PDS_VERSION_ID      = PDS3                                                    
LABEL_REVISION_NOTE = "M.K.  GORDON,2003-07-20"                               
RECORD_TYPE         = "STREAM"                                                
                                                                              
OBJECT     = INSTRUMENT                                                       
  INSTRUMENT_HOST_ID = "LICK1M"                                               
  INSTRUMENT_ID      = "CCDC"                                                 
                                                                              
  OBJECT     = INSTRUMENT_INFORMATION                                         
    INSTRUMENT_NAME = "STOVER CCD SPECTROGRAPH CAMERA"                        
    INSTRUMENT_TYPE = { "CCD CAMERA", "SPECTROGRAPH" }                        
    INSTRUMENT_DESC = "                                                       
                                                                              
      Instrument Overview                                                     
      ===================                                                     
      The following information was taken from the Lick Observatory           
      web site, http://mthamilton.ucolick.org/ on July 20, 2003.              
                                                                              
      The Stover CCD Spectrograph/Camera at the Nickel Telescope is a         
      modular instrument which may be configured in a variety of ways.        
      The basic choice is to use it as a spectrograph or as a camera. In      
      either mode, the throughput is quite hight, but absorption in the       
      CCD camera lens cuts off the UV response below ~3850 Angstroms and      
      the IR above ~8000 Angstroms.                                           
                                                                              
      The spectrograph is a straight-through design (see Figure below).       
      After passing through the slit aperture and the filter wheel, the       
      light passes through the shutter and then through a collimating         
      lens about midway down the body of the spectrograph. Traveling a        
      roughly equal distance again, the collimated beam is dispersed by       
      one of three remotely selected grisms, and then focused onto the        
      CCD by the camera lens. Between the camera and the CCD is a             
      manually operated dark slide, which is routinely rediscovered by        
      many observers on the first night of each run. The CCD and its          
      dewar are mounted on an x-y stage which allows choice of central        
      wavelength and position of the spectrum on the CCD.                     
                                                                              
      A variety of direct camera configurations are available which are       
      described in detail later, but their configurations are all             
      conceptually variants of the spectrograph without the dispersers.       
                                                                              
      It is most unfortunate that one may not conveniently switch             
      between spectroscopy and imaging. This is because the TV camera         
      may not be offset, and spectroscopic guiding is done directly on        
      the aluminized aperture plates, so if they are removed to allow a       
      two dimensional image to fall on the CCD then guiding is no longer      
      possible. If it is enough for you to have just an unguided              
      snapshot of a field, that may be done.                                  
                                                                              
      The spectrograph/camera is controlled remotely from the readout         
      room. At present, the only functions that cannot be controlled          
      remotely are the manual darkslide and movement of the x-y stage in      
      the y direction, perpendicular to to dispersion. These are very         
      small inconveniences, since the y stage setting usually stays           
      constant during a given run, and the dark slide is usually only         
      changed at the beginning and end of the night. Thus, the observer       
      generally does not need to go onto the dome floor at night, but         
      makes all required adjustments remotely.                                
                                                                              
      Data taking and preliminary analysis is done from two terminals in      
      the control room. The data taking process is a menu driven system,      
      which most observers find to be extraodinarily user-friendly.           
      "                                                                       
                                                                              
  END_OBJECT = INSTRUMENT_INFORMATION                                         
                                                                              
  OBJECT     = INSTRUMENT_REFERENCE_INFO                                      
    REFERENCE_KEY_ID = "N/A"                                                  
  END_OBJECT = INSTRUMENT_REFERENCE_INFO                                      
                                                                              
END_OBJECT = INSTRUMENT                                                       
                                                                              
END