研究目的
Investigating the properties of the binary cluster Gamma Velorum using the Gaia DR2 astrometric parameters of cluster members pre-selected by spectroscopic observations.
研究成果
The study concludes that Gamma Vel A and B are two independent clusters seen along the same line of sight, with Gamma Vel A being closer than Gamma Vel B by ~38 pc. Gamma Vel A is probably bound and formed the massive star γ2 Vel, while Gamma Vel B is expanding.
研究不足
The study does not take into account possible systematic errors or correlations in Gaia DR2 parallaxes and proper motions. The relative errors on parallaxes are below ~10%, and a conservative systematic error of ±0.1 mas was assumed.
1：Experimental Design and Method Selection:
The study uses Gaia DR2 data for a sample of high-probability cluster members to analyze the 3D kinematics and distances of the two populations, Gamma Vel A and B.
2：Sample Selection and Data Sources:
The list of Gamma Velorum members published by Je?ries et al. (2014) was crossmatched with the Gaia DR2 catalogue.
3：List of Experimental Equipment and Materials:
Gaia DR2 data was used for the analysis.
4：Experimental Procedures and Operational Workflow:
The study performed a maximum-likelihood fit of the 3D distribution of parallaxes and proper motions using two multivariate Gaussian components, one for each population.
5：Data Analysis Methods:
The analysis included deriving astrometric membership probabilities and comparing the parallaxes and proper motions of the cleaned subsamples with the RVs from Je?ries et al. (2014).
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