Authors
Junaid Aasi, BP Abbott, Richard Abbott, Thomas Abbott, MR Abernathy, Kendall Ackley, Carl Adams, Thomas Adams, Paolo Addesso, RX Adhikari, Vaishali Adya, C Affeldt, Nishu Aggarwal, OD Aguiar, Anirban Ain, P Ajith, A Alemic, Bruce Allen, D Amariutei, SB Anderson, WG Anderson, K Arai, MC Araya, C Arceneaux, JS Areeda, G Ashton, S Ast, SM Aston, P Aufmuth, C Aulbert, BE Aylott, S Babak, PT Baker, SW Ballmer, JC Barayoga, M Barbet, S Barclay, BC Barish, D Barker, B Barr, L Barsotti, J Bartlett, MA Barton, I Bartos, R Bassiri, JC Batch, C Baune, B Behnke, AS Bell, C Bell, M Benacquista, J Bergman, G Bergmann, CPL Berry, J Betzwieser, S Bhagwat, R Bhandare, IA Bilenko, G Billingsley, J Birch, S Biscans, C Biwer, JK Blackburn, L Blackburn, CD Blair, David Blair, O Bock, TP Bodiya, P Bojtos, C Bond, R Bork, M Born, Sukanta Bose, PR Brady, VB Braginsky, JE Brau, DO Bridges, M Brinkmann, AF Brooks, DA Brown, DD Brown, NM Brown, S Buchman, A Buikema, A Buonanno, Laura Cadonati, J Calderon Bustillo, JB Camp, KC Cannon, J Cao, CD Capano, S Caride, S Caudill, M Cavaglià, C Cepeda, R Chakraborty, T Chalermsongsak, SJ Chamberlin, S Chao, P Charlton, Y Chen, HS Cho, M Cho, JH Chow, N Christensen, Qi Chu, S Chung, G Ciani, F Clara, JA Clark, C Collette, L Cominsky, M Constancio, D Cook, TR Corbitt, N Cornish, A Corsi, CA Costa, MW Coughlin, S Countryman, P Couvares, DM Coward, MJ Cowart, DC Coyne, R Coyne, K Craig, JDE Creighton, TD Creighton, J Cripe, SG Crowder, A Cumming, L Cunningham, C Cutler, K Dahl, T Dal Canton, M Damjanic, SL Danilishin, K Danzmann, L Dartez, I Dave, H Daveloza, GS Davies, EJ Daw, D DeBra, W Del Pozzo, T Denker, T Dent, V Dergachev, RT DeRosa, R DeSalvo
Publication date
2015/3/3
Journal
Classical and quantum gravity
Volume
32
Issue
7
Pages
074001
Publisher
IOP Publishing
Description
The Advanced LIGO gravitational wave detectors are second-generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA, USA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in Initial LIGO, Fabry–Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than Initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic …
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J Aasi, BP Abbott, R Abbott, T Abbott, MR Abernathy… - Classical and quantum gravity, 2015