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~
\vspace{1cm}

\centerline{\huge {\bf WHIRCAM User's Guide \ver}} 
\vspace{7mm}

\centerline{\Large Shaun Hughes (RGO), Pat Roche (Oxford)} 
\vspace{7mm}

\centerline{\Large  Vik Dhillon (LPO)} 

\vspace{2cm}

\begin{figure}[h]
\psfig{figure=fig1_optics.eps,width=16cm}
\caption{WHIRCAM at GHRIL}
\label{fig1_optics}
\end{figure}

\vfill

\centerline{\Large 29 February 1996} 

%

\newpage
{\large
\tableofcontents
}
\newpage
\markboth{}{\it WHIRCAM User's Guide \ver}
%
{\large
This manual is intended to give enough detail for astronomers to take IR 
images with WHIRCAM on the WHT.  Many thanks are due to Colin Aspin (JAC) for
supplying a preliminary version of the IRCAM3 manual, upon which much of these
notes are based, especially Appendices A and B.  A more detailed document 
describing WHIRCAM's optics, ALICE, mounting and alignment, etc, has been 
produced by P.F.Roche, and is available on request (a copy is also held in 
the WHT control room). 

WHIRCAM is an infrared imaging camera built for the WHT (the 4.2 m 
William Herschel Telescope on La Palma) by Pat Roche (Oxford) in
collaboration with Joel Sylvester, Magnus Patterson, David Laird and 
Phil Puxley (ROE).  


\section{Observing in the IR}

If you haven't observed in the infrared with arrays before, then there a 
few extra problems (and techniques for overcoming these), compared to visible
CCD observing, that you should know about! Further details can be found in the
article {\em Observing with IR arrays} by Richard R. Joyce in 
{\em Astronomical CCD Observing and Reduction Techniques} (1992, ASP Conference
Series, Vol. 23, p 258, ed. Steve. B. Howell). A copy of this article
is held in the WHT control room. 

\subsection{Obtaining Optimum Images}
There are three particular `features' of the WHIRCAM array, that differentiates
it from modern optical CCDs in terms of observing procedure.  These are
{\em residual imaging} where a recent high count in any pixel causes a larger
count than normal in a subsequent exposure, a {\em high DARK current}, and a 
{\em large number of hot pixels}, some of which are unstable and come and go on
very short timescales (seconds).  The residual imaging effect means that
observing a bright object will result in a `ghost' in the subsequent image,
and the high DARK current means that if the array is idle for a time, most of 
the pixels will have a high count, so that 
a subsequent exposure will have a spurious higher count level. 
Hence each exposure sequence should be preceded by
at least two DARKs, to ensure that the pixel response returns to nominal
for the OBJECT exposures.  And the large number of hot pixels means that it
is essential that each of these OBJECT exposures consists of at least three 
(preferably more) dithered images, such that median or other suitable 
filtering can be employed to remove the hot pixels.  {\em This applies to 
standards as well as objects!}  Dithering also
enables accurate sky subtraction for point sources, removes
cosmic rays, ensures good temporal and spatial correlation between object
and sky, and removes detector dark current automatically. All at no 
additional cost in observing time.

Fortunately this observing sequence is easily achieved by the use of
EXEC files (see \S~\ref{Imaging menu}) that specify a dithered pattern 
of exposures per filter,
preceded by two DARKs.  Make sure that the dither pattern is not exactly 
square, otherwise the bad column ($\sim$\# 55, see Figure~\ref{fig2_bad-pix}) 
will create a residual series of streaks in the final montage.

You will also need to obtain good estimates of the sky, which is very much
brighter in the IR compared to the optical.  For example, at $K$, the sky
is typically 12 mag/arcsec$^2$, compared to $\sim$22 mag/arcsec$^2$ in $V$.
This means that most broad band
imaging will be sky limited, and the maximum exposure times to avoid
saturation will be determined by the sky brightness in most observations.
Also, if your aim is to measure surface brightnesses and your source is 
extended, or the background is not uniform (eg a gradient
on a galactic field) and covers a large fraction of the WHIRCAM FOV,
then you'll need to take offset skies (ie offset the telescope
to a patch of true sky), of comparable exposure time, similar airmass and 
UT as your object exposures.  Such offset sky exposures should also be 
taken in a dithered pattern, to remove faint stars, hot pixels 
and the occasional cosmic ray.

\subsection{Calibration Frames: Darks and Flatfields}
The pixels on IR arrays are produced by generating voltages across the
substrate applied to individual electrodes.  Captured photons are converted
to an effective charge, which changes the voltage in a given pixel, and it is
this voltage which is read out.  Thus the output counts consist of a reset 
level produced by the initial bias voltage,\footnote{The initial voltage is 
called the bias, which is thus different to the bias in optical CCDs (a 
signal added at readout), but has a similar effect in the raw frame (ie an 
extra `constant' level added to the image which must be removed).}
 dark current produced within the
substrate, and (normally) a signal generated by the source and sky photons.  
Thus from an observed count at any pixel ($N_{obs}(i,j)$), to recover the 
source signal from the object ($N_{obj}(i,j)$), 
the reset level ($N_R(i,j)$), dark current ($N_D(i,j)$), and sky ($N_S(i,j)$)
must all be measured, as well as a flatfield which measures the variations in 
pixel-to-pixel response and vignetting from optical components ($F(i,j)$):

$N_{obs}(i,j) = N_R(i,j) + N_D(i,j) + N_S(i,j)F(i,j) + N_{obj}(i,j)F(i,j)$

A DARK exposure will give $N_R(i,j) + N_D(i,j)$ (but make sure it has the
same exposure time as your object exposure, as the dark current isn't
linear with integration time).  In IR observing, the flatfield often varies 
on timescales of hours, due to changes in thermal emission from various 
components, hence the best flatfield is generated from sky frames ($N_{sky}$)
obtained with the object exposures, thus:

$F(i,j) = \frac{N_{sky}(i,j) - N_R(i,j) - N_D(i,j)}{N_S(i,j)}$

Because the sky is so bright in the IR, and because the flatfield can vary,
it is important to subtract the sky from object before flatfielding.  This also
has the advantage of not needing to explicitly subtract a DARK from the
OBJECT, as the dark current is already in the sky exposure (but a DARK is
still needed to generate the flatfield).  Thus the object
signal is then obtained from:

$N_{obj}(i,j) = \frac{N_{obs}(i,j) - N_{sky}(i,j)}{F(i,j)}$

WHIRCAM has two main observing modes: STARE and ND\_STARE.  In STARE,
one readout at the end of the exposure is made, giving $N_{obs}$, while
in ND\_STARE, an initial readout is made immediately after the initial reset 
is applied, and this reset level is subtracted from another readout at the
end of the exposure, giving $N_{obs} -  N_R$.  Thus it is important not to
mix DARKs taken in STARE mode (ie $N_R + N_D$) with DARKs taken in ND\_STARE 
mode (ie just $N_D$).

In the WHIRCAM array, Well depths, and hence saturation, vary across the chip,
and in particular the odd column pixels have a lower well depth than the even column 
pixels.  To reduce the problems of different saturation levels on the odd and even
columns (which would be difficult to measure in real time), different reset
levels have been applied to the odd and even columns, such that at 80\% of
saturation the odd and even column counts are approximately the same 
(see Figure~\ref{fig5_non-lin}). A side effect of this is that the flatfields 
are dominated by an odd-even column fixed pattern noise.  Consequently, most 
faint images will not be seen on the raw image display.  To confirm the
presence of a faint image while observing, you'll need to subtract off sky
and divide by a flatfield (eg. using IRCAM\_CLRED -- see Appendices A and B).

The sky counts in narrow band images may not give enough signal to noise to
generate an accurate flatfield.  In this case, use either the bright twilight 
sky, or dome flates obtained during the afternoon from the halogen 
flatfield lamp (ask your TO or SA where this is stored).

\newpage
\section{WHIRCAM Characteristics}
\label{characteristics}
The detector is a Santa Barbara Research Corporation
(SBRC) InSb array
enclosed in the old UKIRT IRCAM-1 cryostat.  The internal optics 
were designed by Eli Atad (ROE), and consists of a doublet (the fore-optics),
which collimates an expanding f/11 beam, two filter wheels, and an f/6.2 
triplet that re-images the collimated beam onto the array.

The detector is cooled to 30K by a closed-cycle high pressure He cooling 
system, consisting of a vibrationally isolated heat pump mounted on top
of the cryostat, connected to a compressor in the oil pump room on the
ground floor by $\sim$ 60 m of high pressure stainless steel piping.
The triplet lense and filters are also cooled, to $\sim$70 K, with the doublet
probably a little warmer, as it sits in an extended snout.

The InSb detector currently installed is serial number FPA40348, and has 
the following characteristics:
\begin{itemize}
\item Array size = 256$\times$256 of 30 \micron\ pixels 
\item Image scale (direct) = 0.24\arcsec/pix, 
giving a full FOV = 61\arcsec$\times$61\arcsec
\item Image scale (Martini $\times$3) = 0.08\arcsec/pix, 
giving a full FOV = 20\arcsec$\times$20\arcsec
\item Image scale (Martini $\times$5) = 0.05\arcsec/pix, 
giving a full FOV = 13\arcsec$\times$13\arcsec
\item Quantum efficiency $\sim$ 80\% over 1 -- 4 \micron\ (includes 
{\sl J, H, K}) 
\item Dark current = 1 e$^-$/s, but is effectively $\sim$10 e$^-$/s due to
thermal emission leaks within the cryostat 
\item Gain $\sim$ 6 e$^-/$DN 
\item Readout noise $\sim$ 40 e$^-$ for ND\_STARE, 55 e$^-$ in STARE 
\item Reset level (STARE mode) $\sim$22,000 DN (even columns), $\sim$30,000 DN
(odd columns).
\item Non-linearity: like most IR arrays, WHIRCAM's response is non-linear,
as a function of well depth, and the well depth varies with bias voltage.  
1\% non-linearity sets in at about 3000 counts,
and reaches 10\% at counts of 17000 for odd columns and 20000 for even
columns, in ND\_STARE mode with a bias voltage of 0.68 V.  If this proves to 
be stable, then corrections up to the 10\% level can be applied afterwards.  
\item Saturation $\sim$ 10,000 DN for ND\_STARE,  
and 37,500 DN for STARE (both 80\% full well capacity),
for a bias of 0.68 V (see \S~\ref{Array Saturation}).
\item Readout times of: 120 ms (256$\times$256 full array) \newline
~ \hspace*{3.3cm}  ~36 ms (128$\times$128 subarray) \newline
~ \hspace*{3.3cm}  ~12 ms (64$\times$64 subarray).  \newline
\end{itemize}

Although the detector
is sensitive over the wavelength range 0.8--5.5 \micron, the WHT is not
optimised for the IR (in particular, it doesn't have a chopping secondary,
the secondary is oversized with respect to the primary beam, plus the central
obstruction and the baffles on the 
chimney and secondary are seen by the beam), so that most 
imaging will be restricted to 0.8 -- 2.3 \micron\ (i.e. {\sl J} to {\sl Ks}).

The total throughputs (includes sky absorption, all optical surfaces,
lens and filter absorption, and detector quantum efficiency)  are 
$\sim$16\% for {\sl J}, 17\% for {\sl H} and 17\% for {\sl Ks} 
(this is for GHRIL, which has an
all-reflecting image de-rotator, thus adding an extra 3 reflections.
There are plans to mount WHIRCAM at Cassegrain Auxiliary Port, which should
give higher throughput, plus the use of the offset guider, but
this probably won't be ready until after semester 96B).  

There are a number of known bad (i.e. dead and permanently hot) pixels on 
the array (see Figure~\ref{fig2_bad-pix}), the main feature being a few bad columns between pixel positions
(55, 81) and (54, 256).  The
brightest of these are recorded in a bad pixel map, and are masked off
for display purposes (see \S~\ref{Imaging menu}), but the frames are written 
to disk unmasked. 
\begin{figure}
\psfig{figure=fig2_bad-pix.eps,width=10cm}
\caption{The location of the main hot pixels.}
\label{fig2_bad-pix}
\end{figure}

The readout/detector control is a virtual copy of the Array
Limited Infrared Control Environment (ALICE) rack built for UKIRT's IRCAM-3 
and CGS-4, which is controlled by a DEC VAXstation 4000 via Ethernet.  
The chip can also be continuously displayed 
via 3 coax cables to an RGB monitor.  Control software is a copy of UKIRT's 
IRCAM-3, except for the stepping motor controllers (two filter wheels and 
one focus) and the telescope interface (for writing coords, etc to the 
headers).

Normally WHIRCAM sits on its own optical breadboard at the GHRIL Nasmyth 
focus (Figure~\ref{fig1_optics}).  At GHRIL, the beam passes through an 
all-reflecting (silver plus MgF coated)
image de-rotator to an optically flat dichroic, which reflects most of
the light
longward of 0.9 \micron, and transmits the optical light 
(Figure~\ref{fig3_dichroic}) to
an optical CCD autoguider, via an f/6 re-imaging lens.  The CCD autoguider 
has a field of view of 52\arcsec(NS)$\times$70\arcsec(EW) (but is vignetted 
beyond a diameter of 40\arcsec),  a scale of 
0.2\arcsec/pix, and a limiting magnitude of 
$\sim$17 mag in {\sl V} for an integration time of $\sim$4 sec (this is for a 
typical full moon sky brightness and 0.8\arcsec\ seeing, but it will of course 
vary depending on the sky brightness and seeing). The centre of the WHIRCAM
field lies at a position (230, 180) on the Autoguider CCD (ie is not centred).
\begin{figure}
\psfig{figure=fig3_dichroic.eps,height=24cm}
\caption{Dichroic's transmission (upper) and reflectance (bottom) curves.}
\label{fig3_dichroic}
\end{figure}

\newpage
\section{Observing with WHIRCAM}

\subsection{Introduction}
WHIRCAM is controlled by a Vaxstation 4000 running a slightly modified 
version of the UKIRT IRCAM package, which employs Screen Management System
(SMS) screens running under 
Adam. Status screens display the instrument configuration and the transputer
activity while an SMS menu is used to control the instrument and initiate
data taking sequences. Instrument configurations can be retrieved from the
Vaxstation disk and combined in observing sequences within EXEC files. 
The telescope can be controlled from within the EXECs; for example it can be 
stepped in a grid pattern to form a mosaic and/or a dither pattern (for median
filtering of hot pixels, etc from frames). Alternatively, a sequence of 
measurements in different filters with a number of different telescope 
offsets can be initiated. The data are stored on a 2 Gbyte disk in SDF format. 


\subsection{Starting up}
If you are intending to observe with WHIRCAM (as opposed to simply starting
it to familiarise yourself with the commands and create EXEC and CONFIG files),
then you need to ensure the Telescope Control System
(TCS) is up so that WHIRCAM's SLIDE commands etc will communicate with
the telescope.  First, verify that an ICL session is running on the computer 
specified on the whiteboard (lpvf or lpvg).  Ask your Support
Astronomer (SA) or Telescope Operator (TO) if you are unsure.  You should 
also make sure you start
WHIRCAM after 10:00 am, as the directory and filename nomenclature 
(see \S~\ref{Data Storage}) incorporates
the current date, and this is incremented at 10:00 am so that an entire night's
observations will be written with the same prefix in the same directory.

If ICL isn't running, then log onto LPVS3 or LPVS2 as OBSERVER, select the
correct system (lpvf or lpvg), type `ICL', and accept all the defaults.

Your TO should also ensure that TCS is running with the following:
\begin{itemize}
\item Select {\em GHRIL Derotator}
\item Select {\em GHRIL Autoguider}
\item Select {\em Own} instrument
\item Select a SKY PA of 0
\item Enter the correct temperature and humidity
\item Enter the correct wavelength for observations
\end{itemize}
Also, at the autoguider terminal, select the {\em GHRIL Autoguider}
application.
 
Once ICL is running, log on to the WHIRCAM Vaxstation 
(IRCMVX) (or telnet from the LPVS3 terminal next to the ALICE screen if
you want to be near the camera display)
as user WHIRCAM (get the current password from your SA or TO).
In the DECterm window type:
\begin{verbatim}
	whircam_start
\end{verbatim}
which will start up the WHIRCAM control software.

