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\begin{center}
\vspace{60mm}
{\LARGE \bf INTEGRAL \bf{USERS} \bf{MANUAL}}\\ 
\vspace{80mm}
Version 1.1 (January 1998)\\
\vspace{30mm}
S.Arribas, C. del Burgo, D. Carter, L. Cavaller, R. Edwards, J.
Fuentes, A. Garc\'\i a, B. Gentles, J.M., Herreros, L. Jones, E.
Mediavilla, M. Pi, D. Pollacco, P. Rees, N. Sosa\\ \vspace{30mm}
{\LARGE \bf IAC-RGO-ING }\\ 

\end{center}
\newpage

\tableofcontents  

\section{INTRODUCTION}

The {\sc wyffos} spectrograph was originally conceived to allow
science exploitation of light carried by fibres from the {\sc
autofib2} prime-focus robotic positioner. However, it quickly became
apparent that other fibre fed instruments could take advantage of the
spectrograph's optimized geometry. {\sc integral} extends the power of
{\sc wyffos} to an increasingly important observational technique --
that of area (integral) spectroscopy of extended objects.

{\sc integral} is mounted at the GHRIL Nasmyth platform, where in
addition to the fibre bundles themselves, new acquisition, guiding,
and calibration units have been developed. Furthermore,
new/experimental bundles can easily be installed once the focal plane
and {\sc wyffos} mechanical interfaces have been constructed.  The
acquisition, guiding, and calibration units of {\sc integral} can also
be used with other fibre fed spectrographs ({\it i.e.}, IR spectrographs).


\begin{figure}
\psfig{figure=outline.ps} 
\caption{Outline of the {\sc integral} system}
\end{figure}

\section{DESCRIPTION}

\subsection{General Description}

{\sc integral} is mounted in the Nasmyth No. 1 platform (GHRIL) of the
WHT. The general layout of the system is shown in Figure 1 and a more
detailed description of the focal plane area is shown in Figure 2.

A cylindrical structure (Acquisition, Guiding, and Calibration box
structure) is bolted to the Nasmyth mechanical rotator.  As this
structure rotates synchronously with the focal plane when the
telescope tracks, the sky position angle is fixed during an
observation.

The Swing Plate (SP) is located in the telescope focal plane area, and
this is the connection point for the acquisition and scientific fibre
bundles.  By rotating the SP any installed bundle can be placed at the
centre of the focal plane, while the other bundles are light
blocked. Hence, only one bundle at any one time can feed the
spectrograph.


For acquisition a coherent fibre bundle transmits the light from the focal
plane (via the SP) to a standard TV camera.


\begin{figure}
\psfig{figure=focalplane.ps} 
\caption{Focal plane area}
\end{figure}


Up to six scientific bundles can be simultaneously mounted in the SP,
although in the standard configuration only three are used (called sb1, sb2,
and sb3). These bundles are 5.5\,m long, while their fibre core
diameter (in sky units) is: 0.45 (sb1), 0.9 (sb2), and 2.7 (sb3)
arcsec respectively. The bundles are simultaneously connected at the
entrance ({\it pseudo-slit}) of the {\sc wyffos} spectrograph. They
can be interchanged very easily, with an overhead of a few
seconds.  Hence, depending on the prevailing seeing conditions the
instrument can be easily optimized for the scientific program.

Guide stars may be acquired by moving an XY slide containing two coherent
fibre bundles. This unit moves in an off-axis region and the bundles feed
a TV based autoguider.

A liquid fiber is used to feed a calibration source (currently
Copper-Argon, Copper-Neon, or Tungsten lamps) to the focal plane.


\subsection{Acquisition System}

A schematic representation of the acquisition unit is shown in Figure 3.
 
A coherent fibre bundle transports light from the focal plane
(via the SP) to a standard TV camera. Figure 4 indicates where this
bundle is connected into the SP. It has a field of view of 22.5
$\times$ 30.2 arcsec $^2$ in the telescope focal plane.

\begin{figure}
\psfig{figure=acquisition.ps} 
\caption{Acquisition system. The focussing mechanism is at bottom-left
of the main unit}
\end{figure}

The acquisition system is equipped with a filter wheel which can
accommodate up to six filters. The filters must be circular and 25\,mm
in diameter.  In the standard configuration the following filters are
provided: CLEAR, BG38, GG495, OG530, and RG630.

A lens (with magnification 1:1.5) forms the image of the bundle output
over the chip of the TV camera.

The TV acquisition system consists of a Westinghouse ISEC TV camera
connected to the TV camera controller, a VME camera microprocessing system, 
a display monitor, and the control terminal. 



\begin{figure}
\psfig{figure=swingplate.ps,height=200mm,width=170mm} 
\caption{View of relevant regions/components at the telescope focal
plane area.  On the Swing Plate all possible bundle mount points are marked
along with those currently used (the standard positions for bundles 1,
2, and 3 -- code 3, 4, and 2 respectively). The acquisition
bundle location is also shown.  The rectangular shaded areas
illustrate the available region for guiding, which can be scanned by
the two coherent bundles. Numbers in the table indicate the coordinates
of the extremes of this region. The circular shaded area represents the
region which can be illuminated by the calibration lamp.  This
orientation corresponds to a view {\it from} the GHRIL table at Sky 
Position Angle (SPA) = 0 degrees. Therefore, North is Top.}
\end{figure}

\subsection{Guiding System}

The general layout of the Guiding system is shown in Figure 5.

A remotely driven XY slide simultaneously moves two coherent optical
fibre bundles over the focal plane (see also Figure 4). An area of
30$'^2$ (2 $\times$ 15$'^2$) is available for guiding purposes. Each
bundle has a field of view of 18$\times$18 arcsec $^2$ on
the focal plane.

\begin{figure}
\psfig{figure=guiding.ps} 
\caption{Guiding system}
\end{figure}

The Guiding unit is equipped with a filter wheel housing up to six
filters. The filters must be circular and 25\,mm in diameter.  In the
standard configuration the following filters are installed: CLEAR,
BG38, GG495, OG530, and RG630.

The two guiding bundles are focussed onto a standard CCD
autoguider head with thermoelectric cooler, through a prism and a lens
(magnification 1:1).


\subsection{Calibration Unit}

Figure 6 shows the general layout of the Calibration system.

The unit is equipped with a white and two arc lamps. The standard arc
lamps are CuAr and CuNe and manufactured by S.\& J. Juniper, with
references 4114QA and 4114QN, respectively. They can be switch on
simultaneously. The white lamp is a quartz-halogen tungsten lamp
supplied by Dolan-Jenner of the type DDL.
 
\begin{figure}
\psfig{figure=calibration.ps} 
\caption{The Calibration system}
\end{figure}

A liquid lightguide is used to illuminate a region of the focal plane, 
accessible to the scientific bundles by rotating the SP (see also Figure 4).

A set of coloured filters are available within {\sc wyffos} to suppress
strong arc lines.

A more detailed description may be found in INT-IAC-DDD-004.

 
\subsection{Observing Bundles}

The SP has six focal stations for science bundles (see Figure 4).
However, only three bundles are mounted in the standard configuration.
The different SP positions are described in Table 1.

\begin{table}[htpb*]
\caption{Swing Plate/Bundles Codes}
\begin{center}
\begin{tabular}{lcccc}
 & & & &\\
\hline\hline
code & bundle & Calibration/Observation & SP position&\\ 
 & & & &\\
\hline
01 & void & OBS & 5&\\	 
02 & void & CAL	& 6&\\
03 & sb2 & OBS	& 4&\\
04 & void & CAL	& 5&\\ 
05 & sb1 & OBS	& 3&\\ 
06 & sb2 & CAL	& 4&\\ 
07 & sb3 & OBS	& 2&\\
08 & sb1 & CAL & 3&\\
09 & void & OBS	& 1&\\
10 & sb3 & CAL & 2&\\
11 & void & OBS	& 6&\\
12 & void & CAL	& 1&\\
13 & ACQ  & OBS	&  &\\
 & & & &\\
\hline
\end{tabular}
\end{center}
\end{table}

These bundles were manufactured by the IAC, using Ceramoptec fibres.
The bundles sb1 and sb2 use `ultradry special' hydrogen
treated fibres.  Bundle sb3 uses Optram `UV' fibres.  Each is 5.5\,m
long. Their spectral response can be found in figures 7 and 8.


\begin{figure}[htpb*]
\psfig{figure=transmission12.ps,height=115mm,width=180mm} 
\caption{Transmission of the fibers (5.5m) used for sb1 and sb2, according to the 
fiber manufacturer}
\end{figure}


\begin{figure}[htpb*]
\psfig{figure=transmission3.ps,height=115mm,width=180mm} 
\caption{Transmission of the fibers (5.5m) used for sb3, according to the fiber 
manufacturer}
\end{figure}

At the focal plane the fibres are arranged in two groups, one forming
a rectangle, and the other a ring which is intended for collecting
background light (for small-sized objects). Table 2 and Figure 9 show
the main characteristics of each bundle.


