We report on the Suzaku observation of the intermediate polar V1223 Sagittarii .
Using a multi-temperature plasma emission model with its reflection from a cold matter , we obtained the shock temperature to be 37.9 ^ { +5.1 } _ { -4.6 } keV .
This constrains the mass and the radius of the white dwarf ( WD ) in the ranges 0.82 ^ { +0.05 } _ { -0.06 } \MO and ( 6.9 \pm 0.4 ) \times 10 ^ { 8 } cm , respectively , with the aid of a WD mass-radius relation .
The solid angle of the reflector viewed from the post-shock plasma was measured to be \Omega / 2 \pi = 0.91 \pm 0.26 .
A fluorescent iron K \alpha emission line is detected , whose central energy is discovered to be modulated with the WD rotation for the first time in magnetic-CVs .
Detailed spectral analysis indicates that the line comprises of a stable 6.4 keV component and a red-shifted component , the latter of which appears only around the rotational intensity-minimum phase .
The equivalent width ( EW ) of the former stable component \sim 80 eV together with the measured \Omega indicates the major reflector is the WD surface , and the shock height is not more than 7 % of the WD radius .
Comparing this limitation to the height predicted by the Aizu model ( 1973 ) , we estimated the fractional area onto which the accretion occurs to be < 7 \times 10 ^ { -3 } of the WD radius , which is the most severe constraint in non-eclipsing IPs .
The red-shifted iron line component , on the other hand , can be interpreted as emanating from the pre-shock accretion flow via fluorescence .
Its EW ( 28 ^ { +44 } _ { -13 } eV ) and the central energy ( 6.30 _ { -0.05 } ^ { +0.07 } keV ) at the intensity-minimum phase are consistent with this interpretation .