The physical centres of the various imaging arrays on the LT are not necessarily aligned with the optical axis of the telescope. The LT's normal acquisition procedure is therefore to first place the telescope's nominal pointing centre on the target (i.e., "blind pointing") and then issue a "Focal Plane" command which offsets the centre of the instrument field-of-view onto the requested coordinates. This process may be subject to an absolute pointing error of around 10 arcseconds. While this is usually adequate for imaging, more precise acquisition is required for spectroscopy.
Target acquisition for spectroscopy may be achieved in two ways. Initially, an image of the target field is always obtained using the LT's work-horse wide-field optical imager (currently IO:O). That image is then used either to identify the brightest source in the field and to centre on that target, or to calibrate the pointing of the telescope by identifying stars in the field and fitting a world-coordinate system (WCS) to the image. Based on this WCS-fitting process, the telescope is offset to move the target position onto the spectrometer (for FRODOspec this is to within 2 arcsec of the centre of the fibre bundle). Two or three images may be used to fine-tune the telescope position before switching to spectroscopy mode and beginning the observation.
For more details see the FRODOspec instrument page. Note that this FINE TUNE acquisition process can in principle be used for any instrument, not just with the LT's spectrometers. However, this process increases the overheads on the project (by a few minutes) and should therefore only be used if telescope pointing at the ±2arcsec level is important.
Due to flexibility problems with the coolant pipes, we were forced to dispense with the practice of routing them through the cable wrap in the cassegrain axis rotator. For most observations the rotator is therefore set to one of the "cardinal" sky angles of 0, 90, 180 or 270 degrees. This means that images will be automatically rotated to one of these angles, the choice being the one that will give the longest possible uninterrupted observing time before reaching a mechanical rotator limit. It is possible that the sky angle will change during a (very) long series of exposures - but not during an exposure!
Specific control of field rotation is available for cases where the science requirements of the programme demand it, but in general we recommend leaving the rotator on its default automated setting.
Though observations at different epochs may be obtained at different sky orientations, the default choice of "cardinal" sky angles means that the overlap between repeated images of the same field is always maximized, which is important for programmes relying on secondary standards within the fields. The standard "North at the top" image display orientation is simple to achieve in an image viewer, using only 90 degree rotations.
Pointing below altitude 40 degrees
Occasionally the telescope does not point well below Alt ~ 40 degrees. This is due to a problem with the mirror support on one of the three sectors behind the mirror cell. Images can be obtained that are shifted by 30-40 arcsec. However, this problem does not affect telescope tracking or guiding, so the image quality itself should not be affected. If your science requires that a target be positioned on the same spot on the CCD each time it is observed, acquisition similar to what is used for spectroscopy can be used (as noted above). Please contact us for further details.