Keck/HIRES precision radial velocities of HD 207832 indicate the presence of two Jovian-type planetary companions in Keplerian orbits around this G star .
The planets have minimum masses of M \sin i = 0.56 { M _ { Jup } } and 0.73 { M _ { Jup } } , with orbital periods of \sim 162 and \sim 1156 days , and eccentricities of 0.13 and 0.27 , respectively .
Strömgren b and y photometry reveals a clear stellar rotation signature of the host star with a period of 17.8 days , well separated from the period of the radial velocity variations , reinforcing their Keplerian origin .
The values of the semimajor axes of the planets suggest that these objects have migrated from the region of giant planet formation to closer orbits .
In order to examine the possibility of the existence of additional ( small ) planets in the system , we studied the orbital stability of hypothetical terrestrial-sized objects in the region between the two planets and interior to the orbit of the inner body .
Results indicated that stable orbits exist only in a small region interior to planet b .
However , the current observational data offer no evidence for the existence of additional objects in this system .