We present an independent examination of the parallax zero-point of the Third Gaia Early Data Release (hereafter EDR3), using the LAMOST primary red clump (PRC) stellar sample. A median parallax offset of around 26 μas, slightly larger than that found by examination of distant quasars, is found for both the five- and six-parameter solutions in EDR3, based on samples of over 63,000 and 2000 PRC stars, respectively. Similar to the previous investigation of Lindegren et al., to which we compare our results, the parallax zero-point exhibits clear dependencies on the G magnitudes, colors, and positions of the objects. Based on our analysis, the zero-point of the revised parallax can be reduced to a few μas, and some significant patterns, e.g., discontinuities with stellar magnitude, can be properly removed. However, relatively large offsets (>10 μas) are still found for the revised parallaxes over different positions on the sky.

我们使用 LAMOST 主红团 (PRC) 恒星样本对第三次盖亚早期数据发布（以下简称 EDR3）的视差零点进行了独立检查。根据分别超过 63,000 和 2000 颗PRC 恒星的样本，在 EDR3 中的五参数和六参数解中发现了大约 26 μ 的中值视差偏移，比通过检查遥远类星体发现的略大。与 Lindegren 等人之前的研究类似，我们将我们的结果与之进行比较，视差零点表现出对G大小、颜色和物体位置的明显依赖性。根据我们的分析，修正视差的零点可以减少到几个μ因为，一些重要的模式，例如，恒星大小的不连续性，可以被适当地去除。然而，对于天空不同位置的修正视差，仍然发现相对较大的偏移（>10 μ as）。