WFC3 Instrument Handbook for Cycle 25
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Wide Field Camera 3 Instrument Handbook for Cycle 25 > Chapter 7: IR Imaging with WFC3 > 7.6 IR Optical Performance

7.6
Following its alignment to the OTA (WFC3 ISR 2009-46), a series of observations through a variety of filters were obtained to demonstrate the WFC3 optical performance. The WFC3 IR channel meets or exceeds all image quality expectations. The following subsections summarize the measured flight optical performance for the IR channel, as described by its point-spread function (PSF), i.e., the spatial distribution of the flux in an image of a point source. The results shown are produced using an optical model which has been adjusted and correlated to the PSFs measured on-orbit and represent mean values averaged over the field. (See WFC3 ISR 2009-37.) This PSF model includes the pupil geometry, including the cold stop, residual aberration, the mid-frequency wavefront error of the OTA, the effect of the detector inter-pixel capacitive cross-talk, and first-order geometric distortion.
7.6.1 PSF Width and Sharpness
The IR channel PSFs are well approximated by Gaussian profiles (before pixelation). As was discussed in more detail for the UVIS channel in Section 6.6.1, the PSFs can usefully be characterized by their FWHM or their sharpness (effectively the reciprocal of the number of pixels occupied by a point source, as defined in Section 6.6.1). Table 7.5 lists the FWHM of the model PSF core (i.e., before pixelation) in units of pixel and arcsec and the sharpness parameter for 10 wavelengths. The sharpness range shown for each wavelength indicates the values for the PSF centered on the pixel corners and center. The monotonic increase in FWHM and decrease in sharpness with wavelength is due to diffraction.
Table 7.5: WFC3/IR PSF FWHM (pre-pixelation, in units of pixels and arcseconds), and sharpness, vs. wavelength. (Note that attempts to measure the FWHM by fitting functions to the pixelated PSF will generally give larger values.)
Figure 7.4 plots the azimuthally-averaged model OTA+WFC3 PSF at three different IR wavelengths., indicating the fractional PSF flux per pixel at radii from 1 pixel to 5 arcsec.
Figure 7.4: Azimuthally averaged WFC3/IR PSF.
7.6.2 Encircled and Ensquared Energy
As described in more detail in Section 6.6.2 for the UVIS channel, encircled energy, the fraction of light contained in a circular aperture, and ensquared energy, the fraction of energy falling within a certain number of pixels, are two other useful ways of characterizing well-behaved profiles.
Encircled-energy profiles for the IR channel at three representative wavelengths are plotted in Figure 7.5. The corresponding numerical values are presented in Table 7.6. The ensquared energy, which provides the flux per pixel, is presented in Table 7.7.
Figure 7.5: Encircled Energy for the WFC3/IR channel.
Table 7.6: WFC3/IR PSF Encircled Energy Fraction vs. Aperture Radius (arcsec).
Table 7.7: WFC3/IR PSF Ensquared Energy Fraction vs. Aperture size (pixels), where the target is centered on the aperture. Row 1 indicates the maximal (PSF centered on the pixel) peak pixel fraction, useful for determining the exposure time at which saturation may occur.
11
33
55
77
99
1111
1313
1515
1717
1919
2121
2323
2525
5151
101101
1
For the 22 aperture, the target is located at the center of the array.

