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\documentnumber{JKT RBS  Version 1.3}

\begin{document}

\title{Observers Guide to the JKT RBS}          
\author{Phil Rudd
\thanks{La Palma Observatory}}
\date{20 September 1996}
\maketitle

%\vspace{-55mm}
%\vspace{75mm}


\newpage
\tableofcontents
\newpage

\section{Scope of this Guide}

    This guide is {\it not} intended to replace Roger Edwin's {\it The
    St Andrews RBS User Manual}, which should always be consulted
    before using the instrument. However the {\it User Manual} is seriously
    out of date, and contains no guidance about actually setting up the
    CCD, and the dispersion tables refer only to the small RCA type CCD's.
    Updating the latter for EEV and TEK will be the next task. This guide
    is a first draft and may contain errors - please inform the author of
    any discrepancies, so that they may be incorporated in later versions.
    
\section{AFTERNOON ACTIVITIES}
   \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

      \item  Fill cryostat with LN2 (usually every 12 hours)

    \end{list}
      
    \subsection{Computers}

           See computer startup instructions on wall above each system
              console. Usually computers are left up and running, since
              installation of UPS. Check for response from keyboards.

        \begin{verbatim}

           TCS3210 (TCS) - will give UI> prompt.
           ICS3220 (ICS) - will give * prompt.

        \end{verbatim}

     \subsection{Adam Login} 

        \begin{verbatim}
 
           * SI XYZ,n,n     XYZ=observer n= PE account (see whiteboard).
                            Write initials on board, dates resident and
                            write NO in the 'ok to delete?" column.
     
           * ADAM           and answer prompts: f/15, A&G+RBS, EEV7/TEK4 etc,
                            run#(n) and D to dump to disk only. 
                    
                            To abort from an Adam command press break, then
                            SEND CON:, unless the Adam terminal hangs during
                            readout, in which case type RESET at the ICS
                            system terminal, which forces an automatic restart.

                            To abort from Adam altogether press break then
                            * CA (cancel).

        \end{verbatim}

     Note that the new SCSI ICS disk drives are 2Gb capacity, and can store up
     to approximately 450 full-frame big chip images, a factor of 3 improvement
     over the old drives, with the Sparcstation having 18 Gb capacity.
 
     \subsection{Setting up the RBS}
        \subsubsection{Changing Optics}

     The RBS has exchangeable optics, optimised for blue or red ($>$5000A).
     Changing the optics is straightforward, and can be done in about 20
     minutes. Follow the instructions in Roger Edwins {\it The St Andrews 
     RBS User Manual}, and you can't really go wrong. There are up to five
     components to change: slit assembly (either 1 or 1.5 arcs), collimator,
     grating, camera mirror and corrector unit. The change procedure for
     each optical component is accurately described in the 
     Manual: note only that the screw on cap protecting the collimator is
     very stiff, due to some unfortunate impact with the telescope pier,
     so care must be taken when replacing the cap, to prevent cross-threading.
     All the RBS optics are stored in an aluminium case in the left-hand
     cupboard below the worktop in the "darkroom", adjacent to the dome
     area. You will also need Allen keys to remove the grating and camera
     mirror assemblies. \\
     {\bf Before you start to set up the RBS, ensure that you have the correct
     optics mounted, and with the grating angle set for the appropriate
     spectral region, for the grating in use.}

        \subsubsection{RBS external controls}

     Good, so you've changed the optics. The RBS is a {\bf REAL} spectrograph,
     all RBS functions being controlled from the observing floor. Externally
     there are four controls of interest during setting up, and to a lesser
     extent during observing: grating angle clamp, slit and dekker slide, 
     Hartmann mask, and finally the micrometer on the camera mirror unit,
     used for focussing. \\

     The grating angle is changed by first unclamping the grating using the
     bronze knurled clamp on the grating scale, rotating the grating to
     the desired angle using the knob on the side of the spectrograph,
     labelled {\it Unclamp grating before rotating}, then re-clamping. \\
     
