We observed Proxima Centauri with the Spitzer Space Telescope Infrared Array Camera five times in 2016 and 2017 to search for transits of Proxima Centauri b. Following standard analysis procedures, we found three asymmetric, transit-like events that are now understood to be vibrational systematics. This systematic is correlated with the width of the point-response function (PRF), which we measure with rotated and nonrotated-Gaussian fits with respect to the detector array. We show that the systematic can be removed with a novel application of an adaptive elliptical-aperture photometry technique, and compare the performance of this technique with fixed and variable circular-aperture photometry, using both BiLinearly Interpolated Subpixel Sensitivity (BLISS) maps and nonbinned Pixel-Level Decorrelation (PLD). With BLISS maps, elliptical photometry results in a lower standard deviation of normalized residuals, and reduced or similar correlated noise when compared to circular apertures. PLD prefers variable, circular apertures, but generally results in more correlated noise than BLISS. This vibrational effect is likely present in other telescopes and Spitzer observations, where correction could improve results. Our elliptical apertures can be applied to any photometry observations, and may be even more effective when applied to more circular PRFs than Spitzer’s.

我们在2016年和2017年使用Spitzer太空望远镜红外阵列相机五次观察了Proxima Centauri，以搜索Proxima Centauri b的过境。按照标准的分析程序，我们发现了三个不对称，类似过渡的事件，这些事件现在被认为是振动系统的。该系统与点响应函数（PRF）的宽度相关，我们通过旋转和非旋转高斯拟合相对于检测器阵列进行测量。我们显示，可以使用自适应椭圆孔径光度测量技术的新颖应用来删除该系统，并使用双线性内插子像素灵敏度（BLISS）图和非binned像素将这种技术与固定和可变圆形孔径光度测量的性能进行比较级别解相关（PLD）。有了BLISS地图，与圆形光圈相比，椭圆光度法可降低归一化残差的标准偏差，并减少或类似的相关噪声。PLD更喜欢使用可变的圆形光圈，但与BLISS相比，通常会产生更多的相关噪声。这种振动效应很可能出现在其他望远镜和Spitzer观测中，在这些观测中进行校正可以改善结果。我们的椭圆孔径可以应用于任何测光观测，并且在应用于比Spitzer更为圆形的PRF时甚至更有效。这种振动效应很可能出现在其他望远镜和Spitzer观测中，在这些观测中进行校正可以改善结果。我们的椭圆孔径可以应用于任何测光观测，并且在应用于比Spitzer更为圆形的PRF时甚至更有效。这种振动效应很可能出现在其他望远镜和Spitzer观测中，在这些观测中进行校正可以改善结果。我们的椭圆孔径可以应用于任何测光观测，并且在应用于比Spitzer更为圆形的PRF时甚至更有效。