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Damped and Sub-damped Lyman-alpha Absorbers: What Are They, and What Do They Tell Us About Galaxy Evolution?

阻尼和亚阻尼莱曼阿尔法吸收器：它们是什么，它们告诉我们关于星系演化的什么信息？

基本信息

批准号：
0908890
负责人：
Varsha Kulkarni
金额：
$ 26.45万
依托单位：
University South Carolina Research Foundation
依托单位国家：
美国
项目类别：
Standard Grant
财政年份：
2009
资助国家：
美国
起止时间：
2009-09-01 至 2013-08-31
项目状态：
已结题

来源：
https://www.nsf.gov/awardsearch/showAward?AWD_ID=0908890&HistoricalAwards=false
关键词：
Damped Sub damped Lyman alpha

项目摘要

This award is funded under the American Recovery and Reinvestment Act of 2009 (Public Law 111-5).Dr Kulkarni will study the gas between galaxies and around nascent galaxies by observing its absorption lines in the spectra of more distant bright quasars. Generally, the densest gas, in the damped Lyman-alpha absorbers, is already forming stars. If these absorbers represented young galaxies, we would expect the abundance of heavy elements to rise from a low value towards roughly the solar levels at the present day, as dying stars return these elements to the gas. Instead, most such gas clouds are metal-poor. Dr Kulkarni and her collaborators have shown that 'sub-damped Lyman-alpha absorbers', of slightly lower density, do become more metal-rich over time as expected. This suggests that much star-forming activity happens in these less-dense clouds. Dr Kulkarni will conduct further studies of both damped and sub-damped Lyman-alpha absorbers. She will take spectra for a larger sample, to elucidate the physical and chemical differences between systems of low and high metal content. Using adaptive-optics techniques at the Gemini and Keck telescopes, she will obtain deep images of their star-forming regions in the near infrared. With European collaborators, she will obtain spatially resolved spectroscopy at the Very Large Telescope, to trace the motions of gas ionized by the young stars and examine gradients in gas properties. Spectroscopy of binary quasars and gravitationally lensed quasars with the Magellan telescopes will probe the spatial extent of the absorbing gas.A graduate student will be trained by participating in the research. Dr Kulkarni will continue her outreach talks at local schools and organizations, and public observing sessions at the campus observatory. She has a strong record of mentoring students from under-represented groups in research, which she will continue.

该奖项由 2009 年美国复苏和再投资法案（公法 111-5）资助。库尔卡尼博士将通过观察更遥远的明亮类星体光谱中的吸收线来研究星系之间和新生星系周围的气体。一般来说，阻尼莱曼阿尔法吸收体中密度最大的气体已经形成恒星。如果这些吸收体代表年轻的星系，我们预计重元素的丰度将从低值上升到当今太阳水平，因为垂死的恒星将这些元素返回到气体中。相反，大多数此类气体云都缺乏金属。库尔卡尼博士和她的合作者已经证明，密度稍低的“次阻尼莱曼α吸收体”确实会随着时间的推移变得更加富含金属，正如预期的那样。这表明许多恒星形成活动发生在这些密度较小的云中。库尔卡尼博士将对阻尼和亚阻尼莱曼阿尔法吸波器进行进一步研究。她将采集更大样本的光谱，以阐明低金属含量和高金属含量系统之间的物理和化学差异。利用双子座和凯克望远镜的自适应光学技术，她将获得近红外恒星形成区域的深层图像。她将与欧洲合作者一起在甚大望远镜中获得空间分辨光谱，以追踪年轻恒星电离的气体的运动并检查气体特性的梯度。使用麦哲伦望远镜对双类星体和引力透镜类星体进行光谱分析将探测吸收气体的空间范围。一名研究生将通过参与这项研究来接受培训。库尔卡尼博士将继续在当地学校和组织进行外展演讲，并在校园天文台举办公众观察活动。她在指导来自代表性不足群体的学生进行研究方面有着良好的记录，她将继续这样做。