标题： Hyper Suprime-Cam CCD上的更亮更胖效应的校正 显示英文标题

标题： Correction of the brighter-fatter effect on the CCDs of Hyper Suprime-Cam

摘要： 明亮-更大效应在所有CCD传感器中以不同的程度存在。 深耗尽的厚传感器受到严重影响，对于宇宙剪切测量中的星系形状测量，需要对科学图像中的该效应进行准确校正。 我们描述了为昴星团望远镜上的超广角相机CCD实现的完整校正链。 我们从一组新的平场图像序列中推导出非线性校正，并测量它们的统计特性，即它们的两像素函数。 我们从平场统计中约束一个静电模型，并用于校正科学图像。 我们发现，观察到的方差和一些协方差的一部分并非由泊松统计和静电的组合引起——原因仍然不明。 因此，在推导静电模型时，我们必须忽略一些测量结果。 在广泛的图像质量和成像器的5个波段中，校正后的科学图像中的恒星表现出与流量相关的尺寸变化，这种变化足够小，可以预测暗弱天体的点扩散函数，其精度优于$10^{-3}$的二阶矩轨迹——而对于椭圆率和第四径向矩，精度甚至更高。 这种性能足以满足即将到来的大规模宇宙剪切调查，如鲁宾/LSST。 显示英文摘要

摘要： The brighter-fatter effect affects all CCD sensors to various degrees. Deep-depleted thick sensors are seriously affected and the measurement of galaxy shapes for cosmic shear measurements requires an accurate correction of the effect in science images. We describe the whole correction chain we have implemented for the CCDs of the Hyper Suprime-Cam imager on the Subaru Telescope. We derive non linearity corrections from a new sequence of flat field images, and measure their statistics, namely their two-pixel function. We constrain an electrostatic model from flat field statistics that we use to correct science images. We find evidence that some fraction of the observed variance and some covariances is not due to the combination of Poisson statistics and electrostatics -- and the cause remains elusive. We then have to ignore some measurements when deriving the electrostatic model. Over a wide range of image qualities and in the 5 bands of the imager, stars in corrected science images exhibit size variations with flux small enough to predict the point spread function for faint objects to an accuracy better than $10^{-3}$ for the trace of second moments -- and even better for the ellipticity and the fourth radial moment. This performance is sufficient for upcoming large-scale cosmic shear surveys such as Rubin/LSST.