A LAMOST survey observation plate should have a bright star in the center for Shack-Hartmann wave front
estimation. Given the plate position, there should be at least one proper guide star on each guide CCD after
a small angle focal plate rotation. The detailed requirements vary according to different observation condition.
As a consequence, the plate center cannot be placed arbitrarily. Using the HIPMAIN star catalog as the
initial candidates and the USNO-B1.0 catalog for neighbor star reference, several lists of acceptable survey plate
centers are generated for different observation conditions. The sky area coverage is tested with each plate list.
Tiling algorithms using these finite plate centers are optimized for the purpose of evenly sampling and catalog
completeness. The tiling is much easier for dark nights than bright nights as there are more optional plate
centers. The result is applied in the LAMOST pilot survey for verification and feedback is used to update the
32 scientific CCD cameras within 16 low-dispersion spectrographs of LAMOST are used for object spectra. This paper
introduced the CCD Master system designed for camera management and control based on UCAM controller. The layers
of Master, UDP and CCD-end daemons are described in detail. The commands, statuses, user interface and spectra
viewer are discussed.
The 4 m large aperture, 5 degrees field of view and 4000 fibers make LAMOST an important optical
spectrum astronomical telescope in the world. It will take a survey observation on about 10,000,000
stars in 20,000 square degrees field of view of north celestial sphere within several years. In order to
fully utilize the advantages of a large number of goal optic fibers of LAMOST, carry out the survey
observation with better efficiency, and economize valuable astronomical observation time, it is very
essential and worthy to make a series of observation plans with utilization ratio of optic fiber as high as
possible, which is exactly the scientific goal of Survey Strategy System (SSS) of LAMOST. Various
kinds of static and dynamic restraint conditions affecting a survey observation are analyzed and
modeled. On the basis of looking for tile with the largest density, the Mean-Shift algorithm is adopted,
effectively improving the utilization ratio of optic fiber. With the progress of LAMOST project, new
restraints and algorithms will be involved.