     The slit and dekker slide has two detents, although finding the inner
     one can be a little tricky, as it is not well defined:

        \begin{verbatim}
           Fully In     -  whole slit covered
           Inner detent -  star slot uncovered - central 2mm exposed
           Outer detent -  arc slots uncovered - 2 x 2mm exposed
           Fully out    -  whole 20mm slit exposed - Longslit
        \end{verbatim}

     A 2mm slit length projects to about 0.5mm wide spectra at the camera
     focus. During observing stellar and comparison spectra are usually
     exposed on separate frames, using Longslit mode (slide fully out). \\

     The Hartmann mask has three positions:

         \begin{verbatim}
            In      -  first Hartmann position
            Detent  -  second Hartmann position
            Out     -  for normal operation, secured in stowed position
                          using fork clamp.
         \end{verbatim}

     The micrometer on the camera mirror is used to adjust the spectrograph
     focus. {\bf Initial focus for the red optics is about 7.5mm, and 7.4mm for
     the blue}. Unless the focus is apalling, micrometer increments of 0.1mm
     should be used initially. The Hartmann focus test is described later,
     but beforehand the mounting of the cryostat itself should be discussed. \\

     The CCD cryostat is mounted on the RBS using the familiar RGO kinematic
     mounting plate. This has three capstans with micrometers - the capstan
     settings are contained in the black RBS logbook in the control room,
     and should be set-up initially by the Duty Engineers. Hope and pray that
     these are correct, and that the CCD is orthogonal to the RBS focal plane,
     as correcting any tilt on the CCD is not for those of a nervous
     disposition - suitable tranquilisers may be found in the RBS optics
     case: these will almost certainly be required when squaring-on TEK4.
     The capstans are mounted at about 8, 4 and 1 o'clock, and are referred
     to by the letters A (Cone), B (Slot) and C (Flat), engraved on the 
     kinematic mount. The
     cryostat is mounted so that it's dispersion direction is horizontal
     when viewed from behind the cryostat so A and B should correct tilt in
     the dispersion direction, and C, spatial tilt. If you do determine new
     capstan settings for a particular detector, please ensure that these
     are recorded in the RBS logbook for future reference. \\

     The other crucial adjustment is the micrometer controlling cryostat
     rotation, thus allowing the dispersion direction to be accurately
     aligned with the rows of the CCD. Before attempting to adjust the
     micrometer the six 10mm faceplate bolts must be loosened. \\

     The Ellis A\&G, on which the RBS is mounted has 2 hollow cathode
     calibration lamps and a Tungsten lamp for flat fields. All three can
     be fitted to the integrating sphere on the A\&G box, or alternatively
     either of the hollow cathode lamps can be mounted directly on the
     same A\&G port, secured by a locking collar. Note that the Tungsten
     gives flat-fields about as flat as La Palma when used in the
     integrating sphere; use dome or sky FF's instead. The three lamps
     are connected to a power supply on the A\&G as follows:

        \begin{verbatim}
            CuNe    Position 1   
            CuAr    Position 2   
            W       Position 3   
        \end{verbatim}

     Since the control room reorganisation during 1995, with the electronics
     racks being moved into the ICS room, the RBS handset can no longer be
     used (as the cable is not long enough), instead all handset functions
     are now controlled by Adam commands, as follows:

       \begin{verbatim}
          CUNE ON/OFF        turns on/off the cune lamp
          CUAR ON/OFF        turns on/off the cuar lamp
          TUNG ON/OFF        turns on/off the tungsten lamp

          COMP IN/OUT        moves the Comp/Acq mirror into/out of the beam
          SLIT IN/OUT        moves the slit view mirror into/out of the beam
       \end{verbatim}

