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tokens: GARSTEC increase the grid size considerably. The advantage of one such giant grid is that we can reuse it for the newly observed stars unlike the grid constructed using the MESA. The disadvantage is that we need much larger disc space (current grid needs 4TBs of disc space to store the local properties of the models needed for the frequency computation). Furthermore, the models on a track have poorer temporal resolution. We obtained models for the individual stars from the above tracks following the same procedure as for the MESA, i.e. we scanned all the models in a track and located the age range where T eff , [Fe/H] s , and 〈Δν〉 were all within 4σ of the observed values, subsequently we fitted the surface-corrected model frequencies (Kjeldsen et al. 2008 ) to get a representative model for the star. Repeating this for all the 6000 tracks, we obtain several tens to few hundred models per star. 3.3 YREC models We used YREC with OPAL high-temperature opacities (Iglesias Rogers 1996 ) supplemented with low-temperature opacities of Ferguson et al. ( 2005 ). The metallicity mixture from Grevesse Sauval ( 1998 ) was used. We used the 2005 version of the OPAL equation of state (Rogers Nayfonov 2002 ). All the nuclear reaction rates were from Adelberger et al. ( 1998 ) except for the 14 N( p , γ) 15 O reaction, for which we used the updated rates of Formicola et al. ( 2004 ). A step overshoot (Maeder 1975 ) of α OV = 0.2 H p , where H p is the pressure scale height, was used for all the stars. The YREC models were used to isolate the impact of the atomic diffusion on Y s determination by using the models with and without diffusion. The adiabatic oscillation frequencies were calculated using a code described in Antia Basu ( 1994 ). The Yale Monte Carlo Method (Silva Aguirre et al. 2015 ) was used to get a set of representative models for each star. We started with using the average large frequency separation and frequency of maximum power along with the spectroscopically determined effective temperature to get an estimate of the mass and radius of the star using the Yale Birmingham Grid-Based modelling pipeline (Basu, Chaplin Elsworth 2010 ; Gai et al. 2011 ). Since each of the observables has the associated observational error, we created thousands of realizations of M, R, T eff , and [Fe/H] s . For each realization, we used the YREC in an iterative mode to obtain a model of given M and [Fe/H] s that had the required R and T eff . This was done in two different ways: in the first approach, we kept α MLT fixed at different values and iterated over Y i to get the model; and in the second approach, we kept Y i fixed at different values and varied α MLT to get the required model. Finally, a set of representative models of the star was obtained based on the merit function, where and are the reduced chi-squares for the oscillation frequencies and frequency ratios, r 02 and r 01 (for the definition of ratios, see Roxburgh Vorontsov 2003 ). The was computed