arXiv 2103.019702021-03astro-ph.GA

盖亚EDR3揭示的星系螺旋结构

Galactic spiral structure revealed by Gaia EDR3

E. Poggio, R. Drimmel, T. Cantat-Gaudin, P. Ramos, V. Ripepi, E. Zari, R. Andrae, R. Blomme, L. Chemin, G. Clementini, F. Figueras, M. Fouesneau, Y. Frémat, A. … 展开作者

E. Poggio, R. Drimmel, T. Cantat-Gaudin, P. Ramos, V. Ripepi, E. Zari, R. Andrae, R. Blomme, L. Chemin, G. Clementini, F. Figueras, M. Fouesneau, Y. Frémat, A. Lobel, D. J. Marshall, T. Muraveva, M. Romero-Gómez

备注：: 10 pages, 7 figures. Accepted for publication in A&A. The maps presented in this paper are publicly available in the form of a Jupyter Notebook at https://github.com/epoggio/Spiral_arms_EDR3.git
发表信息：: A&A 651, A104 (2021)
DOI：: 10.1051/0004-6361/202140687

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摘要：

利用盖亚早期数据发布3（EDR 3）的天体测量和综合测光，我们绘制了银河系盘中距离太阳几千秒差距内的年轻上主序星（UMS）、疏散星团和经典造父变星的密度变化分布。利用二元核密度估计和小波变换导出了银河系盘中UMS星相对过/欠密度区域的地图。由此产生的高密度图显示出大规模的拱门，在整个采样体积上以一种密集但连贯的方式延伸，表明太阳附近的旋臂部分的位置。UMS超密度的峰值与年轻且本征明亮的疏散星团的分布相匹配。通过对经典造父变星的样本进行小波变换，我们发现它们的超密度可能在更大的尺度上（距离太阳约10 kpc）延伸了旋臂部分。虽然基于UMS样本得到的地图与之前的人马座-船底座旋臂模型基本一致，但第III象限（银河系圆拱$180^\circ < l < 270^\circ$）旋臂的几何形状与许多之前的模型有很大不同。特别是，我们发现我们的地图有利于英仙座臂的更大的俯仰角，并且本地臂延伸到第三象限至少4 kpc，超过太阳的位置，使其总长度至少为8 kpc。

英文摘要：

Using the astrometry and integrated photometry from the Gaia Early Data Release 3 (EDR3), we map the density variations in the distribution of young Upper Main Sequence (UMS) stars, open clusters and classical Cepheids in the Galactic disk within several kiloparsecs of the Sun. Maps of relative over/under-dense regions for UMS stars in the Galactic disk are derived, using both bivariate kernel density estimators and wavelet transformations. The resulting overdensity maps exhibit large-scale arches, that extend in a clumpy but coherent way over the entire sampled volume, indicating the location of the spiral arms segments in the vicinity of the Sun. Peaks in the UMS overdensity are well-matched by the distribution of young and intrinsically bright open clusters. By applying a wavelet transformation to a sample of classical Cepheids, we find that their overdensities possibly extend the spiral arm segments on a larger scale (~10 kpc from the Sun). While the resulting map based on the UMS sample is generally consistent with previous models of the Sagittarius-Carina spiral arm, the geometry of the arms in the III quadrant (galactic longitudes $180^\circ < l < 270^\circ$) differs significantly from many previous models. In particular we find that our maps favour a larger pitch angle for the Perseus arm, and that the Local Arm extends into the III quadrant at least 4 kpc past the Sun's position, giving it a total length of at least 8 kpc.

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