     The point to watch here is that if one mirror assembly is in the beam
     and you want the other mirror, you {\bf MUST} move the unwanted mirror
     out of the beam before attempting to move the other into the beam.
     Failure to observe this may lead to Adam becoming confused and acting
     strangely (nothing new there!). So for example, if you've just done an
     arc, and want to return to slit view, you must type COMP OUT and then
     SLIT IN. Each mirror movement will take about 25 seconds, so be patient.
     \\


        \subsubsection{CCD rotation}
     
     First set-up priority is to ensure that the CCD rotation is correct, and
     that the dispersion direction co-incides exactly with the rows of the
     CCD. The RBS is very critical here, since a 2mm slit length projects
     to about 0.5mm at the detector. Ensure that the micrometer on the
     camera mirror has been set to 7.5mm for the red optics, and 7.4mm for
     the Blue optics, or check the RBS logbook for the most recent values.
     Rotation is best done using arc lines,
     so take an arc with the dekker in longslit mode and the Hartmann
     shutter out, and measure the centroids at top, middle and bottom.
     Adjusting the cryostat rotation  requires the six bolts on the
     cryostat faceplate to be loosened, and the cryostat rotated away from
     the stop. Do {\bf not} attempt to rotate the cryostat with the
     micrometer - back off, move the micrometer, rotate the cryostat
     back until it touches the micrometer, then retighten the bolts, and
     try again. Ideally the rotation along the dispersion direction should
     not exceed 0.1 pixels.

        \subsubsection{Correcting for CCD Tilt}   

     Now take an exposure with the right Hartmann shutter in, and then one
     with the left Hartmann in, still in longslit mode (dekker out).
     Measure the centroids of the arclines in the right and left Hartmann
     images. The difference between the left and right Hartmanns gives the
     focus shift as a function of CCD position (i.e. the tilt). Once the
     tilts are known, adjust the capstans, and repeat, until the tilt
     in both spatial and dispersion directions is $<$0.3 pixels.
     Capstans A and B should correct for tilt along the dispersion direction
     whilst C, or C and A/B should correct for tilt along the less critical
     spatial direction. 

        \subsubsection{Focussing the RBS}

     In longslit mode (with dekker out), make two exposures as above,
     with the right and then the left Hartmann shutters in. Measure the
     centroids of the arclines in both images, the difference being the
     focus shift as a function of CCD position. Adjust the camera focus
     until the shift is zero.

        \subsubsection{LOG IT!!}

     {\bf After all your painstaking efforts please ensure that you record
     the capstan settings, rotation micrometer reading and camera mirror
     focus micrometer readings in the RBS logbook in the control room,
     date it, sign it, and indicate clearly which detector was mounted
     and which optics set was installed}.

        \subsubsection{Wavelength Calibration}

     If the observers central wavelength is known, then set the grating
     angle accordingly for the grating in use (from the RBS Manual), and
     take an arc exposure. Identify the lines in the resulting spectrum
     using the arc maps in the {\it IDS Calibration Lamp Arc Maps} manual
     ,{\it La Palma Technical Note No. 70}. SQUISHing the image may help 
     here since the Lexidata only shows the central region of the chip.
     Should the orientation of the spectrum be incorrect there are three
     commands available which will flip the image:

        \begin{verbatim}
            Adam:>  XYSWAP=1
                    LRSWAP=1
                    TBSWAP=1
        \end{verbatim}

     Finally, in preparation for observing, ensure that the Hartmann mask
     is fully out, and secured in place with the plastic fork clamp, and 
     that the dekker slide is also fully out, in longslit mode. \\

     Put the kettle on - You've earned it!



