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tokens: line and the corrected as a dashed line after an overall shift of 0.09 dex; different markers and colors stand for different reporters. The right panel shows the distribution of differences between A (Li) LAMOST and A (Li) H.Res. and the result of the Gaussian fit overplotted with a red solid line. Table 1 Information of the Li-rich Giants Reported by Previous Works 3.3.2. Random Errors In our results, 2746 giants have repeated observations; these could be used to estimate the random errors. We plotted the differences in A (Li) between repeated observations as a function of S/N, T eff , log g , [Fe/H], and A (Li) in Figure 6 . In panel (a), all the 2746 objects with repeated observations are included, which shows that the random errors are sensitive to the S/N decreasing from 0.3 to 0.1 dex with an increasing S/N. In order to avoid the influence of the S/N, only 1118 objects with high-quality data (S/N ≥ 200) were used in the rest panels. Panels (b) and (c) show that the random errors increase from 0.1 to 0.2 dex with increasing T eff or log g , which may be due to the fact that the lithium line at 6708 Å is stronger at low T eff or log g . The random errors have no obvious relation to the [Fe/H], as shown in panel (d), which may be because the strength of the lithium line has no obvious relationship to [Fe/H]. And panel (e) shows that the scatter of the differences of A (Li) remains same when A (Li) goes from 2.0 to 4.5 and is slightly larger in the bin of 1.5 ≤ A (Li) 2.0. Note that the lithium line at 6708 Å is strong enough to be detected when A (Li) is higher than 2.0. The typical value of random errors is 0.2 dex. Figure 6. Differences in A (Li) between multiple observations vs. S/N, T eff , log g , [Fe/H], and A (Li). All the 2746 objects with repeated observations are included in panel (a); only 1118 objects with high-quality data (S/N ≥ 200) were used in the rest panels. The bin sizes are 100, 200 K, 0.3 dex, 0.3 dex, and 0.5 dex, respectively. The red dots are the mean value and the error bars are the standard deviation of the differences in every bin. 4. Results The giants with A (Li) ≥ 1.5 are usually defined as Li-rich giants. In our results, 10,535 Li-rich giants are identified. Their information is listed in Table 2 , including the LAMOST ID, positions, stellar atmospheric parameters provided by LASP, A (Li), and the observed date. Figure 7 shows the histograms of the number of our Li-rich giant sample versus T eff , log g , and [Fe/H], respectively. For the distribution of temperature, there is a peak around 4800 K, and there might be another peak around 5100 K. There are two clear peaks around log g ∼ 2.5 and 3.5 dex, the first is corresponding to the red giant branch and red clump stars. In addition, the distribution of metallicity shows a clear peak around [Fe/H] ∼ −0.15 and a symmetric profile from ∼−0.8 to +0.5 dex. For the stars with metallicity lower than −0.8 dex, there seems to be a second peak in the range of −1.5 to