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ACS Instrument Handbook Cycle 23
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Advanced Camera for Surveys Instrument Handbook for Cycle 23 > Chapter 8: Overheads and Orbit-Time Determination > 8.2 ACS Exposure Overheads

8.2
 
Exposure overheads are summarized in Table 8.1 and Table 8.2. All numbers given are approximate; they do not make detailed differentiations between overheads for different ACS modes and configurations. These overhead times are to be used (in conjunction with the actual exposure times and the instructions in the HST Primer to estimate the total number of orbits for your proposal. After your HST proposal is accepted, you will be asked to submit a Phase II proposal to support scheduling of your approved observations. At that time you will be presented with actual, up-to-date overheads by the APT scheduling software. Allowing sufficient time for overhead in your Phase I proposal is important; additional time to cover unplanned overhead will not be granted later.
The following list presents important points for each type of overhead:
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Table 8.1: Science Exposure Overheads: General
Table 8.2: ACS Science Exposure Overhead Times (Minutes)
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Note that exposures with identical observing modes are automatically generated if the observer specifies:
Phase 2 proposal optional parameter CR-SPLIT with a value greater than or equal to 2. (The default value is CR-SPLIT=2 if the Phase 2 exposure log sheet field Number_of_Iterations is at its default value of 1.)
Phase 2 exposure log sheet field Number_of_Iterations is greater than or equal to 2 (where CR-SPLIT must be set to “NO”.)
Phase 2 special requirement PATTERN is used to execute a dither pattern. In this instance, overheads will also include slew overheads.
The overhead time for serial buffer dumps arises, in certain cases, from the overheads associated with the onboard data management and switching over the cameras. The onboard buffer memory has the capacity of a single full-frame WFC image. The next WFC image can be placed into the buffer only after the buffer has dumped the previous image, which takes 349 seconds.
Sequences of many short SBC exposures can also lead to serial dumps when the buffer becomes full. In this case the buffer dump time becomes an overhead to be included into the orbit time budget. This overhead can severely constrain the number of short exposures one can squeeze into an orbit. Subarrays can be used to lower the data volume for some applications.
8.2.1 Subarrays
At the end of each exposure, data are read out into ACS’s internal buffer memory where they are stored until they are dumped into HST’s solid state data recorder. The ACS internal buffer memory holds 34 MB or the equivalent of 1 full WFC frame, or 16 SBC frames. Thus, after observing a full WFC frame, the internal buffer memory must be dumped before the next exposure can be taken. The buffer dump takes 349 seconds and may not occur while ACS is being actively commanded. Of this time, 337 seconds is spent dumping the image. The buffer dump cannot be done during the next exposure if the latter is shorter than 337 seconds. If, however, the next exposure is less than 337 seconds the buffer dump will create an extra 5.8 minutes of overhead.
If your science program is such that a smaller FOV can be used, then one way of reducing the frequency and hence overheads associated with buffer dumps is to use WFC subarrays. During subarray readouts, only the selected region of the detector is stored in the buffer, and many more frames can be stored before requiring a buffer dump: four 2K-frames; sixteen 1K-frames; or sixty-four 512-frames. Using subarrays also modifies the readout duration, which for 2K subarray exceeds the full-frame readout. The Astronomer's Proposal Tool currently assesses exposure overheads for each readout mode as: 512=73sec; 1K=106sec; 2K=188sec; and full-frame=138sec.

Advanced Camera for Surveys Instrument Handbook for Cycle 23 > Chapter 8: Overheads and Orbit-Time Determination > 8.2 ACS Exposure Overheads

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