At this point you'll be asked to enter a unique ID (usually the observer's 
initials).  This will then either direct the ALICE software to your own
unique directory where your personal CONFIG and EXEC files are stored
(there are also several standard example files in the system directory), 
or else create one to store any such files you may create during your run.

The colour monitor (ALICE Graphics Display) and ALICE Transputer/Occam
control software will be initialized, and three windows will be created:
\begin{itemize}
\item A large DECterm window, the {\em instrument status} screen, containing 
current values for detector, array size, bias voltage, observing mode, 
filters, exposure time, number of integrations, observation number, and 
current and planned CONFIG and EXEC files.
\item A small DECterm window, the {\em ALICE occam status} screen, showing
current status of ALICE communications with WHIRCAM.
\item Another DECterm window, the {\em IRCAM3 Instrument Control} screen,
where you can load and edit CONFIG and EXEC files, and execute them, or
take exposures directly.
\end{itemize}

During initialization, check that one of the status
messages scrolling up the {\em IRCAM3 Instrument Control} screen reads:
\begin{verbatim}
connected to Telescope Control Task.
\end{verbatim}
This means the ICL system was running, and that the ICL tasks and WHIRCAM
can talk to each other.  Initialisation should take about 4 minutes.

Before you start taking exposures, you should start AUTOFITS running
(see \S~\ref{Data Storage}) to record your frames to tape as they are
taken.

If you wish to analyse your data as they are taken, it is usually easier
(and less messy) to do this from the RODIR directory (see \S~\ref{Data 
Storage}), in which case you should also start up an ACVT session which
automatically copies frames from IDIR to RODIR as they are taken.
To do so, open another DECterm window, and simply type:
\begin{verbatim}
ircam_setup
ACVT
\end{verbatim}
You can then iconise this window and it will run in the background.

\subsubsection{Menu Control}
The WHIRCAM instrument control and data acquisition system is 
currently run from a Starlink supported menu system called SMS, in the
{\em IRCAM3 Instrument Control} screen.  This 
menu system makes extensive use of the keyboard keypad (to the right of 
the main section of the keyboard) and particularly the PF (Programmable
Function) keys. 

The main features to be aware of are: \\

You DO NOT use the mouse at all under the SMS menu system!! (apart from
defining which window is currently active) \\

Use the Enter key to go down into the menus. \\

Use the PF1 key (top left of the keypad) to Exit menus and execute
options. \\

Use the arrow keys (left, right, up, down) to move between menu items. \\

Hit the dot key the keypad and you can then use the prev screen or next 
screen buttons to scroll the message display. \\

The optimum usage of the PF keys is always noted on the bottom line of 
the SMS menu screen. \\

Use the Select key (usually above the arrow keys) to run an ICL command.
This tends to be most useful in running DCL commands, for which you must 
prefix each command with DCL. For example, if your user ID is XYZ, and 
you'd like to list the contents of your personal EXEC directory, hit the
Select key, which will produce a `Command:' prompt at the bottom of the 
screen, at which you type:
 
\begin{verbatim}
DCL DIR DISK$USERSPACE:[XYZ.IRCAMEXEC]
\end{verbatim} 

To refresh the screen, use cntrl\^{~}R. \\

Alternatively, you can create a new DECterm session using the same screen
by typing SPAWN at the command prompt.  When you have finished your DCL
session, simply LOGOUT and the {\em Instrument Control} screen will
reappear.

\subsubsection{Startup Menu}
Go into the {\it `Startup'} menu. This menu should contain the following: 
\begin{verbatim}
Observer_name   ?
PATT_reference  ?
Instrument      WHIRCAM
Detector        FP40348
\end{verbatim}

Enter the relevant information in the spaces provided. Your PATT reference 
number can be found on the WHT schedule.  Use the PF1 key to exit this 
menu and go back to the top level menu.

\subsubsection{Defining Telescope Pointing Model}
At the start of every WHIRCAM run, and whenever the telescope structure is
changed (eg if another instrument is changed during the day, which will cause
a slight shift in the telecope balance), a pointing calibration must be 
performed on a set of astrometric stars.  This is done by your TO, but it
must be done with respect to the WHIRCAM ALICE display.  Therefore, go into
{\it Movie} mode (see \S~\ref{Setup on Source}), choose the filter you'll be 
using most of the night, set the integration time to 0.3 sec,  and aquire the 
first of the position standards (ask for the faint set, as the normal set 
saturate on WHIRCAM).   You now need to define the the telescope rotation 
centre: 
\begin{itemize}
\item{(1)} Position the telescope such that the star is 
near the top edge of the ALICE display, and mark this with a whiteboard marker
pen.
\item{(2)} Ask your TO to change the SKY PA to 180, and you'll see the star
describe a half circle on the ALICE display, and mark this new position  
(If it looks like it will move off screen, mark the approximate centre of 
rotation, go back to SKY PA 0, move the star closer to the rotation centre, 
and start again.)
\item{(3)} The telescope rotation centre will be the point halfway 
between your two marks.
\end{itemize}
The TO should then centre each of the position standard stars on this centre.
You can find out where this centre is with respect to the WHIRCAM array by
going into the {\it `Set\_graphics', `statistics\_window'} menus, and
changing the X and Y position of the statistics box until it is centred on
the rotation centre.

\subsection{Initial Engineering Tests}
\label{tests}
Once the instrument control software has finished running up, the default
{\it `Set\_observation'} option is:
\begin{verbatim}
Object = Array Tests 
Obs_type = EXEC (ie highlighted)
EXEC_name = ARRAY_TESTS 
\end{verbatim}
which will run the EXEC called ARRAY\_TESTS.  
This takes a standard set of 8 dark images which, when analysed, give an 
indication of how the array is currently performing (ie. dark current and 
readout noise). If these are not the defaults, enter them yourself.  
Hit PF1 to exit this menu.  Upon exit, the contents of the EXEC 
ARRAY\_TESTS will be loaded into the execution stack and displayed on 
the {\sl IRCAM parameter
status} screen.  Move to the {\it `Run'} item to execute the EXEC
ARRAY\_TESTS by hitting Enter.  Note down the start observation number
of the ARRAY\_TESTS EXEC. Let's call this start observation number N. \\

Once the EXEC has finished (a message will appear in the scroll region
of the IRCAM instrument control SMS screen), the user should process
the images acquired.  (The very first ARRAY\_TESTS almost always
produces a larger than real dark current, so take
two sets of ARRAY\_TESTS, and only analyse the second.) \\ 

Within the IRCAM\_CLRED window (see \S~\ref{IRCAM-CLRED} for how to
start this up), type ARRAY\_TESTS. Enter the start
observation (N) of the ARRAY\_TESTS data. The current STARE and
ND\_STARE readout noises and the current dark current will be estimated
from the dataset and the values printed at the end of the analysis. Also
given is an evaluation as to whether these values are in the valid
operational range.  An example of output expected is: \\
\begin{verbatim}
STARE    mode readout noise (e-) =  55.474
ND_STARE mode readout noise (e-) =  36.892
DARK CURRENT (e-/sec)            =  2.231

** STARE readout noise is nominal **
** ND_STARE readout noise is nominal **
** Dark current is nominal **
\end{verbatim}

If these values are not nominal, then you need to check if the temperatures
are too warm or if the chip is
being properly read out (see \S\ref{problems}). 

\newpage
\subsection{Observing Modes}
\label{Observing Modes}
There are currently four observing modes with WHIRCAM.  These are:
\begin{itemize}
\item STARE -- the array is reset, read after the user-defined
on-chip exposure times, and reset again. 
\item ND\_STARE -- the array is reset and read immediately and read again
after the user-defined on-chip exposure time.  The difference between
the post-exposure and pre-exposure images is taken and stored. 
\item S+A -- In Shift-and-Add mode, images are pre-processed in ALICE. 
The peak pixel in a user-definable area is found and the image is
shifted (by integer pixels) so the peak pixel falls onto a fiducial mark on 
the array.  N images are co-added in this manner.  S+A mode works in STARE 
mode only and is used to sharpen images and reduce seeing/tracking effects.  
The user is referred to \S~\ref{SAA Mode} for more details.
\item Atmospheric Monitoring imaging -- intended to allow monitoring of
such things as seeing and image stability, but not yet implemented. 
\end{itemize}

The two advantages of ND\_STARE over STARE is that (1) the direct read-out 
architecture of the detector means that the integrated 
charge may be sampled non-destructively and an improvement in read-noise 
is thus obtained by making multiple reads, and (2) the reset level can vary,
so you automatically subtract the latest reset in ND\_STARE. However, there is
also an extra time overhead in each readout, so for very short exposures 
(as in S+A) STARE is better. The shortest integration where
ND\_STARE is likely to be beneficial is about 1 sec. 

\newpage
\subsection{Taking an Exposure}
\subsubsection{Imaging menu}
\label{Imaging menu}
Imaging parameters (filter, exposure time, number of exposures per
integration) are controlled by CONFIG files. These in turn can either
be recalled, or loaded via EXEC files.  EXEC files specify a small
program of observations and telescope operations, such as executing
DARK, SKY, or OBJECT exposures, and using a series of SLIDE commands to
perform a mosaic and/or dither pattern of exposures.  Both
of these are accessed (and executed) from within the {\it `Imaging'} menu:
\begin{itemize}
\item {\it `Set\_instrument'} : 
The instrument parameters are defined by loading an {\em instrument 
configuration} (CONFIG) file. For example, the observer chooses the filter 
from a list in the {\em instrument configuration} screen and the appropriate 
filter combination and focus offset is automatically loaded. The exposure time 
must be short enough to avoid saturation (see \S~\ref{Array Saturation}) and 
long enough to ensure that the observation is background limited for 
maximum sensitivity (see \S~\ref{Background-Limited});
it can vary from 120ms at nb{\sl L}
(or as short as 12 ms if you read out a 64$\times$64 subarray) to tens of 
seconds in narrow band filters. With short integration times, 
many exposures may be coadded by selecting a number of exposures per 
integration, before the data are written to disk. This saves on disk space
and readout time overheads.  The final image written to disk is divided by
the number of exposures, thus giving an {\em average} exposure.  This may
be confusing as the exposure time in the header gives the total integration
time (ie $N \times $exposure time).  The log produced at the end of the night
keeps a record of the number of exposures per integration.


\item {\it `Set\_EXECs'} : Telescope offsets (for mosaics, etc) and sequences 
of different filter
exposures can be specified with {\em execution} (EXEC) files.
These are text files containing a list of commands to be executed
in sequence by the software.  A list of valid EXEC commands is given
below (Table~\ref{tab1} in \S~\ref{Valid EXEC Commands}).  An EXEC controls 
how data are taken 
with WHIRCAM (e.g. which CONFIG to use, where the telescope points relative 
to the slew coordinates, whether to take an OBJECT, SKY or DARK exposure etc).
This menu allows the user to define and/or edit
operational EXECs. 
The editor for the EXEC files is EDT, so the PF1 and Enter keys become
redefined as part of the EDT keypad during an EXEC edit.  To exit the
editor, type cntrl\^{~}Z. 

\item {\it `Set\_observation'} : This menu allows the user to define the 
type of observation being made (e.g. whether to execute an EXEC or a direct
observation of the OBJECT, SKY, DARK etc. 

\item {\it `Run'} : Entering this item runs the currently defined setup 
(by Set\_observation).  Data are actually taken and stored on disk.
To avoid writing rubbish to disk (and to tape), it
is a good idea to add a BREAK at the beginning of every EXEC
(see \S~\ref{Setup on Source}) so that you have an oportunity to review
a proposed EXEC, and to ensure that the telescope is tracking properly
(especially if you are autoguiding).

\item {\it `Movies'} : This menu allows you to take data in movie mode.  Movie
mode takes images of a pre-defined on-chip exposure time and displays
them on the ALICE display without storing data to disk. \

\item {\it `Set\_ALICE'} : This menu allows the user to define ALICE
Transputer setup parameters, such as varying the size of the array being
read out. 

\item {\it `Set\_graphics'} : This menu allows the user to change the ALICE
on-line display setup.  The user can change, for example, the plotting range 
for image display (don't attempt to change the colour table (LUT), as this
can often hang), or the position and size of the statistics window on the
ALICE image display.  You can also specify the bad pixel mask to be applied 
to the display.  Choose either `BPM\_FPA40348\_DEAD', which locates the 
brightest
hot pixels, or `BPM\_FPA40348\_SAA' which locates most hot pixels, and should
be used whenever taking frames in Shift+Add mode.
\end{itemize}

(Don't be too concerned if the above menu titles don't appear exactly
as described, as they may change under a new release of the IRCAM3 software.)
 
\subsubsection{Valid EXEC Commands}
\label{Valid EXEC Commands}
\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab1}: ~~ Valid EXEC Commands} \\[3mm]
\begin{tabular}{|l|l|}
\hline
EXEC Command & Description \\
\hline 
CONFIG NGC1333\_J & loads and executes CONFIG named NGC1333\_J \\
BREAK          & breaks current EXEC until Resume\_EXEC is hit \\
	       & Normally put after a CONFIG, to allow the observer to \\
	       & check correct configuration.  You can also append a \\ 
	       & label that will appear as a comment on the screen, to \\
	       & remind you what the BREAK is for (eg `check autoguider') \\
DARK           & takes a dark observation with dark setup (it is good \\
	       & practice to have two DARKs before an OBJECT or SKY -- \\
	       & the first removes any residual counts, the second is \\
	       & the proper DARK) \\
OBJECT         & takes an object observation with object setup \\
SKY            & takes a sky observation with object setup \\
SLIDE -20 +50  & slides telescope to offset -20,+50 in arcsec\\
               & SLIDE can be used when autoguiding or not, but must be \\
	       & done with the telescope tracking at SKY PA 0 \\
TOFF -20 +50   & moves telescope (alone) to offset -20,+50 \\
               & TOFF can only be used when NOT autoguiding \\
\hline 
\end{tabular}
\end{center}
\label{tab1}
\end{table}

\subsubsection{Initial Setup}
The following procedure describes taking data in STARE and ND\_STARE modes,
which are the normal modes for WHIRCAM.  See \S~\ref{SAA Mode} for 
taking exposures in Shift+Add mode.