\begin{table}[htpb*]
\caption{Characteristics of {\sc integral} fibre bundles}
\begin{center}
\begin{tabular}{lccccccc}
 & & & & & & &\\
\hline\hline
Bundle & 1 &   2  &  3  &  4 &  5 & 6 &\\ 
 & & & & & & &\\
sb1 &  0.45   & 0.7  &  205 (175+30)  &  7.80$\times$6.40 & variable&90&\\
sb2 &  0.90   & 1.4  &  219 (189+30)  &  16.0$\times$12.3 & 4.6 &90&\\
sb3 &  2.70   & 4.0  &  135 (115+20)  &  33.6$\times$29.4 & 7.4 &90&\\
 & & & & & & &\\
\hline
 & & & & & & &\\
\multicolumn{7}{l}{1 -- fibre core diameter (arcsec)} \\
\multicolumn{7}{l}{2 -- fibre image size on the detector (to be convolved 
with a 1.4-2.6 pixel PSF)} \\
\multicolumn{7}{l}{3 -- total number of fibres (rectangle + ring) } \\
\multicolumn{7}{l}{4 -- spatial coverage of the central rectangle 
(arcsec $\times$ arcsec)} \\
\multicolumn{7}{l}{5 -- distance between adjacent fibre/spectra at the CCD 
(in pixels)} \\
\multicolumn{7}{l}{6 -- diameter of the outer ring (arcsec)} \\

\end{tabular}
\end{center}
\end{table}

For each bundle the fibre correspondence between the focal plane and
slit position is given in Appendix 1.

\begin{figure}
\psfig{figure=bundles.eps} 
\caption{Configuration of the fibres of the standard bundles, 
at the focal plane end.}
\end{figure}


\section{PERFORMANCE}

\subsection{Throughput}

Figure 10 gives a first estimation of the performance of the whole
system (atmosphere + telescope + {\sc integral} + {\sc wyffos}). This
is based on data taken for the flux calibrator PG1708+602 (Massey et
al., ApJ, 328, 315) under average observing conditions. These results
were derived using the R1200B grating in $\sim$1.5 arcsec seeing.
Repeated observations lead to a realistic uncertainty of about
$\pm$0.5 mag. The background was removed by subtracting a sky
exposure of equal observing time. No significant differences were
found between the different bundles.

 
\begin{figure}
\vspace{10.5truecm} 
\special{psfile=throughtput.eps hscale=40. vscale=40.}
\caption{AB magnitude for obtaining 1 count/sec/\AA, with {\sc integral}}
\end{figure}

  

\subsection{Spectral Resolutions}

For any particular grating the spectral resolution depends on the fibre
bundle as a consequence of the different fibre sizes. Table 3 lists the
mean spectral resolution and linear dispersions for different gratings
and bundle (reflexion mode). Note that due to the variation of the {\sc
wyffos} focus over the CCD (which affects the FWHM) the spectral
resolution {\it also} changes over the CCD.

\begin{table}[htpb*]
\caption{Spectral Characteristics$^*$}
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\ \hline\hline & 2400 g/mm & 1200 g/mm & 600 g/mm & 316 &
300 &\\ & & & & & &\\ 
\hline 
Resolution (sb1) ($\AA$)& & 2.7 & 5.8 & 10.8 & 11. &\\ 
Resolution (sb2) ($\AA$)& & 3.1 & 6.7 & 12.5 & 13.2&\\ 
Resolution (sb3) ($\AA$)& & 6.2 & 13.5 & 25. & 26.5&\\ 
Linear dispersion ($\AA$/px)& & 1.4 & 3.07 & 5.7 & 6.&\\ 
Spectral Coverage ($\AA$)& & 1445 & 3140 & 5837 & 6144&\\ 
& & & & & &\\ 
\multicolumn{5}{l}{$^*$Derived from calibration data with a mean PSF
of 1.8 pixels, and $\lambda_c$=6000$\AA$} \\ 
\hline 
& & & & & &\\
\end{tabular}
\end{center}
\end{table}


\subsection{Stability}

i) Arc and Flat-Field Calibrations \\
In principle we expect the system to be stable over sustained
periods, and indeed test data obtained during the commissioning runs
show this to be {\it generally} the case. However, very occasionally
relatively large variations have been seen that defies explanation. While 
this problem remains under-investigation, `over-calibration' would seem a
wise procedure to adhere to (especially as the overheads in obtaining
calibration data are small).


ii) Swing Plate Mechanism\\
The SP mechanism is stable at the level of our uncertainties when
determining centroids ({\it i.e.}, less than 0.2 arcsec / 40 microns).


\section{SET UP PROCEDURES}

\subsection{Mechanical Installation}
Details on the mechanical installation of {\sc integral} can be found
in the document INT-IAC-PRC-003.

\subsection{Electronic Installation}
Details on the electronic installation of {\sc integral} can be found
in the document INT-IAC-DDD-009.

\subsection{Software Installation}
Details on the software installation of {\sc integral} can be found in
the document INT-IAC-STD-001.


\subsection{Focusing the Slit Assembly}

A detailed procedure for aligning the slit unit can be found in
document INT-IAC-PRC004. As the {\sc integral} slit unit is similar to
that of {\sc autofib2}, the slit focus procedure is identical for both
instruments.

Note, the {\sc wyffos} optical design results in some field curvature.
Hence it is not possible to obtain a similar focus for all parts of
the chip, therefore a compromise value for the focus must be
reached. Figure 11 shows an example of the de-focusing on the CCD
and its effect on the measured FWHM.

\begin{figure}
\vspace{23.truecm}
\hspace*{15.cm}
\special{psfile=focus1.ps hscale=55. vscale=55. angle=90. hoffset=0 voffset=350}
\special{psfile=focus2.ps hscale=55. vscale=55. angle=90. hoffset=-4 voffset=20}
\caption{Top: FWHM (in pixels) of arc lines over the CCD at the best focus
position.  Bottom: Best focus value (encoder units) over the CCD.
These were obtained with the bundle sb2 (200 micron fibres) and the
R1200B grating.}
\end{figure}

When the {\sc integral} slit assembly is in proper alignment within
{\sc wyffos} all science bundles have the same focus. Further details
may be found in INT-IAC-TRP-009.

\subsection{Focusing and Orientation of the Acquisition Bundle}
 
The end of the acquisition bundle in front of the TV camera should be
focussed, using the manual mechanism (see Figure 3). In principle
there are two procedures, both requiring the interaction of two
people: one at the GHRIL (moving the focus mechanism), and the other in
the control room watching the TV screen.

i) With the bundle connected to the to the SP, the inside of AG\&C box
is illuminated ({\it e.g.}, with a torch, a faint dome light, etc).
By inspecting the edges of the image bundle on the TV screen, the best
focus can be determined. If the focus remains unsatisfactory 
the following procedure must be used (as a last resort).

ii) The bundle is dismounted from the SP (see INT-IAC-PRC001), and
connected to a dedicated focusing system. This system allows
a test image ({\it e.g.}, a number) to be seen through the
bundle. 

Currently, a painted mark is used to fix the bundle orientation. 
However, we anticipate that before the instrument reaches
common user status the bundles will be doweled in the correct
positions.

In order to aid night-time acquisition the outline of the bundle
should be marked on the TV screen.

\subsection{Focusing and Orientation of the Guiding Bundle}

The end of the guiding bundle in front of the TV camera can be
focussed using the manual mechanism (see Figure 5). The same
procedures as those described for focusing the acquisition bundle should
be adhered to here. If procedure i) is used, the sharpest image
of the space between the two bundles indicates the best focus
position.

As is the case with the acquisition bundle the correct orientation is
currently indicated by a painted mark, but again, we anticipate that
the bundle will be shortly doweled into position.

In the standard configuration the inner (outer) field is to the right (left)
of the TV screen.


\subsection{Observing System}

Log out of lpss3 and lpvs1. Log-on to the main system terminal lpvs1 as 
observer.

We will see a banner asking which system computer to use- type LPVF at the
command prompt.

Log-in to LPVF as observer.

When asked if you want to start the observing system reply NO.

At the VMS command prompt type-

$@$v9-0b1$\_$system

This sets the default observing system to V9-OB1$\_$system.com and
starts it up.

When asked if you want to start the observing system reply YES.

At the VMS command prompt, type-

ICL

Answer the observer name and the PATT reference questions. Then when
asked if you want to use the current setup respond NO, then select
option 11 ({\sc wyffos} using {\sc integral}).

Answer YES to the question about loading the system.

Then at the ICL prompt (hh:mm:ss$>$) type-\\

load fixfits\\
fixfits\\

Then go to the Sparc Real time Display (lpss3) and login as observer.
Everything starts up automatically.


As this instrument reaches common user status we anticipate that it
will be fully brought into the normal start up procedures common to
all WHT instrumentation. Hence, the above startup procedure will
reduce to logging onto the system computer (lpvf/g) under username
`observer', starting ICL, and then selecting the instrument
combination required for that nights observing.

