|Space Telescope Science Institute|
|WFC3 Instrument Handbook|
5.5.1 OverviewThe infrared channel of WFC3 employs a low-noise, high-QE, 1024×1024 pixel HgCdTe array manufactured by Teledyne Imaging Sensors (formerly Rockwell Science Center). The detector area sensitive to light is 1014×1014 pixels. Active cooling by a six-stage thermoelectric cooler (TEC) keeps the detector at a nominal operating temperature of 145 K. Although the IR detector is sensitive between 400 and 1700 nm, the detector coating is optimized for wavelengths longward of ~1000 nm, where the QE reaches its peak (Figure 5.18). The IR channel filter set is also limited to wavelengths above 900 nm, making the IR channel complementary to the UVIS channel.Compared to CCD detectors, IR detectors like the one used in the WFC3 IR channel have higher read noise and dark current. Unlike CCDs, however, IR detectors allow the accumulated signal in each pixel to be measured non-destructively multiple times. The capability to sample the signal multiple times during the integration can be exploited to reduce the effective read-out noise significantly. IR exposures are called “ramps” due to this capability to sequentially read the detector as signal accumulates. IR detectors are also immune to the charge bleeding exhibited by CCDs at high signal levels. Saturation is still a concern, however, because pixels subject to the highest signal levels show higher dark-current rates (“image persistence” or afterglow) in subsequent exposures (WFC3 ISR 2010-17). (See Section 7.9.4 for the on-orbit characterization of persistence on the WFC3/IR detector and Appendix D:Bright-Object Constraints and Image Persistence for discussion of planning observations to minimize the impact of persistence.)The capability of multiple readouts and the absence of bleeding makes IR detectors capable of very high dynamic-range observations. Non-destructive readouts also allow for the recovery of pixels affected by cosmic rays (CRs), because CR hits can be recognized and removed between adjacent reads. Unlike CCDs, IR detectors also show minimal long-term on-orbit CTE degradation, because they do not employ the charge transfer mechanism used in CCDs. IR detectors, however, are intrinsically non-linear. Nevertheless, at low and intermediate signal levels, the departure from linearity is quite modest and can be well calibrated by a low-order polynomial fit, whose parameters can in principle be determined for each pixel.5.5.2 IR Detector BasicsIn this section, we briefly describe the operational principles of the WFC3/IR detector. Figure 5.13 (adapted from McLean 1997, Electronic Imaging in Astronomy: Detectors and Instrumentation) shows the basic physical structure of the photovoltaic HgCdTe detector used in WFC3.Figure 5.13: Cross-section of a WFC3-IR detector (not to scale).Infrared detectors used in astronomy today are basically two-dimensional arrays of p-n junctions working as photodetectors (photodiodes). In a p-n junction, negative charges migrate from the n-type doped material to saturate the unmatched covalent bonds of the adjacent p-type material. The displaced carriers establish an electric field across the junction, setting up an intermediate region depleted of free carriers. The depletion region is therefore both charged and highly resistive. The strength of the electric field and the size of the depletion region may be increased by applying an external electric field (“negative bias”). This biasing corresponds to the initial RESET applied at the beginning of the integration. When an incident IR photon is absorbed by the photosensitive material, it creates a free electron-hole pair. The two photo-generated charges drift in the material and would eventually recombine. However, if the mobility of the charge carrier (a hole in an n-type material) is high enough, it will reach the depletion region before recombining and be swept to the other side of the junction by the electric field. There, in the p-type region, it will recombine with one of the electrons of the ionized holes, causing a reduction of the voltage across the junction. This change of voltage can be measured and, being proportional to the number of photo-generated charges, provides a direct measure of the photons captured on each pixel.In the case of the WFC3 IR detector, the photosensitive material is made of HgCdTe grown with a molecular beam epitaxial (MBE) process on a ZnCdTe substrate. The fraction (stoichiometric ratio) of Hg vs. Cd controls the long-wavelength cutoff of the material, whereas the doping material (As for the p-type, In for the n-type) creates the p-n junction. The MBE growth process is different from that used in the NICMOS detectors on HST, in which the HgCdTe was grown on sapphire in a liquid phase (PACE process). MBE growth on a ZnCdTe substrate is expected to provide a better lattice match to HgCdTe than sapphire, creating fewer defects and charge traps at the interface between the two materials. The MBE growth process is followed by the processing phase, in which the implants and contacts of each pixel are manufactured.As usual with IR arrays, the readout circuitry is made on a separate CMOS chip (multiplexer or MUX), which is eventually hybridized to the detector with an indium contact for each pixel (see Figure 5.14). After the two chips have been hybridized, the ZnCdTe substrate is removed to reduce the susceptibility of the device to cosmic-ray events and to increase the sensitivity at short wavelengths. The final chip therefore is a CMOS device connected through indium columns to a thin layer of HgCdTe photosensitive material.In the MUX, each pixel has its own dedicated readout circuitry (unit cell). In particular, the voltage change across the p-n junction is monitored by a field-effect transistor (FET) configured as a source-follower amplifier, which has gain of 1 and effectively decouples the detection process from the noisy readout circuitry. Two other FETs connect the pixel to the reset voltage and the output line. Figure 5.15 shows the equivalent circuit diagram for the WFC3 detector unit cell. Each WFC3 IR unit cell contains three transistors. For comparison, the NICMOS detectors have four transistors, whereas the latest generation of Hawaii-2RG detectors for JWST has seven transistors per unit cell. A higher number of transistors increases the versatility of the device. For example, on the NICMOS detectors it is possible to reset each individual cell, whereas on WFC3 detectors the reset is sent simultaneously to all cells on the same row. Note that since there are no potential barriers between pixels, pixels do not spill charges into nearby pixels when they reach a certain level (“blooming full well”) of accumulated charges, as in typical multiphase CCDs. Therefore, IR detectors do not show “bleeding” along columns. Moreover, due to individual readout, bad pixels do not block the rest of the column as they do in a CCD.Figure 5.15: Equivalent circuit diagram of the WFC3/IR unit cell.