{"paper":{"title":"Sensitivity Studies for Third-Generation Gravitational Wave Observatories","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"A. Chincarini, A. Cumming, A. Di Virgilio, A. Freise, A. Gennai, A. Giazotto, A. Gurkovsky, A. Paoli, A. Pasqualetti, A. Rocchi, A. R\\\"udiger, A. Sintes, A. Th\\\"uring, A. Vecchio, A. Vicere, B. Barr, B. Krishnan, B Mours, B. Sassolas, B. Sathyaprakash, B. Willke, C. Bradaschia, C. Colacino, C. D. Ott, C. Gr\\\"af, C. Michel, C. Palomba, C. Schwarz, C. Van Den Broeck, D. Friedrich, D. Heinert, D. Passuello, D. Rabeling, E. Calloni, E. Chassande Mottin, E. Coccia, E. Cuoco, E. Genin, E. Hennes, E. Majorana, F. Acernese, F. Barone, F. Frasconi, F. Khalili, F. Ricci, F. Richard, F. Speirits, F. Vetrano, G. Cella, G. Gemme, G. Guidi, G. Hammond, G. Jones, G. Parguez, G. Woan, H. Grote, H. L\\\"uck, H. M\\\"uller-Ebhardt, H. Rehbein, I. Heng, I. Mandel, I. Martin, J. Clark, J. Colas, J. Franc, J. Gair, J. Harms, J. Hough, J. Nelson, J. Read, J. van den Brand, J. Veitch, K. Arun, K. Danzmann, K. Glampedakis, K. Kokeyama, K. Kokkotas, K. Somiya, K. Strain, K. Yamamoto, L. Bosi, L. Cunningham, L. Di Fiore, L. Pinard, L. Santamar\\'ia, M. Abernathy, M. Barsuglia, M. Beker, M. Doets, M. Granata, M. Hannam, M. Hendry, M. Lorenzini, M. Mantovani, M. Prato, M. Punturo, M. van Veggel, N. Andersson, N. Beveridge, N. Morgado, P. Amaro-Seoane, P. Falferi, P. Fulda, P. Murray, P. Popolizio, P. Puppo, P. Rapagnani, P. Seidel, P. Sutton, R. De Rosa, R. De Salvo, R. Flaminio, R. Nawrodt, R. Oshaughnessy, R. Passaquieti, R. Poggiani1, R. Schnabel, S. Birindelli, S. Bose, S. Braccini, S. Chelkowski, S. Danilishin, S. Hild, S. Husa, S. Huttner, S. Mosca, S. Reid, S. Rowan, S Strigin, S. Tarabrin, S. Vyatchanin, T. Bulik, T. Dent, T.G.F. Li, T. Regimbau, V. Fafone, V. Mandic, W. Plastino, Y. Minenkov","submitted_at":"2010-12-04T12:17:06Z","abstract_excerpt":"Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope, a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this article we describe sensitivity models for the Einstein Telescope and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10Hz where a complex mixture of seismic, gravity gradient, suspension t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1012.0908","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"}