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Arsenic doped back illuminated blocked impurity band (BIBIB) silicondetectors have advanced near and mid-IR astronomy for over thirty years; theyhave high quantum efficiency (QE), especially at wavelengths longer than 10$\mu$m, and a large spectral range. Their radiation hardness is also an assetfor space based instruments. Three examples of Si:As BIBIB arrays are used inthe Mid-InfraRed Instrument (MIRI) of the James Webb Space Telescope (JWST),observing between 5 and 28 $\mu$m. In this paper, we analyze the parametersleading to high quantum efficiency (up to $\sim$ 60\%) for the MIRI devicesbetween 5 and 10 $\mu$m. We also model the cross-shaped artifact that was firstnoticed in the 5.7 and 7.8 $\mu$m Spitzer/IRAC images and has since also beenimaged at shorter wavelength ($\le 10~\mu$m) laboratory tests of the MIRIdetectors. The artifact is a result of internal reflective diffraction off thepixel-defining metallic contacts to the readout detector circuit. The lowabsorption in the arrays at the shorter wavelengths enables photons diffractedto wide angles to cross the detectors and substrates multiple times. This isrelated to similar behavior in other back illuminated solid-state detectorswith poor absorption, such as conventional CCDs operating near 1 $\mu$m. Weinvestigate the properties of the artifact and its dependence on the detectorarchitecture with a quantum-electrodynamic (QED) model of the probabilities ofvarious photon paths. Knowledge of the artifact properties will be especiallyimportant for observations with the MIRI LRS and MRS spectroscopic modes.

publications of the astronomical society of the pacific

The quantum efficiency and diffractive image artifacts of Si:As IBC  mid-IR detector arrays at 5 $-$ 10 $\mu$m: Implications for the JWST/MIRI  detectors