     \subsection{D Tape Dumping}

        With the introduction of the Perkin-Elmer to Sparcstation networking,
        image and header files are transferred to the Sparc as soon as they
        become available at the Perkin-Elmer. Consult Gary Mitchell's notes
        on how to set the networking in motion, which should be near the
        Sparc. \\

        For all data, two tapes are generated. The D tape is made by the
        observer, normally at the end of each observing session, and goes
        into the ING data archive. Before then, it is copied, either by
        the observer or by the tape copier, to produce the copy or C-tape,
        for the observer. \\

        General rules for D tape usage are to append data to them, not to
        use a new one each night, and to not append more that say 300-500
        files to a single D-tape, since this makes data retrieval from the
        archive laboriously slow. The D tape must always be a DAT tape,
        although the C tape can be either DAT or EXAB. \\

        \subsubsection{D tapes}

        At the end of the session, insert the D-tape into the lpss6 Sparc
        DAT drive. Make sure that all your files have been transferred to
        the Sparc, then pull up a new Xterm window and type:
        \begin{verbatim}

            AUTOFITS    and answer the prompts

        \end{verbatim}

        Within AUTOFITS is an option to initialise the tape. {\bf DO NOT do
        this unless it is a NEW tape}. If you initialise a tape which
        contains data, then any data on that tape will be
        irrecoverably lost. \\

        Whenever you are dumping data, please leave a note on the terminal
        to say which files you are dumping, and give your name and time you
        started dumping.

        \subsubsection{C-Tapes}

        You have two choices here. Either copy the data yourself and verify
        it using the FITSLIST option within the TPCOPY facility in the WHT, 
        or fill in a Mag Tape Copy Request form and let the tape copier 
        do it. \\

        To do it yourself, load a C-tape in the DAT drive again of the Sparc
        and repeat AUTOFITS as described above. This tape {\bf MUST} then
        be verified using the TPCOPY facility in the WHT terminal area.

        Alternatively, fill out a MTCR form for the tape copier and leave it 
        in the filing tray in the control room.

      \subsection{Purging files from disk}

           After all files have been dumped to D tape and copied to C tape
           you will have to delete them from the disk, to maintain your
           working space. The command to use for this is PURGE, which will
           only delete those files which have previously been archived to
           tape. Before you PURGE any files contact your SA who will check
           the JKT tapes status (maintained by the tape copier), which will
           indicate which D tapes have been copied and verified. The tape
           copier (or observer, if producing and verifying their own C tapes)
           should write YES in the 'ok to delete?' column on the whiteboard,
           but the tape status file must always be checked before purging
           any data.

          \begin{verbatim}

              lpss6% more /home/lpss1/vbf/tapes/jkt.tapes

              Adam:> PURGE     which will delete a specified range of files
                                  from the disk. The prompts are:
                                     which disk volume> SYS
                                     Detector> CCD
                                     Initials> XYZ (as for Login)
                                     Files to be purged> R1-R150

                               The above will purge files:

                                     SYS:CCDxyz.001  to
                                     SYS:CCDxyz.150  incl.
                                     
          \end{verbatim}


      \subsection{Bias frames}

          \begin{verbatim}

              Adam:> RUN 0 "BIAS"     does a zero second exposure (reading
                                         out CCD with shutter closed), and
                                         creates a bias frame, with title
                                         "bias".

              Adam:> MULTRUN          takes multiple bias frames. Simply
                                         reply to the prompts.
          \end{verbatim}

          Check bias value using STATS mode of PHOT. If different from
          default value when you initialised Adam, enter:

          \begin{verbatim}

             Adam:> NEW_BIAS n

          \end{verbatim}

    
   \section{TWILIGHT/EVENING ACTIVITIES}

      \subsection{Telescope}

         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}
 
           \item Fill cryostat.

           \item Check observing floor, and lower rising floor so instrument
                 will not foul floor during observing.

           \item Telescope power ON (Engineering mode).

           \item RUN oil pump and  cancel alarm(s) if necessary by pressing 
                 CANCEL button and green RESET button, if lit. The alarms
                 may have to be cancelled twice.

         \end{list}

      \subsection{Zeroset encoders}

         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

           \item In ENG mode with dome lights on.

           \item Set slew rate knobs set to green marks.