\subsection{Autoguider}

The {\sc integral} autoguider application must be run from the
software version 4.5 DEV9. Currently this is loaded from a floptical disk. To
configure the autoguider for {\sc integral}, do the following:

1) ensure that the floptical disk marked V4.5 DEV9 is in the insite
drive in the autoguider VME cabinet (if not, it should be in the green
ring-binder which resides in the same cabinet).

2) power-cycle the autoguider VME and interrupt the startup after several
seconds by entering CTRL$\_$C at the autoguider terminal.

3) enter the following commands at the autoguider terminal\\
 EMPTY\\
 INSITE\\
 RELOAD\\

4) wait for the system to load from the floptical disk, and select
{\sc integral} when prompted during the startup.

In order to configure the autoguider for other focal stations (CASS or UES),
which use the default software on hard disk, power-cycle the autoguider 
VME and select the appropriate focal station when prompted during startup.

Note that the {\sc integral} autoguider application uses the PRIME
serial port.  CASS and UES use their normal allocated ports.


\subsection{TCS}

Before observing with {\sc integral}, be sure to issue the following commands
(along with the usual ZEROSET's, CAL LAST's and so on) when setting up
the TCS:

USER$>$ GHRIL ROT\\
USER$>$ INSTRUMENT OWN\\
USER$>$ AGSELECT GHRIL\\

Note that having done a calibrate on the rotator centre, a nominal
aperture (aperture zero) can be defined in order to place the
telescope reference position at the center of the acquisition
field. GSS will take account of such an aperture if you enter APERTURE
$<$x$>$ $<$y$>$ at the GSS prompt before searching for guide stars.


\subsection{Rotator Limits}

The GHRIL rotator has hardware switches limiting its motion to
slightly less than one revolution. The TCS software limits are set
about 1 degree inside the hardware limits, constraining the rotator
mount position angle to a range of 3 to 358 degrees. The safety of
{\sc integral} should not be entrusted to these mechanisms -- the
rotation of the instrument should be checked visually several times
during each night, after which an assessments of the reliability of
the limits can be made.

\subsection{Rotator Zero Set}

Owing to the fact that the absolute encoder `wraps' at a certain point,
it is very important to zeroset the incremental encoder against the
absolute at a known physical position. That position is mount PA 180,
and it is the `park' position for {\sc integral}. When the rotator is at this
position the `180' label marked on the rotator in indelible ink is at the
12 `O' Clock position when viewed from the GHRIL bench. Before observing with
{\sc integral} it is important to ensure that the rotator is in this position
(to within twenty degrees or so is adequate).  The local controls can
be used to move it if necessary. The incremental encoder can then be
zeroset against the absolute in the usual way. It must not be zeroset
without a visual check that the rotator is in the required position.


\subsection{The Guide Star Server -- GSS}

The GSS with configurations for WHT INTEGRALINNER and WHT INTEGRALOUTER is
selected when you log on to the GSS account and select WHT.

%Old instructions:- 

%Until both autoguider fields have been commissioned, the arrangement
%here is temporary to allow easy write access to a development version
%of the GSS configuration file. Log on as GSS in the normal way and
%enter WHT when prompted for the telescope name. The issue the command
%@INTEGRAL. This will put you into a special {\sc integral}
%subdirectory, and select a version of the GSS which has configurations
%for WHT INTEGRALINNER and WHT INTEGRALOUTER.


\subsection{Control in Engineering Mode}

To start the {\sc wyffos} mimic, log in to lpss3 (from a xterm), as
user {\sc wyffos} (username: wyffos; password: wht$\_$wyffos) and
type

start$\_$eng


To start the {\sc integral} mimic log in to orion.roque (from a
xterm) as user integral (username: integral; password:
wht$\_$integral) and type

start$\_$eng 

The low level {\it Software Users Manual} has the reference INT-IAC-MNL-001

\subsection{Data Analysis Software Installation}

For the installation of the different scientific software tasks and
source programs see {\sl
http://www.iac.es/project/integral/index.html}.



\section{OBSERVING PROCEDURES}

\subsection{Acquisition and Telescope Focusing}

Locate the acquisition bundle at the center of the field using the SP
mechanism (ISPFC ACQ OBS).  The field of view of this bundle is 22.5
$\times$ 30.2 arcsec $^2$.

At SPA=0 degrees, the orientation on the TV screen is such that North
is up and East is left (when H down, and V up on the TV switches at the control room).

By moving the rotator, the acquisition (and observing) bundle can be aligned 
at the desired angle. 

Limiting magnitude of the acquisition TV without integration is V$\sim$15.

The following filters are currently installed in the acquisition system: 
CLEAR, BG38, GG495, OG530, and RG630. 

\subsection{Focusing the Telescope}

{\sc integral} is focused by visually inspecting the image of a faint star
on the acquisition TV system. A typical telescope focus encoder value is 97.7.


\subsection{Adjustment of the Rotator Axis and Orientation}

Determine the X and Y coordinates of a star on the TV acquisition
screen.  Change the Sky Position Angle (SPA) by 180 degrees. The star
describes a semi-circle reaching a final location on the TV ({\it i.e.},
[Xf,Yf]). The center of this circle [(X+Xf)/2,(Y+Yf)/2] should be the
rotator center. Repeating this process will lead to a more accurate
determination of the rotator centre.

To minimize tracking uncertainties, select a star near the pole.

After the rotator centre has been determined a CALIBRATE should be done at 
this point.

\subsection{Guiding}

In order to check that the guiding bundles are properly mounted the following
check can be done:

i) Locate the slide unit at (65237, 0.). For that use the commands IXS and 
IYS.\\
ii) Align a star at the rotator centre\\
iii) Applying an off-set of 212 (386) arcsec (Telescope to the South) the star
should appears at the centre of inner (outer) guiding bundle.\\

With the handset in the XY mode, at SPA=0 degrees, the up button will
cause an object to move down the TV screen while the handset left
button will cause an object to move left on the TV screen.

Use the WHT INTEGRALINNER and WHT INTEGRALOUTER configurations of the GSS
for finding guide stars within the inner and outer fields (see Figure 3). 

The ICL commands IXSlideAbs and IYSlideAbs are used to moved the XY slide
to the GSS indicated position .

\subsection{Feeding the Science Bundles}

To locate the scientific bundles at the center field, move the SP using
(ISPFC [sb1,sb2,sb3] [obs]).

There are small off-sets between the rotator center and the positions
of the central fibres. If high spatial consistency is required
individual apertures can be defined for each bundle. If it proves
necessary to re-determine the offsets for any particular bundle(s)
software is available for quick image reconstruction (see Section
5.8). In this case, to save time, make sure the autoguider is setup
and the chip readout speed is set to turbo.

\subsection{Calibrating}

The bundles are located at the calibration position using the SP mechanism
(ISPFC [sb1,sb2,sb3] [cal] [1,2,white]).

CuAr, CuNe and a tungsten lamps are housed in the calibration unit. The two
arc lamps can be switched on simultaneously. Typical exposure times with the 
R1200B/R gratings are a few seconds.

Arc maps obtained with {\sc integral} are shown in INT-IAC-TRP011.

\subsection{Controlling INTEGRAL: A Glossary of Commands}

Details of the commands available from ICL are given below, Commands
may be issued in any mixture of upper and lower case. Most commands
offer help and prompt if no parameters are specified.

IAF\ \ \ \                   Move AU filter wheel to new position\\
IGF\ \ \ \                   Move GU filter wheel to new position\\
IXA\ \ \ \                   Set autoguider slide X axis to absolute position\\
IYA\ \ \ \                   Set autoguider slide Y axis to absolute position\\
IXR\ \ \ \                   Move autoguider slide X axis by relative position\\
IYR\ \ \ \                   Move autoguider slide Y axis by relative position\\
ISA\ \ \ \                   Move autoguider X/Y slides to absolute position\\
ISR\ \ \ \                   Move autoguider X/Y slides by relative position\\
ILA\ \ \ \                   Turn on/off any of the calibration lamps\\
IDA\ \ \ \                   Move mechanism to datum point\\
IUP\ \ \ \                   Update position of a mechanism\\
IST\ \ \ \                   Stop a mechanism\\
ISP\ \ \ \                   Move Swing plate to a new position\\
IG  \ \ \ \                  General purpose command covering all the above options\\


\underbar {IAF} \\
Move the acquisition filter wheel to a new position. This command can also 
set a default position for the filter wheel. The default position can then
be set by just typing IAF $<$CR$>$. 

Command long-form: IAFW

ICL Command Format:

IAF posn \ \ \                 Move AU filter wheel to $<$posn$>$\\
IAF SetDefault posn \ \ \      Set default position to $<$posn$>$\\
IAF \ \ \                      Move filter wheel, prompt for $<$posn$>$\\


\underbar {IGF}\\
Move the guider filter wheel to a new position. This command can also set
a default position for the filter wheel. The default position can then
be set by just typing IGF$<$CR$>$. 


