SET UP Procedures

SET UP Procedures

Starting the computer system

Log on to the main system terminal lpvs1 as observer. Check the password at the whiteboard.
We will see a banner asking which system computer to use, LPVF or LPVG, check the whiteboard for the right.
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.
When ask if you want to use the current setup, select the option with WYFFOS using INTEGRAL.
Answer YES to the question about loading the system.

Changing gratings

1.: To change gratings on WYFFOS you must use wchange at the ICS.
2.: Go up to the GHRIL
3.: open access panels to the grating mount
4.: press the clamps control botton on the grating mount, which is situated facing the user. Press until red is alight.
5.: Take out the actual grating in WYFFOS
6.: mount the new grating with the label on its back right way up.
7.: Press again the clamp control botton to fix the grating clamps.
8.: Do not forget to update the new grating in the ICS with wchange command.

At the change position (-25.0), a central wavelength, of 7810 Å will be obtained. Any other can be selected with the WYFFOS command wcenwave. Changing gratings should normally be done by your support astronomer or ING technical staff.

WYFFOS grating data

grating angle offset

ICL> wchange
option? [0] 3
:
:
Current grating angle offset is xxxx mdeg (If different from 6170 mdeg, change it!)
New value? [0] > 6170

In the table 1 is shown for each grating leads the central wavelength 6328 Å(He-Ne Laser).

**Table1:** Grating angle for obtaining a central wavelength of 6328 Å
Grating	Angle (o)
R300B	- 2.44
R316R	-2.73
R600R	-7.95
R1200R	-19.35

Slit traslation (height) adjustment

1.: Setup spectrograph to obtain a flat:; Use int_slit to check if all fibers are on the CCD:; If 205 fibers are not present at any line, traslate in height the slit:

Focusing of the spectrograph

The previous steps to be carried on are:

mount the R1200B grating and select a central wavelength of ~5500 Å

ICL> wcenwave 5500

mount the BG39 filter and put in the beam

ICL> wfiltA in

put the STD3 in the calibration position

ICL> ISP STD3 CALIBRATION

Turn on the spectral calibration lamps (CuAr+CuNe)

ICL> ILA CuAr on

ICL> ILA CuNe on

Set WYFFOS to the start focus position (nominal=0)

ICL> wslitf 0

close the right Hartmann shutter

ICL> whart R

Take an exposure
close the left Hartmann shutter

ICL> whart L

Take other exposure
Select at least 9 position on the detector including an spectral line, and write the x, y position on an ascii file
run the task int_focus to obtain the Hartmann shifts for each selected position. The best focus should have values for shifts similar to the ones shown in Figure 1. There is no serious degradation in performance if the shifts are within 0.3 of this values, as the resolution of the spectrograph is limited by the fibre size. At the central position, the shift should be keep close to 0.5. This should be normally accommodated using the slit focus: a change of 1000 microns in slit focus corresponds to -0.4 in Hartmann shift.

**Figure 1:** Hartmann shifts
$\begin{figure}\begin{center}\psfig{figure=hart.eps}\end{center}\end{figure}$

Do not forget to open the Hartmann shutters after Hartmann test.
whart OUT

The focus can be also obtained looking for the minimum FWHM of the fibre images at the CCD. For this:

1.: Take one arc exposure with both Hartmann shutters open.
2.: Select at least 9 position on the detector including an spectral line, and write the x, y position on an ascii file
3.: run the task int_fwhm to obtain the Hartmann shifts for each selected position. The best focus should have values for shifts similar to the ones shown in Figure 2.

**Figure 2:** FWHM countours at the best focus
$\begin{figure}\psfig{figure=focus1.ps,angle=90,width=\textwidth}\vspace{0.8cm}\end{figure}$

Focusing and Orientation of the Acquisition Bundle

i) With the bundle connected to the to the SP, the inside of AG&C box is illuminated (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 (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.

Focusing and Orientation of the Guiding Bundle

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.

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 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.

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 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 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.

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.

Control in Engineering Mode

To start the wyffos mimic, log in to lpss3 (from a xterm), as user wyffos (username: wyffos; password: wht_wyffos) and
type

start_eng

To start the 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 Software Users Manual has the reference INT-IAC-MNL-001

Last updated March 2000
Begoña García-Lorenzo (Instrument specialist)
bgarcia@ing.iac.es

Ana M. Pérez-García (Deputy)
aperez@ing.iac.es