First, load a CONFIG appropriate to your planned observing.  If you
don't do this you may be in an incorrect filter or have an incorrect
observing mode selected in the setup phase. 
\begin{itemize}
\item Start from the {\it `Imaging'} menu and go into the {\it
`Set\_instrument'} menu. 
\item Select the {\it `Recall\_configuration'} menu and enter the name
of the pre-defined CONFIG to be used and select YES for {\it
`Apply\_now'} option.  PF1 twice to exit back to the {\it `Imaging'}
menu. The named CONFIG will load into the system and will be executed
(i.e. filters will move, the exposure time set, etc). 
\end{itemize}

\subsubsection{Setup on Source}
\label{Setup on Source}
\begin{itemize}
\item Go into {\it `Movies'} menu.  Go into the {\it `Set\_movie'} menu
and select a movie exposure time (which is independent of the observing
exposure time in your CONFIG), say, 0.5 sec, and a number of movie
exposures per integration, say, 1 exposure/integration. PF1 to exit. 
\item If you are using ND\_STARE mode, go to next item below.  If you
are using basic STARE mode you may need to subtract a recent DARK or SKY 
exposure before you can see your source in movie mode.  If you need to 
subtract a DARK or SKY, go into the {\it `Set\_graphics'} menu, then go
into the {\it Background\_subtraction} menu.  Use either the {\it 
Subtract last integration} or {\it Subtract specified integration}
items to define the DARK or SKY to be downloaded into ALICE and 
subtracted prior to movie display.  Definition of a background to be
subtracted automatically enables background subtraction.  Remember
to disable background subtraction once you are finished with it.
(By the way, don't try and load a different LUT within {\it `Set\_graphics'}
as it causes the system to crash).
\item Select the {\it `Run\_movie'} item.  You will need to {\it
`Abort\_movie'} before you can exit from this item.  In movie mode,
images of the defined exposure time are taken and displayed
automatically on the ALICE movie screen.  Note: {\it No data are stored
to disk in this mode}. 
\item Ask the TO to centre the object at the position you require on
the array.  Check that the object is not saturated by inspecting the
statistics displayed (see \S~\ref{Array Saturation} on saturation levels).  
If necessary, {\it `Abort\_movie'} and reduce the movie exposure time and
repeat the above.  Because of the hot pixels, you must be careful about 
checking for saturation from sky.  Rather than looking at the peak count, 
try and choose an area of the array relatively free of hot pixels, and divide
the sum total by the number of pixels in the statistics box, to obtain
a mean count.  You can also change the display stretch from `nsigma'
to `zero-to-saturation' within {\it `Set\_graphics'}.
\item When you are happy with the source positioning and exposure time,
end the movie with {\it `Abort\_movie'} option. PF1 twice to return to
{\it `Imaging'} menu. 
\end{itemize}

\subsubsection{Taking Data On-source}
\begin{itemize}
\item Go into {\it `Set\_observation'} menu and type in name of object,
set EXEC mode (move through the options with the left/right arrow key
until EXEC is highlighted), and enter the name of the EXEC to be run. PF1 to
exit.  Doing this will load the EXEC into the stack displayed on the
IRCAM parameter status screen.  Check that the values selected are OK. 
\item Execute the {\it `Run'} item.  Generally, an EXEC will have a
BREAK command in it like CGS4.  This serves the purpose in WHIRCAM of
allowing a final check of the EXEC to be run (rather than allowing
peakup as in CGS4).  Once you have checked the EXEC, select {\it
`Resume\_EXEC'} and the EXEC will run to either termination or until the
{\it `Break\_EXEC'} item is selected in the {\it `IRCAM3\_running'} menu. 
\item Once the system is running you will see messages on the Instrument
control (menu) window of the the form: 
\begin{verbatim}
OBJECT configuration achieved OK
Starting observation 5
Started   IDIR:I960229_5_1
Completed IDIR:I960229_5_1
Starting observation 6
Started   IDIR:I960229_6_1
Filed     IDIR:I960229_5_1
Completed IDIR:I960229_6_1
Filed     IDIR:I960229_6_1
\end{verbatim}
The three messages can appear asynchronously since the software works in
that manner. 
\item Once the message starting with `Filed' has been issued by the
system, the image of that number will soon be available for 
plotting/processing. 
\item On the IRCAM\_CLRED window, a message of the form:
\begin{verbatim}
Observation file RODIR:RO960229_7 available!
\end{verbatim}
will appear when the image (Observation 7 in this example) is available
to the reduction software.
\end{itemize}

\subsection{Focussing}
The breadboard on which WHIRCAM sits has a series of permanent mounts
that should ensure WHIRCAM is properly aligned with the optical axis
and at a reasonable focus, and your support astronomer will check to
make sure that this is the case in the evening twilight of the first
WHIRCAM night (see \S\ref{problems} in case alignment is lost).  
Acquire a 5-8 mag star, and ask your TO to focus it on WHIRCAM (not
the autoguider!).  Once focussed, the temperature monitors, coupled to
the WHT focus drive, should ensure that focus is maintained throughout
the night.  However, if the seeing does seem to deteriorate, it is
always good procedure to re-check the focus.

The internal lenses are made from combinations of LiF and BaF elements,
which apart from optimising IR transmission, also ensure very good
image quality and only a small 
shift in focus position over the range 1 -- 5 \micron.  To compensate for this
wavelength-dependent focus shift, the detector is attached to a movable
mount, whose position is automatically controlled by the Vaxstation 
software, using a lookup table of internal focus positions for each
filter.  The offset positions, in mm,
are $J = -1.4$, $H = -1.1$, $K = -0.9$, and $L = -1.0$.

\subsection{Shutting Down}
At the end of the night, when all exposures have been taken, simply
hit the PF1 key until you reach the top of the Instrument Control's
menu tree.  You'll then be asked to verify that you want to shut down,
so answer `yes'.  When ALICE has finished shutting down, all but
the ALICE occam screen and the original DECterm window should have
closed.  If you logout of the DECterm window, the ALICE occam screen
should also close, but if it doesn't, simply select its `Files'
button and choose `Exit'.


\newpage
\section{Filters}
Two filter wheels, each with 10 positions are available inside the cryostat.
An extensive set of filters is installed currently, but there is room for 
more in the current configuration.  Changing filters requires the cryostat 
to be opened up, so ANYONE WHO WANTS TO USE A FILTER
NOT LISTED IN TABLE~\ref{tab2} MUST GIVE SUFFICIENT NOTICE FOR THE FILTER TO BE OBTAINED
AND INSTALLED (6 Months). 

In general, broad band filters are placed in the front wheel, while 
pupil apertures and any narrow band
filters that require the broad band filters as blockers   
are installed in the second wheel. 
The Filters and apertures currently installed in WHIRCAM are listed in 
Table~\ref{tab2}.  
\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab2}: ~~ WHIRCAM Filters} \\[3mm]
\begin{tabular}{|c|lc|lc|}
\hline 
Position &  \multicolumn{2}{c}{Wheel 1} & \multicolumn{2}{c}{Wheel 2}  \\
   & Element     & $\lambda$ (\micron) & Element & $\lambda$ (\micron) \\[2mm]
\hline 
1  &  Blank      &    opaque       & 2.10 {\sl K}$_{Cont}$ & 2.10 $\pm$ 0.01 \\
2  &  {\sl J}    & 1.28 $\pm$ 0.15 &  20 mm aperture       & open \\
3  &  {\sl H}    & 1.67 $\pm$ 0.14 &  16 mm aperture       & spider  \\
4  &  {\sl K}    & 2.20 $\pm$ 0.20 &  H$_2$ (v=1-0 S(1))   & 2.12 $\pm$ 0.01 \\
5  &  $K_{\rm sh}$ & 2.16 $\pm$ 0.16 &  Br$\gamma$           & 2.16 $\pm$ 0.01 \\
6  & nb{\sl L}   & 3.42 $\pm$ 0.03 & 7 mm aperture         & open \\
7  & {\sl L'}    & 3.80 $\pm$ 0.30 &  5 mm aperture        & open \\
8  &  Blank      &     opaque      & 2.25 {\sl K}$_{cont}$ & 2.25 $\pm$ 0.02 \\
9  & Spare H$_2$ & 2.12 $\pm$ 0.01 & 3 mm aperture         &  open \\
10 &  Blank      &     opaque      & JOSE array            & lenslets+prisms \\[1mm]
\hline 
\end{tabular}
\end{center}
\label{tab2}
\end{table}

\noindent
The transmission profiles for the main filters are plotted in 
Figure~\ref{fig4_filters}.

The {\sl Ks} filter ($\equiv K_{sh}$) is mounted with a PK-50 long wavelength 
blocker, which unfortunately also cuts transmission by a further 20\%.  
{\sl Ks} is a relatively
new filter from Barr Optical, without a fully characterised transformation
to {\sl K}.  However, as Pahre \& Mould (1994 ApJ 433, 567) point out, its
bandpass is intermediate between {\sl K} and {\sl K'} 
(2.10 $\pm$ 0.18 \micron), and rough corrections
of {\sl Ks}  to {\sl K} can be obtained by taking half those for {\sl K'} to 
{\sl K}.  This transformation is well defined by Wainscoat \& Cowie 
(1992 AJ 103, 332):

$K' - K = (0.22\pm0.03)(H - K)$, {\rm for} $0 < H - K < 0.4$ 

(For stars redder than $H-K = 0.4$, the relation flattens off to 
$K' - K \sim 0.07$ mag.)

The {\sl K} and
{\sl L'} filters are tilted by about 5$^{\rm o}$ to measure any ghosting 
effects, but no serious ghosting is apparent.  This means there may be a 
slight shift in an object's position when you change to/from these filters.

A fixed 17 mm diameter stop is fixed at the pupil (cold stop) near the filter
wheels.  This is slightly oversized with respect to the pupil image to ensure
that all the light from the telescope aperture is used at $J$ and $H$.
The open apertures produce a restricted cold stop (this is not strictly correct
as the rear filter wheel is a few mm from the true cold stop, but is close 
enough to be effective), which should block most
of the thermal emission from the perimeter of the secondary baffle, and should
be automatically selected by WHIRCAM only with filters longward of 2 \micron, 
as the penalty for reduced thermal emission is slightly higher vignetting.  
The different sizes correspond to the different magnifications used with 
Martini (see \S\ref{Martini}).
For direct imaging the calculated telescope pupil diameter is 16.35 mm.  
The apertures with spiders are designed to also block thermal emission from 
the central obstruction.

Each of the filter options available in the CONFIG files will automatically
load the appropriate combination of wheel 1 and 2 options.  Thus selecting 
{\sl Ks} will move wheel 1 to position 5 (the filter), and wheel 2 to 
position 3 (the 16 mm aperture to block thermal emission).  Note that the
CONFIG filters under OTHERS (ie J2, H2, K2 etc) are mostly for MARTINI.  
In particular, don't confuse H2 (which is the {\sl H} filter
plus a 16 mm aperture) with the H$_2$ filter, which is the narrow band
filter centred on the v=1-0 S(1) transition, called s1 in the CONFIG file.
The 2 $\mu$m narrow band filters are used with a broad band filter to block
out of band leaks. DARKs are taken with a blank + Br$\gamma$ to block both reflected and
thermal emission.
The combinations associated with each filter definition are defined
in UKIRT\_SCT:IRCAM.SCT, and while they must be ammended if a filter is 
changed (along with the UKIRT\_CONFIG:WHIRCAM.DATA file), this should only
be done by your SA or one of the telescope software engineers!
\begin{figure}[hb]
\psfig{figure=fig4_filters.eps,height=17cm}
\caption{Filter transmission profiles.}
\label{fig4_filters}
\end{figure}  


\newpage
\section{Exposure Times}
\subsection{Array Linearity}
Like all detectors, the relationship between input photons and output
counts for WHIRCAM is not exactly linear.  But as can be seen in 
Figure~\ref{fig5_non-lin}, 
it is almost linear over most of the dynamic range, up to about 80\% of well
capacity.  While it is possible to correct for the deviations from exact
linearity over this range, via a linearity correction table, this is
currently not available.  Hence if you require very precise photometry,
you would be advised to create a linearity map, by exposing the detector
to a reasonably flat, but constant, light source, over a range of
exposure times, to accurately measure the non-linearities of every
pixel.
\begin{figure*}[h]
\psfig{figure=fig5_non-lin.eps,height=10cm,angle=-90}
\caption{Accumulation of counts in odd and even columns, showing offset for odd
columns in the reset level, the degree of linearity, and the onset of
saturation.}
\label{fig5_non-lin}
\end{figure*}

\subsection{Saturation}
\label{Array Saturation}
An important thing to be aware of is array saturation.  With WHIRCAM,
saturation is defined by the full well capacity of the pixels, 
NOT by the dynamic range of the A-D converter (65,535 DN). 
The full well capacity is controlled by the substrate voltage (called the
bias voltage), but as
this also affects the number of hot pixels, a larger well capacity
is paid for by a larger number of hot pixels.  The default voltage setting
(0.68 V) provides a reasonable well depth and a bearable number of hot pixels.
If fewer hot pixels are required, then you can select a  lower
bias voltage by selecting {\em Imaging}, {\em set\_ALICE}, {\em recall\_setup},
then change {\em recall\_input} to FPA40348\_SHALLOW, followed by
{\em select\_enable} = YES.  This will change the bias voltage to 0.60 V.
The default is FPA40348\_DEEP, with a bias voltage of 0.68 V.

To make life interesting, the well depths, and hence saturation, vary 
across the chip, and vary with
wavelength.  And because of the non-linearity above 80\% of full well capacity,
the effective saturation level is even lower.  In the following, all
saturation figures are defined as 80\% of full well capacity.

For ND\_STARE mode with a bias of 0.68 V, the minimum saturation in {\sl Ks} is 9,500 DN 
(along the lower edge of the chip), and the minimum saturation within the 
central $128\times128$ pixels is 12,000 DN.  There is also an odd/even column effect, 
giving rise to two peaks in the saturation levels, at 13,500 and 17,500 DN.
At {\sl J}, these figures tend to increase, with the minimum saturation being
11,000 DN, the minimum within the central $128\times128$ being 14,000 DN, and the
two odd/even column peaks being at 15,500 and 17,500 DN.  Figure~\ref{fig5_non-lin},
plots the non-linearity for the even and odd columns, but shows simply the
means of these columns.  {\bf Users should be very careful to estimate
exposure times such that the maximum counts will not saturate on the chip
in the area of interest.  As most observations will be taken as combinations
of dithers, then the best practice would be to aim to have final counts
always below 10,000 DN in ND\_STARE.}  For STARE mode, the fixed pattern
noise, dominated by the reset values, has a range of 20,500 to 28,000 DN,
making a comparison with ND\_STARE difficult.  With a bias of 0.68 V and a 
{\sl Ks} filter, STARE mode has a minimum 80\% full well saturation above 
reset level (ie 100\% of reset level plus 80\% from there to saturation) 
is $\sim$37,500 DN, with less well-resolved peaks at
38,000 DN and 40,000 DN.   

The approximate 80\% well depths and number of hot pixels
for each Bias voltage are given in Table~\ref{tab3}.
\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab3}: ~ Bias Voltage} \\ [3mm]
\begin{tabular}{|c|c|c|c|}
\hline 
Bias    & Min Saturation & Min Saturation & Number of  \\
Voltage & DN (STARE) & DN (ND\_STARE) & Hot Pixels \\
\hline 
0.68	&  37500  &  10000	& 1500 \\
0.60	&  34500  &   7000	&  200 \\
\hline 
\end{tabular}
\end{center}
\label{tab3}
\end{table}

A problem with this array is that the odd columns tend to have a lower
well depth than the even columns.  So that both sets of columns will
have 80\% saturation at similar DN values, the reset level has been set up 
such that it is higher for the odd columns (see Figure~\ref{fig5_non-lin}).

In the thermal near-IR (3--5\micron), the background level is always high
and dominates any astronomical signal.  Short on-chip integrations are
always required.  

Although the detector is a 
direct readout device with 4 readouts which each address every fourth column, 
the minimum exposure time for full frame readout is 120 ms, limited by the
multiplexer performance, and it is this minimum exposure time and finite
well depth that defines lower magnitude limits below which stars will
saturate the chip.  Table~\ref{tab4} gives the minimum magnitudes of stars
which will saturate at this minimum exposure time (in 0.5\arcsec\ seeing and 
a scale of 0.24\arcsec/pix):
\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab4}: ~ Brightest observable stars}  \\ [3mm]
\begin{tabular}{|c|c|}
\hline 
{\sl  J}    &  $\sim$8.6 \\
{\sl  H}    &  $\sim$8.4 \\
{\sl  K}    &  $\sim$7.8 \\
\hline 
\end{tabular}
\end{center}
\label{tab4}
\end{table}
Faster exposures can be made (of brighter stars) if subarrays are
employed. 

