{"paper":{"title":"Planck pre-launch status: Design and description of the Low Frequency Instrument","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.IM","authors_text":"A. Banday, A. De Rosa, A. Gregorio, A. Mediavilla, A. Mennella, A. Simonetto, A. Wilkinson, A. Zacchei, A. Zonca, B. Aja, B. Cappellini, B. Partridge, C. Baccigalupi, C. Burigana, C. Franceschet, C. Paine, C. R. Lawrence, C. Sozzi, D. Kettle, D. Lawson P. M. Lubin, D. Maino, D. Pearson, E. Artal, E. Artina, E. Blackhurst, E. Franceschi, E. Martinez-Gonzalez, E. Taddei, F. Cavaliere, F. Colombo, F. Cuttaia, F. Ferrari, F. Gomez, F. Pasian, F. Perrotta, F. Villa, F. Winder, G. Baldan, G. Cafagna, G. C. De Gasperis, G. Crone, G. de Zotti, G. F. Smoot, G. Morgante, J. A. Rubino-Martin, J. Marti-Canales, J. M. Herreros, J. P. Leahy, J. P. Pascual, J. Tauber, J. Tuovinen, J. Varis, K. Gorski, L. A. Wade, L. Boschini, L. Danese, L. De Angelis, L. de la Fuente, L. Figini, L. Pagan, L. Stringhetti, L. Terenzi, L. Valenziano, M. Balasini, M. Bersanelli, M. C. Falvella, M. Janssen, M. Laaninen, M. Malaspina, M. Maris, M. Miccolis, M. Pecora, M. Pospieszalski, M. Prina, M. Sandri, M. Seiffert, M. Tomasi, N. Hughes, N. Mandolesi, n M. J. Salmon, N. Roddis, N. Vittorio, O. D'arcangelo, P. Bastia, P. Battaglia, P. B. Lilje, P. Guzzi, P. Jukkala, P. Leutenegger, P. Meinhold, P. M. Lapolla, P. Natoli, P. Platania, P. Sjoman, R. C. Butler, R.D. Davies, R. Ferretti, R. Hoyland, R.J. Davis, R. Leonardi, R. Nesti, R. Rebolo, R. Silvestri, S. Fogliani, S. Garavaglia, S. Levin, S. R. Hildebrandt, S.R. Lowe, T. Bernardino, T. Gaier, T. Poutanen, V. H. Kilpia","submitted_at":"2010-01-19T15:27:55Z","abstract_excerpt":"In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA program dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100-850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art Indium Phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference sign"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1001.3321","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}