  In the present article, we discuss relativistic anisotropic solutions of the
Einstein field equation for the spherically symmetric line element under the
class I condition. To do so we apply the embedding class one technique using
Eisland condition. Within this approach, one arrives at a particular
differential equation that links the two metric components $e^{\nu}$ and
$e^{\lambda}$. In order to obtain the full space-time description inside the
stellar configuration we ansatz the generalized form of metric component
$g_{rr}$ corresponding to the Finch-Skea solution. Once the space-time geometry
is specified we obtain the complete thermodynamic description i.e. the matter
density $\rho$, the radial, and tangential pressures $p_r$ and $p_t$,
respectively. Graphical analysis shows that the obtained model respects the
physical and mathematical requirements that all ultra-high dense collapsed
structures must obey. The $M-R$ diagram suggests that the solution yields
stiffer EoS as parameter $n$ increases. The $M-I$ graph is in agreement with
the concepts of Bejgar et al. \cite{bej} that the mass at $I_{max}$ is lesser
by few percent (for this solution $\sim 3\%$) from $M_{max}$. This suggests
that the EoSs is without any strong high-density softening due to
hyperonization or phase transition to an exotic state.