           \item Drive telescope $>$3 degs from ZP in HA and Dec, manually. 

         \end{list}

         \begin{verbatim}

           UI> ZEROSET     - hit <cr> to begin. Drive back through zenith in 
                             each axis until each pair of illuminated green 
                             arrow keys goes out. If only one pair
                             illuminate then press ACK to abort, and try
                             again, without moving the telescope. Repeat
                             also if Zeroset drops out immediately. 

         \end{verbatim}

         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

           \item  Turn off dome lights.

           \item  Switch to COMP mode using keyswitch.

           \item  Press GUIDE to energise handset.

         \end{list}


      \subsection{Dome shutters and mirror petals}

         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

           \item  Open dome shutters (hold button in)

           \item  Open primary mirror covers and check not stuck

           \item  Lower blind

         \end{list}


      \subsection{Flat Fields}                  
 
         The easiest method would be to illuminate the slit with the Tungsten
         lamp in the integrating sphere attached to the Ellis A\&G box.
         Tungsten flats should be used for the dispersion direction, and
         sky flats for correcting pixel-to-pixel variations in the spatial
         direction. For sky flats do the following:

         \begin{verbatim}

           UI> IN BLANK        inputs catalogue of blanks fields, suitable
                                 for sky (twilight) flat-fields.

           UI> L              lists directory.

           UI> N BLANKn GO    marks next target as BLANKn, and slews to it.


           Adam:> GLA n       initiates a glance run of n secs.

                              Note:
                                     
                                   WINK n   n secs, image stored in Scratch,
                                            with no header packets, so used for
                                            quick peeks only.

                                   GLANCE n  n secs, image stored in Scratch,
                                             but with header packets. If 
                                             you decide to keep it use KEEP 
                                             which puts it into your directory,
                                             which prompts for a name.

                                   RUN n "title", creating a named file where 
                                             n is the exposure in seconds.


           Adam:> DIP 2 0 65000    changes display range of Lexidata to
           Adam:> DISP                0 to 65000 ADU's. The 2 specifies that
                                      all 16 bits of digitised data be 
                                      displayed.
          \end{verbatim}

           If counts are satisfactory then the Glance file may be saved from
           scratch to a disk file using the KEEP command:

          \begin{verbatim}

           Adam:> KEEP "title"
                              
          \end{verbatim}



      \subsection{SNAFU}

         The SNAFU procedure is necessary to define the collimation and index
            errors, and incorporate these into the pointing model. \\
            (During
            set-up the slit centre should be marked on the TV, using the
            following procedure: illuminate the narrow star dekker by the 
            tungsten lamp, with the SLIT mirror in the beam. You must type 
            OPEN at the Adam terminal first to open the above slit shutter,
            otherwise you wo'nt see anything. Mark the slit centre on the
            TV then revert to longslit dekker afterwards.)


         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

           \item  Go to bright star (5-6mag).

           \item Turn TV on.        Check gain control in clicked-off position.
                                    Press ON.
                                    Wait 10-15secs til delay light goes out.
                                    Select DIRECT.
                                    Turn gain up {\it slowly}.

           \item Type OPEN on Adam terminal to open the above slit shutter.

           \item Adam:$>$ COMP IN     to put the slit-view mirror in the beam.

         \end{list}

         \begin{verbatim}

           UI> SNAFU          Use the green console buttons to centre star on
                              slit centre mark on TV (see above).
                                
           Press ACK          to acknowledge (lower right of control desk).

         \end{verbatim}

         This is the first SNAFU, using the Comparison mirror. In case there
         is any displacement between the Comp and slit mirrors, repeat with
         the slit-mirror, which is more important.

         \begin{verbatim}

           Adam:> COMP OUT    to move the comp mirror out of the beam

           Adam:> SLIT IN     to move the slit-view mirror into the beam

           UI> SNAFU          Use the green console buttons to centre star
                              on slit centre. 

