HD 172189 is a spectroscopic eclipsing binary system with a rapidly-rotating pulsating \delta Scuti component .
It is also a member of the open cluster IC 4756 .
These combined characteristics make it an excellent laboratory for asteroseismic studies .
To date , HD 172189 has been analysed in detail photometrically but not spectroscopically .
For this reason we have compiled a set of spectroscopic data to determine the absolute and atmospheric parameters of the components .
We determined the radial velocities ( RV ) of both components using four different techniques .
We disentangled the binary spectra using KOREL , and performed the first abundance analysis on both disentangled spectra .
By combining the spectroscopic results and the photometric data , we obtained the component masses , 1.8 and 1.7 M _ { \odot } , and radii , 4.0 and 2.4 R _ { \odot } , for inclination i = 73.2 ^ { \circ } , eccentricity e = 0.28 , and orbital period \Pi = 5.70198 days .
Effective temperatures of 7600 K and 8100 K were also determined .
The measured v \sin i are 78 and 74 km s ^ { -1 } , respectively , giving rotational periods of 2.50 and 1.55 days for the components .
The abundance analysis shows [ Fe/H ] = –0.28 for the primary ( pulsating ) star , consistent with observations of IC 4756 .
We also present an assessment of the different analysis techniques used to obtain the RVs and the global parameters .