1. Status of LAMOST ZHAO Yongheng National Astronomical Observatories of China

2. Structure of LAMOST MB mirror Fiber Positioning Fibers MA mirror Spectrographs CCDs

3. Ma: reflecting corrector (24 sub-mirrors) ~ 4.9m Mb: spherical mirror (37 sub-mirrors) ~ 6.1m

4. Basic parameters of LAMOST 4.9m/6.1m Schmidt telescope The declination of observable sky area ranges from -10  to +90 . 20 square degree of the FOV 4000 fibers Spectrum resolution: VPH (Volume Phase Holographic) Grating R=1000, 2000, 5000, 10000

5. Schedules of LAMOST Project Reviewed Approved Proposal Nov. 1996 Apr. 1997 Feasibility Study Jul. 1997 Aug. 1997 Preliminary Design Apr.-May 1999 Jun. 1999 Detailed Design Sep. 2001 Construction 2001-2008 First Light 2008

6. Technical Challenges Active optics Both thin mirror and segmented mirror active optics in M A segmented mirror active optics in M B Fiber positioning 4000 fibers at LAMOST SDSS: 640 fibers 2dF: 400 fibers

7. LAMOST small system June 2007 6Ma and 9 Mb submirror  ~ 2m LAMOST Small focus plane + 250 fibers 1 spectrograph

11. Active optics & supporting

12. Results of Close Loop Active Optics 第九号星闭环跟踪结果（ 2007.6.8 180 组）

15. LAMOST- Positioning for 4000 fibers Double arm scheme Focal Plate for holding 4000 fibers Prototype For 19 fibers In USTC

19. LAMOST-LRS Optical System R1000/2000 R5000/10000 R1000/2000 Blue (370~590nm) Red (570~900nm)

21. VPHG (Volume Phase Holographic Grating)

23. E2V-CCD203

24. Image quality (R=1000) bluered

25. Resolution of the spectrum

26. 蓝区红区 南京 兴隆

27. First light of the small system On May 20 2007 The LAMOST small system (about 2m in diameter and have 250 firbers) got its first spectrum!

28. Sky Skylight in day 5 月 25 日 15 时

29. 6 月 5 日 18 时 Skylight spectra

30. Select the targets

31. Field No. 9 June 22, 02h 203 targets 3600 123 Spectrum

33. Component & Total Efficiency 0.00 0.20 0.40 0.60 0.80 1.00 370450550650750850 Wavelength(A) Efficieny telescope fiber Spectrograph CCD total

34. Efficincy R band Observe data ( Sky) ： 12.0% Theoretical value ： 16.5% 中值为 1

35. Current States

37. MB

38. 37sub-mirrors of MB （ July 13,2008)

39. 24 sub-mirrors of MA

40. Preliminary test on pointing error of telescope

41. 24 sub-mirrors of MA （ Sept. 10, 2008)

42. Oct. 11, 2008 image quality

43. Oct. 11, 2008

44. Oct. 8, 2008 Mean=1.14″, Maintenance Mean=1.00″ 80%=1.21″, 80% Maintenance=1.14″

45. At 5.2 degrees FOV

46. 4000 optical fibers

48. spectrographs

50. Test spectra （ 8 月 25 日 3 号光谱仪） BlueRed

51. Relative efficiency （ No.6spectrograph- blue ）

52. Efficiency of spectrograph 370~900nm Target ： 35% （ peak ） According to test on reach parts: 50% According to test on whole spectrograph: 43%

53. Image quality in spectrographs 达到计算分辨率的 FWHM 值 : 9.2 pixels 红区测试结果： 兰区点数少，像质暂时更好

54. Aug. 30 All hardwares installed Sept. 28 More than 2000 spectra got in one test observation Oct. 13 About 3000 spectra got in one test observation

55. Spectra of stars （ 28/9/2008 ） Red Blue

57. commission period Sep.-Dec., 2008 Fiber positioning units To 4000 objects Spectroscopic calibration Operation software Pipelines for data processing

58. Softwares for automatic observation & data processing catalogue processing observation OCS SSS DPS

59. Operation software OCS SSS TCSICSDHS Input Catalog LAMOST Spectr. Database

60. commission period 2009: Stability Active optics Dome seeing Efficiency Fibers Spectrographs CCDs Scientific test observations Open clusters, nearby galaxies, selected area survey, …

61. regular spectroscopic survey 2010-2015 Working groups for Extragalactic survey Galactic survey  input catalog for LAMOST (end of 2009)

62. Key Projects Extra-galactic spectroscopic survey — Galaxy and QSO redshift survey Stellar spectroscopic survey — Structure of the Galaxy, and so on. Cross identification of multi-waveband survey.

63. Thank You ！