3.3 Comparison of WFC3 with Other Imaging Instruments

3.3.1 Wavelength Coverage

The WFC3 UVIS channel is similar in design to the Wide Field Channel (WFC) of the ACS. There are, however, a few differences. While ACS/WFC is unable to detect wavelengths shorter than about 370 nm (i.e., shortward of the B band), WFC3/UVIS has excellent sensitivity extending down to 200 nm. The design trade-offs adopted to achieve this extended UV wavelength coverage (primarily the CCD coating and the use of aluminum coatings for the reflective optics) lead to a reduced sensitivity of WFC3 at longer optical wavelengths compared to that of ACS/WFC. WFC3/UVIS has no sensitivity in the far-UV region below 200 nm. The far-UV is covered by three MAMA detectors in ACS and STIS. 

As discussed in Section 3.3.5, both the UVIS and IR detectors have significant wavelength overlap with JWST's Near Infrared Camera (NIRCam) instrument. In Section 3.3.6, we discuss wavelength overlap with the Roman Space Telescope Wide Field Instrument (WFI). 

3.3.2 Field of View

Figure 3.1 illustrates the fields of view, at the same scale, for the HST imaging instruments onboard HST in 2024. Note that the pixel scale of the WFC3 UVIS channel is 20% finer in comparison to the ACS/WFC, obtained at the cost of covering only about 64% of the area of the ACS field of view.

Table 3.1 presents a comparison of the wavelength coverage, pixel scale, and field of view of WFC3 and of the other HST imaging instruments that are currently available.

3.3.3 Detector Performance

Table 3.2 summarizes the on-orbit measurements of read-out noise and dark current for the WFC3 detectors, and compares them with the parameters for the other currently available HST imaging detectors. Chapter 5 gives more detailed information about the detectors in both channels. Chapter 9 discusses sensitivities, limiting magnitudes, and exposure times.

Table 3.2: Characteristics of HST CCD and HgCdTe imaging detectors currently available.

¹ WFC3/IR read noise is for a 16-read linear fit. WFC3/IR double sampling read noise is 20.2–21.4 e^–.

3.3.4 System Throughputs and Discovery Efficiencies

Figure 3.2 plots the measured on-orbit system throughputs of the two WFC3 channels as functions of wavelength, compared to those of ACS, NICMOS, and WFPC2. These curves include the throughput of the OTA, all of the optical elements of the instruments themselves, and the sensitivities of the detectors. Throughputs were calculated at the central wavelength (the “pivot wavelength”; see footnote 3 in Table 6.2) of each wide-band filter of each instrument. 

As Figure 3.2 shows, WFC3 offers a unique combination of high sensitivity and wide spectral coverage ranging from the UV to the near-IR. WFC3 extends and complements, over a large field of view, the optical performance of ACS/WFC at wavelengths shorter than ~400 nm and longer than 1000 nm. The good degree of functional redundancy with ACS will help ensure that the unique scientific capabilities of HST, at optical wavelengths, will remain available until the end of its mission.

Another quantity that is useful when comparing different instruments, especially in the context of wide-angle surveys, is the “discovery efficiency,” defined as system throughput times area of the field of view as projected onto the sky. In Figure 3.3, the discovery efficiencies of the HST imaging instruments are plotted as a function of wavelength. Note that the y-axis is now logarithmic. This figure dramatically illustrates the enormous gains that WFC3 offers, compared to current HST instruments, both in the optical/UV below 400 nm, and in the near-IR.Finally, we present WFC3’s strengths by including detector noise and thus showing how its efficiency, wide wavelength coverage, and large field of view apply to general problems: the limiting point-source magnitude reached in 10 hours of observing time (Figure 3.4); and the time needed to survey a sky area about 9 times larger than the Hubble Ultra Deep Field, to a limiting ABMAG of 26 (Figure 3.5).

3.3.5 In Comparison with JWST/NIRCam

Although they have different capabilities, JWST/NIRCam has significant wavelength overlap with WFC3 in both UVIS and IR bandpasses. Here we compare the filter coverage of the two observatory instruments. Figure 3.6 plots the measured on-orbit system throughputs of the wide-band/long-pass filters for WFC3/UVIS channels as functions of wavelength, compared with two wide-band filters on NIRCam. UVIS works at shorter wavelengths than NIRCam but has less throughput at longer wavelengths. Their respective filter bandpasses are different in the central wavelength and span. Figure 3.7 plots the measured on-orbit system throughputs of the wide-band/long-pass filters for WFC3/IR channels as functions of wavelength, compared with four wide/medium-band filters on NIRCam. The WFC3/IR filters are generally broader and contain more overlap than the comparable NIRCam filters, except at the longest wavelengths. 

3.3.6 In Comparison with Roman/WFI

The Roman Space Telescope's Wide Field Instrument (WFI) is an imaging camera and slitless spectrometer with sensitivity from visible to near-infrared wavelengths. It has eight imaging filters with overlapping bandpasses spanning 0.48 to 2.3 µm. Figure 3.8 plots the measured on-orbit system throughputs of four wide-band/long-pass filters for WFC3/UVIS channels as functions of wavelength, compared with the F062 and F087 Roman/WFI filters. Meanwhile, Figure 3.9 plots the measured on-orbit system throughputs of three wide-band/long-pass filters for WFC3/IR channels as functions of wavelength, compared with four Roman/WFI filters: F087, F106, F129, and F158.