Year: 2026
Type: preprint
Abstract: The LiteBIRD satellite mission aims to measure the tensor-to-scalar ratio $r$ with unprecedented sensitivity through observations of the cosmic microwave background (CMB) $B$-mode polarisation. Robust constraints on $r$ require accurate likelihood modelling across a wide range of angular scales. In this work, we validate harmonic-space likelihood methods against pixel-based benchmarks using 20\,000 end-to-end simulations that include CMB, instrumental noise, and Galactic foreground residuals processed through a realistic component-separation pipeline. We compare a debiased pixel-based likelihood, which serves as our benchmark on large scales ($\ell\leq32$), with an offset Hamimeche \& Lewis (oHL) likelihood applicable across the full multipole range. We systematically explore the space of analysis settings, identifying the number of simulations used for covariance estimation and the choice of beam window function as the most critical factors. Over the full multipole range considered ($\ell\leq128$), where the benchmark combines the pixel-based likelihood at $\ell\leq32$ with a harmonic one at smaller scales, the 68\% upper bound on $r$ from the oHL likelihood is $19$--$29\%$ larger than the benchmark one, depending on the beam window function. This demonstrates its viability as a computationally efficient baseline for LiteBIRD data analysis and cosmological inference from the polarisation $B$-mode field.
Source: arXiv (Cornell University)
Authors: Galloni, G., Campeti, P., Gimeno-Amo, C., Carones, A., Rizzieri, A., Chinone, Y., Krachmalnicoff, N., Martínez-González, E., Pagano, L., Adak, D., Allys, E., Anand, A., Aryan, K., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Basyrov, A., Bersanelli, M., Besnard, A., Bouchet, F., Brancadori, N., Brinckmann, T., Casas, F. J., Gomar, L. Castelló, Colombo, L., Columbro, F., Coppolecchia, A., Cruz, M., Cuttaia, F., de Bernardis, P., de la Hoz, E., De Lucia, M., Della Torre, S., Demay, C., Diego-Palazuelos, P., García, J. J. Díaz, Finelli, F., Franceschet, C., Fuskeland, U., Galloway, M., Ganga, K., Gerbino, M., Ghigna, T., Giardiello, S., Gjerløw, E., Gomes, M., Gruppuso, A., Harper, S. E., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Hivon, E., Ikuma, K., Ishino, H., Kohri, K., Lamagna, L., Lattanzi, M., Leloup, C., Lembo, M., Levrier, F., Lonappan, A. I., López-Caniego, M., Maino, D., Maranchery, V., Masi, S., Matarrese, S., Micheli, S., Migliaccio, M., Monelli, M., Montier, L., Morgante, G., Morshed, M., Mousset, L., Najafi, M., Namikawa, T., Natoli, P., Obata, I., Occhiuzzi, A., Paiella, A., Paoletti, D., Paradiso, S., Pascual-Cisneros, G., Piacentini, F., Piccirilli, G., Pinchera, M., Polenta, G., Porcelli, L., Reinecke, M., Remazeilles, M., Ritacco, A., Rubiño-Martín, J. A., Ruiz-Granda, M., Sakurai, Y., Salvati, L., Sanghavi, J., Scott, D., Shenoy, D., Shiraishi, M., Signorelli, G., Stellati, S., Sullivan, R. M., Tassis, K., Terenzi, L., Tomasi, M., Tran, H., Vacher, L., van Tent, B., Vielva, P., Vinzl, S., Watts, D. J., Wehus, I. K., Weymann-Despres, G., Collaboration, for the LiteBIRD
