HD 213597 is an eclipsing binary system which was detected by the STEREO spacecraft and was speculated to host a low-mass stellar companion .
We used high-resolution spectroscopy with the 10-m Hobby-Eberly Telescope and the 1.2-m telescope in Mt Abu for radial velocity ( RV ) measurements of this source .
We performed aperture photometry for this star on the STEREO archival data and thereby confirm the transit signature .
We also did follow-up ground-based photometry with a 10-inch telescope from Mt Abu .
The spectroscopic RV semi-amplitude of the primary ( 33.39 km s ^ { -1 } ) indicates that the secondary is an M dwarf making the system a short period F+M eclipsing binary .
These RVs along with the inclination derived from our combined photometric analysis ( i~ { } = ~ { } 84 \degr . 9 ) , enable us to estimate the mass of the secondary as M _ { B } ~ { } \sim~ { } 0.286 ~ { } M _ { \sun } and radius as R _ { B } ~ { } \sim~ { } 0.344 ~ { } R _ { \sun } using an estimated mass { M _ { A } ~ { } \sim~ { } 1.3 ~ { } M _ { \sun } } and radius { R _ { B } ~ { } \sim~ { } 1.97 ~ { } R _ { \sun } } of the primary .
Our spectral analysis returned the following parameters : T _ { eff } = 6625 ~ { } \pm~ { } 121 K , [ Fe / H ] = -0.095 ~ { } \pm~ { } 0.08 and { log } ~ { } g = 3.72 ~ { } \pm~ { } 0.22 for the primary .
When { log } ~ { } g is constrained to a value of 3.96 , we derive T _ { eff } = 6753 ~ { } \pm~ { } 52K and [ Fe / H ] = -0.025 ~ { } \pm~ { } 0.05 .