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tokens: width measurements of several unblended Fe i lines. Projected rotation velocities () were determined by fitting the profiles of the Fe i lines after convolving with the instrumental resolution ( = 75 000) and a macroturbulent velocity adopted from the calibration of Doyle et al. (2014) . We also estimated from the CCF using the procedure of Boisse et al. (2010) and found consistent results: km s and km s for WASP-113 and WASP-114, respectively. Furthermore, we estimated the spectral type using Teff and Table B1 of Gray (2008) . The derived stellar parameters for WASP-113 and WASP-114 are given in Table 4 . We find that the stellar parameters of WASP-113 and WASP-114 are very similar. Table 4 Stellar parameters of WASP-113 and WASP114 from spectroscopic analysis. Notes. Spectral type estimated from and Table B1 of Gray (2008) . 3.1. Stellar age Fig. 6 Modified H-R diagrams for WASP-113 on the left and WASP-114 on the right . We display the stellar models of YY ( Demarque et al. 2004 ). The isochrones are shown solid black line (for Gyr old stars from left to right ) and and the mass tracks in red ( from left to right we show 1.3, 1.2, and 1.1 ) for the corresponding metallicity given in Table 4 . Combining the sin with the stellar radius we derive an upper limit to the stellar rotation period of days and days for WASP-113 and WASP-114, respectively. These allow us to derive an upper limit to the gyrochronological age of Gyr for WASP-113 and Gyr for WASP-114 using Barnes Kim (2010) . However, the lithium abundance suggests an age of Gyr for both stars ( Sestito Randich 2005 ). A discrepancy between the age indicators is not unusual ( Brown 2014 ; Maxted et al. 2015 ); however, the reason is still not clear. A more precise constraint on the age can be obtained by using theoretical stellar models. We follow the procedure of Brown (2014) using three sets of stellar models: the Padova models of Marigo et al. (2008) and Bressan et al. (2012) , the Yonsei-Yale (YY) isochrones of Demarque et al. (2004) , and the Dartmouth Stellar Evolution Database (DSED) models of Dotter et al. (2008) . We use the values of and [Fe/H] derived from the spectroscopic analyses and the transit derived stellar density whose derivation is explained in the next section. For WASP-113 we found an age of Gyr, Gyr, and Gyr respectively for the models of Padova, YY, and DSED. In the left panel of Fig. 6 we show the isochrones and mass tracks for WASP-113 for the YY models. According to these models WASP-113 has a mass of , which is very close to the critical mass for the stellar cores to become convective. Owing to the convective cores, the evolution and consequently the shape of the evolutionary tracks for higher mass stars is significantly different from lower mass stars, as can be seen in this figure. In this region of the parameter space details on the treatment of convective overshooting become important and the uncertainty in the stellar age and mass are higher. We