# The M4 Core Project with HST -- V. Characterizing the PSFs of WFC3/UVIS by Focus

## TL;DR

This study characterizes the PSFs of HST's WFC3/UVIS across focus variations, enabling improved astrometric measurements and detection of dark companions in globular cluster M4.

## Contribution

We developed a focus-diverse set of PSFs and demonstrated that focus optimization significantly improves star fitting and astrometric accuracy.

## Key findings

- Most PSFs lie along a focus-related one-dimensional locus.
- Five medium-bright stars suffice to determine exposure focus.
- Focus-optimized PSFs outperform library PSFs in star fitting.

## Abstract

As part of the astrometric Hubble Space Telescope (HST) large program GO-12911, we conduct an in-depth study to characterize the point spread function (PSF) of the Uv-VISual channel (UVIS) of the Wide Field Camera 3 (WFC3), as a necessary step to achieve the astrometric goals of the program. We extracted a PSF from each of the 589 deep exposures taken through the F467M filter over the course of a year and find that the vast majority of the PSFs lie along a one-dimensional locus that stretches continuously from one side of focus, through optimal focus, to the other side of focus. We constructed a focus-diverse set of PSFs and find that with only five medium-bright stars in an exposure it is possible to pin down the focus level of that exposure. We show that the focus-optimized PSF does a considerably better job fitting stars than the average "library" PSF, especially when the PSF is out of focus. The fluxes and positions are significantly improved over the "library" PSF treatment. These results are beneficial for a much broader range of scientific applications than simply the program at hand, but the immediate use of these PSFs will enable us to search for astrometric wobble in the bright stars in the core of the globular cluster M4, which would indicate a dark, high-mass companion, such as a white dwarf, neutron star, or black hole.