Command long-form: IGFW

ICL Command Format:

IGF posn \ \ \                Move GU filter wheel to $<$posn$>$\\
IGF SetDefault posn \ \ \     Set default position to $<$posn$>$\\
IGF \ \ \                     Move filter wheel, prompt for $<$posn$>$\\


\underbar {ILA}\\
Turn on or off any of the {\sc integral} calibration lamps. A prompt will be 
issued for the lamp name and for the state if none is supplied on the 
command line.                                                           

Current lamp options are: CuNe, CuAr and White

Command long-form: ILamps

ICL Command Format:

ILA  $<$lamp$>$ $<$On$|$Off$>$     Turn calibration lamp $<$lamp$>$ ON or OFF

\underbar {IXA}\\
Move the autoguider X slide to a new position. The new position is an
absolute position in microns. A prompt will be issued if no parameter is
supplied.

Command long-form: IXSlideAbs

ICL Command Format:

IXA position \ \ \            Move autoguider X slide to $<$position$>$

\underbar {IYA}\\
Move the autoguider Y slide to a new absolute position. The position is
specified in microns. A prompt will be issued if no parameter is given.

Command long-form: IYSlideAbs

ICL Command Format:

IYA position \ \ \            Move autoguider Y slide to $<$position$>$

\underbar {IXR}\\
Move the autoguider X slide by a relative amount specified in microns.
A prompt will be issued if no parameter is specified. The offset is
relative to the current position.

Command long-form: IXSlideRel

ICL Command Format:

IXR  delta \ \ \              Move autoguider X slide by $<$delta$>$

\underbar {IYR}\\
Move the autoguider Y slide by a relative amount specified in microns.
A prompt will be issued if no parameter is specified. The offset is
relative to the current position.

Command long-form: IYSlideRel

ICL Command Format:

IYR  delta  \ \ \             Move autoguider Y slide by $<$delta$>$ 


\underbar {ISA}\\
Move both axes of the autoguider slide to a new absolute position.   
Both axes will move simultaneously and the command will complete when
both have reached their final positions. Positions are specified in
microns.

Command long-form: IAGAbs

ICL Command Format:

ISA X Y  \ \ \                Move autoguider slide to (X,Y)

\underbar {ISR}\\
Move both axes of the autoguider slide by a specified amount relative 
to the current position. Both axes will move simultaneously and the 
command will complete when both moves have finished. The deltas are 
specified in microns.

Command long-form: IAGRel

ICL Command Format:

ISR dX dY  \ \ \              Move autoguider slide by (dX,dY)

\underbar {IDA}\\
Move a selected mechanism to its datum point. The mechanism should be
specified by name or abbreviation, and will be prompted for if not 
supplied.

Command long-form: IMechDatum

ICL Command Format:

IDA  $<$mech$>$  \ \ \       Move $<$mech$>$ to its datum point.

\underbar {IUP}\\
Updates the mechanism's position by instructing the micro to report
the current position.

Command long-form: IMechUpdate

ICL Command Format:

IUP   $<$mech$>$   \ \ \            Update position of $<$mech$>$


\underbar {IST}\\
Stops the specified mechanism if it is currently moving. Any outstanding
ADAM command on the mechanism must be CANCEL'led first.     

Command long-form: IMechStop

ICL Command Format:

IST $<$mech$>$   \ \ \              Stop $<$mech$>$           

\underbar {ISP}\\
Move the swing plate to select a new fibre bundle. The command also 
selects whether the bundle is used at its observing or calibration 
position. Prompts will be offered if parameters are not specified.

Command long-form: ISPFC

ICL Command Format:

ISP   bundle position    Select $<$bundle$>$ at $<$position$>$ where $<$position$>$ = CALIBRATION!OBSERVING

\underbar {IG(General-purpose-command)}\\
General purpose command to control all aspects of {\sc integral} operation.
If parameters are not specified, then appropriate prompts and help are  
supplied.                                 

ICL Command Format:

IG act mech p1 p2        Perform action $<$act$>$ on mechanism $<$mech$>$ parameters $<$p1$>$ and $<$p2$>$ may be supplied if required.


\subsection{Raw and Quick Data Analysis}


This section briefly describes procedures for a quick and
crude analysis of {\sc integral} data. This is done in the IRAF
environment (of which a basic knowledge is assumed).\\

Most of the different steps for the data reduction and analysis can be
performed using standard IRAF tasks, though some particular operations
require some non-standard programs. These programs have been collected
into a separate package called {\sl integral} (see {\it
http://www.iac.es/project/integral/index.html} for availability and
installation instructions).

For loading the relevant (standard and non-standard) tasks type the
following sequence:\\
cl  (to start the IRAF environment)\\   
integral (to load non-standard and standard IRAF tasks required)\\
int\_status (to generate the files required for the 2D reconstruction)

By typing {\sl help integral opt=sys}, a general description of the
INTEGRAL package is printed on the display. To obtain a paper copy of
this help type {\sl help integral opt=sys $|$ lprint}.

\underbar {Listing INTEGRAL tasks.}\\
When the INTEGRAL package is loaded, all {\sl
non-standard tasks} are showed on the display. By typing {\sl help} a
list of these specific tasks and a brief description of each is printed on
display. The non-standard INTEGRAL tasks are the following.


\begin{center}
\begin{tabular}{|l|l|}
\hline
\ Task & Function\\
\hline
\ {\sl int\_hart} & Hartmann test for a list of couples of images\\
\hline
\ {\sl int\_fwhm} & Center, peak, sigma and FWHM of a list of 2D images for a lines array\\
\hline
\ {\sl int\_stat} & Statistics data for a list of images\\
\hline
\ {\sl ms2ascii} & Convert a multispec format 2D image to ASCII format spectra\\
\hline
\ {\sl readfxcor} & Export to a file the values of radial velocities, pixel shifts, or widths obtained\\
\ & using fxcor\\
\hline
\ {\sl int\_map} & 2D reconstruction from a ASCII file with fibre number, x, y,\\
\ & parameter to be mapped, and fiber status columns\\
\hline
\ {\sl int\_rec} & 2D reconstruction from a non-reduced 2D image\\
\hline
\ {\sl int\_spd1f} & Spatial shift between two images for a fibre\\
\hline
\ {\sl int\_spdXf} & Spatial shift between two images for a fibre list\\
\hline
\ {\sl int\_nspec} & Extract a calibrated spectrum of a selected fibre\\
\hline
\ {\sl int\_xyfib} & Show on display xcenter (middle line in the dispersion axis) and ycenter\\
\ &  (spatial coordinate) of the `apfile' parameters for a selected fiber\\
\hline
\ {\sl int\_daref} & Shifts along a.r. and dec. produced by differential atmospheric refraction\\
\hline
\end{tabular}
\end{center}

\underbar {Help on integral tasks}\\
Help is available for each task ({\it e.g.}, {\sl help int\_spdXf})

\underbar {Some examples of the quick data examination}\\ For a raw
analysis of the images standard {\sc integral} tasks, like {\sl
imexamine} or {\sl implot} can be used. With {\sl imexamine} the user
can generate profiles along the dispersion or spatial axes (type {\sl
j} and {\sl k} respectively), contours (type {\sl e}) etc. More complex
operations (e.g. extraction of a fiber aperture, wavelength
calibration, building up a map) require the knowledge of the standard
tasks of IRAF devoted to fiber-data analysis (see, for instance, table
in  next section). The {\sc integral} software offers some specific
tasks which can be used to obtain an extracted spectrum or a 2D
reconstruction of a filter image.

\underbar {2D reconstruction of a filter image}\\

To perform a 2D reconstruction use the task {\sl int\_rec}. In the
example below, an object image ("M32center") was taken with the
sb2 bundle. Using {\sl int\_rec} an intensity map ("M32\_300\_500") between
pixels 300 and 500 in the dispersion axis was obtained.

The first step of the {\sl int\_rec} task is the positional defining,
tracing, and extraction of the apertures in the "referenceflat",
unless this operation has been already done. The name of the file with
the parameters corresponding to the definition, tracing and extraction
is saved in the database as apnamep1\_p2, where 'name' refers to the
flat field image ("referenceflat" in the example), 'p1' is the value
of the first pixel (parameter pix1) along the dispersion axis, and
'p2' is the value of the second pixel (parameter pix2). If this file
is already in existance, the operations will not be repeated.

The definition (width and center), tracing and extraction of the apertures in
"referenceflat" is done interactively.  Within {\sl int\_rec}, this is
achieved using the standard IRAF task {\sl apall}. On execution, the
profile of the apertures along the middle line in the dispersion axis
are displayed.  All apertures will appear identified and ordered,
however, it is possible that a cosmic ray event has been falsely
identified instead of a true aperture.  In this case, this aperture
should be deleted (typing {\sl d}) and the true aperture marked
(typing {\sl m}).  The rest of the apertures will then need to be
selected (typing {\sl a}), and ordered (typing {\sl o}). Help is
available on these commands by typing {\sl ?}.  The widths of the
apertures will not have to changed.

After defining of the aperture positions, they are spectrally traced.
In principle, the user can do this operation interactively (for
each fibre!). Various operations are possible {\it e.g.} changing the
order of the fitting polynomial {\it etc}.  {\sl apall} then displays the
indivually extracted spectra (which may or may not be viewed).


