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Sensitivity studies for third-generation gravitational wave observatories

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.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription
Harms, J.0000-0002-7332-9806
Ott, C. D.0000-0003-4993-2055
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 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) (
Funding AgencyGrant Number
European Commission Framework Programme FP7211743
Issue or Number:9
Classification Code:PACS: 04.80.Nn, 95.75.Kk. MSC: 83C35.
Record Number:CaltechAUTHORS:20110512-085754412
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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.
ID Code:23649
Deposited By: Ruth Sustaita
Deposited On:12 May 2011 17:53
Last Modified:09 Mar 2020 13:19

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