The sensitivity model for JWST's Mid-Infrared Instrument (MIRI) incorporates ground testing measurements to model parameters such as background, photon conversion efficiency, encircled energy, and detector performance.
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The performance of JWST has been measured directly at both the component and system level using the fully assembled MIRI flight model in a flight-like radiative environment with a well-characterized radiometric source (Glasse et al. 2015). The results of the JWST throughput measurements have been integrated into a sensitivity model that includes the following components: (1) background, (2) photon conversion efficiency (PCE), (3) encircled energy, and (4) detector performance (Pontoppidan 2016).
The values in the table and plots below were obtained from ETC 2.0.
The tables and figures below show point source sensitivity values for a 10 ksec (10,000 s) observation to S/N = 10.
Table 1. Minimum detectable flux densities for a S/N = 10 in 10 ksec for MIRI imaging filters assuming FULL array, assuming an unresolved point source.
|Filter||Low Background Detection|
Glasse, A., et al., 2015, PASP, 127, 686
The Mid-Infrared Instrument for the James Webb Space Telescope, IX: Predicted Sensitivity
Pontoppidan, K. 2016, Proc of SPIE, 9910, 16
Pandeia: a multi-mission exposure time calculator for JWST and WFIRST