The second step is the definition, tracing and extraction of the
apertures in the object image, (in this case, "M32center"). If the
previous operations have been carried out on the flat field image (with the
same instrument configuration), then it is safe to assume that
the same extraction parameters will apply (database file
apnamep1\_p2).  This can then be used as a reference for tracing and
extraction in other images taken during the same night because
INTEGRAL/WYFFOS should be very stable. Obviously, if p1 and/or p2 are
changed, a new definition, tracing and extraction paramter file is
required.

The third step is the reconstruction of the image, according to a
interpolation (NAG routines e01saf and e01sbf).

Note that an estimation of the BIAS is required for {\sl int\_rec}.

\small
\begin{center}
\begin{tabular}{ll}
\ PACKAGE=integral & \\
\ TASK=int\_rec & \\
\       object = "M32center"    & Object image\\
\         flat = "referenceflat"& Flat image\\
\         pix1 = 300            & First pixel in the dispersion axis\\
\         pix2 = 500            & Second pixel in the dispersion axis\\
\       bundle = 2              &  SB1(1), SB2(2), SB3(3)\\
\         bias = 1000           &  BIAS\\
\     outimage = "M32\_300\_500"&    Outimage       \\     
\        (mode = "q")& \\
\end{tabular}        
\end{center}
\normalsize

\underbar {Extraction of a particular spectrum}\\
This is done with the task {\sl int\_nspec}. In the example below, the
spectrum $\#$25 of "M32center" will be stored in the file "M32\_25".

The first step of the {\sl int\_nspec} task is the definition,
tracing, and extraction of the "referenceflat" (see the last section).

Secondly, the apertures are defined, traced and extracted for the
object image (see the last section).

After that, a calibrated (or non-calibrated) spectrum of the selected fiber
is showed on
display. The calibration is done acoording to the parameters of the
image header.

Note that an estimation of the BIAS is required.

\small
\begin{center}
\begin{tabular}{ll}
\ PACKAGE= integral & \\
\ TASK=int\_nspec & \\
\        image = "M32center" &   Object image\\
\    reference = "referenceflat"&  Flat image\\
\      fibre\_n = 25            &   Number of fibre\\
\       bundle = 2              &  SB1(1), SB2(2), SB3(3)\\
\         bias = 1000           &  BIAS\\
\     spectrum = "M32\_25"      &  Output image of the spectrum\_n\\
\      calibra = yes            &  Calibrate the spectrum (yes/no)?\\
\        (mode = "q")           &  \\
\end{tabular}        
\end{center}
\normalsize

\subsection{Data Reduction Guide}

\underbar {Steps for {\sc integral} Data Reduction}\\
The following steps are recomended to successfully reduce data obtained with
{\sc integral}:

\begin{center}
\begin{tabular}{|l|l|l|l|}
\hline
\ Step & Function & Package & Task\\
\hline
\ 1 & The BIAS Subtraction & {\sl ccdred} & {\sl ccdproc}\\
\hline
\ 2 & Aperture Definition and Trace & {\sl specred} & {\sl apall}\\
\hline
\ 3 & Scattered Light Correction & {\sl specred} & {\sl apscatter}\\
\hline
\ 4 & Extraction & {\sl specred} & {\sl apall}\\
\hline
\ 5 & Flat Spectra and & {\sl specred} & {\sl msresp1d}\\
\ & Thoughtput Correction & & \\
\hline
\ 6 & Arc Line Identification & {\sl specred} & {\sl identify}, {\sl reidentify}\\
\ & and Dispersion Correction & & {\sl refspectra}, {\sl dispcor}\\
\hline
\ 7 & Sky Subtraction & {\sl specred}	& {\sl skysub}\\
\hline
\ 8 & 2D reconstruction & {\sl integral}	& {\sl int\_map}\\
\hline
\end{tabular}
\end{center}

A detailed guide for the {\sc integral} data reduction can be found in
INT-IAC-MNL-004.

\newpage

\section{Appendix: Positions and Coordinates of Fibres, and 
Orientations of the Scientific Observing Bundles}

\newpage


\begin{figure}[htpb*]
\vspace{23.truecm}
\hspace*{15.cm}
%\special{psfile=sb1.ps hscale=350. vscale=350. hoffset=-1000 voffset=-300}
\special{psfile=sb1numeration.eps hscale=200. vscale=200. hoffset=-550 voffset=0}
\caption{Fibre numeration at the focal plane for sb1. For SPA=0 degrees, North is top, East is left. For SPA=90 degrees, East is top, North is right. Y increases to top and X increases to right }
\end{figure}

\footnotesize
\begin{table}[htpb*]
\caption{Fibre identification: bundle sb1. Values of -$\Delta$alpha and $\Delta$delta, correspond to SPA=0.}
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('')  & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
1&-8&10000&-0,04&45,07&RING&\\
2&-2060&9748&-9,29&43,94&RING&\\
3&-4059&9118&-18,3&41,1&RING&\\
4&-5858&8086&-26,4&36,45&RING&\\
5&-7427&6662&-33,48&30,03&RING&\\
6&-8640&4979&-38,94&22,44&RING&\\
7&-760&-617&-3,43&-2,78&\\
8&-812&-508&-3,66&-2,29&\\
9&-817&624&-3,68&2,81&\\
10&-752&737&-3,39&3,32&\\
11&-9510&3056&-42,86&13,77&RING&\\
12&-637&-628&-2,87&-2,83&\\
13&-689&-515&-3,11&-2,32&\\
14&-745&-403&-3,36&-1,82&\\
15&-812&-295&-3,66&-1,33&\\
16&-818&402&-3,69&1,81&\\
17&-752&512&-3,39&2,31&\\
18&-687&617&-3,1&2,78&\\
19&-622&735&-2,8&3,31&\\
20&-9935&1020&-44,78&4,6&RING&\\
21&-506&-637&-2,28&-2,87&\\
22&-562&-531&-2,53&-2,39&\\
23&-621&-408&-2,8&-1,84&\\
24&-686&-297&-3,09&-1,34&\\
25&-749&-190&-3,38&-0,86&\\
26&-810&-75&-3,65&-0,34&\\
27&-810&172&-3,65&0,78&\\
28&-751&287&-3,38&1,29&\\
29&-696&397&-3,14&1,79&\\
30&-626&508&-2,82&2,29&\\
31&-561&624&-2,53&2,81&\\
32&-489&731&-2,2&3,29&\\
33&-9941&-1070&-44,81&-4,82&RING&\\
34&2&-640&0,01&-2,88&\\
35&-122&-648&-0,55&-2,92&\\
36&-251&-647&-1,13&-2,92&\\
37&-373&-646&-1,68&-2,91&\\
38&-436&-536&-1,97&-2,42&\\
39&-497&-417&-2,24&-1,88&\\
40&-559&-296&-2,52&-1,33&\\
41&-621&-197&-2,8&-0,89&\\
42&-688&-77&-3,1&-0,35&\\
43&-746&48&-3,36&0,22&\\
44&-685&172&-3,09&0,78&\\
45&-623&276&-2,81&1,24&\\
46&-569&392&-2,56&1,77&\\
47&-499&502&-2,25&2,26&\\
48&-429&611&-1,93&2,75&\\
49&-367&732&-1,65&3,3&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}

\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
46&-569&392&-2,56&1,77&\\
47&-499&502&-2,25&2,26&\\
48&-429&611&-1,93&2,75&\\
49&-367&732&-1,65&3,3&\\
50&-240&736&-1,08&3,32&\\
51&-115&723&-0,52&3,26&\\
52&-9527&-3108&-42,94&-14,01&RING&\\
53&-57&-536&-0,26&-2,42&\\
54&-189&-530&-0,85&-2,39&\\
55&-309&-537&-1,39&-2,42&\\
56&-372&-428&-1,68&-1,93&\\
57&-433&-308&-1,95&-1,39&\\
58&-490&-190&-2,21&-0,86&\\
59&-558&-85&-2,52&-0,38&\\
60&-626&28&-2,82&0,13&\\
61&-563&154&-2,54&0,69&\\
62&-500&277&-2,25&1,25&\\
63&-442&391&-1,99&1,76&\\
64&-370&501&-1,67&2,26&\\
65&-299&616&-1,35&2,78&\\
66&-178&611&-0,8&2,75&\\
67&-53&610&-0,24&2,75&\\
68&-8644&-5020&-38,96&-22,63&RING&\\
69&21&-418&0,09&-1,88&\\
70&-&-&-&-&\\
71&-249&-418&-1,12&-1,88&\\
72&-309&-307&-1,39&-1,38&\\
73&-368&-196&-1,66&-0,88&\\
74&-429&-85&-1,93&-0,38&\\
75&-495&30&-2,23&0,14&\\
76&-437&155&-1,97&0,7&\\
77&-375&271&-1,69&1,22&\\
78&-313&384&-1,41&1,73&\\
79&-245&490&-1,1&2,21&\\
80&-119&492&-0,54&2,22&\\
81&-7424&-6720&-33,46&-30,29&RING&\\
82&-46&-314&-0,21&-1,42&\\
83&-170&-309&-0,77&-1,39&\\
84&-244&-194&-1,1&-0,87&\\
85&-306&-86&-1,38&-0,39&\\
86&-368&42&-1,66&0,19&\\
87&-308&153&-1,39&0,69&\\
88&-253&270&-1,14&1,22&\\
89&-185&380&-0,83&1,71&\\
90&-62&372&-0,28&1,68&\\
91&-5864&-8106&-26,43&-36,54&RING&\\
92&7&-207&0,03&-0,93&\\
93&-123&-206&-0,55&-0,93&\\
94&-184&-88&-0,83&-0,4&\\
95&-247&37&-1,11&0,17&\\
96&-186&150&-0,84&0,68&\\
97&-132&259&-0,59&1,17&\\
98&-4053&-9156&-18,27&-41,27&RING&\\
99&-60&-96&-0,27&-0,43&\\
100&-122&24&-0,55&0,11&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}