\subsection{Extinction and Sky Brightness}

The extinction at {\sl J, H} and {\sl K} was estimated from observations of 
standard stars at about 0.10, 0.11 and 0.07 mag/airmass, respectively, but 
these values are likely to vary from night to night, and the best solution
is to monitor a few standards throughout the night, over the same range in 
air mass as your objects.  
A model of the sky emission together with a representation of telescope 
emission is shown in Figure~\ref{fig6_skyem}, while an atmospheric 
transmission spectrum is shown in Figure~\ref{fig7_skytr}.  The winter and 
summer sky brightnesses are given in Table~\ref{tab5}.
\begin{figure}
\psfig{figure=fig6_skyem.eps,height=13cm}
\caption{Calculated sky emission for winter (T = 278~K) under dry conditions 
between 1 and 2.5~$\mu$m. The strong airglow emission lines dominate the 
spectrum shortwards of 2.3 $\mu$m, where thermal emission from the sky starts 
to become apparent. However,  emission from the telescope increases rapidly 
beyond 2.2 $\mu$m and dominates the background. The dotted and dashed curves 
represent the emission from a 20\% emissive telescope at 285 and 275~K 
respectively.}
\label{fig6_skyem}
\end{figure}

\begin{figure}
\psfig{figure=fig7_skytr.eps,height=22cm}
\caption{Calculated sky transmission spectrum for La Palma.}
\label{fig7_skytr}
\end{figure}  

\begin{table}
\begin{center}
{\bf Table~\ref{tab5}: ~ Measured Sky Brightness - Mag/arcsec$^2$}\\[3mm]
\begin{tabular}{|l|c|c|}
\hline 
 & February 95 & June 95 \\
 & & Full Moon \\[2mm]
\hline 
{\sl J} & 16.6  & 15.6 \\
{\sl H} & 14.4  & 13.9  \\
{\sl K} & 11.0  &  11.4 \\
{\sl Ks} & 12.0 & 12.0 \\
{\sl L} & ~2.9 &  ~3.4 \\[1mm]
\hline 
\end{tabular}
\end{center}
\label{tab5}
\end{table}

\subsection{Background-Limited Operation (BLIP)}
\label{Background-Limited}
Minimum exposure times needed for noise due to sky to dominate the 
readout noise (RN $\sim 40 e^-$), assuming gain of 6 e$^-/$DN and a pixel
scale of 0.24\arcsec/pix are given in Table~\ref{tab6}.
\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab6}: ~ BLIP Times} \\ [3mm]
\begin{tabular}{|c|rr|}
\hline 
Band  & \multicolumn{2}{c}{Sky Noise/RN} \\
      &   1.0  &  3.0  \\
\hline 
{\sl  J}    &  $\sim$3s & $\sim$9s \\
{\sl  H}    &  $\sim$1s & $\sim$3s \\
{\sl  K}    &  $\sim$0.5s & $\sim$1.5s \\
\hline 
\end{tabular}
\end{center}
\label{tab6}
\end{table}

\subsection{Limiting Magnitudes}

Figure~\ref{fig8_exptimes} plots the log(Exposure time (secs)) needed to 
reach a given
\begin{figure}
\psfig{figure=fig8_exptimes.eps,height=24cm}
\caption{Calculated exposure times for various conditions.}
\label{fig8_exptimes}
\end{figure}  
magnitude at a S/N of 5 and 20, for seeing conditions of 0.564\arcsec\
(ie 1 \fbox{\rule[1mm]{0cm}{1mm}~}\arcsec, ie for surface brightness), 
0.8\arcsec\ and 1.2\arcsec, and for apertures 
of radius 2.5$\times$seeing, observing in ND\_STARE mode.

\subsection{Throughput}
The total instrument + telescope + atmosphere throughput was measured in June
1995 at about 15\%. This value is lower than expected, compared to the 
estimated total system throughput of about 22\%, based on the figures in
Table~\ref{tab7}.

\begin{table}[h]
\begin{center}
{\bf Table~\ref{tab7}: ~ Estimated Throughput}\\[3mm]
\begin{tabular}{|l|l|}
\hline 
Sky 	&	0.95 \\
3 x Al Telescope mirrors &  0.9$^3$	\\
3 x Ag Derotator mirrors &  0.95$^3$	\\
dichroic (wavelength dependent)	 &  0.95    \\
Window 			 &  0.95	\\
5 x lenses		 &  0.95$^5$	\\
Filter			 &  0.75	\\
Detector		 &  0.8		\\
Stop Vignetting at $\lambda > 2 \mu$m & 0.9 \\[2mm] \hline
Total			 &  0.22 \\
\hline 
\end{tabular}
\end{center}
\label{tab7}
\end{table}

\section{Standards}
\label{Standards}
A list of Faint and Bright (for 3 $\mu$m) IR UKIRT standards can be found 
in Appendix D.  The positions of these standards are also loaded into the
default WHT standards catalogue.
Typical exposure times for most of these will be 1-3 secs, and you
should of course take each standard exposure through each filter used
on your programme objects.  At the very minimum you should take 3-4
standards at the beginning and end of the night and 2-3 in the middle,
and it is always a good idea to take 1-2 throughout the night, every
1-3 hours, to monitor the sky conditions (especially true if there is
any dust around, or the possibility of cirrus).  You should also aim
to observe at least one standard over as large a range of airmass as 
possible, so you can derive extinction coefficients for each night,
as these may change depending on how much dust is around.

And don't forget to take your standards in a series of dithered
exposures, to allow accurate removal of sky and cosmic rays, and to 
remove all the hot pixels!

\section{Data Storage}
\label{Data Storage}
The exposures are written to an external hard disk as .SDF files, which 
should have up to 2 Gb (3.9 M blocks) free space at the start of your run.
Each 256$\times$256 frames is 270 kb (530 blocks) large, hence you should be 
able to store up to $\sim$7000 full sized images on disk, although the amount
of free space will often be less than as WHIRCAM data from previous runs are
generally not deleted until after the D-tape has been varified.  If your
exposure times are short, you should consider using a number of exposures
per integration to save disk space (see \S~\ref{Imaging menu}).


The disk name, directory structure and filename nomenclature are: 
\begin{verbatim}
DISK$IRCAM:[WHIRCAM.DATA.IRCAM_DATA.YYYYMMDD.IDIR]IYYMMDD_N_1.SDF
DISK$IRCAM:[WHIRCAM.DATA.IRCAM_DATA.YYYYMMDD.ODIR]OYYMMDD_N.SDF
DISK$IRCAM:[WHIRCAM.DATA.IRCAM_DATA.YYYYMMDD.RODIR]ROYYMMDD_N.SDF
\end{verbatim}
where YYYYMMDD is the directory date (eg. 1996 Feb 29 = 19960229),
YYMMDD is the filename date (eg. 1996 Feb 29 = 960229), and N is
the run number.  The IDIR directory contains the array+header data,
and it is these files which are written to tape by AUTOFITS (see below).
The files in the ODIR directory are just the header information for each 
frame, and
the RODIR directory is where frames read in and/or produced by
IRCAM\_CLRED are stored (ie Reduced Observations).

At the beginning of each night's observing start AUTOFITS running, which
will automatically back-up your data to a DAT D-tape and a C-tape (DAT or 
exabyte) as each frame is written to disk. AUTOFITS converts the .SDF files 
to FITS format as it writes them to tape.  The C-tape is the observer's copy 
which you can take home with you.  

To use AUTOFITS with WHIRCAM, log onto
one of the VAXcluster machines (LPVE, LPVF or LPVG, usually from
one of the VT220 terminals in the computer terminal room) as TPCOPY 
(no password required), type AUTOFITS, and answer all the questions.
You can currently write up to four tape copies simultaneously (one D tape
and up to 3 C tapes, but remember that more than one C tape must be paid for),
and append files to previous nights' data tapes.
AUTOFITS will write every file stored in the current IDIR directory,
including vector maps (created in Shift+Add integrations) and any 
reduced data frames you may create there (if you don't want these written
to your archive tape, then reduce your data in the RODIR directory).

If you wish to reduce your data at site using IRAF on the unix cluster,
you can either re-read your C-tape copy using rfits in IRAF, or else
create diskFITS copies using WDFITS in Figaro, and copy these to a
unix disk using ftp, followed by rfits in IRAF.

\section{Shift + Add Mode}
\label{SAA Mode}
Although S+A may sound like a good way to obtain sharper images, in
practice it suffers from a number of problems, making its use limited to
bright compact sources, not faint extended structure.  In order to benefit 
from S+A, the exposure times need to be shorter
than the typical variations in seeing (ie as short as possible), for which
the readout noise will dominate the background noise.
And because there are a large number of readouts per stored frame,
the summed readout noise will be quite large.  The effective noise will
be even larger if the number of transient hot pixels confuses
the shift algorithm to occasionally shift to the hot pixel rather than the 
source, hence the limiting magnitude of the guide star needs to be lower
than just a shorter exposure time might imply. 
As well, to obtain very good images, a magnified pixel scale is required,
but there isn't enough room at GHRIL (in direct mode with the dichroic)
to insert the pair of magnifying mirrors.  S+A also requires an offset sky 
frame to be taken beforehand, which is then subtracted from all the object 
frames before they are shifted and added.  And the number of exposures per 
integration must, for some peculiar reason, be a prime number.

You would only ever want to use S+A to sharpen your images, hence
you need exposure times shorter than the seeing variation timescale.
A reasonably bright star (brighter than $\sim$12 mag) is therefore needed for
the S+A centring algorithm to determine the correct shifts. 
Because of the extra readout overhead with an ND\_STARE, S+A is
taken in STARE mode.  This means a SKY frame must be taken before
a S+A sequence, so it can be subtracted from the subsequent OBJECT frames
within ALICE, in order remove most of the hot pixels (but alas not all -- see 
\S~\ref{Observing Modes}) and the fixed pattern of the bias
pedestal and flat field, so that centroiding can be done efficiently. 
SKY subtraction also  minimises the extra noise created by dithering the 
fixed pattern noise.  So before running S+A, offset to a clear
patch of sky, and take a sky frame of the same exposure as your object.

The sequence of commands to get S+A going is:
\begin{itemize}
\item Go into the {\it `Imaging'} menu, then the {\it `Set\_ALICE'} menu,
and then the {\it `Set\_read\_area\_\&\_speed'} menu.  Set {\it `Readout\_area'}
to 128$\times$128 or 64$\times$64, depending on the FOV required and the
frequency of corrections (see readout times in \S\ref{characteristics}).
Also set {\it `Readout\_speed'} to STANDARD.
\item Move telescope to an offset SKY position.
\item Go into {\it `Set\_Instrument'} menu, then into {\it `Direct\_config'} 
menu, and set Filter, Magnifier (2X or 5X if using Martini -- this tells
WHIRCAM to select the appropriate cold stop), Aquisition\_mode (to STARE),
Object\_exposure\_secs (something short, like 0.07 sec), and
Object\_exp\_per\_integ (enough integrations to give a decent S/N.  NOTE
this number MUST BE A PRIME!).
\item Take a SKY exposure: Go into {\it `Set\_observation'}, set to SKY,
then go into {\it 'Run'}.  Make sure this exposure time is the same as for
your object.
\item Move telescope to OBJECT and acquire object.
\item Tell WHIRCAM to subtract the SKY image: go into {\it `Set\_graphics'},
then into {\it `Background\_subtraction'} and set 
{\it `Subtract\_last\_integration'}.
\item Now select S+A: go into {\it `Set\_ALICE'}, then into {\it `S+A'},
and set Enable\_shift\_\&\_add to TRUE, Bid\_area\_dimensions to
32$\times$32 or 64$\times$64 (to define the size of array ALICE searches for
a peak), and Bid\_area\_centre\_X to 128 and Bid\_area\_centre\_Y to 128,
if search area is in centre of chip.  Note that the X and Y coords for the
search area are with respect to the whole chip, not any subarray that may
have been selected to decrease the readout time.
\item Now tell WHIRCAM to ignore bad pixels in its search for the peak:
go into {\it `Specify\_bad\_pixel\_mask'}, and set 
\_for\_shift\_\&\_add\_observations to `bpm\_fpa40348\_saa', and set 
Force\_download\_of\_newmask to TRUE.
\item Finally, go into {\it `Set\_observation'}, set to OBJECT, then
go into {\it 'Run'}.
\end{itemize}

Once the OBJECT integration is finished, a normal (but hopefully better 
resolved) WHIRCAM image file will be created, plus a vector map of all
the centroids determined by ALICE, in an image filename suffixed with `V'.

\newpage
\section{Trouble Shooting}
\label{problems}
It is possible as with all complex instruments and electronic systems,
that a time will come when the user encounters a problem, a hangup or a
crash.  This section details known problems and how to recover from them
cleanly.  Please seek the help of your SA or TO when a problem occurs!  
It is likely they have `seen it all before'.
\\

 WHIRCAM REFUSES TO STARTUP \\
\begin{itemize}
\item The PROBLEM: 
After typing whircam\_startup, at some point you
get an obscure error message and the startup task exits before
all windows are created.  

\item The SOLUTION:
Check to ensure that the ADAMNET task is running on both the WHIRCAM
Vaxstation and on the VAX cluster by typing SH SYS on the
WHIRCAM terminal, and on  LPVS3 or LPVS2, and make sure the ADAMNET task
is running on both.  If it isn't, then type @UKIRT\_DIR:ADAMNET
\\
If ADAMNET was running, or if one of the error messages is ``nonsense SP 
request,'' then shutting down WHIRCAM and logging out,
then logging in and re-starting should solve the problem.  If it still
gets stuck, reboot IRCMVX (the WHIRCAM Vaxstation) (ask your SA or Duty
Engineer).
\\ 
\end{itemize}

 THE ALICE OCCAM/TRANSPUTER SYSTEM HANGS/DIES \\
\begin{itemize}
\item PROBLEM:
At some point, the Occam/Transputer system will crash/die with one of
the following error messages appearing on the IRCAM3\_DEV SMS menu 
window.
\begin{verbatim}
BDS_ERRCHK> Error while getting ackn from CORE of GO completion
- BDS_CORE_SERVER> ERROR: Channel comms timed out on tag receive
WFG_OBEYW> Error completing action COMPLETE in 4^^1 task.
BDS_CORE_SERVER> ERROR: Channel comms timed out on tag receive
!! AIM> After INTEGRATE TASK_DONE SAI-I-ERROR, Error
%SAI-I-ERROR, Error
148013867
\end{verbatim}
or
\begin{verbatim}
BDS_ERRCHK> Error while sending parameter block
- BDS_CORE_SERVER> ERROR: Channel comms timed out on tag send
WFG_CONFIGURE> Action SEND_PARAMETERS in BDS task failed.
- BDS_CORE_SERVER> ERROR: Channel comms timed out on tag send
!! ALICE_DONE> Action failed to complete in WFG : STATUS = 
SAI-I-ERROR, Error
!  ALICE_DONE> Returned OUTVAL =BDS_CORE_SERVER> ERROR: Channel 
comms timed out 
! on tag send
!! AIM> After CONFIGURE TASK_DONE SAI-I-ERROR, Error
%SAI-I-ERROR, Error
148013867
\end{verbatim}

What is happening is that the BDS gets a command (to say, GO) and sends
this onto the CORE transputer system. This should be, and is,
acknowledged.  When the observation completes, the CORE has to send an
acknowledgement to the BDS that the (GO) completed successfully - it is
this acknowledgement that the BDS never receives (e.g. ackn from CORE of
GO completion).  This is a sure sign that the Occam is hanging for some
reason - the subsequent error: \\ 
(starting BDS\_ERRCHK$>$ Error while sending parameter block ...) \\ 
is a further indication that the Occam side cannot communicate with
anything else. \\

\item The SOLUTION:  Try the following first:
\begin{enumerate}
\item Click on small ALICE parameter display window to re-activate it.
\item Do cntrl\^{~}C three times.  The result of this will be to re-gain the DCL
\$ prompt.
\item Open a new DECterm window under the Applications menu of the 
Session Manager. 
\item In the new DECterm type:
\begin{verbatim}
ALICE_CONFIG <CR>
ALICE_OCCAM <CR> 
\end{verbatim}
This will re-load the Occam/Transputer side.
\item Click on IRCAM3\_DEV window to re-activate it again.
\item Go up to the top level IRCAM3 menu.
\item Go into the {\it `Engineering'} menu.
\item Go into the {\it `ALICE\_engineering'} menu.
\item Go into the {\it `Reinitialise\_occam'} item. This will
re-establish communication with the Occam/Transputer system. 
\end{enumerate}
Unfortunately, this appears not to be successful ALL the time.  If this
procedure does not work then run down the whole WHIRCAM system,
logout and start again!  This process will take about 5 minutes. 
\\
\end{itemize}

 THE ALICE/TELESCOPE LINK HANGS/DIES DURING A SLIDE\\
\begin{itemize}
\item The PROBLEM:
If your EXEC calls for a series of SLIDES (eg for a dithered pattern), and
the telescope is also autoguiding, then occasionally the link between
WHIRCAM and the telescope control software (TCS) dies and the EXEC is 
suspended.  This is because the TCS was waiting for a handshake from
the autoguider, telling it that the guide star has been re-acquired
after the SLIDE, but it didn't get it within the default response
time.  

\item The SOLUTION:
On the ICL terminal, type `SEND AUTO CANCEL GUIWIND', which should cancel
the hung state of the TCS.  Then get your TO to re-aquire the guide star 
with the autoguider, then on the {\em IRCAM3 Instrument Control} screen
select {\it `Resume\_EXEC'} and the EXEC should resume where it left off.
\\
\end{itemize}

\newpage
 ETHERNET FAILS \\
\begin{itemize}
\item  The PROBLEM: Communications fail.

\item The SOLUTION:
First, check for a flashing light on the ethernet box in the WHT computer 
room.  WHIRCAM is connected to port 4.  If its flashing, reset the box.