           Press ACK          to acknowledge (lower right of control desk)
         
          \end{verbatim}

      \subsection{Focus}

         The slit jaws are reflective to aid target acquisition and
         field identification. Unfortunately the optimum focus must be
         determined visually from the TV - using a small number of on-target
         integrations to sample the seeing, is probably easier than using
         the direct TV. The best procedure is as follows:
         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}
          
           \item  Select manual focus on lower control desk

           \item  Use the focus controls on the engineering panel to 
                  select optimum focus, using fast/slow mode as necessary.

           \item  When satisfied with the focus, deselect manual focus 
                  to revert to automatic focus tracking, having noted the
                  new focus value first. 

           \item  Adam:$>$ SETFOC to new focus value.

         \end{list}
 
      \subsection{Enter Sources / Create Catalogue (at User Interface)}
        
         \begin{verbatim}
                                   
           Rules: - only 80 char records allowed.
                  - filename must consist of 8 alphanum chars or less,
                       starting with a letter and have the extension .CAT.
                  - no more than 500 objects per file. 

 
           UI> DEL/ALL        to delete all entries in UI directory.

           UI> SO name  R hh mm ss.s  D dd mm ss.s  EQ B1950 (or J2000 etc.)

           Repeat above for each target. At end:

           UI> SAVE MY.CAT    saves catalogue with name MY.

           UI> IN MY          inputs catalogue on subsequent nights.

           UI> L              lists catalogue just INputted.

           UI> N name GO      Slews to Next target 'name'.


           Standard catalogues, loaded into dictionary using UI> IN name :

              PTGRID          pointing grid, with  4 subsets for measuring
                                 seeing:

                 SEE0006      0 hr < RA < 6 hr
                 SEE0612      6 hr < RA < 12 hr
                 SEE1218      12 hr < RA < 18 hr
                 SEE1824      18 hr < RA < 24 hr

              SPECPHOT        spectrophotometric flux standards.

          \end{verbatim}

    \subsection{Network transfer from PE to Sparcstation}

       By the stage you may well have a few runs under your belt, and even if
       you have'nt, now would be a good time to start the network software to
       allow automatic file transfer between the Perkin-Elmer and the 
       Sparcstation (lpss6), and start AUTOFITS if you have'nt already done
       so. The following is {\bf NOT} intended to replace
       Gary Mitchells' more comprehensive notes, which should be beside the
       Sparcstation, {\it only} to be a concise summary. If you experience any
       problems (or even if you don't!), please read Gary's notes before taking
       further action. \\
       In the following summary, assume I signed into Adam account 2
       (e.g. si pjr,2,2). The necessary dialogue is then:
       \begin{verbatim}

           Pull up a command tool window, which is referred to as the "Server"
           window.

           % which peserver
             /home/lpss1/guest/apps/peserver

           % obsdata              (lists obsdata partitions)
           % cd /obsdata/lpss6n   (n=a,b,c,d from preceeding command) 
           % mkdir yymmdd
           % cd yymmdd
           % peserver nnnn    (port number used later)

             to break from server use Cntrl-C
 
           ----------------------------------

           Next pull up an xterm window, which is referred to as the
           "Xterm terminal"

           % telnet jktpe
           * si phil,2,2      (different name but same account, used in Adam)

           % peclient
                > lpss6
                > CCD
                > pjr         (same initials as used in Adam)
                portnumber> nnnn  (as used in Server window)
                first file> 1
                last file > 100   (network grabs each file as it becomes
                                   available)

             to break from xterm use  Cntrl-]
                                      telnet> send brk
                                      * cancel
                                      * so

           \end{verbatim}

    \subsection{OBSERVING}

       \subsubsection{Target Acquisition}

          \begin{verbatim}

           UI> N name GO        Slews to Next target 'name', which is the
                                   name of your SOurce entry in your
                                   catalogue.   
        \end{verbatim}


      \subsubsection{Exposing}

          Before starting an exposure it is best to window the chip in
          the spatial direction:

         \begin{verbatim}

           Adam:> WINDOW        and reply to prompts, which expect lexidata
                                co-ordinates, so use PHOT to get these first. 
  
