|WFC3 Instrument Handbook for Cycle 25|
6.7.1 Exposure TimeExposure times in the UVIS channel are controlled by a rotating mechanical shutter blade (see Section 2.3.3). The time per UVIS exposure must be between 0.5 s and 3600 s, excluding 0.6 s, in steps of 0.1 s.1 Pre-flight testing has verified that shutter exposure times deviate by less than 1% for exposure times of 0.5 s, as well as those greater than or equal to 1 s. For example, typical variations of 4 ms were measured in a set of 1 s exposures. For exposure times between 0.7 s and 0.9 s (inclusive), exposure-time deviations were measured to be 2.6% (see WFC3 ISR 2004-14). On-orbit observations have shown that the shutter fails to meet the repeatability requirement of 0.01 sec (WFC3 ISR 2009-25).The shutter uniformity requirement specifies that any differences in exposure time across the field of view must be <0.01 s. Comparisons of long (30 s) and short (0.5 s) exposures taken during instrument-level ground tests have shown that the shutter provides a uniform exposure time across the field of view to ~0.004 s, easily meeting the requirement. In on-orbit internal tungsten lamp exposures, the exposure time across the field was found to vary by less than 0.0009 sec (WFC3 ISR 2009-25). In tungsten lamp exposures and observations of a standard star made from Oct. 2014 to Aug. 2015, no noticeable difference was seen in the performance of the shutter (WFC3 ISR 2015-12). (Note that the point spread function will be affected by shutter-induced vibration in short exposures; see Section 6.11.4.)To allow for cosmic-ray removal during post-observation data processing, UVIS exposures can be split into multiple exposures. The Optional Parameter CR-SPLIT in the Phase II observing proposal can be used to equally divide the original exposure time into the specified number of subexposures (the default is NO, with option to select 2 to 8 subexposures). Note that the default value of CR-SPLIT was changed from 2 to NO in Cycle 18, because combining dithered exposures with DrizzlePac is generally the preferred method of removing cosmic rays. (See Section 6.12.1.)If CR-SPLIT is requested, the exposure time is first divided by the requested number of subexposures and the subexposure times are rounded down to the nearest multiple of 0.1 s. At the end of this process, if the resulting subexposure times are not legal values, the proposal software adjusts them so that they are allowed and reports those changes to the observer.6.7.2 ACCUM Mode“ACCUM” is the only observing mode for the UVIS channel. In ACCUM mode, the shutter is opened and photons strike the CCDs and generate charge, which is accumulated until the shutter is closed at the end of the requested exposure time and the charge is read out. During the readout, the analog-to-digital (A-to-D) converter translates the charge into data numbers (DN) via the gain setting. There are four gain settings (1.0, 1.5, 2.0, and 4.0 e−/DN) that are possible in principle. However, the only gain setting offered to observers is the default value of 1.5 e−/DN, which provides gain 1.55 e-/DN (Table 5.1).A full detector readout of both UVIS chips takes 96 s. The image contains all the exposed pixels from each CCD (2 times 2051×4096), as well as a variety of overscan pixels, described in more detail later in this section. Shorter readout times are possible by using smaller subarray readout sizes, as discussed in more detail in Section 6.4.4.Each of the two CCD chips contains two on-chip amplifiers used for reading out. The fastest—and default—way to read out the entire detector, at full spatial resolution, is to use all four amplifiers simultaneously. Other full-detector readout modes are possible but take more time and involve more charge transfer shifts. For example, two amplifier full frame readout takes more than twice as long as a four-amplifier readout (~193 s vs. 96 s). Non-default readout modes are not offered to General Observers.Subarray frames, unlike full detector frames, are read out by a single amplifier (the closest amplifier to the subarray center).The UVIS CCD detectors each have 4096×2051 pixels that are exposed to light. In addition, both chips have 25 extra columns at both ends that are not exposed to light; these 25 columns are physical overscan pixels. Moreover, during readout of the chips, extra pixels can be clocked in order to create virtual overscan pixels.The location of the overscan regions in a raw image varies, depending upon the type of readout that is performed. The overscan regions are used to monitor the instrument, and are needed to measure the bias level. The bias level is subtracted from the raw image, normally through the BLEVCORR step in the WFC3 calibration pipeline (see Section E and Section 3.2.2 of the WFC3 Data Handbook).Figure 6.16 shows the format of a raw image obtained with full-chip unbinned four-amplifier readout. The raw image has 25 columns of physical overscan pixels and two areas of virtual overscan: 60 columns of serial overscan in the center of each row and 38 rows (19 per chip) of parallel overscan next to the inter-chip gap. The serial physical overscan pixels are also known as the serial prescan, or leading-edge, overscan; the serial virtual overscan pixels are also called the trailing-edge pixels.Figure 6.16: Format of a Raw Full-Chip WFC3 UVIS Image.As Figure 6.16 illustrates, a raw image resulting from a default full-frame, four-amplifier readout of the UVIS channel contains 110 columns of serial overscan (25×2 physical and 30×2 virtual) plus 38 rows of parallel virtual overscan, which combined with the 4096×2051 science pixels, result in a raw image size of 4206×4140 pixels. Other types of readouts have differing amounts and/or locations of overscan. Subarrays contain no virtual overscan of either type (serial or parallel), although they can contain physical overscan if a subarray is chosen that overlaps the physical overscan region. Subarrays containing physical overscan data are listed in Table 6.1. In general, it is desirable to include some physical overscan in observations using subarrays for accurate bias level subtraction.Exposures taken with on-chip binning are complicated by the need to truncate “odd” pixels and to treat each half of the chip’s row separately. Also, due to the odd number of some overscan pixels, the boundary between the data and overscan pixels of a binned exposure can contain binned pixels resulting from a combination of both data and overscan pixels. A 2×2 binned frame readout, for example, contains 2070 rows × 2102 columns. That is, each binned chip readout has 1035 rows (9 binned virtual overscan + 1 combined data/virtual parallel overscan + 1025 data) and each binned chip readout contains 2102 columns (12 physical overscan + 1 combined data/overscan + 1023 columns of data + 1 combined data/virtual overscan column + 14 virtual overscan pixels for each of the two amps in a chip). A 3×3 binned image contains 1402×1380 pixels (8 overscan + 1 combined overscan/data + 682 data + 10 overscan columns in each amplifier of each chip and 6 overscan + 1 combined overscan/data + 688 data rows in each chip).For completeness, we mention here that WFC3 can also be commanded to take EPER (extended pixel edge response) readouts. This capability is intended for calibration/engineering purposes only. The EPER images are a way to measure and monitor charge transfer inefficiency (CTI) effects using internal images, rather than external, pointed observations that would take HST observing time away from science observations. The EPER frame starts with an internal tungsten lamp flat field; any CTI present causes a fraction of charge from that flat field to be captured temporarily in traps. As the frame is read out, the trapped charge escapes and can appear in the overscan regions as an exponential tail of deferred charge. The EPER readout includes significantly larger areas of overscan so that the full extent of the exponential tail can be measured, ideally down to where it becomes indistinguishable from the nominal noise level of the detector. That is, the EPER image allows direct measurement of the charge losses during the readout since nearly all the lost electrons are expected to appear in the exponential tail.Under normal shutter operations, the 0.5 s exposure would not provide a sufficiently uniform exposure level. However, it has been implemented through a special “continuous sweep” operation, where the shutter disk moves smoothly through 180°, from one closed position to the next, thus meeting the uniformity requirement. All exposures longer than 0.5 s are obtained via pairs of closed-to-open and open-to-closed commands.