If no flashing light, then type SET PROC/PRIV=ALL in WHIRCAM's SMS window,
then type UCX. At the UCX prompt, type `ping cgs' which checks for a response
from ALICE.  If no response, then something is likely wrong with either
the ethernet, the B300, or IRCMVX ethernet.  Call a duty tech.
\\
\end{itemize}

 THE WHIRCAM MOTOR DRIVES FAIL \\
\begin{itemize}
\item  The PROBLEM:
Being a mechanical part, the motor drives that position WHIRCAM's filter 
wheels are the one part that may fail at some time (usually about 3 am).  
As the filter wheels are positioned according to
indents on the wheels tripping a microswitch, ALICE should tell you
if it can't move the filter wheels, such as when a drive motor fails.

\item The SOLUTION:
First, check that it is a problem, and select the {\it `datum\_motors'}
menu in {\it `ircam\_engineering'} (via the {\it `engineering'}
and {\it `set\_instrument'} menus).  If this fails, then reload the
motor drive software, as described in the WHIRCAM DUTY ENGINEER CHANGE
MANUAL (in the WHT control room or the WHT manager's office).
If this fails, then the motor(s) is/are probably stuffed.

Replacing the failed motor drive is the obvious solution, but so as
to avoid losing a large fraction of the night, there is an option of
running WHIRCAM without motor control, in which all the other functions
will continue as normal, but filter changes will have to be done by hand.
In this case, close down WHIRCAM, and restart with `whircam\_manual'
instead of `whircam\_start'.  The motor drives sit on the back of the
WHIRCAM cryostat, and when not powered (switch off the drives in
the GHRIL console area), can be rotated by hand.  The datum position
(position 1) is marked on the drive wheel, and each new position (in the 
direction of the arrow) can be felt by hand as you rotate the wheel.
While this may be time consuming and laborious, real astronomers prefer
this than to going to bed early.
\\
\end{itemize}

 HIGH DARK CURRENT \\
\begin{itemize}
\item  The PROBLEM:
The results from an array\_tests (see \S\ref{tests}) gave non-nominal results
for the dark current.

\item The SOLUTION:
Repeat array\_tests to make sure it wasn't a fluke.  If it still
persists, check that the cold head temperatures on the
temperature displays in the GHRIL room are nominal (Table~\ref{tab8}). \\
\begin{table}
\begin{center}
{\bf Table~\ref{tab8}: ~ Nominal Temperatures} \\ [3mm]
\begin{tabular}{|l|c|}
\hline
Temp Probe & Nom Temp \\
\hline 
Optics    & $\sim$70-80 \\
Detector & 30 \\
Cold head 1 & $\sim$60 \\
Cold head 2 & $\sim$20 \\
\hline 
\end{tabular}
\end{center}
\label{tab8}
\end{table}
If any temperatures aren't nominal, then the He in the closed cycle
cooler may be low, and needs to be topped up.  Call the Duty Tech.
\\
\end{itemize}

\newpage
 HIGH READOUT NOISE \\
\begin{itemize}
\item  The PROBLEM:
The results from an array\_tests (see \S\ref{tests}) gave non-nominal results
for the readout noise.

\item The SOLUTION:
If your ALICE display shows a lot of diagonal streaks, then ALICE probably 
isn't switched on.  The enable switch is a
key in the upper middle part of the ALICE rack up in the GHRIL control room,
and should be fully turned CLOCKWISE (a green LED to the right of the
key will be on if enabled).
\\ 
If the display looks flat (apart from hot/dead pixels), then repeat 
array\_tests to make sure it wasn't a fluke.  If it still
persists, then check if the chip is
being properly read out.  To achieve fast readout times, ALICE uses 4
ADCs, each reading out every 4th column.  Check 
to make sure all readout channels are reading out similarly, by plotting a
histogram of each readout output.  To do this, open another DECterm
window, type `set def DISK\$IRCAM:[WHIRCAM.DATA.IRCAM\_DATA.19960229.RODIR]',
then `ircam\_setup', then type `cgs4dr' (the Data Redustion System for UKIRT's
CGS4 IR spectrograph).  This will create another SMS window session.
Within this, select the {\it `engineer'} menu, then {\it `graphics'},
then {\it `plot\_histogram'}.  Within this menu set Data to the 4th
image in the array\_tests sequence (this is a DARK), and the following:
\begin{verbatim}
Display_port = 1
Data_area = DATA
Number_of_bins = 50
X_step = 4
Y_step = 1
Smooth_size = 0
Soft_or_hard_copy = SOFT
Display_whole_area = FALSE
_xstart_if_not_whole = 1
_ystart_if_not_whole = 1
\end{verbatim}
This should plot a histogram of the first transputer readout in the upper 
left quadrant of the image display. To display the second transputer readout,
reset Display\_port to 2 (shifts to the next display quadrant in upper
right) and \_xstart\_if\_not\_whole to 2.  Repeat for the third and fourth
transputer readout.  You should then end up with 4 histograms, one per display
quadrant.  They should be all about the same mean, with widths of typically a 
few counts.  If one is noticeably wider, then check the cable for that
transputer (in the ALICE rack in the GHRIL control room) to make sure it 
isn't loose.  If the SA doesn't know which cable belongs to which transputer
(eg the brown cable is channel 4),
you'll have to disconnect each in turn, repeat array\_tests and re-plot the
histograms to see which one changes.

If all cables seem to be OK, then it may be that one of the ADC cards is
broken.  Spare cards exist, so call your Duty Engineer.
\\
\end{itemize}

 MISALIGNMENT OF WHIRCAM AND/OR DICHROIC \\
\begin{itemize}
\item  The PROBLEM:
Normally, WHIRCAM should be properly aligned with respect to the rotation and
optical axes by the SA at the start of a run.
However, if some clod happens to later bump into either WHIRCAM or the 
dichroic, then you'll need to call your SA (or the site SA) to re-align
the optics.

\item  The SOLUTION:
This is the method your SA should use to realign.
If only the optical breadboard was bumped, then use the alignment jigs to
re-position it back to its nominal position and orientation.  Stand next to 
the optical table, facing WHIRCAM's snout (ie looking over the dichroic
box towards WHIRCAM, with the telescope and de-rotator to your left).
Get someone else to face you, on the other side of the table (the breadboard is
heavy and won't slide very easily, so you'll need someone else to push/pull
while you pull/push).  There are two metal alignment tabs attached to your
side of the breadboard, and one tab on your left side of the breadboard,
near the re-rotator.  Slide the breadboard such that all 3 tabs touch the 
sides of the optical table.  Make sure that the various location clamps on
the breadboard are still tight.

If the dichroic was moved, then you must tweak the micrometers to re-align it:
\begin{itemize}
\item In the GHRIL control room, disconnect the graphics monitor cable, and 
connect up a PC monitor (which if not in the GHRIL control room will have to be
`borrowed' from someones desk), and place it on the optical table.
\item Run MOVIE with 0.5 sec integration, in ND\_STARE mode, the nbL filter,
and 0.68V BIAS.  Put the statistics window on a dead-pixel-clear part
of the chip (select {\em set\_graphics, statistics\_window} menus, then
set centre\_column to 145, centre\_row to 120, width to 10, height to 10).
Take a DARK and set graphics to
subtract it from subsequent exposures.
\item Point telescope to near zenith, make sure dome and mirror covers are
open, and that you are pointing at blank sky and not a bright star, and
make sure the telescope is tracking.
\item Adjust first one micrometer so as to minimise the total counts from
sky (the night sky at $L$ should always be less emissive than the secondary 
baffle!).
Make sure stray fingers don't touch the dichroic, and are well away from
WHIRCAM's FOV when you take the measurements.  Now do the same for the other
micrometer (ie the other axis).  Finally, repeat for the first micrometer.
\item You should now be re-aligned.  Take note of the micrometer readings.
(In January 1996 these were twist (azimuth) = 5.810 mm, shout (altitude) = 
5.135 mm.)
\item To be sure, you can repeat the above, but first set up on a bright star,
set the filter to $J$, and now try to maximise the total counts (check to make
sure the peak pixel isn't saturated, and keep the whole of the stellar image 
within the statistics box on the monitor).
\item The final micrometer readings should be the same as those obtained on
sky in NBL.  If not, repeat on sky with the NBL filter.
\end{itemize}
You may need to re-determine the rotation centre (your TO should know how),
but make sure it is for SKY PA 0.  (In Jan 1996 the rotation centre was at
WHIRCAM pixel position 103, 195).
\\
\end{itemize}


\newpage
\section{Appendix A. ~~ Data Reduction with IRCAM\_CLRED}
\label{IRCAM-CLRED}
\begin{quote}
These notes are taken from UKIRT's IRCAM3 manual by Colin Aspin (see \newline
http://www.jach.hawaii.edu/\~{ }caa/caa\_ircam3.html),  
and modified for WHIRCAM. 
A UNIX version of IRCAM\_CLRED has also been recently written, called \newline
IRCAMDR (see http://www.jach.hawaii.edu/ukirt\_sw/ircamdr/sun41.html).
\end{quote}

Either log onto any of the Vaxstation terminals (LPVS3 or LPVS5) as
user OBSERVER (get current password from SA or TO), or open another
DECterm window on the WHIRCAM terminal, then type (where YYYYMMDD
is the current year, month and date, eg 19960229):
\begin{verbatim}
	ircam_setup
	set def DISK$IRCAM:[WHIRCAM.DATA.IRCAM_DATA.YYYYMMDD.RODIR]
	ircam_clred
\end{verbatim}

You will be asked to supply the same ID as you entered under
\mbox{IRCAM\_DEV}, a workstation number (always choose 18), the data
format (`NEW' for WHIRCAM data), the UT date relevant for the frames
taken (eg 960229), a filename suffix (choose `none') and the plate
scale (0.24 \arcsec/pix for WHIRCAM direct). \\ 

The IRCAM Command Line REDuction system will now run up and present you
with the IRCAM logo (on the graphics window) and the prompt:
\begin{verbatim}
Ircam-Clred > 
\end{verbatim}

You can, if you like, reduce the size of the DECterm windows to see the
whole of the GKS graphics window by clicking on `Options' and selecting
`Window' and clicking on `Condensed Font' then `Apply' and finally `OK'.

Once in IRCAM\_CLRED, the system is setup to access the 
reduced observation files (prefixed by RO) in the current directory
by their observation number alone.  
\begin{itemize}
\item To display an RO image (eg observation 42) type: 
\begin{verbatim}
NS 42 <CR> 
\end{verbatim}
\item To display the difference between two images (say, an OBJECT and a 
SKY or two OBJECTs at different spatial positions) type:
\begin{verbatim}
DISP 42 41 <CR>
\end{verbatim}
to subtract 41 from 42 and plot the difference.
\item To define a zeropoint use the command:
\begin{verbatim}
STDPHO 41 42 <CR>
\end{verbatim}
where observations 41 and 42 are the first two images of a faint 
standard (FS) 5-point mosaic (see \S~\ref{Standards}).
The difference between the two images will be plotted and you will
be asked to select the standard star with the cursor.
The system will calculate a zeropoint and load it into the system.
\item To reduce STARE and ND\_STARE mosaics type:
\begin{verbatim}
STRED <CR>
\end{verbatim}
Below is an example of the input required by STRED.
\begin{verbatim}
Ircam-Clred > stred
Current IRCAM file prefix =  RO960229_
Current IRCAM file suffix =  NONE
Enter a PREFIX for the output image(s)
Prefix    |IMAGE_| ? field22_
Enter start observation number ?
Start           |1| ? 21
Enter number of images to be reduced ?
Number of Images |1| ? 5
Enter the DARK image number :
Dark number    |1| ? 2
    Observation specified as DARK is truly a DARK!
    CONGRATULATIONS, you did good!!!
Do you want to MEDIAN FILTER the objects for a flat or
use a SEPARATE pre-prepared (normalized) SKY image ?
Median or Separate Sky (M,S) |M| ?
Do you want the images airmass corrected ?
Airmass Correction (Yes or No) |N| : y
Do you want the images auto-mosaiced ?
Mosaicing (Yes or No) |Y| : y
Getting RA,DEC offsets from input images...
  Image  RO960229_21
  Image  RO960229_22
  Image  RO960229_23
  Image  RO960229_24
  Image  RO960229_25
RA,DEC (modified) offsets in image sequence are :
     0.000     0.000
     0.656    -5.297
     6.178    -5.124
     6.268     0.379
     5.633     5.411
Use these offsets or use user-defined telescope  offset (ASCII) file ?
File Offsets or User-defined (F,U) |F| ?
Give name for FINAL mosaiced image :
Final Image |X| ? field22_final
\end{verbatim}

STRED then reduces the specified images and, if requested, puts together 
the final mosaic. Output images will be, as in the e.g. above, 
\begin{verbatim}
FIELD22_21DFGA
FIELD22_22DFGA
FIELD22_23DFGA
FIELD22_24DFGA
FIELD22_25DFGA
FIELD22_FINAL
\end{verbatim}
\end{itemize}
Other useful IRCAM\_CLRED commands include:
\begin{itemize}
\item CSTATS gives statistics (max,min,mean,median,1-sigma
std) on cursor defined box on image. 
\item LIMAG gives 1-,5-,10-,100- sigma limiting magnitudes of
images/mosaics once zeropoint has been defined. 
\item PHO to get photometry of sources - 4$''$ aperture is good for
faint standards, 2$''$ is good for faint sources (e.g. asteroids, QSOs
etc). 
\item EXIT to exit.
\end{itemize}

\section{Appendix B. ~~ IRCAM\_CLRED Commands}

\hspace{2cm} {\bf Image Analysis commands}
\begin{tabbing}
xxxxxxxxxxxxxxxxxxxx\=xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx\kill
Name \> Description \\
ANNSTATS  \> Statistics in annulus in an image. \\                                              
APERADD  \> Statistics in aperture in an image. \\                                              
APERPHOT  \> Aperture photometry in an image. \\                                                
APERPOL  \> Aperture polarimetry in 4 pol images. \\                                            
BINUP  \> Compressed image in size by averaging pixels. \\                                      
BLOCK  \> Block smooths an image. \\                                                            
CALCOL  \> Calculates colours from magnitude images. \\                                         
CALEXP  \> Calculates optimum exposure time for image. \\                                       
CALMAG  \> Calculates magnitude image from flux image. \\                                       
CALZER  \> Calculates zeropoint from flux/inst. mag. \\                                         
CENT2  \> From two cursor positions, calculates source distance and p.a. \\                     
CENTROID  \> Calculates centroid position of stellar image. \\                                  
COMPADD  \> Compresses size of image by adding numbers in NxM box. \\                           
COMPAVE  \> Compresses size of image by averaging numbers in NxM box. \\                        
COMPICK  \> Compresses size of image by picking every Nth, Mth pixel. \\                        
COMPRESS  \> Compresses size of image. \\                                                       
CREFRAME  \> Creates an test image with different output options. \\                            
CSGEN  \> Generates a centro-symmetric polarization pattern THETA image. \\                     
DAOCEN  \> DAOPHOT utility for ... \\                                                           
DAOFIND  \> DAOPHOT utility for ... \\                                                          
DAOGID  \> DAOPHOT utility for ... \\                                                           
DAOGID2  \> DAOPHOT utility for ... \\                                                          
DEVFCS  \> Calculates deviation from centro-symmetry in polarization THETA image. \\            
FINDPEAK  \> Finds a peak (??) \\                                                               
HISTEQ  \> Histogram equalizes an image. \\                                                     
HISTGEN  \> Generates a histogram of an image. \\                                               
IMCOMB  \> Combines images by scaling and insertion. \\                                         
LAPLACE  \> Applies a Laplacian filter to an image. \\                                          
LIMAG  \> Calculates limiting magnitudes using zeropoints set by SETVAR. \\                     
LOOK  \> Shows on terminal sub-array values in an image. \\                                     
MANIC  \> Changes size of an image busing cubic-spline interpolation. \\                        
MEDIAN  \> Applies a median filter to an image. \\                                              
MOFF  \> Mosaic tiles auto DC and spatial offset matching. \\                                   
MOFFLOT  \> Applies MOFF to a sequence of images. \\                                            
OLOOK  \> Shows on terminal sub-array of image referred to by observation number. \\            
PHO  \> Aperture photometry on image using separate sky aperture. \\                            
PHO2  \> Aperture photometry on image using concentric sky annulus. \\                          
PHO3  \> Ap phot on image using concentric sky annulus displaced from object aperture. \\       
RADIM  \> Produces a radial profile image from given image and user-defined position. \\        
SEE  \> Interactive star selection then (KAPPA) PSF fitting for FWHM. \\                        
SHADOW  \> Shadow enhances an image. \\                                                         
STDPHO  \> Performs photometry on images and defines zeropoint. \\                              
STEPIM  \> Steps an image (pseudo-contours) between user-defined flux levels. \\                
STREHL  \> Calculates the Strehl ratio of an image. \\                                          
\end{tabbing}