                                To revert to full chip readout enter:

                                   Adam:> UNWINDOW


           Adam:> RUN t "title"  to do a t seconds integration, which will
                                   be called "title".

                                Alternatively to do multiple exposures of
                                   t secs each enter:

                                   Adam:> MULTRUN n t "name"

                                   Note that when using MULTRUN, the images
                                   are NOT displayed automatically after
                                   each exposure. To abort from MULTRUN use
                                   the command KILLMULTRUN. 


            While the RUN is in progress it is possible to monitor or
            change its status by using the following:
      
               Adam:> RUNSTAT      for elapsed time.

               Adam:> PAUSE        to pause exposure.

               Adam:> CONTINUE     to continue exposure after a PAUSE.

               Adam:> ABORT        to abandon observation - no file produced.

               Adam:> STOP         to force read-out at that time.

               Adam:> TIME         to change exposure time. 
           
           Other useful commands are:

               Adam:> DISP Rn      displays run number n from disk.


           If the RA button sticks, switch to INC and type:

               UI> HA/I 0          so that increment is zero. Then move 
                                      stars by either stopping telescope or
                                      with the REV button.
             \end{verbatim}



      \subsubsection{Displaying Big CCD images}

          Since the Lexidata display has only 640 x 512 pixels, attempts
          to display large CCD images using DISP causes only the central
          part of the image to be displayed. One rather cumbersome way
          to display other areas of the image is to set the Lexidata
          variables LXXC and LXYC explicitly, and then resetting them to
          their default values at the end, e.g.

          \begin{verbatim}

               Adam:> LXXC=320
               Adam:> LXYC=256

          \end{verbatim}

          A neater but more time consuming alternative is to compress or
          SQUISH the
          image by a factor of 2 or 3, and either display this 'squished'
          image using DISPSQ, or the more versatile BIGDISP, e.g.

          \begin{verbatim}

               Adam:> SQUISH Rn       prompts for x and y binning factors
                                      (2 will barely fit an EEV image on the
                                      Lexidata, 3 will do it comfortably).
                                      This takes about 2-3 minutes.

               Adam:> DISPSQ Rn       will display the squished image on the
                                      Lexidata. A flexible alternative is
                                      to use:

               Adam:> BIGDISP Rn      will display the squished image and
                                      run PHOT. Position the cursor on the 
                                      point you would like to have as the
                                      centre of the full-scale image. Press
                                      the blue READ button twice, with a
                                      small time interval in between. Press
                                      the EXIT button which will display
                                      the selected area of the full-scale
                                      image.
                                      You then have the option of exitting
                                      the procedure or displaying the
                                      squished image again and choosing
                                      another point as the centre of the
                                      full-scale display.

          \end{verbatim}

          BIGDISP is very versatile, and avoids having to change the Lexidata
          display variables LXXC and LXYC, although you {\it do} have to 
          squish the image first, which introduces an appreciable time 
          overhead.


      \subsubsection{Readout modes}

          \begin{verbatim}

               Adam:> SETQUICK        turns on the fast readout mode, with
                                      higher noise.

               Adam:> UNSETQUICK      turns off fast readout mode. This is
                                      the system default on start-up.
 

               Adam:> BIN             used to enable on-chip binning. Two
                                      parameters are prompted for, the
                                      x and y bin size: binning can take place
                                      up to a maximum of 4 x 4 pixels,
                                      including combinations such as 2 x 1,
                                      3 x 2 etc. BIN cannot be used with
                                      parameters x=y=1, or in conjunction
                                      with the WINDOW command.

               Adam:> UNBIN           disables on-chip binning. This is the
                                      system default on start-up. Alternatively
                                      use the CHIP command.


