9.2	The WFC3 Exposure Time Calculator (ETC)

In most cases, you will find it convenient to use the online WFC3 Exposure Time Calculator (ETC) to make estimates of the required exposure times for your project. The ETC is available from the WFC3 Web site at:

http://www.stsci.edu/hst/wfc3/tools/etcs/

The ETC calculates counts (e−) and count rates (e−/s) for given source and background parameters and assumed characteristics of the detectors. Once these are entered, the ETC then outputs signal-to-noise (S/N) ratios achieved for a given exposure time, or the exposure times required to achieve a given S/N ratio. The ETC supports both direct-imaging and spectroscopic (grism) observations. The aXeSIM tool is also available for simulation of grism observations (see Section 8.4). A variety of extraction apertures may be assumed in the ETC, both circular and square, allowing the user to select either a radius in arcseconds or a size in pixels. It is also possible to input a calibrated spectral-energy distribution (SED) of your source directly into the ETC. The ETC also outputs peak per-pixel count rates and total count rates, to aid in feasibility assessment. Warnings will appear if the source will saturate the detector, which would not only compromise CCD and IR observations, but might even affect subsequent exposures with the IR channel (see Appendix D:Bright-Object Constraints and Image Persistence). The ETC has online help for its execution and interpretation of results.

There are some items worth noting:

•	For the UVIS channel, the ETC uses a CCD full-well value of 63,000 e–, the minimum value for either CCD chip, to determine saturation; users wishing to strictly avoid this occurrence should allow a buffer of at least 10% below this. (See Section 5.4.5 for a detailed discussion of saturation.)

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For the UVIS channel, one should select Detector chip 2 for UV filter exposures and, to the extent possible, place the target on chip 2 (e.g., aperture UVIS2 in Figure 6.1 or the subarray apertures in the lower left quadrant of Figure 6.2) since chip 2 has better quantum efficiency than chip 1. (See Figure 5.2.)

•	Background added to UVIS exposures by using the post-flash option (Section 6.9.2) is not included in the ETC. See Section 9.6 for equations that show how the post-flash background affects the calculation of S/N and exposure time.

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For the IR channel, when the # of Frames = 1, the ETC assumes a complete timing sequence (NSAMP = 15). For smaller NSAMP, the read noise is greater. (See Section 5.7.3.) For most programs, NSAMP should be greater than 5 for individual exposures, and larger if possible, to provide the best readnoise and best protection against cosmic rays. (See Section 7.10.3.)

It is also possible to use synphot in STSDAS to calculate count rates and the wavelength distribution of detected counts.

The remaining sections of this chapter give detailed information on the sensitivities of the UVIS and IR channels when combined with the various spectral elements, and the use of this information in the determination of count rates, for those who wish to understand the subject in depth.