The data for "Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of aCen A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis"

This repository provides the results of PSF injection-recovery tests performed on three epochs of JWST/MIRI F1550C coronagraphic observations of Alpha Centauri A to characterize our sensitivity to point sources. Two types of products are made available. (1) Point source flux sensitivity at each separation and position angle of PSF injection-recovery for each epoch. The IR_<EPOCH>_<SENSE_TYPE>.csv files record the flux of a point source in mJy detectable at signal-to-noise ratio (S/N) = 5 or at a Gaussian significance level of 5sigma (SENSE_TYPE) at each separation (arcsec) and position angle (East of North in degrees) with respect to Alpha Centauri A for the August 2024, February 2025, and April 2025 observations (EPOCH). There are (separation, position angle) combinations where no flux sensitivity is reported for reasons discussed in Section 7.2 in Sanghi & Beichman et al. (2025). The 1D contrast curves in Figure 20 of the paper, for each epoch, can be reproduced by computing the median and minimum flux sensitivity azimuthally at each separation from these files. (2) Interpolated 2D sensitivity maps for each epoch. The 2D_map_<SENSE_TYPE>_<EPOCH>.fits files store the interpolated 2D flux sensitivity maps generated for each epoch using the data in the above csv files, see Section 7.2 in Sanghi & Beichman et al. (2025). The maps are centered on Alpha Cen A, oriented North up and East left, and the pixel scale is identical to that of the MIRI detector (1 pixel = 0.11 arcsec). Similar to the csv files, these maps show the flux of a point source in mJy detectable at signal-to-noise ratio (S/N) = 5 or at a Gaussian significance level of 5sigma (SENSE_TYPE) in the vicinity of Alpha Centauri A for the August 2024, February 2025, and April 2025 observations (EPOCH). The "combined_mininum" map presents the minimum flux sensitivity achieved across all three observation epochs. For research that benefits from this compilation, please cite Sanghi & Beichman et al. (2025).