论文标题
GAIA数据版本3：热星径向速度
Gaia Data Release 3: Hot-star radial velocities
论文作者
论文摘要
第二个GAIA数据发布DR2包含恒星的径向速度，其有效温度= TEFF = 6900K。第三个数据发布Gaia Dr3将其扩展到TEFF = 14,500K。我们得出了热星的径向速度（即在TEFF = 6900-14.00-14,500 k范围内）radial on radial（即，在teff = 6900-14,14,500 k范围内）。径向速度通过测量模板频谱的多普勒移位的标准技术确定，该技术被比较与观察到的光谱。 RVS波长范围非常有限。钙红外三联体与热星中的氢气线的近距离和系统的蓝色偏移可能导致径向速度的系统偏移。对于热星，我们开发了一个特定的代码来改善模板频谱的选择，从而避免了这种系统的偏移。有了改进的代码，通过校正，我们提出了DR3存档径向速度的提议，我们获得了与参考值在3 km/s以内（中位数）一致的值。由于需要使用改进的代码所需的S/N，因此DR3中的热星径向速度大多限于在RVS波长频带<= 12 mag中大小的恒星。
The second Gaia data release, DR2, contained radial velocities of stars with effective temperatures up to Teff = 6900 K. The third data release, Gaia DR3, extends this up to Teff = 14,500 K. We derive the radial velocities for hot stars (i.e. in the Teff = 6900 - 14,500 K range) from data obtained with the Radial Velocity Spectrometer (RVS) on board Gaia. The radial velocities were determined by the standard technique of measuring the Doppler shift of a template spectrum that was compared to the observed spectrum. The RVS wavelength range is very limited. The proximity to and systematic blueward offset of the calcium infrared triplet to the hydrogen Paschen lines in hot stars can result in a systematic offset in radial velocity. For the hot stars, we developed a specific code to improve the selection of the template spectrum, thereby avoiding this systematic offset. With the improved code, and with the correction we propose to the DR3 archive radial velocities, we obtain values that agree with reference values to within 3 km/s (in median). Because of the required S/N for applying the improved code, the hot star radial velocities in DR3 are mostly limited to stars with a magnitude in the RVS wavelength band <= 12 mag.
