"CAREER: The Stellar Phase Space and Abundance Distributions of the Stars of the Milky Way"

要进行的研究包括创建最深的位置测量、绝对自行测量、多色电荷耦合器件(CCD)光度测量和光谱测量，以便对银河系恒星进行完整的、星等有限的测量。这项研究建立在早期在北银河极(NGP)的单一场中收集高质量自行、光度视差、光度丰度和径向速度的结果的基础上，作为一种手段来探索银晕、盘和中间族II厚盘中恒星的组合维相空间和金属丰度分布。早些时候在NGP进行的高精度自行测量的发现包括：(1)普遍存在的中间种群II(IPII)厚盘恒星的大尺度高度和局部归一化；(2)种群I盘和IPII场星之间明显平滑的运动梯度；以及(3)银晕恒星的逆行自转。将光谱数据添加到深自行中，证实了在银河面上方又发现了4.5kpc的晕星逆行运动群，这一结果使我们能够阐明这一运动学结构只是这部分天空中几个大尺度恒星流之一。这些发现的意义是：(1)光晕不是一个动力学松弛的系统，而是似乎包含恒星聚集破裂时产生的连贯运动的碎片流；(2)光晕探测结果之间的差异可能是由于视线不同造成的，每个视线的特点是局部流动运动，而不是全球描述；(3)大部分晕场恒星群似乎来自恒星系统，最有可能的是银河系卫星。这一结论显然已被射手座矮球星系的发现所证实，射手座矮球星系是银河系潮汐分裂过程中的一个银河系卫星。其目的是在银河系两个垂直的子午面上的其他九个领域进行类似的天体测量、光度和光谱分析。来自Kitt Peak 4米望远镜的照相底片将用弗吉尼亚大学的PDS显微密度计扫描，以构建恒星表并测量自身运动。WIYN 3.5米望远镜上的Hydra系统的多纤维光谱学将提供第三维的速度和光谱丰度。这项调查是有史以来对场矮星进行的最深入的现场研究，它将允许系统地探测薄盘、中间群II和晕，而不会出现影响其他类型的银河系结构调查的选择偏差。通过绘制沿两个子午面的晕相空间分布图，将有可能(A)通过寻找相邻场中的相似结构来约束晕流角相关尺度，(B)测量晕流(在NGP场中被发现为~3)在晕中的体积超填因子，以及c寻找场星流与银河卫星、球状星团和这些天体的排列平面之间的关联。该研究计划涉及本科生和研究生的广泛参与，他们参与了天体测量、光度和光谱分析的所有阶段，实际上是至关重要的。为了增加对银河结构和天体测量研究的了解，弗吉尼亚大学在这些努力中进行了漫长的历史，将启动三项额外的教育推广努力，以造福于大学学生和普通公众。每项工作都集中在将麦考密克天文台改造成独特的一流教育设施：(1)历史悠久的26英寸克拉克折射望远镜的新仪器将提供从目镜到CCD观测的快速转换，作为一种手段，扩大与课程相关的和利用天文望远镜对公众开放的夜间教学的范围。CCD将提高大批参观者观看望远镜的效率，为新型本科生实验室练习提供基础，展示现代天文学方法，允许通过计算机显示实时望远镜图像进行课堂教学，并为老年人、残疾人或非常年轻的参观者提供更容易的望远镜观看途径。(2)增加一名教学光谱仪将填补目前天文专业的一个重要空白。(3)最后，我们将利用麦考密克悠久的天体测量传统，打造一座独一无二的天文测量仪器博物馆。每年大约有5000人将从麦考密克天文台的这些改进中受益。

Abstract - Majewski The research to be carried out involves the creation of the deepest survey of positions, absolute proper motions, multi-color charged-coupled-device (CCD) photometry, and spectroscopy for a complete, magnitude limited survey of Galactic stars. The study builds upon the results from earlier work in a single field at the North Galactic Pole (NGP) to assemble high quality proper motions, photometric parallaxes, photometric abundances and radical velocities as a means to explore the combined dimensional phase space and metallicity distribution of stars in the Galactic halo, disk, and Intermediate Population II thick disk. Among the discoveries of this earlier, high precision proper motion survey at the NGP were: (1), the large scale height and local normalization of the ubiquitous Intermediate Population II (IPII) thick disk stars; (2), an apparently smooth kinematical gradient between the population I disk and IPII field stars; and (3), a retrograde rotation for the Galactic halo stars. The addition of spectroscopy data to the deep proper motions has confirmed the additional discovery of a retrograde moving group of halo stars 4.5 kpc above the Galactic plane, and this result has allowed the elucidation of this kinematical structure as just one of several large scale, stellar streams in this part of the sky. The implications of these findings are: (1) the halo is not a dynamically relaxed system, but rather seems to contain streams of coherently moving debris from the break-up of stellar agglomerations, (2) differences among halo survey results might be attributable to differences in lines of sight, each characterized by local streaming motions rather than by global descriptions, and (3) the bulk of the halo field star population appears to be derived from the accretion of stellar systems, most likely Galactic satellites. This conclusion has apparently been confirmed with the discovery of the Sagittarius dwarf spheroidal galaxy, a Galactic satellit e in the process of tidal disruption by the Milky Way. The aim is to carry out similar astrometric, photometric and spectroscopic analyses in nine other fields that lie along two orthogonal, meridional planes of the Galaxy. Photographic plates from the Kitt Peak 4-m telescope will be scanned with the University of Virginia PDS microdensitometer to construct stellar catalogues and for the measurement of proper motions. Multifiber spectroscopy with the HYDRA system on the WIYN 3.5-m telescope will provide the third dimension of velocity as well as spectroscopic abundances. This survey, the deepest in situ study of field dwarf stars ever carried out, will allow systematic probing of the thin disk, Intermediate population II and halo without the selection biases that affect other types of Galactic structure surveys. By mapping the halo phase space distribution along the two meridional planes, it will be possible to (a) constrain the halo stream angular correlation scale, by looking for similar structures in adjacent fields, (b) measure the volume overfilling factor of streams (found to be ~3 in the NGP field) in the halo, and c look for correlations between the field star streams and Galactic satellites, globular clusters, and the alignment planes of these objects. The research program involves extensive involvement of both undergraduate and graduate students, who are involved, indeed critical, to all phases of the astrometric, photometric and spectroscopic analysis. To increase understanding Galactic structure and astrometric research that has been conducted at the University of Virginia throughout its long history in these endeavors, three additional efforts of educational outreach will be initiated for the benefit of both University students and the general public. Each effort centers on conversion of the McCormick Observatory to a unique, first class educational facility: (1) New instrumentation for the historic 26" Clark refractor telescope will provide a quick c onversion from eyepiece to CCD observation, as a means to broaden the scope of both course- related and "Open to the Public" night instruction with the astrometric telescope. The CCD will increase the efficiency of telescope viewing by large groups of visitors, provide the basis for new kinds of undergraduate laboratory exercises, demonstrate modern methods in astronomy, allow classroom instruction via computer display of live telescope images, and provide easier access to telescope viewing for elderly, disabled or very young visitors. (2) The addition of a teaching spectrograph will fill an important gap in the present astronomy majors program. (3) Finally, we will take advantage of McCormick's long tradition of astrometry to create a one of a kind museum of astronomical measuring devices. On the order of 5,000 people per year will take advantage of these improvements to the McCormick Observatory.