During SMOV, high-dynamic-range isolated star images were obtained through several filters (WFC3 ISR 2009-37). These are shown with a logarithmic stretch in Figure 7.6. The images appear slightly elongated vertically, due to the 24 degree tilt of the detector to the chief ray and the fact that a distortion correction has not been applied. Although the target was chosen to be isolated, a number of field galaxies appear in both the F098M and the F160W filter images; these are also seen in long wavelength UVIS channel images of the same target (Figure 6.13). Some detector artifacts, including cold and warm pixels and imperfectly removed cosmic ray hits are evident.
Figure 7.6: High dynamic range WFC3/IR star images through F098M (left) and F160W (right) subtending ~20 arcsec on each side near field center. No distortion correction has been applied. Stretch is logarithmic from 10–3 to 103 e sec–1 pixel–1. Faint galaxies appear in the background.
7.6.3 Other PSF Behavior and Characteristics
Temporal Dependence of the PSF: HST Breathing
All HST observations are affected to some extent by short-term focus variations (“breathing”), which arise from the changing thermal environment of HST (See Section 6.6.3). For the IR channel, breathing is expected to produce variations of ~0.3% and less than 0.1% in the FWHM of the PSF of WFC3/IR at 700 nm and at wavelengths longer than 1100 nm, respectively, on typical time scales of one orbit.
Intra-Pixel Response
The response of a pixel of an IR detector to light from an unresolved source varies with the positioning of the source within the pixel due to low sensitivity at the pixel's edges and dead zones between pixels. For NICMOS, the intra-pixel sensitivity was found to be an important effect: it varies by as much as 40% (peak to valley). This effect has an impact on point sources which depends on the sampling, and therefore, for a given pixel scale, on the wavelength of the diffraction-limited images. Well-dithered exposures average out this effect, but photometric accuracy for stellar sources with few dither positions can be limited by uncertainties related to intra-pixel response.
For the WFC3/IR flight detector, no measurable intra-pixel sensitivity variation was found during ground testing (WFC3 ISR 2008-29) or in-flight testing (WFC3 ISR 2011-19). The smaller pixel size (18 m vs. 40 m) and the much higher WFC3/IR detector temperature (compared to NICMOS) are probably responsible for this improvement.
Inter-Pixel Capacitance
The small pixel size, relative to that in NICMOS, increases the relevance of capacitive coupling between nearby pixels (see Brown et. al., 2006, PASP, 118, 1443; Moore et. al., 2006, Opt. Eng., 076402). It affects the gain measurements and the PSF. The easiest method of estimating the inter-pixel capacitance is to measure the ratio of DNs in pixels adjacent to a “hot” (high-dark-current) pixel to the DNs in the hot pixel. In the WFC3 IR channel, on the order of 5% of electrons may leak to the adjacent pixels. WFC3 ISR 2008-26 describes a method for correcting inter-pixel capacitance using Fourier deconvolution, and demonstrates its effectiveness on WFC3/IR ground-testing data. WFC3 ISR 2011-10 provides an improved deconvolution kernel with distinct values for each of the 8 pixels surrounding the central pixel.
7.6.4 Supersampled PSF Models
The concept of empirical net (“effective”) models of PSFs is introduced in Section 6.6.4. The WFC3/IR PSF has recently been modeled in WFC3 ISR 2016-12 for five commonly used filters (F105W, F110W, F125W, F140W, and F160W).
Figure 7.7 shows a log image of the F105W PSF in supersampled (4x) pixels. The WFC3/IR PSF is extremely undersampled by the detector pixels: over 40 percent of a star's flux will land in its central pixel if the star is centered on that pixel. Only 4 percent will fall in the directly adjacent pixels. Even with this extreme undersampling, the 4x supersampled grid-base model is easily able to represent the PSF.
Figure 7.7: This is an image of the central WFC3/IR PSF for F105W. The PSF is supersampled by a factor of 4 relative to the WFC3/IR image pixels.
The white circles are drawn at r=5 and r=10 image pixels. The central label (43.4%) shows how much of the star's flux should be received by a pixel if the star happens to be centered on exactly that pixel. The label above it (6.7%) tells us what fraction of a star's flux would land in a pixel that is exactly one image-pixel above the center of the star. The 0.8% label tells us how much light would land in a pixel two up from the center of a star. The other labels show the fraction of light that lands in pixels at various other locations in the PSF: on inner-halo bumps (0.2%), on diffraction spikes at a distance of ~5 image pixels (0.1%), in the outer PSF halo at ~5 image pixels (0.02%) and in the outer halo at ~7.5 image pixels (0.003%).
Figure 7.8 shows how the WFC3/IR PSF varies across the face of the 1014x1014 pixel detector. A 3x3 array of models is adequate to represent the PSF across the detector.
Figure 7.8: For 9 locations on the detector in a 3x3 grid, a greyscale image shows the difference between each supersampled PSF and the average of the PSFs. Dark represents more flux, and light less flux. The largest variation is about 0.04, which is about 10% of the central value of the PSF.
As mentioned in Section 6.6.4, the flt-frames provide the only clean constraints on the scene. Our high-precision PSF models are designed to be used in this frame, even though dithering and distortion make such analysis complicated. The WFC3 instrument team is working to produce some tools that can help users make use of these PSFs. WFC3 ISR 2016-12 contains some FORTRAN routines that show how to use the PSFs, but higher-level tools are also under development.

Wide Field Camera 3 Instrument Handbook for Cycle 25 > Chapter 7: IR Imaging with WFC3 > 7.6 IR Optical Performance

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