The low mass end of the Initial Mass Function (IMF) is a component of star formation that is not well understood. By analyzing Hubble Space Telescope (HST) images of star-forming regions, we aimed to provide data to constrain the shape of the low-mass IMF. We performed point-spread function (PSF) fitting using the Astropy Photutils package v0.6 on shallow HST Wide Field Camera 3 images taken in filters F110W, F139M, and F160W with the goal of identifying low mass stars and brown dwarfs. Residual images from our PSF fitting routine showed that fainter sources were effectively fit while fits to the brighter sources left residuals. Despite this, analysis confirmed that our PSF magnitudes are consistent with aperture magnitudes and mostly have smaller errors; 85%–100% of the flux was captured by the PSF fitting in most cases. PSF fitting of WFC3-IR images using Photutils shows promise for precise photometry.

中文翻译：

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在哈勃太空望远镜影像上执行与Photutils拟合的点扩展函数

初始质量函数（IMF）的低质量端是尚未很好理解的恒星形成的一个组成部分。通过分析恒星形成区域的哈勃太空望远镜（HST）图像，我们旨在提供数据以约束低质量IMF的形状。我们使用Astropy Photutils软件包v0.6在浅HST广角相机3图像上执行了点扩散函数（PSF）拟合，这些图像是在F110W，F139M和F160W滤镜上拍摄的，目的是识别低质量恒星和褐矮星。我们的PSF拟合例行程序的残差图像显示，较暗的光源可以有效地拟合，而较亮的光源则可以保留残差。尽管如此，分析证实我们的PSF幅度与光圈幅度一致，并且大多数情况下误差较小。在大多数情况下，PSF接头捕获了85％–100％的通量。