               Adam:> WINDOW          defines a window for readout. There are
                                      four parameters which are prompted for:
                                         xstart  | window origin relative to
                                         ystart  | top RHS of Lexidata display.
                                         xsize
                                         ysize 

               Adam:> UNWINDOW        selects full-chip readout. Alternatively
                                      use the CHIP command.
  
          \end{verbatim}

 
      \subsubsection{Logbooks}

        \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

         \item   Please feel free to use the red JKT RBS LOG on one of the
                 shelves. Simply xerox at the end of the run (INT
                 first floor, is the nearest).

         \item   Automatic logging occurs anyway at the JKT, for every file
                 produced. The data file is processed into Latex format
                 by Mirza Asif (MWA) and placed in a file in the
                 control room. Observers may copy these if desired or print
                 the raw data file out on the Printronix in the ICS computer
                 room. To do this, log into your PE account (if not already),
                 ensure the printer is switched to ICS (on floor) and type
                 PRINT LYYMMDD.NIT to the PE * prompt (i.e. you must {\it not}
                 be in Adam).
 
         \item   Enter in the OPERATIONS LOG BOOK times of opening/closing
                 dome, filling cryostat, operational problems etc. As explained
                 below please enter all faults into the Defect Database.

         \item   Enter {\bf ALL} faults in the Defect Database held on LPVS3.
                 Login to FAULT and fill in the Fault template, using KP7 to
                 access the next field, and KP8 to access the previous field.
                 Prompts are given in the highlighted bottom line of the
                 template, and use the help screen if you get stuck, by
                 pressing KP0. When the template has been completed, press
                 {\bf PF3 to commit} the fault to the database and {\bf PF4 
                 to exit}.
                 By all means enter anything you consider relevant in the
                 log-sheets, but remember that this may not be seen unless
                 you log the fault in the database first. 

        \end{list}


      \subsubsection{Humidity \& Wind}

         \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

           \item  If $>$50\% humidity in dome, turn on dry N2 to first 'notch'. 
                  Flow is controlled by the flowvalve hanging around the mirror
                  cell, and should be adjusted to deliver 100 L/Hr.

           \item  If $>$90\% humidity outside, close down and wait until 
                  $<$80\% or conditions seem stable.

           \item  Windspeed limit for JKT is 50kph (steady, not gusts). Close
                  dome if this limit is exceeded. If concerned, check with
                  the INT Telescope Operator.

         \end{list}


      \subsubsection{Copying Data}

        \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

          \item  Complete Tape Copy Request Form (in lower filing tray) and
                 leave in top filing tray together with D tape at the end
                 of each night. Copy (C) tape will appear in INT Visitors
                 pigeon hole in due course.

          \item  Otherwise produce your own C-tape as described in the earlier 
                 tape dumping
                 section. PLEASE fill in a Tape Copy Request Form even if
                 you backup your data yourself, otherwise the tape copier
                 gets horribly confused. 

        \end{list}


    \section{MORNING ACTIVITIES}

      \begin{list}{$\circ$}{\setlength{\itemsep}{0mm}}

         \item  Turn TV OFF.

         \item  Press ZP button to zenith park telescope.

         \item  Close mirror covers - check they're not sticking.

         \item  Close dome shutters.

         \item  Turn off oil pump and cancel alarm(s).

         \item  Turn OFF telescope power.

         \item  Adam:$>$ SHUTDOWN       to close down JAG and exit from Adam.
 
         \item  Adam:$>$ SO                to sign-off from PE.

         \item  Transfer any remaining files from the Perkin-Elmer to the 
                Sparc, and dump to D tape as described in the earlier tape
                dumping section. Complete a MTCR form for the tape copier,

         \item  Refill cryostat.

         \item  Turn off dome lights.

         \item  Put the cat out.

         \item  Go to bed.

       \end{list}


\end{document}

