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

翻译后摘要-Mauriski的研究进行涉及创建的最深的调查的位置，绝对自行，多色电荷耦合器件（CCD）测光，和光谱的一个完整的，有限的调查银河系恒星。这项研究建立在早期工作的结果在一个单一的领域在北银河系极（NGP）组装高品质的自行，光度计的光驰，光度丰度和径向速度作为一种手段，探索合并的维度相空间和金属丰度分布的恒星在银河系晕，磁盘，和中间人口II厚盘。在NGP早期高精度自行巡天的发现中有：（1）普遍存在的中间星族II（IPII）厚盘星的大尺度高度和局部归一化;（2）在星族I盘和IPII场星之间有明显平滑的运动学梯度;（3）银河系晕星的逆行旋转。除了光谱数据的深度自行证实了额外的发现逆行移动组晕星4.5千秒差距以上的银道面，这一结果已经允许阐明这种运动学结构只是几个大规模的，恒星流在这一部分的天空。这些调查结果的含义是：（1）晕圈不是一个动态松弛系统，而是似乎含有恒星凝聚体破裂产生的相干移动碎片流，（2）晕圈测量结果之间的差异可能归因于视线的差异，每种情况的特征是局部流动运动，而不是全局描述，（3）晕场星星群的大部分似乎来自恒星系统的吸积，很可能是银河系的卫星。这一结论显然已经被人马座矮球状星系的发现所证实，人马座矮球状星系是银河系潮汐破坏过程中的一颗银河系卫星。 其目的是在银河系沿着两个正交的椭圆面的其他九个区域进行类似的天体测量、光度测量和光谱分析。 将用弗吉尼亚大学PDS显微密度计扫描基特峰4米望远镜的照相底片，以制作恒星目录和测量自行。 WIYN 3.5米望远镜上的HYESTRUCTURE系统的多纤维光谱学将提供速度的第三维以及光谱丰度。这项调查是有史以来对场矮星进行的最深入的原位研究，将允许系统地探测薄盘，中间族II和晕，而不会影响其他类型的银河系结构调查的选择偏差。 通过沿两个正交平面沿着绘制晕相空间分布，将有可能（a）通过寻找相邻场中的类似结构来约束晕流角度相关尺度，（B）测量流的体积过填充因子（在NGP场中发现~3），c寻找场星星流与银河系卫星，球状星团，以及这些对象的对齐平面。 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，光度测量和光谱分析的所有阶段。为了增加对银河系结构和天体测量研究的理解，弗吉尼亚大学在其漫长的历史中一直在进行这些努力，为了大学生和公众的利益，将启动三项额外的教育推广工作。每一项努力都集中在将麦考密克天文台转换为一个独特的、一流的教育设施上：（1）为具有历史意义的26”克拉克折射望远镜配备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，以扩大与课程相关的范围和“向公众开放”的天体测量望远镜夜间教学。CCD将提高大批参观者观看望远镜的效率，为新型本科实验室练习提供基础，演示天文学的现代方法，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方便的望远镜观看机会。(2)教学摄谱仪的增加将填补目前天文学专业课程的一个重要空白。(3)最后，我们将利用麦考密克悠久的天体测量传统，创建一个天文测量设备的博物馆。每年大约有5,000人将利用麦考密克天文台的这些改进。

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.