Institutions: University of Ferrara, Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara, Instituto de Física de Cantabria, Scuola Internazionale Superiore di Studi Avanzati, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Centre National de la Recherche Scientifique, Université Paris Cité, Laboratoire AstroParticule et Cosmologie, University of Oxford, High Energy Accelerator Research Organization, Kavli Institute for the Physics and Mathematics of the Universe, International Center for Quantum-field Measurement Systems for Studies of the Universe and Particles, The University of Tokyo, University of Rome Tor Vergata, Institute for Fundamental Physics of the Universe, Université Paris-Saclay, Institut d'Astrophysique Spatiale, Laboratoire de Physique de l'Ecole Normale Supérieure, Instituto de Astrofísica de Canarias, Université Paris Sciences et Lettres, École Normale Supérieure - PSL, Sorbonne Université, Centre National d'Études Spatiales, Institut de Recherche en Astrophysique et Planétologie, National Central University, University of Manchester, University of California San Diego, Cardiff University, Istituto Nazionale di Fisica Nucleare, Sezione di Padova, National Institute for Astrophysics, University of Padua, Osservatorio Astronomico di Padova, University of Milan, Institut d'Astrophysique de Paris, Istituto Nazionale di Fisica Nucleare, Sezione di Milano, Sapienza University of Rome, Goddard Space Flight Center, Osservatorio di Astrofisica e Scienza dello Spazio, Istituto Nazionale di Fisica Nucleare, Sezione di Roma I, Max Planck Institute for Astrophysics, Istituto Nazionale di Fisica Nucleare, Sezione di Milano Bicocca, University of Oslo, Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Lawrence Berkeley National Laboratory
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: green
Funders: National Aeronautics and Space Administration, European Commission, Deutsche Forschungsgemeinschaft, Ministry of Education, Culture, Sports, Science and Technology, Swedish National Space Agency, Centro para el Desarrollo Tecnológico Industrial, Centre National d’Etudes Spatiales, Vetenskapsrådet, Centre National de la Recherche Scientifique, Istituto Nazionale di Astrofisica, Norges Forskningsråd, Canadian Space Agency, Japan Society for the Promotion of Science, Japan Aerospace Exploration Agency, Agencia Estatal de Investigación, Nuclear Physics, NextGenerationEU
Awards: G1363707852, G1799927510, G231133531, 産業モデルの国際的リンケージに関する計量経済学的研究, Imaging the Infant Universe with future Instruments, G3037510059, G318412399, G3367111595, G4066435496, WE PROPOSE TO ADVANCE THE TRL OF FOCAL-PLANE SUPERCONDUCTING DETECTORS AND READOUT ELECTRONICS FOR THE JAXA LITEBIRD CMB MISSION AND OTHER NEXT GENERATION CMB SPACE MISSIONS. A FUTURE CMB SPACE MISSION WILL MAP POLARIZED FLUCTUATIONS IN THE COSMIC MICROWAVE BACKGROUND (CMB) TO SEARCH FOR THE SIGNATURE OF GRAVITATIONAL WAVES FROM INFLATION POTENTIALLY OPENING A WINDOW ON THE UNIVERSE