The James Webb Space Telescope Absolute Flux Calibration. II. Mid-infrared Instrument Imaging and Coronagraphy

• Published in: The Astronomical journal 2025-01, Vol.169 (1), p.6
• Main Authors: Gordon, Karl D., Sloan, G. C., Garcia Marin, Macarena, Libralato, Mattia, Rieke, George, Aguilar, Jonathan A., Bohlin, Ralph, Cracraft, Misty, Decleir, Marjorie, Gaspar, Andras, Kendrew, Sarah, Law, David R., Noriega-Crespo, Alberto, Regan, Michael
• Format: Article
• Language: English
• Subjects: Apertures; Astronomical models; Atmospheric correction; Calibration; Fluctuations; Flux calibration; Flux density; Infrared imaging; Infrared instruments; Infrared photometry; Infrared stars; Infrared telescopes; James Webb Space Telescope; Point spread functions; Scattering; Space telescopes; Stars; Stellar atmospheres; Stellar models; Time constant; Time dependence; Time measurement; Uncertainty; Wavelengths
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/ad8cd4

The absolute flux calibration of the Mid-Infrared Instrument imaging and coronagraphy is based on observations of multiple stars taken during the first 2.5 yr of James Webb Space Telescope operations. The observations were designed to ensure that the flux calibration is valid for a range of flux densities, different subarrays, and different types of stars. The flux calibration was measured by combining observed aperture photometry corrected to infinite aperture with predictions based on previous observations and models of stellar atmospheres. A subset of these observations was combined with model point-spread functions to measure the corrections to infinite aperture. Variations in the calibration factor with time, flux density, background level, type of star, subarray, integration time, rate, and well depth were investigated, and the only significant variations were with time and subarray. Observations of the same star taken approximately every month revealed a modest time-dependent response loss seen mainly at the longest wavelengths. This loss is well characterized by a decaying exponential with a time constant of ∼200 days. After correcting for the response loss, the band-dependent scatter around the corrected average (i.e., repeatability) was found to range from 0.1% to 1.2%. Signals in observations taken with different subarrays can be lower by up to 3.4% compared to FULL frame. After correcting for the time and subarray dependencies, the scatter in the calibration factors measured for individual stars ranges from 1% to 4% depending on the band. The formal uncertainties on the flux calibration averaged for all observations are 0.3%–1.0%, with longer-wavelength bands generally having larger uncertainties.