论文标题
与DECAM和GAIA的Canis主要恒星过度密度的修订视图：蓝色星星恒星翘曲的新证据
A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars
论文作者
论文摘要
我们提出DECAM成像与Gaia DR2数据相结合，以研究Canis的主要密度。所谓的蓝色羽流星在颜色刻度图的低污垢区域中的存在使我们能够沿其假设核心的视线得出此恒星特征的距离和正确运动。恒星的过度密度在平面下方的低银河纬度（下方）和230 $^\ circ <\ ell <255^\ circ $之间延伸在天空的大面积上。根据Canis Major的轨道轨道，它在银河系周围呈上平面旋转。此外，在平面周围和银河系之间发现了蓝色羽状星的其他过度，证明这些物体不仅与该结构相关联。这些恒星的空间分布是使用Gaia天体数据得出的，证实了Canis主要密度的检测来自银河系磁盘的扭曲结构，而不是从矮星系的积聚。
We present DECam imaging combined with Gaia DR2 data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the color-magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and between 230$^\circ < \ell < 255^\circ$. According to the orbit derived for Canis Major, it presents an on-plane rotation around the Milky Way. Moreover, additional overdensities of Blue Plume stars are found around the plane and across the Galaxy, proving that these objects are not only associated with that structure. The spatial distribution of these stars, derived using Gaia astrometric data, confirms that the detection of the Canis Major overdensity results more from the warped structure of the Milky Way disk than from the accretion of a dwarf galaxy.