A FRACTION OF A SECOND AFTER THE BIG BANG. LITEBIRD IS TECHNICALLY REPRESENTATIVE OF FUTURE CMB POLARIZATION IMAGING MISSIONS. THE LITEBIRD DESIGN HAS TWO 5K-COOLED TELESCOPES AND IT WILL MEASURE IN 15 FREQUENCY BANDS BETWEEN 40 AND 402 GHZ WITH 0.1 K BOLOMETERS RESULTING IN A POWERFUL ABILITY TO SEPARATE GALACTIC FOREGROUND EMISSION FROM THE CMB. THE 40 CM LOW-FREQUENCY TELESCOPE AND THE 20 CM HIGH-FREQUENCY TELESCOPE GIVE 23 AND 20 ARCMINUTE RESOLUTION AT 140 AND 337 GHZ RESPECTIVELY. WE DRAW MATERIAL FROM THE U.S PARTICIPATION IN THE LITEBIRD COSMIC MICROWAVE BACKGROUND POLARIZATION SURVEY CONCEPT STUDY REPORT (CSR) TO DEVELOP THIS TECHNOLOGY PROPOSAL. OUR AREAS OF FOCUS ARE: DETECTOR ARRAYS: WE WILL DEVELOP TWO TYPES OF POLARIZATION-SENSITIVE DETECTORS ARRAYS BASED ON TRANSITION-EDGE SENSOR (TES) BOLOMETERS AND BRING THEIRTRLTO THE RANGE OF 5-6. THE FIRST TYPE IS THE BROADBAND SINUOUS ANTENNA-COUPLED ARRAY THAT MAKES USE OF CONTACTING LENSLETS TO INCREASE ANTENNA GAIN. THE SECOND TYPE IS WAVEGUIDE-PROBE-COUPLED WHICH MAKES USE OF CORRUGATED FEEDHORNS. IN THE LITEBIRD BASELINE DESIGN SINUOUS DETECTORS ARE IMPLEMENTED FROM 40-235 GHZ AND WAVEGUIDE-PROBE-COUPLED DETECTORS ARE IMPLEMENTED FROM 280 TO 402 GHZ. FOR BOTH ARCHITECTURES WE WILL IMPLEMENT TES BOLOMETERS SUITABLE FOR 100MK BASE TEMPERATURE OPERATION WITH SUITABLE OPERATIONAL PARAMETERS FOR READOUT USING A FREQUENCY-DOMAIN MULTIPLEXER (FDM) AND WE WILL DEVELOP METHODS TOMITIGATE DETECTOR DEAD TIME DUE TO COSMIC RAY INTERACTIONS IN THE DETECTORS. BY DEMONSTRATION OF A 3-LAYER THERMAL SPRAY ANTIREFLECTION COATING TECHNIQUE FOR THE LENSLETS AND BY DEMONSTRATION OF SILICON PLATELET FEEDHORN ARRAYS AT 400 GHZ WE WILL IN ADDITION ADVANCE OPTICAL COUPLING SCHEMES FOR CRYOGENICMM-WAVE DETECTOR ARRAYS. FOCAL PLANE MODULES: WE WILL DEVELOP FLIGHT-REPRESENTATIVE FOCAL PLANE MODULES THAT INCLUDE THE BOLOMETER ARRAY WAFERS LENSLETS AND SUPPORT WAFER A METAL FRAME AND MOUNTING OF THE SUPERCONDUCTING FDMREADOUT COMPONENTS. THESE MODULES WILL BE DEVELOPED TO A TRL RANGE OF 5-6 INCLUDING A FULL LAUNCH VIBRATION VALIDATION. SYSTEM INTEGRATION: AN END-TO-END DETECTOR SYSTEM INTEGRATION TEST OF INDIVIDUAL FOCAL PLANE MODULES WILL BE DONE INCLUDING READOUT OF THE DETECTORS USING FLIGHT-REPRESENTATIVE WIRING HARNESSES. THE TESTS WILL INCLUDEMODULES OF ALL TYPES LOW FREQUENCY (LF) MEDIUMFREQUENCY (MF) AND HIGH FREQUENCY (HF). MISSIONSIMULATIONS: SIMULATIONS OF THE MISSIONWILL BE GENERATED AND ANALYZED TO UNDERSTAND THE IMPACT OF THE DETECTOR DESIGN PARAMETERS ON SYSTEMATIC ERRORS AND OF THE FOCAL PLANE LAYOUT INCLUDING FREQUENCY BAND NUMBER AND POSITION ON THE ABILITY TO REMOVE FOREGROUND CONTAMINATION., EXC 2094: ORIGINS: Vom Ursprung des Universums bis zu den ersten Bausteinen des Lebens, G4993905653, G5195188938, G5402378781, 「大家族」制展開過程の実証的研究, G6328286017, G6344031981, G6480333962, G6520718613, G6766340963, 古代説話における諸寺縁起の研究, G7942188893, Advanced Methodologies for Next Generation Large Scale CMB Polarization Analysis, G8670446301, G972786147
OpenAlex ID: W7221778697