effective mass ratio ($M^{\ast}/M \sim 0.8$) compared to the TM1e model
($M^{\ast}/M \sim 0.63$), is employed to construct a new EOS table, EOS5. This
EOS table is designed to offer insights into the influence of effective nucleon
mass on the EOS within a relativistic framework, particularly above the
saturation density. The properties of cold neutron stars, calculated using the
TM1m model, are compared with those of the TM1e and original TM1 models. Both
the TM1m and TM1e models are found to be compatible with the latest constraints
on tidal deformability and radii of neutron stars, derived from astrophysical
observations.
