|Space Telescope Science Institute|
|COS Instrument Handbook|
In ACQ/IMAGE mode COS obtains an NUV image of the target field, moves the telescope to center the object, and obtains a second NUV image as confirmation. ACQ/IMAGE may use either the primary science aperture (PSA) or the bright object aperture (BOA) and either MIRRORA or MIRRORB. All four combinations are illustrated in Figure 8.2. Note the additional structure present in images obtained with MIRRORB and the BOA: The secondary image produced by MIRRORB is half the intensity of the primary image and is displaced by 20 pixels (about 0.5 arcsec) in the dispersion direction. The BOA produces a chevron-like image whose peak is displaced in both the dispersion and cross-dispersion directions. When the BOA is used with MIRRORB, two distorted peaks result. In this configuration, there is some overlap between the wings of the primary and secondary peaks, but they are well enough separated to allow for reliable acquisitions.An ACQ/IMAGE exposure consists of the following steps:
1. An exposure of the internal Pt-Ne lamp is obtained through the WCA aperture. The onboard COS Flight Software (FSW) sets the exposure time for the lamp exposure automatically. The centroid of the WCA image is calculated by the FSW. Using the known offset between the center of the WCA and the science aperture (PSA or BOA), the location of the center of the science aperture on the detector is computed.NUV images of point sources observed through the PSA (top) and BOA (bottom) using MIRRORA (left) and MIRRORB (right). The limits of each plot represent the 170 × 170 pixel image used by ACQ/IMAGE. Also shown are the COS aperture (blue circle of radius 1.25”) and the 9 × 9 checkbox used by ACQ/IMAGE. Histograms show the AD and XD profiles. The pointing is typical of that expected after an ACQ/SEARCH, but before additional peak-ups.
2. The shutter is opened and a TA image of the field is obtained. The telescope is not moved, meaning that an acquisition using ACQ/IMAGE will be successful only if the target lies within (or just outside of) the aperture. An area of 170 × 170 pixels, which corresponds to approximately 4 × 4 arcsec2, centered on the aperture, is read out. This image is recorded and downlinked and becomes part of the archived data package. (It is stored in the first extension of the _rawacq file.)
3. A 9 × 9 pixel checkbox array is then passed over the 170 × 170 pixel image. First, the checkbox with the most counts is identified. In the unlikely instance that two checkboxes have equal counts, the first one encountered is used. The brightest 9 × 9 array is then analyzed using a flux-weighted centroiding algorithm to calculate the target position.
4. Finally, HST is moved to place the calculated centroid at the center of the selected aperture. A second exposure, identical to the first, is taken and recorded for later downlink as a verification of the centering. (It is stored in the fourth extension of the _rawacq file.)