Following the alignment of WFC3 to the OTA (WFC3 ISR 2009-45
), a series of observations through a variety of filters were obtained to demonstrate the WFC3 optical performance (WFC3 ISR 2009-38)
. The WFC3 UVIS channel is meeting or exceeding all image quality specifications. Analysis of repeat observations in March 2010 and November 2011 has shown that the PSF has remained stable over time within a radius of 6 arcsec (WFC3 ISR 2013-13
The following subsections summarize the measured flight optical performance for
the UVIS 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 2009-38
.) This PSF model includes the pupil geometry, residual aberration, the mid-frequency wavefront error of the OTA, the effect of the detector charge diffusion, and first-order geometric distortion.
The PSFs over most of the UVIS wavelength range are well described by gaussian
profiles (before pixelation). Two simple metrics of the size of the PSFs are the full width half maximum (FWHM) and the sharpness, defined as
is the fraction of the flux from a point source in pixel i
. Sharpness measures the reciprocal of the number of pixels that the PSF “occupies,” and can be used to determine the number of pixels for optimal photometric extraction.
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 degradation in image width and other performance measures in the near UV is due predominantly to the OTA mid-frequency, zonal polishing errors, which effectively move power from image core into progressively wider and stronger non-gaussian wings as wavelength decreases.
plots the azimuthally-averaged model OTA+WFC3 PSF at three different UVIS wavelengths, indicating the fractional PSF flux per pixel at radii from 1 pixel to 5 arcsec.
The encircled energy
is the fraction of the total light from a point source that is contained within a circular aperture of a given radius. Since detectors have nominally square pixels, it is often more convenient to evaluate the energy falling within a certain number of pixels (“ensquared energy”
) instead of the encircled energy, which requires interpolation to account for the fractional pixels intercepted by a circular aperture. Correlated model encircled and ensquared energy values are presented in Tables 6.8
respectively. Encircled energies are plotted in Figure 6.11
for 200, 400, and 800 nm.
Short term variations in the focus of HST
occur and affect all of the data obtained from all of the instruments on HST
. A variety of terms, “OTA breathing”, “HST
breathing”, “focus breathing”, or simply “breathing” all refer to the same physical behavior. The focus changes are attributed to the contraction/expansion of the OTA due to thermal variations during an orbital period. Thermally induced HST
focus variations also depend on the thermal history of the telescope. For example, after a telescope slew, the telescope temperature variation exhibits the regular orbital component plus a component associated with the change in telescope attitude. The focus changes due to telescope attitude are complicated functions of Sun angle and telescope roll. More information and models can be found on the “HST
Thermal Focus Modeling” website at:
For WFC3, breathing induces small temporal variations in the UVIS PSF (WFC3 ISR 2012-14
). The variations of the UVIS PSF FWHM are expected to be as large as 8% at 200 nm, 3% at 400 nm and 0.3% at 800 nm, on typical time scales of one orbit. Some variation over the field of the PSF response to breathing is also expected, since the detector surface is not perfectly matched to the focal surface, and the optical design includes some field-dependent aberration. This field dependence has been analyzed using observations of a globular cluster with filter F606W (WFC3 ISR 2013-11
) and deep observations of an isolated star with filter F275W (WFC3 ISR 2013-13
). PSFs near the A amplifier on UVIS1 are noticeably elongated by astigmatism.
The point-spread function (PSF) is the distribution of light from a point source as
spread over a number of pixels. Even with a very compact optical PSF, however, charge diffusion, or migration of charge from one pixel into adjacent neighbor pixels, can degrade the sharpness of a CCD PSF. The effect is usually described in terms of the pixel response function (PRF), which maps the response of the detector to light from a hypothetical very sharp PSF whose light all falls within an individual pixel. Observations using the integrated WFC3 instrument along with optical stimulus point-sources provided empirical PSFs for comparison with, and to provide constraints for, the models. Those models, which included an independent assessment of the low-order wavefront error, the pupil mask, and a reasonable estimate of the detector PRF, yield good agreement with the observed instrumental encircled-energy curves. The resulting best empirical fit to the pixel response convolution kernel is shown in Figure 6.12
The PSF of the UVIS channel was assessed during SMOV. As part of this
assessment exposures of a field containing unsaturated data (highlighting the bright PSF core) were combined with highly saturated data (emphasizing the faint PSF wings). The results are illustrated in Figure 6.13
, which shows the select portions of the composite image with a logarithmic stretch. No geometric distortion correction has been applied, so the images appear elongated along the diagonal, due to the 21 degree tilt of the detector to the chief ray. Although the target was chosen to be isolated, a number of field galaxies appear in the F625W image (right) but are absent in the F275W image; these galaxies are also seen in the IR channel images of the same target (Figure 7.6
). Some detector artifacts, including warm pixels and imperfectly removed cosmic ray hits are evident.
Figure 6.13: High dynamic range composite UVIS star images through F275W
(left) and F625W (right) subtending ~20 arcsec on each side at different locations in the field. No distortion correction has been applied. Stretch is logarithmic from 1 to 106
/pixel. (See text below for description of “ghost” artifacts.)
Two different types of “ghost” artifacts are visible in the images. As expected from
the UVIS channel design, there are low-level ghosts due to reflections between the four surfaces of the two anti-reflection-coated detector windows: these are the sets of relatively large diameter, ring-shaped ghosts seen extending out at PA ~330°
(left panel) and PA ~30°
(right panel) for N up and E to the right. Ghosts due to reflections from the CCD to the windows, as discussed above in Section 6.5.3
, fall further from the PSF, along the diagonal from lower right to upper left of the field of view, and are not visible in these frames which image only subsections of the WFC3 field of view.
Also evident is a filter ghost, due to reflections between the surfaces of the F625W
filter (right). In multi-substrate filters (a stack of two or more substrates bonded or laminated together with a layer of optical adhesive) filter ghosts appear as faint, point-like features, such as the ghost at PA ~65 degrees, radius 1.6 arcsec, in the F625W image, which contains much less than 0.1% of the stellar flux. In single-substrate or air-gap filters (the latter consisting of two substrates joined via thin spacers), filter ghosts appear as small extended shapes (typically rings), closer to the PSF centers than the window ghosts. For the F275W image in Figure 6.13
the filter ghost level is <0.1% and is not obvious. A small number of filters exhibit brighter ghosts and are discussed in detail in Section 6.5.3
and are tabulated in Table 6.6