\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('')  & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
101&-62&140&-0,28&0,63&\\
102&-2073&-9794&-9,34&-44,14&RING&\\
103&1&25&0&0,11&\\
104&14&-9992&0,06&-45,04&RING&\\
105&65&141&0,29&0,64&\\
106&126&28&0,57&0,13&\\
107&67&-88&0,3&-0,4&\\
108&2091&-9774&9,42&-44,05&RING&\\
109&-5&257&-0,02&1,16&\\
110&128&252&0,58&1,14&\\
111&192&138&0,87&0,62&\\
112&251&30&1,13&0,14&\\
113&194&-85&0,87&-0,38&\\
114&131&-197&0,59&-0,89&\\
115&4087&-9124&18,42&-41,12&RING&\\
116&64&383&0,29&1,73&\\
117&187&373&0,84&1,68&\\
118&254&256&1,14&1,15&\\
119&320&144&1,44&0,65&\\
120&376&31&1,69&0,14&\\
121&316&-85&1,42&-0,38&\\
122&255&-194&1,15&-0,87&\\
123&200&-299&0,9&-1,35&\\
124&77&-306&0,35&-1,38&\\
125&5898&-8082&26,58&-36,43&RING&\\
126&13&492&0,06&2,22&\\
127&132&484&0,59&2,18&\\
128&258&496&1,16&2,24&\\
129&313&365&1,41&1,65&\\
130&377&253&1,7&1,14&\\
131&442&145&1,99&0,65&\\
132&503&35&2,27&0,16&\\
133&440&-79&1,98&-0,36&\\
134&383&-191&1,73&-0,86&\\
135&325&-300&1,46&-1,35&\\
136&268&-412&1,21&-1,86&\\
137&148&-417&0,67&-1,88&\\
138&7442&-6679&33,54&-30,1&RING&\\
139&74&603&0,33&2,72&\\
140&200&608&0,9&2,74&\\
141&324&614&1,46&2,77&\\
142&384&497&1,73&2,24&\\
143&443&381&2&1,72&\\
144&506&267&2,28&1,2&\\
145&569&156&2,56&0,7&\\
146&630&35&2,84&0,16&\\
147&564&-75&2,54&-0,34&\\
148&508&-188&2,29&-0,85&\\
149&449&-293&2,02&-1,32&\\
150&394&-407&1,78&-1,83&\\
151&317&-528&1,43&-2,38&\\
152&194&-536&0,87&-2,42&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}

\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('')  & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
153&70&-533&0,32&-2,4&\\
154&8673&-4990&39,09&-22,49&RING&\\
155&7&733&0,03&3,3&\\
156&132&724&0,59&3,26&\\
157&257&725&1,16&3,27&\\
158&384&733&1,73&3,3&\\
159&449&614&2,02&2,77&\\
160&515&499&2,32&2,25&\\
161&572&374&2,58&1,69&\\
162&636&268&2,87&1,21&\\
163&694&154&3,13&0,69&\\
164&768&48&3,46&0,22&\\
165&693&-71&3,12&-0,32&\\
166&635&-183&2,86&-0,82&\\
167&572&-284&2,58&-1,28&\\
168&516&-399&2,33&-1,8&\\
169&444&-522&2&-2,35&\\
170&383&-637&1,73&-2,87&\\
171&257&-638&1,16&-2,88&\\
172&125&-642&0,56&-2,89&\\
173&9526&-3079&42,94&-13,88&RING&\\
174&513&731&2,31&3,29&\\
175&573&613&2,58&2,76&\\
176&645&498&2,91&2,24&\\
177&697&378&3,14&1,7&\\
178&763&273&3,44&1,23&\\
179&820&163&3,7&0,73&\\
180&816&-66&3,68&-0,3&\\
181&758&-179&3,42&-0,81&\\
182&695&-284&3,13&-1,28&\\
183&639&-390&2,88&-1,76&\\
184&565&-514&2,55&-2,32&\\
185&506&-626&2,28&-2,82&\\
186&9974&-1040&44,96&-4,69&RING&\\
187&637&733&2,87&3,3&\\
188&696&624&3,14&2,81&\\
189&768&492&3,46&2,22&\\
190&824&383&3,71&1,73&\\
191&820&-276&3,7&-1,24&\\
192&759&-387&3,42&-1,74&\\
193&691&-506&3,11&-2,28&\\
194&634&-625&2,86&-2,82&\\
195&9952&1060&44,86&4,78&RING&\\
196&765&732&3,45&3,3&\\
197&819&611&3,69&2,75&\\
198&815&-506&3,67&-2,28&\\
199&753&-610&3,39&-2,75&\\
200&9506&3091&42,85&13,93&RING&\\
201&8666&5006&39,06&22,56&RING&\\
202&7420&6706&33,44&30,23&RING&\\
203&5882&8100&26,51&36,51&RING&\\
204&4060&9148&18,3&41,23&RING&\\
205&2079&9777&9,37&44,07&RING&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}

\normalsize


\begin{figure}[htpb*]
\vspace{23.truecm}
\hspace*{15.cm}
%\special{psfile=sb2.ps hscale=350. vscale=350. hoffset=-1000 voffset=-300}
\special{psfile=sb2numeration.eps hscale=200. vscale=200. hoffset=-550 voffset=0}
\caption{Fibre identification: bundle sb2. For SPA=0 degrees, North is top, East is left. For SPA=90 degrees, East is top, North is right. Y increases to top and X increases to right }

