Table 1
Parameters in the comparison of metallicity distributions [Fe/H] for different subsamples of LAMOST-DR3 giants with R1 < R < R1 + ΔR, |z| < 5 kpc, and R2 < R < R2 + ΔR, |z| ≥ 5 kpc, respectively, such that ⟨r1⟩≈⟨r2⟩.
| R1 | Δ R | R2 | N1 | N2 |  |
 |
PK−S |
|---|---|---|---|---|---|---|---|
| 16 | 2 | 11.5 | 2160 | 1850 | 18.8 | 0.23 | 1.9E−298 |
| 18 | 2 | 13.5 | 699 | 1352 | 17.3 | 0.25 | 1.0E−99 |
| 20 | 4 | 15.0 | 359 | 1813 | 15.5 | 0.25 | 1.6E−27 |
| 24 | 4 | 18.5 | 88 | 992 | 14.2 | 0.26 | 0.014 |
| 28 | 8 | 21.5 | 54 | 936 | 12.6 | 0.24 | > 0.32 |
| 36 | 16 | 26.0 | 17 | 649 | 11.0 | 0.28 | > 0.32 |
Notes. Thefirst three columns indicate the Galactocentric radial range, Cols. 4 and 5 give the number of stars, Col. 6 gives the average signal-to-noise ratio of the first subsample, Col. 7 gives the average error of the [Fe/H] measurement in the first subsample, and Col. 8 gives the probability derived from a Kolmogorov-Smirnov test that the two metallicity distributions are identical within the random fluctuations. The distances are listed in kpc.
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