国际评估 LAM ST O LAM ST 将会是一个适合于研究广泛领域中重 O 大天体物理问题的世界级巡天设备。 鉴于其集光面积和光纤数目， LAM ST 潜在的 O 功能将比 SD 数字巡天和 2dF 高出 10 到 15 SS 倍。如果能达到了这样高的指标，它将是一个 巨大的飞越，并打开了一个广阔的“探索空 间”。 LAM ST 将会有非常好的科学产出。望远镜一 O 定能够在河外天文学与银河系天文学方面产生 世界级的研究成果。
Richrd Ellis ，美国加州理工学院技术研 究所天文学部的斯蒂尔教授、光学天文台 台长，曾任英国剑桥大学天文研究所所长。。。 光谱是天文研究中最重要的一个方面。有些人 没有注意到过去的 5 年中许多成像巡天望远镜 Multi-object spectroscopic has rich heritage but it only goes back to about 1970s on largetelescopes. My first encounter with LAMOST project was when I was in Cambridge England, and we 的开始投入使用，… 但是我们还是不断地意识had a visitation from Chinese astronomers who were proposing the LAMOST project, the extremelyexciting ambitious, and during the time the England involved in the 2dF red shift survey which 到我们需要光谱信息才能深入研究天体。现在was a modest 400 fibers on a 4m telescope. If I can just agress a moment we have seen so muchdiscovery space with the 2dF survey and it is comparative survey in United States for Sloan 中国天文界在大视场光谱巡天方面占据了强有Digital Sky Survey. But it shows us so much value in spectroscopy. I think spectroscopy is afundamental aspect of astronomy. Someone neglected over the last 5 years we commissioned the 力的位置，足以让国际天文同行羡慕中国可以large numbers of imaging telescopes, the PanStarrs, the Dark Energy Survey, VISTA UK infraredsurvey, huge investment in imaging. And time to time again, we learned we need spectra to 充分利用这些新的成像巡天观测结果。interpret the objects. And Chinese astronomy is now in tremendously powerful position to forinternational envying in China to exploit these new imaging surveys. I am fully confident I havebeen in a workshop that Chinese astronomy was rised for the challenge of making the extremelyimportant collaborate adventures with the international astronomy.。。。
河外星系光谱巡天 Spectroscopic Surveys in the NGC of 7700 sq degrees (SDSS sky) and in the SGC of about 3500 sq degrees: Galaxies of r<19.5 in 3700 sq deg; 90 min ； Galaxies of r<18.8 in the rest 7500 sq deg ； 30 min Luminous Red Galaxies (LRGs) of ideV<20.0 ； QSOs of i<20.5, combining UKIDSS if available; A data base of 7 million extragalactic spectra
Simulations of NGC LRGs 距今 42亿 年 SLOAN 2Tw SLOAN 2 o-poi nt CF 距今 67亿 年 LAMOST LAMOST 赤道两侧 3度范围内的亮红 Cheng LI 星系的分布情况（模拟）
Constraining the EOS of dark energy, e.g.,w(z)=w0+w1 z/(1+z)Wang,X, Chen,X et al. Hong LI et al.
QSO sample Since part of the QSO sample is based on UKIDSS , it is very useful for studying obscured quasars, testing the unified model of AGN and constraining the growth history of super massive black holes; Will probably detect the luminosity dependence of QSO clustering, and be very powerful to study the coevolution of galaxies and central black holes Will be an ideal sample to explore DE at z=2;
高速星（ HVS ） 估计银河系中共有约 1000 颗高 速星， 2005 年在 SDSS 巡天 光谱中发现了第一个后，到目 前共发现了 10 几颗。 高速星：银河系中心黑洞、暗 物质的引力势 LAM ST 将发现超过 50 颗 O 高速星 .MPIA, January 09
Anticenter SurveyIn the region |b|<30°, 150°<l<210°:(1) We will use a weighted random selection of 2MASS objects with J<15.8. Proper motion and color may be used in the weighted selection. About one in five objects will be observed, making sure that each population of stellar type is well sampled statistically.The goals of the anticenter survey are to study the composition, kinematics and structure of the thin and thick disks and their interface with the halo; and to study disk substructure (including streams). F main sequence stars will be observed to six kiloparsecs from the Sun (fourteen kpc from the Galactic center).
Disk SurveySelect bright stars (V<16) from GSC II, withpositions from 2MASS and proper motionsfrom UCAC3. We will not use dereddenedmagnitudes for bright stars near the Galacticplane. Note that very bright stars in GSC IIoverlap with the Tycho 2 catalog, which willsupply position and proper motions withoutadditional cross-matching.
In the region |b|<20°, 20°<l<230° (but little data for l<80°):(1) Select all bright O, B, T Tauri, and HH stars from a special list of known objects.(2) Within 0.5° radius of any open cluster, select only stars with proper motion, color, magnitude consistent with cluster membership (these object lists may be generated from separate special catalogs).(3) Observe bright (V<12) K and M stars from the Tycho 2 catalog.(4) Randomly select stars from the magnitude- limited sample.