论文标题
Gaia Edr3揭示了银河盘的翘曲和耀斑
Warp and flare of the Galactic disc revealed with supergiants by Gaia EDR3
论文作者
论文摘要
外带圆盘包含一些特征，例如翘曲和耀斑，其起源仍在争论中。 Gaia数据提供了一个很好的机会，可以在大距离内探测银河盘并研究这些特征。我们得出了平均（老）整体和超级群（代表年轻人口的代表）的密度分布，并使用它们来限制其翘曲和耀斑。通过比较结果，我们研究了这些现象的性质如何取决于研究的人群。我们使用露西的反卷积方法来恢复校正后的恒星计数作为距离的函数，从中我们得出密度分布。我们发现，超级巨人具有不对称的经线，最大幅度为$ z_w = 0.658 $ kpc，最小振幅为$ z_w = -0.717 $ kpc，距离为$ r = [19.5,5,20] $ kpc，$ kpc几乎是两张数份量的幅度，这是整个人群的振幅的两个。我们发现整个人群的爆发很大，尤其是在厚盘中。比例高度从$ h_ {z，厚} \大约0.8 $ kpc和$ h_ {z，thin} \大约0.3 $ kpc在太阳能社区中，到$ h_ {z，厚} \ 3 $ kpc和$ kpc和$ h_ {z，thin}，thin} \ of thin 0.7 $ kpc in the emote of the Emernegions of the Miles of the MILK）（$ kp）（$ kp）（$ kp）（$ kp）（$ kp）（$ kp）（$ k。 Supergiants的人口只有很小的耀斑。
The outer Galactic disc contains some features such as the warp and flare, whose origin is still debated. The Gaia data provide an excellent opportunity to probe the Galactic disc at large distances and study these features. We derive the density distributions of the average (old) whole population and the supergiants (representative of a young population), and we use them to constrain their warp and flare. By comparing the results, we study how the properties of these phenomena depend on the studied population. We used Lucy's deconvolution method to recover corrected star counts as a function of distance, from which we derive the density distribution. We find that supergiants have an asymmetric warp, reaching a maximum amplitude of $z_w=0.658$ kpc and minimum amplitude of $z_w=-0.717$ kpc at a distance of $R=[19.5,20]$ kpc, which is almost twice as high as the amplitude of the whole population of the disc. We find a significant flare of the whole population, especially in the thick disc. The scale height increases from $h_{z,thick}\approx 0.8$ kpc and $h_{z,thin}\approx 0.3$ kpc in the solar neighbourhood, to $h_{z,thick} \approx 3$ kpc and $h_{z,thin}\approx 0.7$ kpc in the remote regions of the Milky Way ($R\approx 18$ kpc). The supergiants' population has only a small flare.
