论文标题
引入新的Spitzer Master Bliss地图以删除仪器系统 - 相曲线参数退化，如4.5 $μm$ WASP-43B相曲线的重新分析所证明的那样
Introducing a New Spitzer Master BLISS Map to Remove the Instrument-Systematic -- Phase-Curve-Parameter Degeneracy, as Demonstrated by a Reanalysis of the 4.5$μm$ WASP-43b Phase Curve
论文作者
论文摘要
尽管普遍了解Spitzer IRAC系统学，但每个数据集都可以提供自己的挑战，这些挑战继续向我们传授这些系统学的基本功能形式。多个组已经通过不同的下降技术分析了黄蜂43B的相曲线，每个技术都获得了不同的结果。在这项工作中，我们在探索双线性间隔的子像素灵敏度（Bliss）映射之间的退化关系，点响应函数完全宽度（PRFF-FWHM）下降和相位曲线参数之间的全宽度。我们发现，两个模型中的脱键参数之间存在很强的相关性，并且当数据被暂时纳入数据时，最佳拟合相位曲线幅度差异很大。为了删除这种退化，我们提出了一个新的高斯centraid centro的内膜内灵敏度图（以下节目的固定灵敏度图），该图是使用3,712,830次暴露，涉及5年的3,712,830，以4.5 $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $。我们找到了3.6 $ $ $的灵敏度的时间变化的证据，并且不会为此通道生成独立的访问地图。使用固定的4.5 $ $ $ $ Intrapixel灵敏度图，WASP-43B的最佳拟合不再随着bin尺寸而变化，并且不再需要PRF-FWWHM下降以消除相关噪声。对于不完全属于最佳位置的数据集，不应在Spitzer相相曲线的分析中使用时间箱。我们确认WASP-43B的夜侧排放，磁盘集成的夜间温度为806 $ \ pm $ 48 k，4.5 $ $ $ $ $。 4.5 $μm$ $地图可在\ url {github.com/kevin218/poet}上找到
While Spitzer IRAC systematics are generally well understood, each data set can provide its own challenges that continue to teach us about the underlying functional form of these systematics. Multiple groups have analyzed the phase curves of WASP-43b with varying detrending techniques, each obtaining different results. In this work, we take another look at WASP-43b while exploring the degenerate relation between Bilinearly-Interpolated Subpixel Sensitivity (BLISS) mapping, point response function full width at half-maximum (PRF-FWHM) detrending, and phase curve parameters. We find that there is a strong correlation between the detrending parameters in the two models, and best fit phase curve amplitudes vary strongly when the data are temporally binned. To remove this degeneracy, we present a new Gaussian centroided intrapixel sensitivity map (hereafter fixed sensitivity map), generated using 3,712,830 exposures spanning 5 years, for a variety of aperture sizes at 4.5$μm$. We find evidence for time variability in the sensitivity at 3.6$μm$ and do not generate a visit-independent map for this channel. With the fixed 4.5 $μm$ intrapixel sensitivity map, the best fits for WASP-43b no longer vary strongly with bin size and PRF-FWHM detrending is no longer required to remove correlated noise. For data sets that do not fall completely within the sweet spot, temporal binning should not be used in the analysis of Spitzer phase curves. We confirm night side emission for WASP-43b with a disk integrated nightside temperature of 806 $\pm$ 48 K at 4.5$μm$. The 4.5$μm$ maps are available at \url{github.com/kevin218/POET}
