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We describe and compare two types of microwave sky simulations which are good for small angular scales. The first type uses expansions in spherical harmonics, and the second one is based on plane waves and the Fast Fourier Transform. The angular power spectrum is extracted from maps corresponding to both types of simulations, and the resulting spectra are appropriately compared. In this way, the features and usefulness of Fourier simulations are pointed out. For $ell geq 100$, all the simulations lead to similar accuracies; however, the CPU cost of Fourier simulations is $sim 10$ times smaller than that for spherical harmonic simulations. For $ell leq 100$, the simulations based on spherical harmonics seem to be preferable.
We create realistic, full-sky, half-arcminute resolution simulations of the microwave sky matched to the most recent astrophysical observations. The primary purpose of these simulations is to test the data reduction pipeline for the Atacama Cosmology
We present 500 high-resolution, full-sky millimeter-wave Deep Learning (DL) simulations that include lensed CMB maps and correlated foreground components. We find that these MillimeterDL simulations can reproduce a wide range of non-Gaussian summary
Recent observations of the cosmic microwave background (CMB) have extended the measured power spectrum to higher multipoles $lgtrsim$1000, and there appears to be possible evidence for excess power on small angular scales. The primordial magnetic fie
In this paper, we focus our attention on the following question: How well can we recover the power spectrum of the cosmic microwave background from the maps of a given experiment?. Each experiment is described by a a pixelization scale, a beam size,