\end{figure}


\footnotesize
\begin{table}[htpb*]
\caption{Fibre identification: bundle sb2. Values of -$\Delta$alpha and $\Delta$delta correspond to SPA=0.}
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('')  &$\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
1&33&9985&0,149&45,005&RING&\\
2&-2036&9775&-9,177&44,059&RING&\\
3&-4019&9133&-18,115&41,165&RING&\\
4&-5852&8086&-26,377&36,446&RING&\\
5&-7393&6686&-33,322&30,136&RING&\\
6&-1734&-1190&-7,816&-5,364&\\
7&-1737&1313&-7,829&5,918&\\
8&-8638&4998&-38,934&22,527&RING&\\
9&-1493&-1188&-6,729&-5,355&\\
10&-1621&-980&-7,306&-4,417&\\
11&-1745&-774&-7,865&-3,489&\\
12&-1755&899&-7,91&4,052&\\
13&-1615&1098&-7,279&4,949&\\
14&-1495&1312&-6,738&5,914&\\
15&-9493&3092&-42,788&13,937&RING&\\
16&-1245&-1186&-5,612&-5,346&\\
17&-1379&-986&-6,216&-4,444&\\
18&-1499&-777&-6,756&-3,502&\\
19&-1616&-566&-7,284&-2,551&\\
20&-1745&-361&-7,865&-1,627&\\
21&-1741&480&-7,847&2,163&\\
22&-1612&689&-7,266&3,106&\\
23&-1486&898&-6,698&4,048&\\
24&-1370&1101&-6,175&4,963&\\
25&-1243&1313&-5,603&5,918&\\
26&-9942&1048&-44,811&4,724&RING&\\
27&-1006&-1190&-4,534&-5,364&\\
28&-1137&-985&-5,125&-4,44&\\
29&-1253&-777&-5,648&-3,502&\\
30&-1377&-574&-6,207&-2,587&\\
31&-1500&-357&-6,761&-1,609&\\
32&-1626&-149&-7,329&-0,672&\\
33&-1747&62&-7,874&0,279&\\
34&-1611&277&-7,261&1,249&\\
35&-1490&481&-6,716&2,168&\\
36&-1366&688&-6,157&3,101&\\
37&-1245&900&-5,612&4,057&\\
38&-1119&1099&-5,044&4,954&\\
39&-997&1311&-4,494&5,909&\\
40&-9924&-1034&-44,73&-4,661&RING&\\
41&-33&-1193&-0,149&-5,377&\\
42&-278&-1194&-1,253&-5,382&\\
43&-521&-1190&-2,348&-5,364&\\
44&-761&-1190&-3,43&-5,364&\\
45&-890&-986&-4,011&-4,444&\\
46&-1011&-779&-4,557&-3,511&\\
47&-1133&-569&-5,107&-2,565&\\
48&-1259&-364&-5,675&-1,641&\\
49&-1384&-150&-6,238&-0,676&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
50&-1505&56&-6,783&0,252&\\
51&-1368&275&-6,166&1,24&\\
52&-1245&478&-5,612&2,154&\\
53&-1122&689&-5,057&3,106&\\
54&-998&899&-4,498&4,052&\\
55&-877&1100&-3,953&4,958&\\
56&-758&1312&-3,417&5,914&\\
57&-515&1312&-2,321&5,914&\\
58&-271&1311&-1,221&5,909&\\
59&-9504&-3088&-42,837&-13,918&RING&\\
60&-157&-984&-0,708&-4,435&\\
61&-404&-987&-1,821&-4,449&\\
62&-648&-985&-2,921&-4,44&\\
63&-768&-779&-3,462&-3,511&\\
64&-894&-573&-4,03&-2,583&\\
65&-1016&-359&-4,579&-1,618&\\
66&-1139&-153&-5,134&-0,69&\\
67&-1262&60&-5,688&0,27&\\
68&-1125&275&-5,071&1,24&\\
69&-1003&483&-4,521&2,177&\\
70&-879&691&-3,962&3,115&\\
71&-758&896&-3,417&4,039&\\
72&-632&1098&-2,849&4,949&\\
73&-390&1100&-1,758&4,958&\\
74&-145&1100&-0,654&4,958&\\
75&-8661&-5007&-39,038&-22,568&RING&\\
76&-35&-775&-0,158&-3,493&\\
77&-278&-778&-1,253&-3,507&\\
78&-522&-772&-2,353&-3,48&\\
79&-650&-568&-2,93&-2,56&\\
80&-773&-363&-3,484&-1,636&\\
81&-898&-153&-4,048&-0,69&\\
82&-1014&57&-4,57&0,257&\\
83&-880&272&-3,966&1,226&\\
84&-759&478&-3,421&2,154&\\
85&-637&687&-2,871&3,097&\\
86&-512&897&-2,308&4,043&\\
87&-272&894&-1,226&4,03&\\
88&-7421&-6686&-33,449&-30,136&RING&\\
89&-159&-566&-0,717&-2,551&\\
90&-402&-568&-1,812&-2,56&\\
91&-531&-364&-2,393&-1,641&\\
92&-653&-153&-2,943&-0,69&\\
93&-775&58&-3,493&0,261&\\
94&-640&272&-2,885&1,226&\\
95&-514&479&-2,317&2,159&\\
96&-392&683&-1,767&3,078&\\
97&-147&689&-0,663&3,106&\\
98&-5879&-8101&-26,498&-36,514&RING&\\
99&-36&-362&-0,162&-1,632&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
100&-280&-361&-1,262&-1,627&\\
101&-407&-155&-1,834&-0,699&\\
102&-524&54&-2,362&0,243&\\
103&-390&269&-1,758&1,212&\\
104&-271&480&-1,221&2,163&\\
105&-4065&-9151&-18,322&-41,246&RING&\\
106&-159&-155&-0,717&-0,699&\\
107&-284&57&-1,28&0,257&\\
108&-149&272&-0,672&1,226&\\
109&-2085&-9794&-9,398&-44,144&RING&\\
110&-39&55&-0,176&0,248&\\
111&-3&-10026&-0,014&-45,19&RING&\\
112&97&272&0,437&1,226&\\
113&207&53&0,933&0,239&\\
114&85&-155&0,383&-0,699&\\
115&2069&-9809&9,326&-44,212&RING&\\
116&-28&477&-0,126&2,15&\\
117&215&483&0,969&2,177&\\
118&336&267&1,514&1,203&\\
119&446&53&2,01&0,239&\\
120&327&-153&1,474&-0,69&\\
121&204&-366&0,919&-1,65&\\
122&4066&-9161&18,327&-41,291&RING&\\
123&96&687&0,433&3,097&\\
124&336&685&1,514&3,087&\\
125&462&477&2,082&2,15&\\
126&581&263&2,619&1,185&\\
127&692&52&3,119&0,234&\\
128&572&-155&2,578&-0,699&\\
129&447&-363&2,015&-1,636&\\
130&325&-571&1,465&-2,574&\\
131&88&-568&0,397&-2,56&\\
132&5883&-8126&26,516&-36,626&RING&\\
133&-27&896&-0,122&4,039&\\
134&214&896&0,965&4,039&\\
135&461&894&2,078&4,03&\\
136&584&681&2,632&3,069&\\
137&706&474&3,182&2,136&\\
138&826&266&3,723&1,199&\\
139&930&51&4,192&0,23&\\
140&809&-160&3,646&-0,721&\\
141&685&-364&3,087&-1,641&\\
142&567&-571&2,556&-2,574&\\
143&448&-780&2,019&-3,516&\\
144&205&-778&0,924&-3,507&\\
145&7437&-6722&33,521&-30,298&RING&\\
146&96&1100&0,433&4,958&\\
147&342&1096&1,541&4,94&\\
148&586&1100&2,641&4,958&\\
149&707&893&3,187&4,025&\\
150&823&683&3,709&3,078&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
137&706&474&3,182&2,136&\\
138&826&266&3,723&1,199&\\
139&930&51&4,192&0,23&\\
140&809&-160&3,646&-0,721&\\
141&685&-364&3,087&-1,641&\\
142&567&-571&2,556&-2,574&\\
143&448&-780&2,019&-3,516&\\
144&205&-778&0,924&-3,507&\\
145&7437&-6722&33,521&-30,298&RING&\\
146&96&1100&0,433&4,958&\\
147&342&1096&1,541&4,94&\\
148&586&1100&2,641&4,958&\\
149&707&893&3,187&4,025&\\
150&823&683&3,709&3,078&\\
151&945&475&4,259&2,141&\\
152&1068&265&4,814&1,194&\\
153&1176&50&5,301&0,225&\\
154&1056&-158&4,76&-0,712&\\
155&929&-364&4,187&-1,641&\\
156&812&-572&3,66&-2,578&\\
157&689&-782&3,106&-3,525&\\
158&568&-989&2,56&-4,458&\\
159&329&-987&1,483&-4,449&\\
160&81&-982&0,365&-4,426&\\
161&8673&-5036&39,092&-22,699&RING&\\
162&-27&1311&-0,122&5,909&\\
163&221&1313&0,996&5,918&\\
164&459&1309&2,069&5,9&\\
165&707&1313&3,187&5,918&\\
166&827&1099&3,728&4,954&\\
167&945&893&4,259&4,025&\\
168&1071&680&4,827&3,065&\\
169&1189&471&5,359&2,123&\\
170&1312&266&5,914&1,199&\\
171&1421&49&6,405&0,221&\\
172&1299&-159&5,855&-0,717&\\
173&1179&-364&5,314&-1,641&\\
174&1053&-572&4,746&-2,578&\\
175&936&-782&4,219&-3,525&\\
176&812&-989&3,66&-4,458&\\
177&692&-1198&3,119&-5,4&\\
178&451&-1192&2,033&-5,373&\\
179&211&-1192&0,951&-5,373&\\
180&9534&-3132&42,972&-14,117&RING&\\
181&947&1310&4,268&5,905&\\
182&1070&1095&4,823&4,935&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
183&1191&894&5,368&4,03&\\
184&1311&681&5,909&3,069&\\
185&1433&468&6,459&2,109&\\
186&1552&259&6,995&1,167&\\
187&1661&46&7,487&0,207&\\
188&1542&-159&6,95&-0,717&\\
189&1421&-371&6,405&-1,672&\\
190&1298&-576&5,85&-2,596&\\
191&1175&-780&5,296&-3,516&\\
192&1055&-992&4,755&-4,471&\\
193&935&-1197&4,214&-5,395&\\
194&9958&-1075&44,884&-4,845&RING&\\
195&1188&1309&5,355&5,9&\\
196&1318&1097&5,941&4,944&\\
197&1432&888&6,454&4,002&\\
198&1561&680&7,036&3,065&\\
199&1683&468&7,586&2,109&\\
200&1667&-370&7,514&-1,668&\\
201&1544&-579&6,959&-2,61&\\
202&1420&-786&6,4&-3,543&\\
203&1295&-991&5,837&-4,467&\\
204&1175&-1204&5,296&-5,427&\\
205&9959&1003&44,888&4,521&RING&\\
206&1449&1303&6,531&5,873&\\
207&1565&1088&7,054&4,904&\\
208&1688&884&7,608&3,984&\\
209&1668&-786&7,518&-3,543&\\
210&1543&-992&6,955&-4,471&\\
211&1413&-1205&6,369&-5,431&\\
212&9527&3054&42,941&13,765&RING&\\
213&1696&1299&7,644&5,855&\\
214&1658&-1206&7,473&-5,436&\\
215&8688&4965&39,159&22,379&RING&\\
216&7454&6657&33,597&30,005&RING&\\
217&5905&8068&26,616&36,365&RING&\\
218&4086&9110&18,417&41,061&RING&\\
219&2102&9771&9,474&44,041&RING&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize



\begin{figure}[htpb*]
\vspace{23.truecm}
\hspace*{15.cm}
%\special{psfile=sb3.ps hscale=150. vscale=150. hoffset=-500 voffset=0}
\special{psfile=sb3numeration.eps hscale=200. vscale=200. hoffset=-550 voffset=0}
\caption{Spatial distribution of the fibres at the focal plane for sb3. For SPA=0 degrees, North is top, East is left. For SPA=90 degrees, East is top, North is right. Y increases to top and X increases to right }
\end{figure}

