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While Spitzer IRAC systematics are generally well understood, each data setcan provide its own challenges that continue to teach us about the underlyingfunctional form of these systematics. Multiple groups have analyzed the phasecurves of WASP-43b with varying detrending techniques, each obtaining differentresults. In this work, we take another look at WASP-43b while exploring thedegenerate 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 strongcorrelation between the detrending parameters in the two models, and best fitphase curve amplitudes vary strongly when the data are temporally binned. Toremove this degeneracy, we present a new Gaussian centroided intrapixelsensitivity map (hereafter fixed sensitivity map), generated using 3,712,830exposures spanning 5 years, for a variety of aperture sizes at 4.5$\mu m$. Wefind evidence for time variability in the sensitivity at 3.6$\mu m$ and do notgenerate a visit-independent map for this channel. With the fixed 4.5 $\mu m$intrapixel sensitivity map, the best fits for WASP-43b no longer vary stronglywith bin size and PRF-FWHM detrending is no longer required to removecorrelated noise. For data sets that do not fall completely within the sweetspot, temporal binning should not be used in the analysis of Spitzer phasecurves. We confirm night side emission for WASP-43b with a disk integratednightside temperature of 806 $\pm$ 48 K at 4.5$\mu m$. The 4.5$\mu m$ maps areavailable at \url{github.com/kevin218/POET}

the astronomical journal

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$\mu m$ WASP-43b Phase Curve