  In the present work, we constrain the equation of the state of dense matter
in the context of heaviest observed neutron star mass M$_{max}$ = 2.35$\pm
0.17$ M$_{\odot}$ for the black widow pulsar PSR J0952-0607. We propose three
interactions HPU1, HPU2 and HPU3 (named after Himachal Pradesh University)for
the relativistic mean field model which include different combinations of
non-linear, self and cross-couplings among isoscalar-scalar $\sigma$,
isoscalar-vector $\omega$ and isovector-vector $\rho$ meson fields up to the
quartic order. These interactions are in harmony with the finite nuclei and
bulk nuclear matter properties. The equations of state computed by using newly
generated interactions for the $\beta$-equilibrated nucleonic matter satisfy
the heaviest observed neutron star mass M$_{max}$ = 2.35$\pm 0.17$ M$_{\odot}$
for the black widow pulsar PSR J0952-0607. The results for the radius
($R_{1.4}$) and dimensionless tidal deformability (${\Lambda_{1.4}}$)
corresponding to the canonical mass are also presented and agree well with the
GW170817 event and astrophysical observations. The radius of $2.08M_{\odot}$
neutron star mass is predicted to be in the range $R_{2.08}$ = 12.98 -13.09 Km
which also satisfies the NICER observations by Miller et al. (2021) and Riley
et al.(2021). A covariance analysis is also performed to assess the theoretical
uncertainties of model parameters and to determine their correlations with
nuclear matter observables.
