tokens: metallicity, we illustrate the corresponding comparison in Fig. 11 . It shows that the two samples are similar in metallicity, spanning from −1.4 dex to 0.5 dex. Comparing with LAMOST, KIC metallicities of both samples were underestimated in the metal-poor regime but overestimated in the metal-rich region. In panel (b), we clearly observe this trend with a mean and standard deviation of −0.061 and 0.210 dex, respectively, in the sense of KIC minus LAMOST. This is consistent with the metallicity trend found by Dong et al. ( 2014 ). Figure 11. Same with Fig. 9 but for metallicity. We also checked if the lack of seven independent colours (derived from eight filters: KIC griz , D51 and 2MASS JHK ) contributes to the incorrect KIC-predicted ν max values. However, only three stars do not have a full set of colours and therefore we excluded this effect as a dominant cause for the larger errors in log g . In Fig. 12 , we compare Kepler magnitudes, KIC reddening, asteroseismic masses and spatial distribution for our sample (red data) with the samples from Huber et al. ( 2011 , grey data) and Stello et al. ( 2013 , blue data). Note that we have restricted both comparison samples to seismic gravities in the same ranges as our sample (from 2.2 to 3.5 dex). Figure 12. Histograms for Kepler magnitude K p [panel (a)] and KIC reddening [panel (b)], spatial distribution in Kepler field of view [panel (c)] and histogram of asteroseismic mass [panel (d)]. The red data represents targets of our entire sample, the grey data indicates those from Huber et al. ( 2011 ) while the blue data are targets from Stello et al. ( 2013 ). From Fig. 12(a) , we can see, due to the preferential selection of bright stars by the Kepler Asteroseismic Science Consortium, our sample is systematically fainter by nearly 2 mag, compared to Huber et al. ( 2011 ). We note that Huber et al. ( 2011 ) used data spanning from Q0 to Q6 for long-cadence light curves and Q0 to Q4 for short-cadence light curves, whereas we used data from the entire nominal Kepler Mission (Q0–Q17). Longer time series enhance the probability of detecting oscillations in fainter stars. Both our sample and the Stello et al. ( 2013 ) sample show a sharp cut at K p = 14 mag due to the Kepler selection function (Batalha et al. 2010 ). Panel (b) shows most targets in our sample have reddening around 0.13 mag, which is consistent with the sample of Huber et al. ( 2011 ) but shifted by 0.03 mag compared to the Stello et al. ( 2013 ) sample. Inspection of panel (b) also reveals there are a population of stars with lower reddening peaking at 0.035 mag. To understand if this population of stars reside in special location, we plotted the spatial distribution of targets for our sample (red dots) and Stello et al. ( 2013 , blue dots) in the entire Kepler field of view. We see fewer targets located in the three modules at the bottom-right corner, which are closest to the Galactic plane and have less stars because of the Kepler
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