Mapping of Milky Way Cepheid Variables

银河系造父变星绘图

• 批准号: 1945519
• 金额: --
• 依托单位: University of Cambridge
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2017
• 资助国家: 英国
• 起止时间: 2017 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-1945519
• 关键词: Mapping; Milky; Way; Cepheid; Variables

Cepheid Variables are young stars that physically pulsate causing a variation in their luminosity over time. An intrinsic relation exists between the period of these pulsations and the luminosity of these stars. They have therefore become vital distance indicators. Their young age implies they should mostly be found within the galactic disk. Any outliers would be of interest to merging history of the Milky Way: dwarf satellite galaxies interacting and colliding with our galaxy. Such events could throw the young Cepheids out of the disk to higher latitudes. The current Gaia DR1 data and the future DR2 release do no contain any time domain information of the cepheids contained within. Therefore, other selection criteria is needed to identify these stars in the data. This causes issues of contamination from other stellar types. Work in this project seeks to formulate optimal selection criteria to map the Cepheids and then devise theoretical models to explain how the observed distribution could have formed. Such work could be combined with the previous mappings of RR Lyrae variables to identify substructure within our Galaxy.

头孢虫变量是年轻的恒星，随着时间的流逝，物理脉动会导致其发光度变化。这些脉动的时期与这些恒星的光度之间存在固有的关系。因此，它们已成为至关重要的距离指标。他们的年龄意味着它们主要应该在银河磁盘中找到。合并银河系的历史的任何离群值都将有兴趣：矮卫星星系与我们的星系互动并相撞。这样的事件可能会使年轻的头虫从磁盘上降到更高的纬度。当前的GAIA DR1数据和未来的DR2发行版不包含内部包含的头域信息的任何时间域信息。因此，需要其他选择标准来识别数据中的这些恒星。这导致其他恒星类型的污染问题。该项目中的工作旨在制定最佳选择标准以绘制头目，然后设计理论模型，以解释观察到的分布如何形成。此类工作可以与先前的RR Lyrae变量映射结合使用，以识别我们银河系中的子结构。