\footnotesize
\begin{table}[htpb*]
\caption{Fibre identification: bundle sb3. Values for -$\Delta$alpha and $\Delta$delta correspomnd to SPA=0.}
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
1&21&9987&0,095&45,014&RING&\\
2&-3075&9525&-13,860&42,932&RING&\\
3&-5883&8101&-26,516&36,514&RING&\\
4&-3237&-2990&-14,590&-13,477&\\
5&-3584&-2382&-16,154&-10,736&\\
6&-3568&2444&-16,082&11,016&\\
7&-3218&3042&-14,504&13,711&\\
8&-8090&5881&-36,464&26,507&RING&\\
9&-2549&-2977&-11,489&-13,418&\\
10&-2895&-2388&-13,049&-10,763&\\
11&-3227&-1791&-14,545&-8,073&\\
12&-3577&-1184&-16,123&-5,337&\\
13&-3557&1233&-16,032&5,557&\\
14&-3217&1851&-14,500&8,343&\\
15&-2874&2443&-12,954&11,011&\\
16&-2518&3042&-11,349&13,711&\\
17&-9527&3096&-42,941&13,955&RING&\\
18&-489&-2994&-2,204&-13,495&\\
19&-1176&-2979&-5,301&-13,427&\\
20&-1861&-2995&-8,388&-13,499&\\
21&-2203&-2384&-9,930&-10,745&\\
22&-2537&-1793&-11,435&-8,082&\\
23&-2890&-1170&-13,026&-5,274&\\
24&-3214&-559&-14,486&-2,520&\\
25&-3561&38&-16,050&0,171&\\
26&-3205&628&-14,446&2,831&\\
27&-2867&1247&-12,922&5,621&\\
28&-2538&1853&-11,439&8,352&\\
29&-2183&2440&-9,839&10,998&\\
30&-1829&3042&-8,244&13,711&\\
31&-1127&3041&-5,080&13,707&\\
32&-436&3023&-1,965&13,626&\\
33&-10001&6&-45,077&0,027&RING&\\
34&-139&-2385&-0,627&-10,750&\\
35&-830&-2386&-3,741&-10,754&\\
36&-1517&-2388&-6,838&-10,763&\\
37&-1852&-1796&-8,347&-8,095&\\
38&-2198&-1170&-9,907&-5,274&\\
39&-2523&-570&-11,372&-2,569&\\
40&-2876&30&-12,963&0,135&\\
41&-2525&616&-11,381&2,776&\\
42&-2179&1217&-9,821&5,485&\\
43&-1854&1836&-8,357&8,275&\\
44&-1497&2432&-6,747&10,962&\\
45&-796&2431&-3,588&10,957&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('') & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
46&-9511&-3052&-42,869&-13,756&RING&\\
47&-475&-1794&-2,141&-8,086&\\
48&-1164&-1796&-5,246&-8,095&\\
49&-1509&-1162&-6,801&-5,237&\\
50&-1844&-572&-8,311&-2,578&\\
51&-2178&24&-9,817&0,108&\\
52&-1831&622&-8,253&2,804&\\
53&-1490&1237&-6,716&5,576&\\
54&-1142&1831&-5,147&8,253&\\
55&-450&1827&-2,028&8,235&\\
56&-8113&-5861&-36,568&-26,417&RING&\\
57&-133&-1177&-0,599&-5,305&\\
58&-819&-1179&-3,691&-5,314&\\
59&-1138&-577&-5,129&-2,601&\\
60&-1487&12&-6,702&0,054&\\
61&-1146&617&-5,165&2,781&\\
62&-799&1227&-3,601&5,530&\\
63&-5878&-8097&-26,494&-36,495&RING&\\
64&-455&-582&-2,051&-2,623&\\
65&-804&25&-3,624&0,113&\\
66&-432&603&-1,947&2,718&\\
67&-3095&-9524&-13,950&-42,927&RING&\\
68&-98&9&-0,442&0,041&\\
69&-14&-10031&-0,063&-45,213&RING&\\
70&250&613&1,127&2,763&\\
71&582&12&2,623&0,054&\\
72&225&-598&1,014&-2,695&\\
73&3076&-9541&13,864&-43,004&RING&\\
74&-99&1203&-0,446&5,422&\\
75&588&1228&2,650&5,535&\\
76&946&598&4,264&2,695&\\
77&1268&-1&5,715&-0,005&\\
78&915&-598&4,124&-2,695&\\
79&552&-1197&2,488&-5,395&\\
80&5869&-8124&26,453&-36,617&RING&\\
81&236&1824&1,064&8,221&\\
82&937&1820&4,223&8,203&\\
83&1276&1198&5,751&5,400&\\
84&1626&608&7,329&2,740&\\
85&1954&-8&8,807&-0,036&\\
86&1595&-607&7,189&-2,736&\\
87&1245&-1198&5,612&-5,400&\\
88&898&-1800&4,048&-8,113&\\
89&215&-1793&0,969&-8,082&\\
90&8091&-5912&36,468&-26,647&RING&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize

\footnotesize
\begin{table}[htpb*]
\begin{center}
\begin{tabular}{lcccccc}
 & & & & & &\\
\hline\hline
slit position & X(microns) & Y(microns) & -$\Delta$alpha('')  & $\Delta$delta('') &  Ring (?)&\\ 
 & & & & & &\\
91&-107&2421&-0,482&10,912&\\
92&597&2420&2,691&10,908&\\
93&1294&2423&5,832&10,921&\\
94&1625&1817&7,324&8,190&\\
95&1965&1214&8,857&5,472&\\
96&2314&588&10,430&2,650&\\
97&2641&-12&11,904&-0,054&\\
98&2283&-601&10,290&-2,709&\\
99&1929&-1203&8,695&-5,422&\\
100&1591&-1795&7,171&-8,091&\\
101&1233&-2394&5,557&-10,790&\\
102&549&-2391&2,475&-10,777&\\
103&9520&-3098&42,909&-13,964&RING&\\
104&252&3034&1,136&13,675&\\
105&940&3018&4,237&13,603&\\
106&1626&3030&7,329&13,657&\\
107&1983&2420&8,938&10,908&\\
108&2303&1811&10,380&8,163&\\
109&2651&1197&11,949&5,395&\\
110&3004&589&13,540&2,655&\\
111&3323&-29&14,978&-0,131&\\
112&2979&-606&13,427&-2,731&\\
113&2624&-1200&11,827&-5,409&\\
114&2275&-1802&10,254&-8,122&\\
115&1927&-2399&8,686&-10,813&\\
116&1568&-2998&7,067&-13,513&\\
117&884&-2996&3,984&-13,504&\\
118&199&-2994&0,897&-13,495&\\
119&10014&-16&45,136&-0,072&RING&\\
120&2314&3020&10,430&13,612&\\
121&2670&2416&12,034&10,890&\\
122&2988&1806&13,468&8,140&\\
123&3339&1198&15,050&5,400&\\
124&3314&-1203&14,937&-5,422&\\
125&2965&-1804&13,364&-8,131&\\
126&2610&-2404&11,764&-10,836&\\
127&2259&-2996&10,182&-13,504&\\
128&9559&3023&43,085&13,626&RING&\\
129&3007&3018&13,553&13,603&\\
130&3367&2423&15,176&10,921&\\
131&3295&-2416&14,852&-10,890&\\
132&2946&-3004&13,278&-13,540&\\
133&8126&5815&36,626&26,210&RING&\\
134&5899&8064&26,588&36,347&RING&\\
135&3112&9497&14,027&42,806&RING&\\
 & & & & & &\\
\hline
 & & & & & &\\
\end{tabular}
\end{center}
\end{table}
\normalsize
\newpage


\begin{figure}[htpb*]
\psfig{figure=orientation.ps,height=115mm,width=180mm} 
\caption{Orientation of the fibres bundles at the telescope 
focal plane. For SPA=0 degrees, North is top and East is left.}
\end{figure}



\begin{figure}[htpb*]
\vspace{23.truecm}
\hspace*{15.cm}
\special{psfile=slitorientations.ps hscale=230. vscale=230. hoffset=-850. voffset=0.}
\caption{Orientation of the fibres bundles at the spectrograph slit and 
detector levels.}
\end{figure}


\end{document}


