In several papers, I have designed, utilized, and characterized my double PSF-fitting for various instruments and science cases. Currently, my code is being used across seven JWST and HST instruments: NIRCam, NIRISS, MIRI, ACS/WFC, WFC3/IR, WFC3/UVIS, and WFPC2/PC. It is being used to identify: 1) stellar and sub-stellar binary systems both in star-forming regions and the solar neighborhood, 2) search for Jupiter mass companions to white dwarfs, and 3) directly image gas giant companions to stars in young star-forming regions. In each of the following images, the left panel is a cutout from the data, the middle panel is the empirical PSF model, and the right panel is the residual. To date, the sensitivity of my technique has been characterized with rigorous injection and retrieval analyses, showing the ability to resolve between 0.5-1λ/D given sufficient signal for NIRCam, ACS/WFC, and WFC3/IR. Current programs are characterizing the sensitivity of MIRI, WFC3/UVIS, and WFPC2/PC with the expectation of publication of all three in 2026.

JWST/NIRCam:

JWST/NIRISS:

JWST/MIRI:

HST ACS/WFC:

HST WFC3/IR:

HST WFC3/UVIS:

HST WFPC2/PC: