  HW Vir is a short-period binary that presents eclipse timing variations.
Circumbinary planets have been proposed as a possible explanation, although the
properties of the planets differ in each new study. Our aim is to perform
robust model selection methods for eclipse timing variations (ETV) and error
calculation techniques based on a frequentist approach for the case of the HW
Vir system. We initially performed simultaneous light and radial velocity curve
analysis to derive the masses of the binary. We then analyzed the eclipse
timing variation of the system by fitting multiple models. To select the best
model, we searched the confidence levels for the best model by creating an
$\chi^2$ surface grid and bootstrap methods for each pair of parameters. We
searched for stable orbital configurations for our adopted ETV model. The
masses of the binary are found as 0.413 $\pm$ 0.008 $M_\odot$ and 0.128 $\pm$
0.004 $M_\odot$. Under the assumption of two light time effects superimposed on
a secular change, the minimum masses of the circumbinary objects are calculated
as $25.0_{-2.2}^{+3.5} \ M_{Jup}$ and $13.9_{-0.45}^{+0.60}\ M_{Jup}$. The
projected semi-major axes are found to be $7.8_{-1.0}^{+1.4}\ au$ and
$4.56_{-0.22}^{+0.27}\ au$ in respective order. We find that this configuration
is unstable within a 3$\sigma$ range on the semi-major axis and eccentricity of
the outer circumbinary object.
