中文摘要：

我们在场 48 个金属穷人星系在的一件样品在 LAMOST 调查从 92 510 个星系选择了。这些星系被他们黎明的排放的察觉识别在水平上面衬里 4363，它允许电子温度和氧丰富的直接大小。排放线流动用 Balmer 减少方法为内部灰尘扑灭被改正。与源于的电子温度和电子密度从，我们在我们从的样品获得氧丰富) 到 8.46 () 。我们发现一极其金属穷人星系与。与 multiband 从 FUV 的光度计的数据到 NIR 和大小，我们也决定星的群众和星形成率，基于光谱精力分发试穿和光明分别地。我们发现我们的星系有低、中间的星的群众与，并且高担任主角形成率(SFR ) 与。我们也发现我们的星系的 metallicities 与本地基于的 mass-metallicity 关系一致，当 scatter 是大约 0.28 dex 时。另外，假定系数，我们发现大多数我们的星系跟随本地 mass-metallicity-SFR 关系，但是一大约 0.24 dex 的 scatter 存在，建议 mass-metallicity 关系弱依赖于为那些金属穷人星系的 SFR。

英文摘要：

We present a sample of 48 metal-poor galaxies at z 〈 0.14 selected from 92 510 galaxies in the LAMOST survey. These galaxies are identified by their detection of the auroral emission line[OⅢ]λ4363 above the 3σ level, which allows a direct measurement of electron temperature and oxygen abundance. The emission line fluxes are corrected for internal dust extinction using the Balmer decrement method. With electron temperature derived from [OⅢ]λλ4959, 5007/[OⅢ]λ4363 and electron density from [SⅡ]λ6731/[SⅡ]λ6717, we obtain the oxygen abundances in our sample which range from 12 ＋ log（O/H） = 7.63（0.09 Z_⊙） to 8.46（0.6 Z_⊙）. We find an extremely metal-poor galaxy with 12 ＋ log（O/H） = 7.63 ± 0.01. With multiband photometric data from FUV to NIR and Hαmeasurements, we also determine the stellar masses and star formation rates, based on the spectral energy distribution fitting and Hα luminosity, respectively. We find that our galaxies have low and intermediate stellar masses with 6.39 ≤ log（M/M_⊙） ≤ 9.27, and high star formation rates（SFRs） with-2.18 ≤ log（SFR/M_⊙yr~（-1）） ≤ 1.95. We also find that the metallicities of our galaxies are consistent with the local T_e-based mass-metallicity relation, while the scatter is about 0.28 dex. Additionally,assuming the coefficient of α = 0.66, we find most of our galaxies follow the local mass-metallicity-SFR relation, but a scatter of about 0.24 dex exists, suggesting the mass-metallicity relation is weakly dependent on SFR for those metal-poor galaxies.