标题： 基本金属丰度关系的对比研究：方法对观测演化的影响 显示英文标题

标题： A comparative study of the fundamental metallicity relation: the impact of methodology on its observed evolution

摘要： 我们使用了从 VIPERS 提取的 5487 个红移 z ~ 0.63 的恒星形成星系和来自 GSWLC 目录的本地宇宙中的 143774 个对比星系。我们采用了两类方法：参数化方法和非参数化方法。在前一类方法中，我们在不同红移下比较了受观测偏差影响的 FMR 投影，并在不同构建的控制样本上进行了分析。然后，在 M*-SFR 值区间内比较了不同红移之间的金属丰度差异。在后一种方法中，我们将金属丰度与归一化的 sSFR 进行了关联。用于构建公平且完整样本以研究 MZR 和 FMR 的方法得到了一致的结果，表明这两种关系在 z ~ 0.63 时有小幅但仍然具有统计学意义的演化。特别是，我们观察到一个系统性趋势，即 z = 0.63 样本的中位数金属丰度低于相同 M* 和 SFR 的本地样本。在 M*-SFR 值区间内，低红移和中间红移之间的平均金属丰度差异约为中间红移样本中值金属丰度标准差的 1.8 倍。我们通过 Kolmogorov-Smirnov 检验确认了这一结果。当应用 M*- 完整性标准时，红移间的金属丰度差异减小到中值金属丰度标准差的大约 0.96 倍，因此不再具有统计学显著性。这个结果可能受到限制参数空间的影响，因为较低 M* 的星系差异更大且不在分析范围内。仔细阅读结果及其背后的选取标准对于质量-金属丰度和 FMRs 的研究至关重要。 显示英文摘要

摘要： We used 5487 star-forming galaxies at redshift z~0.63 extracted from the VIPERS and 143774 comparison galaxies in the local Universe from the GSWLC catalog. We employed two families of methods: parametric and non-parametric. In the former approaches, we compared the FMR projections plagued by observational biases on differently constructed control samples at various redshifts. Then, the metallicity difference between different redshifts in M*-SFR bins. In the latter approach, we related the metallicity and the normalized sSFR. The methodologies implemented to construct fair, complete samples for studying the MZR and the FMR produced consistent results showing a small, but still statistically significant evolution of both relations up to z~0.63. In particular, we observed a systematic trend where the median metallicity of the sample at z=0.63 is lower than that of the local sample at the same M* and SFR. The average difference in the metallicity of the low and intermediate redshifts is approximately 1.8 times the metallicity standard deviation of the median, of the intermediate redshift sample, in M*-SFR bins. We confirmed this result using the Kolmogorov-Smirnov test. When we applied the M*-completeness criterion to catalogs, the metallicity difference in redshifts decreased to approximately 0.96 times the metallicity standard deviation of the median, thus not statistically significant. This result may be dominated by the limited parameter space, being the lower M* galaxies where the difference is larger out from the analysis. A careful reading of the results, and their underlying selection criteria, are crucial in studies of the mass-metallicity and FMRs.