  Asteroseismic scaling relations can provide high-precision measurements of
mass and radius for red giant (RG) stars displaying solar-like oscillations.
Their accuracy can be validated and potentially improved using independent and
accurate observations of mass, radius, effective temperature and metallicity.
We seek to achieve this using long period SB2 eclipsing binaries hosting
oscillating RGs. We explore KIC 8430105, for which a previous study found
significant asteroseismic overestimation of mass and radius when compared with
eclipsing binary measurements. We measured dynamical masses and radii for both
components to be significantly lower than previously established, increasing
the discrepancy between asteroseismic and dynamical measurements. Our dynamical
measurements of the RG component were compared to corresponding measurements of
mass and radius using asteroseismic scaling relations. Uncorrected scaling
relations overestimated the mass of the RG by 26%, the radius by 11%, and the
average density by 7%, in agreement with studies for other systems. However,
using a theoretical correction to $\Delta \nu$, we managed to obtain an
asteroseismic average density that is $1\sigma$ consistent with our dynamical
result. We obtained several measurements of $\nu_{max}$ that are not fully
consistent. With $\nu_{max} = 76.78 \pm 0.81\mu $Hz, the $\Delta \nu$
correction provided $2 \sigma$ consistent mass and radius for the giant. The
age of the system was estimated to be $3.7 \pm 0.4$ Gyr.
