Constraining isoscalar–vector and isovector–vector couplings from very heavy neutron stars and GW190814 observations

We constrain the nuclear matter \ac{eos} within the relativistic mean field model by including the isoscalar-vector and isovector-vector coupling term at a fundamental level using the Bayesian analysis. We utilised the nuclear saturation properties and recent astrophysical observations to constrain the equation of state (EOS) of dense matter. We obtained approximately 20,000 sets of equations of state from sampling about 60 million sets of equations of state. All 20000 equations of state satisfy nuclear matter saturation properties at saturation densities and produce high mass \ac{ns}s. In our findings, we find that the non-zero value of the scalar-vector and isovector-vector coupling parameter and the negative value of the sigma meson self-coupling stiffen the \ac{eos}. Our sets of equations of state produce \ac{ns}s of mass larger than 2.5 M$_{\odot}$ to include the recent gravitational waves observation GW190814. There are two sets of data files are collected in two separate zipped files, which are like with and without GW190814 constraint on equation of state. Each file contains four different datafiles: 1) couling constants (cplngs), 2) nuclear saturation properties (nprp_sel20), 3) equation of state (eosset) and 4) mass-radius data (amrset) for corresponding to each set assigned with an ID. The unit of quanties are like mass in M$_{\odot}$, radius in km, baryon density in 1/fm^3, energy density in MeV/fm^3, pressure in MeV/fm^3 etc. All the dimensions are giving with the column names themselve.