{
  "id": "2011.05609",
  "version": "v1",
  "published": "2020-11-11T07:49:27.000Z",
  "updated": "2020-11-11T07:49:27.000Z",
  "title": "BeyondPlanck I. Global Bayesian analysis of the Planck Low Frequency Instrument data",
  "authors": [
    "BeyondPlanck Collaboration",
    "K. J. Andersen",
    "R. Aurlien",
    "R. Banerji",
    "M. Bersanelli",
    "S. Bertocco",
    "M. Brilenkov",
    "M. Carbone",
    "L. P. L. Colombo",
    "H. K. Eriksen",
    "J. R. Eskilt",
    "M. K. Foss",
    "C. Franceschet",
    "U. Fuskeland",
    "S. Galeotta",
    "M. Galloway",
    "S. Gerakakis",
    "E. Gjerløw",
    "B. Hensley",
    "D. Herman",
    "M. Iacobellis",
    "M. Ieronymaki",
    "H. T. Ihle",
    "J. B. Jewell",
    "A. Karakci",
    "E. Keihänen",
    "R. Keskitalo",
    "G. Maggio",
    "D. Maino",
    "M. Maris",
    "A. Mennella",
    "S. Paradiso",
    "B. Partridge",
    "M. Reinecke",
    "M. San",
    "A. -S. Suur-Uski",
    "T. L. Svalheim",
    "D. Tavagnacco",
    "H. Thommesen",
    "D. J. Watts",
    "I. K. Wehus",
    "A. Zacchei"
  ],
  "comment": "77 pages, 46 figures. All BeyondPlanck products and software will be released publicly at http://beyondplanck.science during the online release conference (November 18-20, 2020). Connection details will be made available at the same website. Registration is mandatory for the online tutorial, but optional for the conference",
  "categories": [
    "astro-ph.CO"
  ],
  "abstract": "We describe the BeyondPlanck project in terms of motivation, methodology and main products, and provide a guide to a set of companion papers that describe each result in fuller detail. Building directly on experience from ESA's Planck mission, we implement a complete end-to-end Bayesian analysis framework for the Planck Low Frequency Instrument (LFI) observations. The primary product is a joint posterior distribution P(omega|d), where omega represents the set of all free instrumental (gain, correlated noise, bandpass etc.), astrophysical (synchrotron, free-free, thermal dust emission etc.), and cosmological (CMB map, power spectrum etc.) parameters. Some notable advantages of this approach are seamless end-to-end propagation of uncertainties; accurate modeling of both astrophysical and instrumental effects in the most natural basis for each uncertain quantity; optimized computational costs with little or no need for intermediate human interaction between various analysis steps; and a complete overview of the entire analysis process within one single framework. As a practical demonstration of this framework, we focus in particular on low-l CMB polarization reconstruction, paying special attention to the LFI 44 GHz channel. We find evidence of significant residual systematic effects that are still not accounted for in the current processing, but must be addressed in future work. These include a break-down of the 1/f correlated noise model at 30 and 44 GHz, and scan-aligned stripes in the Southern Galactic hemisphere at 44 GHz. On the Northern hemisphere, however, we find that all results are consistent with the LCDM model, and we constrain the reionization optical depth to tau = 0.067 +/- 0.016, with a low-resolution chi-squared probability-to-exceed of 16%. The marginal CMB dipole amplitude is 3359.5 +/- 1.9 uK. (Abridged.)",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-11-11T07:49:27.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "planck low frequency instrument data",
      "global bayesian analysis",
      "complete end-to-end bayesian analysis framework",
      "beyondplanck"
    ],
    "tags": [
      "conference paper"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 77,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}