论文标题
GAIA数据发布3个属性和径向速度的验证
Gaia Data Release 3 Properties and validation of the radial velocities
论文作者
论文摘要
GAIA数据发布3（Gaia DR3）包含第二次释放的径向速度。它基于名义任务的前34个月收集的光谱。较长的时间基线和管道的改进使得将处理极限从Gaia DR2中的GRVS = 12推到GRVS = 14 mag成为可能。在本文中，我们描述了为Gaia DR3实施的新功能，这是在处理和后处理过程中应用的质量过滤器以及已发布速度的属性和性能。对于Gaia DR3，升级或添加了几个功能。 （删节）Gaia DR3包含33 812 183星的径向速度的组合。对于Gaia Dr2，对于明亮的星（GRVS \ leq 12 mag），温度间隔已从[3600，6750] k中的Teff \ teff \ in [3100，14500] k中膨胀到teff \ in [3100，14500] k中，[3100，14500] k对于fainter恒星而言。径向速度采样了银河系的重要部分：它们到达了圆盘中银河中心以外的几公斤PARSEC，并垂直垂直进入内部光环约10-15 kpc。速度的正式精度为1.3 km/s，在GRVS = 12和6.4 km/s时，GRVS = 14 mag。速度零点表现出很小的系统趋势，幅度从grvs = 11 mag开始，在GRVS = 14 mag处达到约400 m/s。提供了一个更正公式，可以应用于已发布的数据。 GAIA DR3速度量表与Apogee，Galah，Ges和Rave达成满意的一致性，并且系统的差异通常不超过几百m/s。还用特定的对象说明了径向速度的特性：开放簇，球形簇以及大麦芽云（LMC）。例如，数据的精度允许映射球状群集47 TUC和LMC的视线旋转速度。
Gaia Data Release 3 (Gaia DR3) contains the second release of the combined radial velocities. It is based on the spectra collected during the first 34 months of the nominal mission. The longer time baseline and the improvements of the pipeline made it possible to push the processing limit, from Grvs = 12 in Gaia DR2, to Grvs = 14 mag. In this article, we describe the new functionalities implemented for Gaia DR3, the quality filters applied during processing and post-processing and the properties and performance of the published velocities. For Gaia DR3, several functionalities were upgraded or added. (Abridged) Gaia DR3 contains the combined radial velocities of 33 812 183 stars. With respect to Gaia DR2, the interval of temperature has been expanded from Teff \in [3600, 6750] K to Teff \in [3100, 14500] K for the bright stars ( Grvs \leq 12 mag) and [3100, 6750] K for the fainter stars. The radial velocities sample a significant part of the Milky Way: they reach a few kilo-parsecs beyond the Galactic centre in the disc and up to about 10-15 kpc vertically into the inner halo. The median formal precision of the velocities is of 1.3 km/s at Grvs = 12 and 6.4 km/s at Grvs = 14 mag. The velocity zero point exhibits a small systematic trend with magnitude starting around Grvs = 11 mag and reaching about 400 m/s at Grvs = 14 mag. A correction formula is provided, which can be applied to the published data. The Gaia DR3 velocity scale is in satisfactory agreement with APOGEE, GALAH, GES and RAVE, with systematic differences that mostly do not exceed a few hundreds m/s. The properties of the radial velocities are also illustrated with specific objects: open clusters, globular clusters as well as the Large Magellanic Cloud (LMC). For example, the precision of the data allows to map the line-of-sight rotational velocities of the globular cluster 47 Tuc and of the LMC.