\hspace{2cm} {\bf Image Display commands}
\begin{tabbing}
xxxxxxxxxxxxxxxxxxxx\=xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx\kill
Name \> Description \\
ABLOCK  \> Plots colour block at at user-defined location. \\                                   
AGAIN  \> Re-displays last image plotted. \\                                                    
ANNCOL  \> Sets colour of displayed annotation. \\                                              
BORDER  \> Draws a simple box border around an image. \\                                        
BOX  \> Plots a rectangular box on an image. \\                                                 
CABLOCK  \> Plots a colour block at cursor selected position. \\                                
CBOX  \> Plots a rectangular box at cursor position on image. \\                                
CCIRCLE  \> Plots a circle at cursor position on image. \\                                      
CCROSS  \> Plots a cross at cursor position on image. \\                                        
CCUT  \> Plots a cross-cut through an image from x1,y1 to x2,y2. \\                             
CELLIPSE  \> Plots an ellipse at cursor position on image. \\                                   
CIRCLE  \> Plots a circle at user-defined position on image. \\                                 
CLEAR  \> Clears the plotting window of all images/line graphics. \\                            
CLEARIT  \> Clears a user-defined area of images/line graphics. \\                              
CLINE  \> Plots a line between cursor defined positions on image. \\                            
CNSIGMA  \> Plots an image with NSIGMA scaling at cursor position. \\                           
COLCYCLE  \> Cycles a pre-defined colour table (LUT) N times. \\                                
COLINV  \> Inverts the colour table (LUT) colours. \\                                           
COLTAB  \> Write a pre-defined colour table (LUT) to plotting window. \\                        
CONTOFF  \> Defines offsets on screen (in pixels) for contour map plot. \\                      
CONTOUR  \> Plots a contour map of image defined in SETCONT. \\                                 
CONT\_TITLE  \> Defines the title for a contour map plot. \\                                    
CPLOT  \> Plots an image with X to Y scaling at cursor position. \\                             
CRANPLOT  \> Plots an image with +-X on mean scaling at cursor position. \\                     
CRECOLT  \> Creates a colour table (LUT) with user-defined colours. \\                          
CROSS  \> Plots a cross at user-defined position on image. \\                                   
CROSSCUT  \> Plots cross-cuts through user-defined point in image. \\                           
CROSSCUT\_PEAK  \> Plots cross-cuts through peak closest to user-defined images.\\              
CURSOR  \> Puts up cursor and returns value a selected position. \\                             
CUT  \> Plots cut/slice through user-defined points in image. \\                                
CUT2FF  \> Allows/disallows writing of CUT values to ASCII file. \\                             
CUT\_TITLE  \> Sets title of CUT plot. \\                                                       
CVARGREY  \> Plots image with dual-slope scaling at cursor position. \\                         
CXWIN  \> Increase or decreases plotting window size by 10\% \\                                 
DISP  \> Subtracts two images, displays the result and allows simple photometry. \\             
DISP2  \> Plots two images side by side with annotation. \\                                     
DISP4  \> Plots four images in quadrants with annotation. \\                                    
ELLIPSE  \> Draws ellipse at user-defined on image. \\                                          
FPSTRIPLOT  \> Plots an FP strip chart. \\                                                      
GETCM  \> Returns current calculated plot limits. \\                                            
GETRAST  \> Gets size of workstation in raster coordinates. \\                                  
GRID  \> Draws a grid of user-defined width on image. \\                                        
HARDCOPY  \> Makes a hardcopy of image or line graphics. \\                                     
HARDLOT  \> Makes a hardcopy of a sequence of images. \\                                        
LAGAIN  \> Plots last line graphics (CUT,CONTOUR,VEC) again. \\                                 
LINE  \> Plots a line between user specified points on image. \\                                
LINECOL  \> Sets colour of lines plotted on images. \\                                          
LINE\_WIDTH  \> Sets line width of lines plotted on images (useful for HARDCOPYs). \\           
LOGO  \> Plots IRCAM3 logo image. \\                                                            
MANYCOL  \> Plots all available colour tables (LUTs) in sequence. \\                            
MCURSOR  \> Displays cursor N times and returns values in image. \\                             
MORENSIGMA  \> Re-plots last NSIGMA plot with different stretch. \\                             
MOREPLOT  \> Re-plots last PLOT with different limits. \\                                       
MORERANPLOT  \> Re-plots last RANPLOT with different range on mean. \\                          
MOREVARGREY  \> Re-plots last VARGREY with different parameters. \\                             
NSIGMA  \> Plots an image with $\pm$N-sigma on mean scaling. \\                                 
PCLOSE  \> Closes plotting on current device. \\                                                
PENCOL  \> Sets user-defined pen to user-defined colour. \\                                     
PENINT  \> Sets user-defined pen to user-defined RGB intensities. \\                            
PLOT  \> Plots an image using user-defined scaling limits. \\                                   
PLOTGLITCH  \> Plots an image (NSIGMA) and removes user-selected bad pixels. \\                 
PLOTLOT  \> Plots a sequence of images with user-defined scaling limit. \\                      
POPEN  \> Opens plotting on a user-specified device. \\                                         
RANPLOT  \> Plots an image using user-defined range on mean for scaling limits. \\              
SETCEN  \> Defines centre point for image display. \\                                           
SETCOMORI  \> Sets orientation of comments written to display. \\                               
SETCONT  \> Setup definition for CONTOUR. \\                                                    
SETCONTIC  \> Sets contour tick mark ... \\                                                     
SETCUR  \> ... \\                                                                               
SETCURMARK  \> Defines whether cross is drawn on cursor selected points. \\                     
SETCUT  \> Setup definition for CUT, CCUT. \\                                                   
SETCUTAXRAT  \> Defines cut axis ratio on display. \\                                           
SETFONT  \> Defines font used for comments. \\                                                  
SETHARD  \> Defines hardcopy device used in HARDCOPY.\\                                         
SETMAG  \> Defines magnification factor used in image display. \\                               
SETMAX  \> Defines maximum value for limit scaling of image display using PLOT. \\              
SETMIN  \> Defines minimum value for limit scaling of image display using PLOT. \\              
SETMM  \> Runs both SETMAX and SETMIN above. \\                                                 
SETNUM  \> Defines axis annotation in terms of RA,DEC or offsets. \\                            
SETNUMORI  \> Defines number orientation on image axes. \\                                      
SETNUMSCA  \> Allows user to scale numbers on axes. \\                                          
SETPOLCOL  \> Sets colour of polarization vectors on display. \\                                
SETPRE  \> Sets file prefix for old style container file reduction. \\                          
SETPS  \> Defines current pixel scale in images. \\                                             
SETQUAD  \> Defines which is 5 quadrants (incl. centre) images are displayed in. \\             
SETRADEC  \> Defines RA,Dec of fiducial mark in image for axis annotation. \\                   
SETVAR  \> Defines various parameters for image analysis (eg scale, ap sizes, zp's). \\         
SETVARGREY  \> Defines parameters for a VARGREY image display. \\                               
SETVEC  \> Defines polarization vector map setup. \\                                            
STRIPLOT  \> Plots a stripchart data set obtained with STRIPCHART. \\                           
SURROUND  \> Displays axis annotation around an image and defined by SETNUM. \\                 
TICKIO  \> Defines whether plot ticks are plotted inside or outside the border box. \\          
TICKLEN  \> Defines the length of the tick marks plotted. \\                                    
VANS  \> Displays a S+A vector array image. \\                                                  
VARGREY  \> Displays an image using variable grey scaling. \\                                   
VEC  \> Plots a polarization vector map defined by SETVEC. \\                                   
VEC\_TITLE  \> Defines the title plotted on a polarization vector map produced by VEC. \\    
WRCCOM  \> Writes a comment on the display device using cursor selection. \\                    
WRCOM  \> Writes a comment on the display device at user-defined positions. \\                  
WRITELUT  \> Writes a colour table (LUT) to device using numeric code of COL LUTs. \\           
\end{tabbing}

\hspace{2cm} {\bf Image Mathematics commands}
\begin{tabbing}
xxxxxxxxxxxxxxxxxxxx\=xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx\kill
Name \> Description \\
ADD  \> Adds two images. \\                                                                     
CMULT  \> Multiplies image by a constant. \\                                                    
CSTATS  \> Returns statistics in cursor selected area in image. \\                              
CSUB  \> Subtracts a constant from an image. \\                                                 
DIV  \> Divides two images. \\                                                                  
EXP10  \> Raises image to power 10. \\                                                          
EXPE  \> Raises image to power e. \\                                                            
EXPON  \> Raises image to arbitrary power. \\                                                   
HISTO  \> Calculates statistics on an image. \\                                                 
LOG10  \> Takes Log10 of an image. \\                                                           
LOGAR  \> Takes LogX of image where X is user-defined. \\                                       
LOGE  \> Takes LogE of image. \\                                                                
MULT  \> Multiplies two images together. \\                                                     
OADD  \> Adds two images referred to by observation number. \\                                  
OCADD  \> Adds a constant to an image referred to by observation number \\                      
OCDIV  \> Divides an image referred to by observation number by a constant. \\                  
OCMULT  \> Multiplies an image referred to by observation number by a  constant. \\             
OCSTATS  \> Statistics on sub-array of image referred to by observation number. \\              
OCSUB  \> Subtracts a constant to an image referred to by observation number \\                 
ODIV  \> Divides two images referred to by observation number. \\                               
OHISTO  \> Calculates statistics on an image referred to by observation number. \\              
OMULT  \> Multiplies two images referred to by observation number. \\                           
OSTATS  \> Calculates statistics on image referred to by observation number. \\                 
OSUB  \> Adds a constant to an image referred to by observation number \\                       
POW  \> raises image to arbitrary power. \\                                                     
ROOT  \> Takes the square root of an image. \\                                                  
STATS  \> Returns statistics on an image. \\                                                    
TRIG  \> Takes trig function of image cos(image) etc. \\                                        
\end{tabbing}

\hspace{2cm} {\bf Image Reduction commands}
\begin{tabbing}
xxxxxxxxxxxxxxxxxxxx\=xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx\kill
Name \> Description \\
ACCOFF  \> Calculates accurate offsets between mosaic tiles. \\                                 
AMCORR  \> Airmass corrects an image. \\                                                        
AMCORRLOT  \> Airmass corrects a sequence of images. \\                                         
APPLYMASK  \> Applies bad pixel mask to an image. \\                                            
APPLYMASKLOT  \> Applies bad pixel mask to sequence of images. \\                               
ARRAY\_TESTS  \> Reduces array test data. \\                                                    
AUTOMOS  \> Corrects mosaic tiles for DC offsets. \\                                            
CADD  \> Adds a constant to an image. \\                                                        
CDIV  \> Divides an image by a constant. \\                                                     
CHPIX  \> Changes a pixel value in an image. \\                                                 
CHRED  \> Reduces CHOP mode observations. \\                                                    
COFF  \> Calculates/stores accurate offsets between mosaic tiles.\\                             
COLMED  \> Median filters down image columns and creates 1D slice. \\                           
CREQUILT  \> Creates QUILT format mosaic file from image/offset lists.\\                        
CURHOT  \> Auto-removed hot pixels in cursor defined area of image. \\                          
DARKLOT  \> Dark subtracts a sequence of old format container file images. \\                   
DEFGRAD  \> Defines a gradient across image from edge-to-edge. \\                               
DEGLOT  \> Removes bad pixels from sequence of images. \\                                       
DISPICK  \> Extracts sub-image from image using cursor definition. \\                           
FCOADD  \> Sums a sequence of images. \\                                                        
FLAT2  \> Flat-fields two images, A with B and B with A. \\                                     
FLATLOT  \> Flat-fields a sequence of images. \\                                                
FLIP  \> Flips an image horizontally or vertically. \\                                          
GAUSS  \> Applies a gaussian filter to image. \\                                                
GAUSSTH  \> Applies a gaussian filter to pixels $>$ threshold. \\                               
GETOFF  \> Gets spatial offsets from RO data files of mosaic. \\                                
GLITCH  \> Removes glitches from image. \\                                                      
GLITCHMARK  \> Interactive bad pixel definition from image. \\                                  
HOTSHOT  \> Auto-removal of hot pixels in image. \\                                             
INDEX  \> Indexes through a old-style IRCAm container file. \\                                  
INSETB  \> Sets pixels inside box to user value. \\                                             
INSETC  \> Sets pixels inside circle to user value. \\                                          
INTLK  \> Creates an integer representation of sub-array of image. \\                           
IO2RO  \> Converts I/O (archival) files to RO files. \\                                         
JITREG  \> Calculates accurate mosaic offsets using request offsets as template. \\             
MAKEBAD  \> Makes a bad list from N-sigma cut on an image. \\                                   
MAKEGLITCH  \> Makes a bad pixel mask from glitch file (eg created by GLITCHMARK). \\           
MAKEMASK  \> Makes a bad pixel mask from glitch file (eg created by GLITCHMARK). \\             
MED3D  \> Median filters scaled image stack for flat-field creation. \\                         
MEDLOT  \> Calculates median in image and subtracts it for sequence of images. \\               
MOS2  \> Mosaics and displays 2 images with calculated spatial offsets. \\                      
MOSAIC  \> Mosaics N images in spatial mosaic. \\                                               
MOSAIC2  \> Mosaics 2 images with user-defined spatial offsets. \\                              
MOSCOR  \> Calculates DC offset between two images. \\                                          
NUMB  \> Informs user of number of pixels above user specified DN value in image. \\            
OBSEXT  \> Extracts a sequence of images from an old style IRCAM container file. \\             
OBSLIST  \> Lists items from an old style IRCAM container file. \\                              
OUTSETB  \> Sets values outside box to user-defined value. \\                                   
OUTSETC  \> Sets values outside circle to user-defined value. \\                                
PICKIM  \> Extracts sub-array with user-defined position,size from image. \\                    
PICKLOT  \> Same as PICKIM, but from sequence of images. \\                                     
PIXDUPE  \> Increases size of image by pixel duplication. \\                                    
POLCAL  \> Calculates polarization images from 4 polarization flux images. \\                   
POLLY  \> Calculates polarization values from 4 polarization flux values. \\                    
POLREG  \> Registers 4 polarization flux images to average position. \\                         
POLSHOT  \> Corrects polarization p image for shot-noise bias. \\                               
POLTHRESH  \> Thresholds 4 polarization images. \\                                              
QUILT  \> Mosaics tiles of mosaic together with specified spatial offsets. \\                   
REMOS  \> Re-mosaics a sequence of mosaic tile images using user-specified offset file. \\      
RFLOT  \> ... \\                                                                                
RODARKLOT  \> Dark subtracts a sequence of new format RO images. \\                             
ROINDEX  \> Give list of observation with parameters. \\                                        
ROMED  \> Median filters a stack sequence of images. \\                                         
ROTATE  \> Rotates an image by an arbitrary amount. \\                                          
ROTLOT  \> Rotates a sequence of images by an arbitrary amount. \\                              
ROWMED  \> Median filters along image rows. \\                                                  
SCALEDARK  \> Scales an old format container file dark by exposure time/coadd number. \\        
SCALELOT  \> Scales a sequence of images. \\                                                    
SETFILE  \> Defines input data file type (old or new format). \\                                
SETVAL  \> ... \\                                                                               
SHIFT  \> Shifts an image by ractional pixel amounts. \\                                        
SHIFT2  \> Shifts 2 images to average position. \\                                              
SHIFT3  \> Shifts 3 images to average position. \\                                              
SHSIZE  \> Shows size of an image in pixels. \\                                                 
SKYSUB4  \> Sky subtracts 4 (polarization) images using user-defined sky area. \\               
SPLITLOT  \> Creates N small images from a sequence of images into large images. \\             
SQORST  \> Changes image size by bi-linear interpolation. \\                                    
STCOADD  \> ... \\                                                                              
STRED  \> Reduces a mosaic sequence of images. \\                                               
SUB  \> Subtracts two images. \\                                                                
THETAFIX  \> Corrects polarization position angle to be 0-180 degrees.\\                        
THRESH  \> Thresholds an image both below and above user-defined values. \\                     
THRESH0  \> Thresholds an image below user-defined value to zero. \\                            
TOMAG  \> Converts a flux image to magnitude images using input zeropoint. \\                   
TRACE  \> Lists complete data file structure elements. \\                                       
TRANDAT  \> ASCII lists of offsets,fluxes to SDF image. \\                                      
TSLOT  \> Thresholds and scales a sequence of images. \\                                        
WMOSAIC  \> Produces a weighted mosaic from mosaic tile images. \\                              
WQUILT  \> Produces a weighted mosaic from mosaic tile images using ASCII file input. \\        
WRAPCOR  \> Corrects images for wraparound. \\                                                  
WRAPLOT  \> Corrects a sequence of images for wraparound. \\                                    
X2MAG  \> Defines the pixel scale when using the 2x magnifier. \\                               
X5MAG  \> Defines the pixel scale when using the 5x magnifier. \\                               
YADD  \> Averages an image along the Y-axis producing a linear image. \\                        
YGROW  \> Expands the linear image produced by YADD to a 2D image. \\                           
ZAPLIN  \> Removes bad rows and columns from an image by interpolation. \\                      
ZAPLOT  \> Removes bad rows and columns from a sequence of images. \\                           
\end{tabbing}

