论文标题
基于GAIA EDR3目录的OB2星的速度的银河螺旋密度波参数的估计
Estimation of Galactic Spiral Density Wave Parameters Based on the Velocities of OB2 stars from the Gaia EDR3 Catalogue
论文作者
论文摘要
我们已经通过Xu等人选择的正确运动和视差分析了9750 OB2星的运动学。来自Gaia EDR3目录。这些恒星的相对视差错误不超过10 \％。基于整个星星样本，我们发现了速度$（u，v）_ \ odot =（7.17,7.37）\ pm（0.16,0.24）$ s $ s $ s $ s $^{ - 1} $，以及银河系旋转的角度速度的成分kpc $^{ - 1} $，$ω^{'} _ 0 = -4.008 \ pM0.022 $ km s $ s $^{ - 1} $ kpc $^{ - 2} $，$ω^{'} _ 0 = 0.671太阳能距离的星系的线性旋转速度为$ v_0 = 240.6 \ pm3.0 $ km s $ s $^{ - 1} $，用于所采用的$ r_0 = 8.1 \ pm0.1 $ kpc。从它们计算出1812颗OB2星，具有测量线速度，空间速度$ v_r $和$ΔV_{CRICE} $是根据它们计算的。基于对径向和残留切向速度的光谱分析，我们获得了以下估计值：$ f_r = 4.8 \ pm0.7 $ km s $ s $^{ - 1} $，$f_θ= 4.1 \ pm0.9 $ km s $ s $ s $ s $ s $ $λ_θ= 2.2 \ pm0.4 $ kpc，$（χ_\ odot）_r = -116 \ pm12^\ circ $和$（χ_\ odot）_θ= -156 \ pm14^\ pm14^\ circ $ circ $用于所采用的四臂（$ m = 4 $）superal模式。因此，两个速度扰动幅度在高显着性水平上都是非零的。
We have analyzed the kinematics of 9750 OB2 stars with proper motions and parallaxes selected by Xu et al. from the Gaia EDR3 catalogue. The relative parallax errors for these stars do not exceed 10\%. Based on the entire sample of stars, we have found the velocities $(U,V)_\odot=(7.17,7.37)\pm(0.16,0.24)$ km s$^{-1}$ and the components of the angular velocity of Galactic rotation: $Ω_0 =29.700\pm0.076$ km s$^{-1}$ kpc$^{-1}$, $Ω^{'}_0 =-4.008\pm0.022$ km s$^{-1}$ kpc$^{-2}$, and $Ω^{''}_0 = 0.671\pm0.011$ km s$^{-1}$ kpc$^{-3}$, where the linear rotation velocity of the Galaxy at the solar distance is $V_0=240.6\pm3.0$ km s$^{-1}$ for the adopted $R_0=8.1\pm0.1$ kpc. There are 1812 OB2 stars with measured line-of-sight velocities, and the space velocities $V_R$ and $ΔV_{circ}$ have been calculated from them. Based on a spectral analysis independently for the radial and residual tangential velocities, we have obtained the following estimates: $f_R=4.8\pm0.7$ km s$^{-1}$, $f_θ=4.1\pm0.9$ km s$^{-1}$, $λ_R=2.1\pm0.2$ kpc, $λ_θ=2.2\pm0.4$ kpc, $(χ_\odot)_R=-116\pm12^\circ$, and $(χ_\odot)_θ=-156\pm14^\circ$ for the adopted four-armed ($m = 4$) spiral pattern. Thus, both velocity perturbation amplitudes are nonzero at a high significance level.
