Nearly Full-Sky Low-Multipole CMB Temperature Anisotropy: I. Foreground Cleaned Maps
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| Main Authors: | , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866916931958734848 |
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| author | Nofi, Hayley C. Addison, Graeme E. Bennett, Charles L. Herold, Laura Weiland, J. L. |
| author_facet | Nofi, Hayley C. Addison, Graeme E. Bennett, Charles L. Herold, Laura Weiland, J. L. |
| contents | Studies of cosmic microwave background (CMB) are often limited by foreground contamination. Foreground cleaning is performed either in harmonic or pixel space after data cuts have excluded sky areas of strong contamination. We present a nearly full-sky CMB temperature map with only 1% of pixels masked. To derive this map, we make use of six full-sky template maps at foreground-dominated frequencies from different experiments smoothed to $1^\circ$ and rely on the combination of these weighted maps to trace the morphology of foreground contamination. We do not impose any spectral index constraints, but only fit for template amplitudes at each target frequency. We clean WMAP and Planck maps at a set of target frequencies and conduct quality tests at the level of the maps, pixel histograms and power spectra to select four CMB maps that are cleaned with negligible foreground contamination and only 1% masked pixels and no inpainting. We recommend use of these cleaned CMB maps for low multipole ($\ell < 30$) studies. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2509_03718 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Nearly Full-Sky Low-Multipole CMB Temperature Anisotropy: I. Foreground Cleaned Maps Nofi, Hayley C. Addison, Graeme E. Bennett, Charles L. Herold, Laura Weiland, J. L. Cosmology and Nongalactic Astrophysics Studies of cosmic microwave background (CMB) are often limited by foreground contamination. Foreground cleaning is performed either in harmonic or pixel space after data cuts have excluded sky areas of strong contamination. We present a nearly full-sky CMB temperature map with only 1% of pixels masked. To derive this map, we make use of six full-sky template maps at foreground-dominated frequencies from different experiments smoothed to $1^\circ$ and rely on the combination of these weighted maps to trace the morphology of foreground contamination. We do not impose any spectral index constraints, but only fit for template amplitudes at each target frequency. We clean WMAP and Planck maps at a set of target frequencies and conduct quality tests at the level of the maps, pixel histograms and power spectra to select four CMB maps that are cleaned with negligible foreground contamination and only 1% masked pixels and no inpainting. We recommend use of these cleaned CMB maps for low multipole ($\ell < 30$) studies. |
| title | Nearly Full-Sky Low-Multipole CMB Temperature Anisotropy: I. Foreground Cleaned Maps |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2509.03718 |