\hspace{2cm} {\bf On-line image reduction/display}
\begin{tabbing}
xxxxxxxxxxxxxxxxxxxx\=xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx\kill
Name \> Description \\
NOMAG  \> Informs system there is no external magnifier and plate scale is 0.286$''$/pixel. \\  
SEE  \> Interactive star selection then (KAPPA) PSF fitting for FWHM. \\                        
SETFILE  \> Defines input data file type (old or new format). \\                                
X2MAG  \> Defines the pixel scale when using the 2x magnifier. \\                               
X5MAG  \> Defines the pixel scale when using the 5x magnifier. \\                               
\end{tabbing}

\newpage
\section{Appendix C. ~~ WHIRCAM with Martini}
\label{Martini}

\begin{quote}
Martini-III is an interim adaptive optics imaging instrument developed by the 
University of Durham, which uses WHIRCAM as the IR detector.  For more 
information than is provided here, contact Peter Doel (A.P.Doel@durham.ac.uk) 
or Richard Myers (R.M.Myers@durham.ac.uk) at Durham, or Vik Dhillon
(vsd@ing.iac.es) at La Palma.
\end{quote}

\subsection*{Overview}
In order to sample the high resolution images delivered by the Martini
Adaptive Optics system, a reflective 
f-converter can be inserted upstream of the telescope focal plane to 
produce image scales of 0.08 or 0.05 \arcsec/pixel in WHIRCAM. The 
f-converter consists of two 25 mm diameter gold-coated mirrors (M1 and
M2, see Figure~\ref{fig9_mart-setup}) which are 
used off-axis to convert the f/11 beam to f/33 or f/55 before entering the
WHIRCAM cryostat. Cold stops matched to the size of the telescope pupil 
image formed inside the cryostat are installed in the rear filter wheel and 
are automatically rotated into position when the f-converter is used to limit 
the background emission, by choosing the relevant magnifier option in the
CONFIG file. The FWHM diffraction limit of the WHT at 2.2 $\mu$m is 
0.13\arcsec, and the 0.05 arcsec/pixel scale is designed to sample the
diffraction-limited core of well-corrected K-band images. The instrument
field of view in this mode is 13$\times$13\arcsec\ at 0.05 \arcsec/pixel.
(Due to space contraints, the f-converter can't be used in direct
imaging mode.)
\begin{figure}[h]
\psfig{figure=fig9_mart-setup.eps,height=10cm}
\caption{Martini and WHIRCAM setup at GHRIL (courtesy of Peter Doel).}
\label{fig9_mart-setup}
\end{figure}  

\subsection*{Imaging with Martini}

In Martini a 6-segment adaptive mirror is placed downstream of the telescope
focus at a conjugate of the turbulent layer. An off-axis toroid mirror
reimages the telescope focal plane further down the 
GHRIL table. A dichroic placed about 300 mm upstream of the reimaged 
Martini focus diverts the infrared light to WHIRCAM  via the f-converter. 
The visible light is transmitted to the CCD wavefront sensor where the
corrections to be applied to the adaptive mirror segments are measured. 
The converging f/11 beam reflected by the dichroic falls on a convex mirror 
(M1: 100 mm radius of curvature) mounted 50 mm upstream of the reimaged focus 
and tilted at 5$^\circ$ to the axis. This mirror collimates the beam and 
reflects it onto a concave mirror (M2: 500 mm radius of curvature) which is 
mounted 200 mm from M1 and tilted so that it sends the beam to WHIRCAM 
parallel with the beam from the dichroic. The concave mirror converts the 
beam to f/55 and forms a focus 250 mm from its front surface, which is in 
the same plane as the reimaged focus from Martini but translated across 
by 25 mm.  

The 100 mm r$_c$ convex mirror gives an image scale on WHIRCAM 
of 0.05 \arcsec/pixel.  It can be substituted by a 160 mm r$_c$ mirror (M1a) 
placed 175 mm from the dichroic to give an image scale of 0.08 \arcsec/pixel. 
The pupil images formed inside the cryostat by these f-converters have 
diameters of 3.3 mm and 5.2 mm respectively, and for maximum sensitivity, these
should be matched by cold stops. The rear filter wheel currently contains 
stops with diameters of 7, 5 and 3 mm which can be rotated into position just 
ahead of the fixed cold stop. The stops do not lie precisely at the position 
of the pupil images and it has not yet been possible to evaluate which stops 
give the best performance. Furthermore, the small pupil image sizes make the 
alignment of the instrument very critical and it is probably wise to use
oversized stops until the alignment accuracy has been assessed. 

The concave f-converter mirror can be aligned to the optical axis of WHIRCAM 
by positioning the mirror 250 mm in front of the WHIRCAM focal plane (which is
125mm from the front of the snout) and running movie mode after selecting the nbL 
filter with one of the small stops (say 5 mm for the 0.05 \arcsec/pixel option). 
The mirror can then be tipped so that it reflects back into the cryostat 
and adjusted so that it is centred by altering its height (which should be 
very close to 150 mm above the GHRIL table) and translation so that the 
signal is minimised. When it is aligned, out-of-focus images of 
the corners of the mirror may be faintly visible. 

The Martini beam from the dichroic can be aligned using the Martini laser beam 
injected into the telescope focal plane. The beam from the dichroic is centred 
onto M1 by tipping and tilting the dichroic with the micrometer adjusters. 
From M1, the beam is directed to the centre of M2 by tilting the 
M1 kinematic mirror mount with hex wrenches. Finally, the beam from M2 is 
aligned with the WHIRCAM optical axis by pointing it at the dimple in the
centre of the cryostat window cover; this is achieved by tilting M2 
with the hex wrench adjusters. 

The mirrors are glued into holders which are held in kinematic mirror mounts 
supported on posts and bases (Thorlabs). 
The f-converter mirrors were supplied by Technical Optics (Isle of Man).  
Their surface accuracy is $\lambda /10$ and they are coated with a protected 
gold coating. 

\subsection*{Performance} 

Although the off-axis mirrors introduce significant 
aberrations, the images are still diffraction-limited at 2 $\mu$m across the
entire 12\arcsec\ field at 0.05 \arcsec/pixel. The aberrations are more 
significant with the 0.08 \arcsec/pixel image scale particularly in the J band,
but as a diffraction-limited image cannot be fully sampled with this pixel 
scale, the images are completely adequate.  Encircled energy plots are 
shown in Figure~\ref{fig10_mart-energy}. 
\begin{figure}
\psfig{figure=fig10_mart-energy.eps,height=23cm}
\caption{Encircled Energy diagrams for Martini}
\label{fig10_mart-energy}
\end{figure}  


\newpage
\section{Appendix D. ~~ UKIRT Standards}

\subsection*{Faint Standards}
\vspace{0.5cm}

Standards are on the UKIRT system as defined by the UKIRT bright
standards. 1 sigma errors are shown in parentheses. 

\begin{tabular}{lrrrrrll}
Name & \multicolumn{2}{c}{   RA (1950)     Dec} & \multicolumn{1}{c}{\sl K} 
& \multicolumn{1}{c}{\sl J--K} & \multicolumn{1}{c}{\sl H--K} & 
Other Name  & Ref \\
\\[-0.5mm]
FS 1  &  00 31 22.7 & $-$12 24 29 & 12.967 (0.021) &  0.462 (0.011) &  0.081 (0.012) & G158-100 & 2 \\[-0.5mm]
FS 2  &  00 52 36.0 &  00 26 58 & 10.466 (0.003) &  0.247 (0.003) &  0.038 (0.003) & SA92-342 & 1 \\[-0.5mm]
FS 3  &  01 01 46.6 &  03 57 34 & 12.822 (0.007) & $-$0.222 (0.011) & $-$0.097 (0.007) & F11      & 1,2 \\[-0.5mm]
FS 4  &  01 52 03.7 &  00 28 20 & 10.264 (0.005) &  0.292 (0.003) &  0.040 (0.007) & SA93-317 & 1 \\[-0.5mm]
FS 5  &  01 52 04.7 & $-$07 00 47 & 12.342 (0.006) & $-$0.007 (0.004) & $-$0.002 (0.004) & F16      & 1,2 \\[-0.5mm]
\\[-0.5mm]
FS 6  &  02 27 39.2 &  05 02 34 & 13.374 (0.015) & $-$0.135 (0.014) & $-$0.069 (0.012) & F22      & 1,2 \\[-0.5mm]
FS 7  &  02 54 47.2 &  00 06 39 & 10.940 (0.005) &  0.165 (0.012) &  0.037 (0.010) & SA94-242 & 1 \\[-0.5mm]
FS 8  &  02 55 12.9 &  00 04 04 &  8.313 (0.006) &  0.766 (0.002) &  0.129 (0.004) & SA94-251 & 1 \\[-0.5mm]
FS 9  &  02 55 38.8 &  00 58 54 &  8.266 (0.006) &  0.884 (0.003) &  0.158 (0.005) & SA94-702 & 1 \\[-0.5mm]
FS 10 &  03 46 17.4 & $-$01 07 38 & 14.919 (0.072) & $-$0.170 (0.077) & $-$0.049 (0.060) & GD50     & 2 \\[-0.5mm]
\\[-0.5mm]
FS 11 &  04 50 25.4 & $-$00 19 34 & 11.278 (0.018) &  0.076 (0.025) &  0.016 (0.019) & SA96-83  & 1 \\[-0.5mm]
FS 12 &  05 49 34.8 &  15 52 37 & 13.898 (0.003) & $-$0.217 (0.014) & $-$0.091 (0.018) & GD71     & 1 \\[-0.5mm]
FS 13 &  05 54 33.8 &  00 00 53 & 10.135 (0.003) &  0.382 (0.002) &  0.047 (0.005) & SA97-249 &  1 \\[-0.5mm]
FS 14 &  07 21 41.2 & $-$00 27 10 & 14.261 (0.012) & $-$0.153 (0.005) & $-$0.079 (0.020) & Rubin 149 & 2 \\[-0.5mm]
FS 15 &  08 48 21.9 &  11 55 02 & 12.360 (0.021) &  0.418 (0.008) &  0.060 (0.007) & M67-I-48 &  3 \\[-0.5mm]
\\[-0.5mm]
FS 16 &  08 48 31.0 &  12 00 36 & 12.631 (0.008) &  0.340 (0.006) &  0.038 (0.005) & M67-IV-8 &  3 \\[-0.5mm]
FS 17 &  08 48 35.4 &  12 03 26 & 12.270 (0.007) &  0.411 (0.007) &  0.073 (0.003) & M67-IV-27 & 3 \\[-0.5mm]
FS 18 &  08 51 02.1 & $-$00 25 14 & 10.522 (0.008) &  0.292 (0.003) &  0.031 (0.003) & SA100-280 & 1 \\[-0.5mm]
FS 19 &  10 31 14.5 & $-$11 26 08 & 13.796 (0.025) & $-$0.231 (0.021) & $-$0.142 (0.047) & G162-66  &  1,2 \\[-0.5mm]
FS 20 &  11 05 27.6 & $-$04 53 04 & 13.473 (0.017) & $-$0.120 (0.015) & $-$0.069 (0.012) & G163-50  &  1,2 \\[-0.5mm]
\\[-0.5mm]
FS 21 &  11 34 27.6 &  30 04 35 & 13.132 (0.004) & $-$0.184 (0.033) & $-$0.101 (0.037) & GD140    &  4 \\[-0.5mm]
FS 33 &  12 54 35.1 &  22 18 08 & 14.240 (0.016) & $-$0.223 (0.010) & $-$0.078 (0.024) & GD153    &  4 \\[-0.5mm]
FS 23 &  13 39 25.7 &  28 44 59 & 12.374 (0.000) &  0.623 (0.004) &  0.072 (0.018) & M3-193    &  4 \\[-0.5mm]
FS 24 &  14 37 33.3 &  00 14 36 & 10.753 (0.008) &  0.151 (0.006) &  0.019 (0.004) & SA106-1024 & 1 \\[-0.5mm]
FS 25 &  15 35 59.9 &  00 24 03 &  9.756 (0.017) &  0.475 (0.003) &  0.070 (0.005) & SA107-1006 & 1 \\[-0.5mm]
\\[-0.5mm]
FS 26 &  16 34 26.3 & $-$00 28 39 &  7.972 (0.009) &  0.858 (0.004) &  0.155 (0.006) & SA108-475  & 1 \\[-0.5mm]
FS 27 &  16 38 54.2 &  36 26 56 & 13.123 (0.018) &  0.371 (0.013) &  0.058 (0.014) & M13-A14    & 4 \\[-0.5mm]
FS 28 &  17 41 32.5 & $-$00 23 44 & 10.597 (0.016) &  0.148 (0.010) &  0.047 (0.005) & SA109-71   & 1 \\[-0.5mm]
FS 35 &  18 24 44.5 &  04 01 17 & 11.757 (0.017) &  0.474 (0.008) &  0.089 (0.005) & G21-15     & 2 \\[-0.5mm]
FS 34 &  20 39 41.9 & $-$20 15 21 & 12.989 (0.011) & $-$0.170 (0.008) & $-$0.070 (0.009) & EG141      & 4 \\[-0.5mm]
\\[-0.5mm]
FS 29 &  21 49 53.0 &  02 09 16 & 13.346 (0.024) & $-$0.171 (0.011) & $-$0.075 (0.012) & G93-48     & 1,2 \\[-0.5mm]
FS 30 &  22 39 11.3 &  00 56 55 & 12.015 (0.020) & $-$0.092 (0.013) & $-$0.036 (0.005) & SA114-750  & 1 \\[-0.5mm]
FS 31 &  23 09 50.4 &  10 30 46 & 14.039 (0.010) & $-$0.241 (0.02 ) & $-$0.120 (0.017) & GD246      & 1,2 \\[-0.5mm]
FS 32 &  23 13 38.2 & $-$02 06 58 & 13.664 (0.012) & $-$0.205 (0.011) & $-$0.088 (0.015) & F108     & 1,2 \\[-0.5mm]
\\[-0.5mm]
     & \multicolumn{4}{l}{1. Landolt  1983  A.J. 88,439} \\[-0.5mm]
     & \multicolumn{4}{l}{2. Turnshek et al 1990  A.J. 99,1243} \\[-0.5mm]
     & \multicolumn{4}{l}{3. Eggen and Sandage  Ap.J. 140,130} \\[-0.5mm]
     & \multicolumn{4}{l}{4. Priv. Comm.} \\[-0.5mm]
\end{tabular}

\newpage
\subsection*{Bright Standards}
\vspace{0.5cm}
  The magnitudes in this list have been revised following 1990/91 UKT9
  photometry. Asterisks refer to the most frequently re-observed stars. 
  The results define the UKIRT/UKT9 natural photometric system. The K 
  zeropoint is defined as identical to that of the CIT (Elias) system for 
  A0 stars. Transformations to CIT are also given. 

