揭开NGC 0959的面纱：基于像素的2D消光校正的重要性
Lifting the Veil of Dust from NGC 0959: The Importance of a Pixel-Based 2D Extinction Correction
摘要：
我们介绍了晚型螺旋星系NGC 0959的研究结果，在应用Tamura等人2009年（论文I）中描述的基于像素的尘埃消光校正之前和之后。通过像素色幅图（pCMD）和像素色色图（pCCD）研究了银河演化探测器（GALEX）的远紫外（FUV）和近紫外（NUV）、地基梵蒂冈先进技术望远镜（VATT）UBVR和斯皮策/红外阵列相机（IRAC）3.6、4.5、5.8和8.0微米图像。我们根据消光校正后像素在（B - 3.6微米）与（FUV-U）颜色的pCCD中的分布来定义像素组。在相同的pCCD中，我们在应用消光校正之前跟踪它们的位置。这表明，当使用未校正灰尘的颜色时，选择像素组没有意义。我们还追踪了星系像素坐标图上像素组的分布。我们发现，基于像素的（二维）消光校正是至关重要的，以揭示占主导地位的恒星星族的空间变化，平均在每个分辨率元素。不同类型和混合的恒星星族，和星系结构，如以前未识别的酒吧，成为容易辨别的消隐校正的pCCD和相干空间结构的像素坐标图。
英文摘要：
We present the results of a study of the late-type spiral galaxy NGC 0959, before and after application of the pixel-based dust extinction correction described in Tamura et al. 2009 (Paper I). Galaxy Evolution Explorer (GALEX) far-UV (FUV) and near-UV (NUV), ground-based Vatican Advanced Technology Telescope (VATT) UBVR, and Spitzer/Infrared Array Camera (IRAC) 3.6, 4.5, 5.8, and 8.0 micron images are studied through pixel Color-Magnitude Diagrams (pCMDs) and pixel Color-Color Diagrams (pCCDs). We define groups of pixels based on their distribution in a pCCD of (B - 3.6 micron) versus (FUV - U) colors after extinction correction. In the same pCCD, we trace their locations before the extinction correction was applied. This shows that selecting pixel groups is not meaningful when using colors uncorrected for dust. We also trace the distribution of the pixel groups on a pixel coordinate map of the galaxy. We find that the pixel-based (two-dimensional) extinction correction is crucial to reveal the spatial variations in the dominant stellar population, averaged over each resolution element. Different types and mixtures of stellar populations, and galaxy structures such as a previously unrecognized bar, become readily discernible in the extinction-corrected pCCD and as coherent spatial structures in the pixel coordinate map.
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