Hild, S. and De Salvo, R. and Harms, J. and Ott, C. D. and Santamaría, L. and Somiya, K. (2011) Sensitivity studies for third-generation gravitational wave observatories. Classical and Quantum Gravity, 28 (9). Art. No. 094013. ISSN 0264-9381 http://resolver.caltech.edu/CaltechAUTHORS:20110512-085754412
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Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
|Additional Information:||© 2011 IOP Publishing Ltd. Received 4 December 2010, in final form 7 January 2011. Published 18 April 2011. The ET-D sensitivity data are available at http://www.et-gw.eu/etsensitivities. The authors are grateful for support from their hosting institutions and national funding agencies. This work has been performed with the support of the European Commission under the Framework Programme 7 (FP7) ‘Capacities’, project Einstein Telescope (ET) design study (grant agreement 211743) (http://www.et-gw.eu/).|
|Classification Code:||PACS: 04.80.Nn, 95.75.Kk. MSC: 83C35.|
|Official Citation:||Sensitivity studies for third-generation gravitational wave observatories S Hild, M Abernathy, F Acernese, P Amaro-Seoane, N Andersson, K Arun, F Barone, B Barr, M Barsuglia, M Beker, N Beveridge, S Birindelli, S Bose, L Bosi, S Braccini, C Bradaschia, T Bulik, E Calloni, G Cella, E Chassande Mottin, S Chelkowski, A Chincarini, J Clark, E Coccia, C Colacino, J Colas, A Cumming, L Cunningham, E Cuoco, S Danilishin, K Danzmann, R De Salvo, T Dent, R De Rosa, L Di Fiore, A Di Virgilio, M Doets, V Fafone, P Falferi, R Flaminio, J Franc, F Frasconi, A Freise, D Friedrich, P Fulda, J Gair, G Gemme, E Genin, A Gennai, A Giazotto, K Glampedakis, C Gräf, M Granata, H Grote, G Guidi, A Gurkovsky, G Hammond, M Hannam, J Harms, D Heinert, M Hendry, I Heng, E Hennes, J Hough, S Husa, S Huttner, G Jones, F Khalili, K Kokeyama, K Kokkotas, B Krishnan, T G F Li, M Lorenzini, H Lück, E Majorana, I Mandel, V Mandic, M Mantovani, I Martin, C Michel, Y Minenkov, N Morgado, S Mosca, B Mours, H Müller–Ebhardt, P Murray, R Nawrodt, J Nelson, R Oshaughnessy, C D Ott, C Palomba, A Paoli, G Parguez, A Pasqualetti, R Passaquieti, D Passuello, L Pinard, W Plastino, R Poggiani, P Popolizio, M Prato, M Punturo, P Puppo, D Rabeling, P Rapagnani, J Read, T Regimbau, H Rehbein, S Reid, F Ricci, F Richard, A Rocchi, S Rowan, A Rüdiger, L Santamaría, B Sassolas, B Sathyaprakash, R Schnabel, C Schwarz, P Seidel, A Sintes, K Somiya, F Speirits, K Strain, S Strigin, P Sutton, S Tarabrin, A Thüring, J van den Brand, M van Veggel, C van den Broeck, A Vecchio, J Veitch, F Vetrano, A Vicere, S Vyatchanin, B Willke, G Woan and K Yamamoto doi: 10.1088/0264-9381/28/9/094013|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||12 May 2011 17:53|
|Last Modified:||10 Sep 2012 16:03|
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