发表机构
Institute of Astronomy of V.N. Karazin Kharkiv National University; INAF–Osservatorio Astrofisico di Torino; Main Astronomical Observatory of the NAS of Ukraine（哈尔科夫国立大学V.N.卡拉金天体物理研究所; 意大利国家天体物理研究所都灵天文台; 乌克兰国家科学院主天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用Gaia DR3约1300万颗亮巨星，基于Bottlinger方程非线性最小二乘自洽求解，测得太阳银心距8.165 kpc、本地角速度28.477 km/s/kpc及太阳本动速度，并发现银心距受示踪星垂直结构影响。
AI 中文摘要
太阳银心距$R_0$与银河系本地运动学参数一起，为银河系结构和旋转提供了基本约束。随着Gaia DR3星表的高精度天体测量，其精确测定已成为可能。我们采用基于Bottlinger方程的非线性最小二乘框架中的自洽方法，确定了银心距、太阳本动速度分量$(u_0,v_0,w_0)$以及银河系旋转的本地角速度$\omega_0$。Bottlinger方程应用于从Gaia DR3中选取的约1300万颗亮巨星$(M_G<4)$。分析针对两个子样本进行：一个以薄盘为主的样本（|z|<0.5 kpc）和一个薄盘与厚盘混合的样本（|z|<1.0 kpc）。运动学参数使用非线性广义最小二乘法估计。对于以薄盘为主的样本，我们得到$R_0=8.165\pm0.024$kpc和银河系旋转的本地角速度$\omega_0=28.477\pm0.002$ km/s/kpc。太阳本动速度分量为$(u_0,v_0,w_0)=(9.261\pm0.006,16.593\pm0.008,7.686\pm0.008)$km/s。包含薄盘和厚盘混合恒星导致$R_0$出现系统性偏移，得到$R_0=8.333\pm0.022$kpc，而太阳本动速度和本地角速度在不确定度内保持一致。所得到的银河系运动学参数与最近独立测定结果一致。太阳本动速度参数和本地角速度在不同垂直选择下保持稳定，但恢复的银心距对所采用的恒星样本表现出系统性依赖，表明在确定$R_0$时应考虑示踪星群的垂直结构。
英文摘要
The solar Galactocentric distance, $R_0$, together with the local kinematic parameters of the Milky Way, provides fundamental constraints on the Galactic structure and rotation. Their accurate determination has become possible with the hight astrometric precision of Gaia DR3 catalogue. We determine the Galactocentric distance, the Solar peculiar motion components $(u_0,v_0,w_0)$, and the local angular velocity of Galactic rotation, $ω_0$, using a self-consistent approach based on Bottlinger's equations within a nonlinear least-squares framework. Bottlinger's equations were applied to approximately 13 million luminous giant stars $(M_G<4)$ selected from Gaia DR3. The analysis was carried out for two subsamples: a thin disk dominated sample (|z|<0.5 kpc) and a mixed thin and thick disk sample (|z|<1.0 kpc). The kinematic parameters were estimated using a nonlinear generalized least-squares method. We obtained $R_0=8.165\pm0.024$kpc and a local angular velocity of Galactic rotation $ω_0=28.477\pm0.002$ km/s/kpc for the thin disk dominated sample. The Solar peculiar motion components are $(u_0,v_0,w_0)=(9.261\pm0.006,16.593\pm0.008,7.686\pm0.008)$km/s. Including mixed thin and thick disk stars resulted in a systematic shift in $R_0$, yielding $R_0=8.333\pm0.022$kpc, while the Solar peculiar motion and local angular velocity remain consistent within uncertainties. The Galactic kinematic parameters derived are consistent with recent independent determinations. The Solar peculiar motion parameters and the local angular velocity remain stable for different vertical selections, the recovered Galactocentric distance exhibits a systematic dependence on the adopted stellar sample, indicating that the vertical structure of the tracer population should be taken into account when determining $R_0$.
Comments12 pages, 10 figures