\begin{tabular}{cllrrrrrrr}
\multicolumn{2}{c}{Name} & \multicolumn{1}{c}{Sp} & \multicolumn{2}{c}{   RA (1950)     Dec} & 
\multicolumn{1}{c}{\sl J} & \multicolumn{1}{c}{\sl H} & 
\multicolumn{1}{c}{\sl K} & \multicolumn{1}{c}{\sl L} &
\multicolumn{1}{c}{\sl L'} \\
\\[-0.5mm]
* & HD 225023 & A0     &  0 00 11.8  &  35 32 14.0  &  7.082 & 6.993 & 6.962 &  6.94 &  6.96  \\
* & G158-27   & M5     &  0 04 12.0  &  -7 47 54.0  &  8.378 & 7.781 & 7.447 &       &  7.04   \\   
* & BS 33     & F7V    &  0 08 43.2  & -15 44 32.0  &  3.964 & 3.689 & 3.636 &  3.60 &  3.60   \\   
* & HD 1160   & A0     &  0 13 23.1  &   3 58 24.0  &  7.060 & 7.051 & 7.040 &  7.05 &  7.04   \\   
  & HD 2811   & A2     &  0 28 53.0  & -43 52 58.0  &  7.178 & 7.093 & 7.067 &  7.04 &         \\   
  & HD 3029   & A3     &  0 31 02.3  &  20 09 30.0  &  7.263 & 7.125 & 7.093 &       &  7.06  \\    
\\[-0.5mm]
  & BS 337    & M0III  &  1 06 55.5  &  35 21 22.0  & -0.908 & -1.703 & -1.853 & -2.00 & -1.98 \\
  & BS 696    & B2Iae  &  2 21 43.1  &  56 23 04.0  &  5.587 & 5.499 & 5.443 &  5.37 &  5.33  \\
* & BS 718    & B9III  &  2 25 29.8  &   8 14 13.0  &  4.374 & 4.390 & 4.390 &  4.40 &  4.41  \\
  & BS 739    & gG3    &  2 29 36.6  &  -1 15 17.0  &  3.748 & 3.218 & 3.121 &       &  3.04  \\    
  & BS 740    & F4IV   &  2 29 43.0  & -15 27 48.0  &  3.879 & 3.623 & 3.585 &  3.56 &  3.56   \\   
* & GL 105.5  & M0     &  2 38 07.6  &   0 58 57.0  &  7.305 & 6.663 & 6.539 &  6.47 &  6.46  \\    
\\[-0.5mm]
  & BS 816    & gF0    &  2 42 43.4  &   4 30 08.0  &  5.502 & 5.384 & 5.353  &      &  5.38   \\   
  & HD 18881  & A0     &  3 00 20.5  &  38 12 53.0  &  7.130 & 7.135 & 7.140 &  7.15 &  7.14  \\
  & HD 19904  & A2     &  3 08 49.1  & -39 14 24.0  &  6.727 & 6.662 & 6.642 &  6.62 &         \\   
  & G77-31    & M4?    &  3 10 40.5  &   4 35 12.0  &  8.816 & 8.187 & 7.857 &  7.52 &         \\   
* & HD 22686  & A0     &  3 36 18.7  &   2 36 07.0  &  7.196 & 7.190 & 7.185 &  7.20 &  7.19   \\   
  & BS 1140   & B7IV   &  3 41 49.5  &  24 08 01.0  &  5.520 & 5.500 & 5.510 &  5.60 &  5.64  \\
\\[-0.5mm]
  & BS 1457   & K5III  &  4 33 02.9  &  16 24 37.0  & -1.848 & -2.614 & -2.783 & -2.97 & -2.89 \\
  & BS 1543   & F6V    &  4 47 07.4  &   6 52 32.0  &  2.353 & 2.117 & 2.095 &       &  2.07   \\   
  & BS 1552   & B2III  &  4 48 32.4  &   5 31 16.0  &  4.029 & 4.087 & 4.138 &  4.18 &  4.18  \\
  & BS 1641   & B7V    &  5 03 00.2  &  41 10 08.0  &  3.518 & 3.646 & 3.677 &  3.71 &  3.74  \\
  & BS 1637   & F0V    &  5 06 40.6  &  51 35 52.0  &  4.312 & 4.204 & 4.153 &  4.11 &  4.14  \\
  & BS 1713   & B8Iae  &  5 12 08.0  &  -8 15 29.0  &  0.240 & 0.241 & 0.211 &  0.13 &  0.09  \\
\\[-0.5mm]
  & BS 1708  &  G4III  &  5 12 59.5  &  45 56 58.0  & -1.334 & -1.717 & -1.802 & -1.87 & -1.85 \\
  & SAO112626 & F8     &  5 16 41.4  &   1 39 15.0  &  8.934 & 8.670 & 8.596 &       &  8.65    \\  
  & BS 1869   & dF0    &  5 36 15.9  &  47 42 56.0  &  5.532 & 5.454 & 5.393 &  5.36 &  5.39  \\
  & HD 38921  & A0     &  5 45 41.0  & -38 14 51.0  &  7.572 & 7.551 & 7.536 &  7.53 &         \\   
* & HD 40335  & A0     &  5 55 37.6  &   1 51 09.0  &  6.555 & 6.473 & 6.452 &  6.43 &  6.43  \\
  & BS 2228   & F0V    &  6 17 34.6  &  46 25 57.0  &  6.012 & 5.943 & 5.892 &  5.84 &  5.88  \\
\\[-0.5mm]
* & HD 44612  & A0     &  6 21 09.7  &  43 34 35.0 &   7.075 & 7.041 & 7.041 &  7.04 &  7.03   \\   
  & BS 2491   & A1V    &  6 42 56.7  & -16 38 46.0 &  -1.300 & -1.319 & -1.320 & -1.35 & -1.36 \\
* & BD+0 1694 & ?      &  6 52 07.3  &   0 00 52.0 &   5.750 & 4.857 & 4.606 &  4.43 &  4.43    \\  
  & BS 2721   & G0V    &  7 12 07.6  &  47 19 51.0 &   4.475 & 4.180 & 4.126 &       &  4.08    \\  
  & BS 2943   & F5IV   &  7 36 41.1  &   5 21 16.0 &  -0.437 & -0.564 & -0.646 & -0.66 &       \\
  & BS 2990   & K0IIIb &  7 42 15.6  &  28 08 55.0 &  -0.523 & -0.975 & -1.050 & -1.15 & -1.17 \\
\end{tabular}

\newpage
\centerline{{\bf Bright Standards} (continued)}
\vspace{0.5cm}

\begin{tabular}{cllrrrrrrr}
\multicolumn{2}{c}{Name} & \multicolumn{1}{c}{Sp} & \multicolumn{2}{c}{   RA (1950)     Dec} & 
\multicolumn{1}{c}{\sl J} & \multicolumn{1}{c}{\sl H} & 
\multicolumn{1}{c}{\sl K} & \multicolumn{1}{c}{\sl L} &
\multicolumn{1}{c}{\sl L'} \\
\\[-0.5mm]
  & BS 3314   & A0V    &  8 23 09.7  &  -3 44 31.0 &   3.920 & 3.919 & 3.940 &  3.94 &  3.92  \\    
  & HD 75223  & A0     &  8 45 29.8  & -39 36 54.0 &   7.329 & 7.296 & 7.281 &  7.26 &        \\    
* & HD 77281  & A2     &  8 59 05.4  &  -1 16 45.0 &   7.111 & 7.052 & 7.031 &  7.00 &  7.06  \\
* & GL 347A   & M3.5   &  9 26 25.0  &  -7 08 30.0 &   8.483 & 7.881 & 7.658 &  7.41 &  7.36  \\    
* & HD 84800  & A2     &  9 45 35.9  &  43 53 56.0 &   7.592 & 7.549 & 7.538 &  7.55 &  7.54  \\
  & BS 3888   & F2IV   &  9 47 27.1  &  59 16 30.0 &   3.162 & 3.005 & 2.983 &  2.98 &  2.94  \\
\\[-0.5mm]
  & BS 3903   & G7III  &  9 49 04.3  & -14 36 40.0 &   2.617 & 2.136 & 2.050 &  1.98 &         \\   
  & V 569     & M3     & 10 09 46.3  &  -3 29 41.0 &   5.992 & 5.310 & 5.106 &  4.93 &  4.89   \\   
  & BS 4069   & M0III  & 10 19 21.5  &  41 45 06.0 &   0.132 & -0.654 & -0.803 & -0.94 & -0.96 \\
  & GL 390    & M1.5   & 10 22 44.0  &  -9 58 36.0 &   6.939 & 6.275 & 6.061 &  5.87 &         \\   
  & GL 406    & M6     & 10 54 06.0  &   7 19 12.0 &   7.143 & 6.469 & 6.099 &  5.69 &        \\    
  & BS 4358   & K3III  & 11 11 25.9  &   8 20 05.0 &   3.879 & 3.299 & 3.202 &       &  3.14  \\    
\\[-0.5mm]
  & HD101452  & A2     & 11 37 45.1  & -38 52 09.0  &  7.018 & 6.890 & 6.848 &  6.81 &        \\    
  & Y 2730    & dM4.5  & 11 45 08.2  &   1 05 56.0  &  6.532 & 5.935 & 5.646 &  5.34 &  5.26  \\   
  & BS 4550   & G8V    & 11 50 06.2  &  38 04 39.0 &   4.957 & 4.466 & 4.400 &  4.35 &  4.38  \\
  & HD105601  & A2     & 12 06 56.1  &  38 54 39.0 &   6.821 & 6.719 & 6.687  & 6.64  & 6.65  \\
* & HD106965  & A2     & 12 15 24.0   &  1 51 10.0 &   7.380 & 7.337 & 7.316  & 7.30  & 7.34  \\
* & BS 4689   & A2IV   & 12 17 20.8  &   0 23 21.0 &   3.810 & 3.781 3& .781  & 3.79  & 3.79  \\
\\[-0.5mm]
  & BS 4935   & F7V    & 13 01 05.1  & -20 18 55.0 &   4.604 & 4.290 & 4.266  &       &       \\  
  & BS 4983   & G0V    & 13 09 32.5  &  28 07 52.0 &   3.194 & 2.929 & 2.886  & 2.88  & 2.89  \\
  & BS 5340   & K1IIb  & 14 13 22.8  &  19 26 31.0 &  -2.200 & -2.878 & -2.976 & -3.09 & -3.05 \\
* & BS 5447   & F2V    & 14 32 30.2  &  29 57 41.0 &   3.723 & 3.522 & 3.489  & 3.48  & 3.49  \\
  & HD129653  & A2     & 14 40 38.2  &  36 58 07.0 &   6.985 & 6.942 & 6.921  & 6.91  & 6.93  \\
* & HD129655  & A2     & 14 41 11.0  &  -2 17 38.0 &   6.826 & 6.724 & 6.692  & 6.67  & 6.68  \\    
\\[-0.5mm]
  & HD130163  & A0     & 14 44 36.2  & -39 43 04.0 &   6.856 & 6.846 & 6.835  & 6.81  &       \\    
  & BD+3 2954 & M0     & 14 52 23.2  &   3 11 33.0 &   5.926 & 5.026 & 4.825  & 4.64  &       \\     
  & BS 5685   & B8V    & 15 14 18.7  &  -9 11 59.0 &   2.759 & 2.789 & 2.799  &       & 2.85  \\
* & HD136754  & A0     & 15 19 24.3  &  24 31 19.0 &   7.155 & 7.146 & 7.135  & 7.14  & 7.14  \\    
* & BD+2 2957 & K2     & 15 22 29.0  &   1 41 06.0 &   5.280 & 4.454 & 4.263  & 4.08  & 4.19  \\    
  & BS 6084 & B2II+O9V & 16 18 08.7  & -25 28 29.0 &   2.491 & 2.442 & 2.421  & 2.43  & 2.42  \\
\\[-0.5mm]
* & BS 6092   & A9III  & 16 18 14.1  &  46 25 54.0 &   4.192 & 4.257 & 4.298  &       & 4.35  \\
  & S-R 3     & ?      & 16 23 07.7  & -24 27 26.0 &   7.804 & 7.001 & 6.543  & 6.25  &       \\    
  & OPH S1    & ?      & 16 23 32.8  & -24 16 44.0 &   9.007 & 7.344 & 6.378  & 5.71  &       \\    
  & BS 6136   & K4III  & 16 26 00.9  &   0 46 32.0 &   2.898 & 2.184 & 2.036  & 1.86  &       \\    
  & BS 6147   & G8IIIa & 16 28 16.4  & -16 30 19.0 &   2.767 & 2.334 & 2.269  & 2.19  & 2.22  \\
  & BS 6406   & M5Ib   & 17 12 22.0  &  14 26 45.0 &  -2.276 & -3.110 & -3.351 & -3.70 & -3.66 \\
\end{tabular}

\newpage
\centerline{{\bf Bright Standards} (continued)}
\vspace{0.5cm}

\begin{tabular}{cllrrrrrrr}
\multicolumn{2}{c}{Name} & \multicolumn{1}{c}{Sp} & \multicolumn{2}{c}{   RA (1950)     Dec} & 
\multicolumn{1}{c}{\sl J} & \multicolumn{1}{c}{\sl H} & 
\multicolumn{1}{c}{\sl K} & \multicolumn{1}{c}{\sl L} &
\multicolumn{1}{c}{\sl L'} \\
\\[-0.5mm]
  & HD161743  & A0     & 17 45 31.8  & -38 06 11.0 &   7.620 & 7.620 & 7.615  & 7.61  &       \\    
* & HD161903  & A2     & 17 45 43.3  &  -1 47 34.0 &   7.172 & 7.059 & 7.023  & 6.99  & 7.01  \\
* & HD162208  & A0     & 17 46 20.7  &  39 59 40.0 &   7.223 & 7.141 & 7.112  & 7.09  & 7.14  \\
  & BS 6707   & F2II   & 17 56 35.3  &  30 11 32.0 &   3.470 & 3.252 & 3.210  & 3.16  & 3.18  \\
* & Y 4338    & dM4.5e & 18 46 44.1  & -23 53 32.0 &   6.297 & 5.680 & 5.416  & 5.12  & 5.03  \\    
  & BS 7120   & K3II  &  18 52 05.8  & -22 44 08.0 &   2.739 & 2.120 & 2.033  & 1.91  &       \\    
\\[-0.5mm]
* & GL 748    & dM4   &  19 09 38.0  &   2 48 36.0 &   7.105 & 6.557 & 6.319  & 6.05  & 6.00  \\    
  & BS 7615   & K0III &  19 54 25.7  &  34 56 58.0 &   2.199 & 1.716 & 1.640  & 1.51  & 1.56  \\
* & BS 7773   & B9.5V &  20 17 53.5  & -12 55 04.0 &   4.825 & 4.859 & 4.859  & 4.86  & 4.86  \\    
* & GL 811.1  & dM4   &  20 54 04.0  & -10 37 36.0 &   7.832 & 7.185 & 6.946  & 6.70  & 6.69  \\
* & HD201941  & A2    &  21 10 13.6 &    2 26 12.0 &   6.696 & 6.657 & 6.626  & 6.60  & 6.61  \\    
  & BS 8143   & B9Iab &  21 15 27.0  &  39 11 04.0 &   3.886 & 3.838 & 3.797  & 3.73  & 3.73  \\
* & HD203856  & A0    &  21 21 37.1  &  39 48 12.0 &   6.926 & 6.887 & 6.861  & 6.84  & 6.84  \\    
\\[-0.5mm]
  & HD205772  & A3    &  21 35 33.6  & -41 16 26.0 &   7.775 & 7.688 & 7.657  & 7.64  &        \\   
  & SAO34401  & F0    &  22 21 47.7  &  54 57 12.0 &   7.933 & 7.766 & 7.734  &       & 7.74  \\    
* & BS 8541   & B9Iab &  22 22 29.0  &  49 13 21.0 &   4.305 & 4.267 & 4.235  & 4.23  & 4.22  \\
  & BS 8551   & K0III &  22 25 19.6  &   4 26 39.0 &   2.956 & 2.378 & 2.312  & 2.25  & 2.24  \\
* & Y 5546    & dM5   &  22 50 36.2  & -14 31 34.0 &   5.980 & 5.344 & 5.066  & 4.80  & 4.74  \\    
\\[-0.5mm]
\end{tabular}


\end{document}