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This paper provides a detailed description of the data reduction and analysisprocedures that have been employed in our previous studies of spatialfluctuation of the cosmic infrared background (CIB) using deep Spitzer IRACobservations. The self-calibration we apply removes a strong instrumentalsignal from the fluctuations which would otherwise corrupt our results. Theprocedures and results for masking bright sources, and modeling faint sourcesdown to levels set by the instrumental noise are presented. Various tests areperformed to demonstrate that the resulting power spectra of these fields arenot dominated by instrumental or procedural effects. These tests indicate thatthe large scale (>~30') fluctuations that remain in the deepest fields are notdirectly related to the galaxies that are bright enough to be individuallydetected. We provide the parameterization of these power spectra in terms ofseparate instrument noise, shot noise, and power law components. Ourmeasurements of spatial fluctuations of the CIB intensity indicate the meanemission from the objects producing the fluctuations is quite low (>~1 nW m-2sr-1 at 3-5 micron), and thus consistent with current gamma-ray absorptionconstraints. The source of the fluctuations may be high-z Population IIIobjects, or a more local component of very low luminosity objects withclustering properties that differ from the resolved galaxies. Finally, wediscuss the prospects of the upcoming space-based surveys to directly measurethe epochs inhabited by the populations producing these source-subtracted CIBfluctuations, and to isolate the individual fluxes of these populations.

Cosmic Infrared Background Fluctuations in Deep Spitzer IRAC Images: Data Processing and Analysis