ACAM has no equivalent of the slit-viewing camera used with ISIS. Targets are acquired onto the slit in imaging mode (LIRIS and OASIS observers use similar techniques), using the new ACAM acquisition tool (commissioned 2010 October, by Samantha Rix). The telescope operator can take care of the target acquisition, but the tool is easy to use, and observers with many targets may want to do most of the acquisition themselves.

If for any reason the acquisition tool is unavailable, the target can be acquired manually (but this is fiddly, and takes longer).

The acquisition procedure is as follows:

1. Start the ACAM acquisition tool.
2. Point the telescope at the target / blind-offset star
3. Take an image of the back of the slit, measure the x,y position at which the target is to be acquired.
4. Take an image of the field, centre the target on the slit.
5. Check the through-slit image, finish acquisition.
6. Insert the VPH grism and expose.
7. Record an acquisition image, if required (after science exposures, or after step 4 above).

A short description of each step is given below. For detailed information about use of the acquisition tool, refer to the ACAM acquisition-tool cookbook.

A 1-page word-format summary of the procedure, written by Fiona Riddick (observing support assistant), is also available.

1 - Start the ACAM acquisition tool

Start the acquisition tool by by typing:

acqtool &

in the pink WHTICS window. When the display comes up, click on the 'grab' button at the top and select 'Grab ACAM...' to bring up the image-acquisition window. Then click on the 'View' button on the main display, and select 'Pick object' to bring up a third window. The three windows, all of which are needed for target acquisition, look something like this:

In the 'ACAM image acquisition' window, select from the slit-width menu the slit width with which the tool is to be used (this affects the position at which the slit is over-plotted).

On the same window, select from the filter menu a filter of similar wavelength to the range of interest, particularly when observing at other than the parallactic angle, or at large airmass.

2 - Point the telescope
Point the telescope to the target, or the blind-offset star (if the target is not easily visible on exposures lasting a few sec) with:

TO> gocat target-name &

Ask the telescope operator to set the rotator angle to the required position angle (usually parallactic). The operator will then also look for guide stars.

3 - Identify the x,y position of the centre of the slit

The y position of the slit (1) depends on the slit to be used, and (2) can change by several pixels when the telescope is pointed to a new target (flexure due to change of elevation and of Cassegrain rotator angle). Checking the position of the slit takes only a few seconds and is recommended whenever changing the slit to be used, or when there's a large change of elevation or rotator angle.

Typically, the centre of the 1.0-arcsec slit lies at y ~ 1150 when using the standard window (1:2148,800:3300). The y position of the slit varies slightly along the length of the slit (curvature). The small differences (< 1 arcsec) between the y positions of ACAM's individual slits, when nominally on-axis, are reported on the ACAM slit-positions page.

To check the poition of the slit, select 'Grab through-slit image' on the 'ACAM acquisition window'. This configures ACAM in imaging mode, with the specified filter and exposure time, but with the required slit also in the light path, in order to take an image of the back of the slit. An exposure of a few sec should be enough to see the slit, even on a moonless night.

If the green overlay does not coincide (in the y direction) with the displayed slit, click on 'Select new slit-centre position' on the 'Pick object' menu, click on the new position and then on 'Apply new slit centre'.

To save time, the slit position can safely measured while waiting for completion of the azimuth slew, if the telescope has finished slewing in elevation and in rotator angle,

The same filter should be used throughout steps 3 - 7 of the acquisition sequence (changing filter may change the position of the image on the CCD by a few arcsec).

4 - Take an image of the field, centre the target on the slit
The telescope and rotator should be in position ('tracking').

On the 'ACAM image acquisition' window:

• Set the exposure time ('Duration') to 1 sec (for bright targets) or a few 10s sec (faint targets).
• Tick 'Archive Acquisition Image' to save the acquisition image.
• Click on 'Grab field image'. A windowed (and fast-readout) exposure will be displayed, and the orientation on the sky will be indicated. The 'Low' and 'High' values for the lookup table often need tweaking.
• If your target isn't visible, try a longer exposure time.

NB the acquisition tool changes the CCD binning set by the observer, and restores it after acquisition.

On the 'Pick object' window, click on 'Select object', click on the target in the displayed image, then click on 'Move object to slit centre' to offset the telescope appropriately. If the target isn't well-centred in the window, repeat this procedure. More than two iterations should not be needed.

5 - Check the through-slit image, finish acquisition

Click on 'Grab through-slit image' on the 'ACAM acquisition window', you should see something like this:

If the object acquired at this point is the science target, ask the telescope operator to start autoguiding, and ask him/her to make any final adjustment needed to centre the target in the slit.

If on the other hand the object acquired is the blind-offset star rather than the science target itself, ask the operator to blind-offset to the target, and then start autoguiding as quickly as possible. The blind-offset accuracy is < 0.2 arcsec over an offset of at least 20 arcmin.

6 - Insert the VPH, start exposing

TO> acamspec v400 1 (for a 1-arcsec slit)

E.g. for an 1800-sec exposure:

TO> run acam 1800 "M51 OIII"

7 - Record an acquisition image
When obtaining a spectrum of an object in a crowded field, it may be helpful to record an acquisition image, so that the spectrum can unambiguously be identified with the target, e.g.:

TO> run acam 60

If no blind-offsetting is involved, this could be done after step 4 above, but otherwise it's probably best to leave it until after the science exposure, to avoid moving components in and out. Take an arc first though, if wavelength calibration is important.

Position of spectrum on the CCD
The x position of the spectrum on the CCD will be slightly different from the x position on the image. The difference dx (spectrum - image) in June 2009 was:

 x    400    520   630   1100   1600   1700

dx   -9.1  -13.1  -6.9   -1.9    7.5    8.4