ASAS J174406+2446.8 was originally found as a \delta Scuti-type pulsating star with the period P=0.189068 days by ASAS survey .
However , the LAMOST stellar parameters reveal that it is far beyond the red edge of pulsational instability strip on the \log g - T diagram of \delta Scuti pulsating stars .
To understand the physical properties of the variable star , we observed it by the 1.0-m Cassegrain reflecting telescope at Yunnan Observatories .
Multi-color light curves in B , V , R _ { c } and I _ { c } bands were obtained and are analyzed by using the W-D program .
It is found that this variable star is a shallow-contact binary with an EB-type light curve and an orbital period of 0.3781 days rather than a \delta Scuti star .
It is a W-subtype contact binary with a mass ratio of 1.135 ( \pm 0.019 ) and a fill-out factor of 10.4 ( \pm 5.6 ) \% .
The situation of ASAS J174406+2446.8 resembles those of other EB-type marginal-contact binaries such as UU Lyn , II Per and GW Tau .
All of them are at a key evolutionary phase from a semi-detached configuration to a contact system predicted by the thermal relaxation oscillation theory .
The linear ephemeris was corrected by using 303 new determined times of light minimum .
It is detected that the O - C curve shows a sinusoidal variationthat could be explained by the light-travel-time effect via the the presence of a cool red dwarf .
The present investigation reveals that some of the \delta Scuti-type stars beyond the red edge of pulsating instability strip on the \log g - T diagram are misclassified eclipsing binaries .
To understand their structures and evolutionary states , more studies are required in the future .