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Advanced LIGO: the next generation of gravitational wave detectors

06 Apr 2010-Classical and Quantum Gravity (IOP Publishing)-Vol. 27, Iss: 8, pp 084006
TL;DR: The Advanced LIGO gravitational wave detectors (ALGWR) as mentioned in this paper are the next generation instruments which will replace the existing initial LIGA detectors and are currently being constructed and installed.
Abstract: The Advanced LIGO gravitational wave detectors are next generation instruments which will replace the existing initial LIGO detectors. They are currently being constructed and installed. Advanced LIGO strain sensitivity is designed to be about a factor 10 better than initial LIGO over a broad band and usable to 10 Hz, in contrast to 40 Hz for initial LIGO. This is expected to allow for detections and significant astrophysics in most categories of gravitational waves. To achieve this sensitivity, all hardware subsystems are being replaced with improvements. Designs and expected performance are presented for the seismic isolation, suspensions, optics and laser subsystems. Possible enhancements to Advanced LIGO, either to resolve problems that may arise and/or to allow for improved performance, are now being researched. Some of these enhancements are discussed along with some potential technology being considered for detectors beyond Advanced LIGO.

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IOP PUBLISHING CLASSICAL AND QUANTUM GRAVITY
Class. Quantum Grav. 27 (2010) 089602 (4pp) doi:10.1088/0264-9381/27/8/089602
The LIGO Collaboration
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0264-9381/10/089602+04$30.00 © 2010 IOP Publishing Ltd Printed in the UK & the USA 1

Class. Quantum Grav. 27 (2010) 089602 The LIGO Collaboration
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arka
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1
(The LIGO Scientific Collaboration, http://www.ligo.org)
1
LIGO - California Institute of Technology, Pasadena, CA 91125, USA
2
Albert-Einstein-Institut, Max-Planck-Institut f
¨
ur Gravitationsphysik, D-30167 Hannover, Germany
3
University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA
4
Stanford University, Stanford, CA 94305, USA
2

Class. Quantum Grav. 27 (2010) 089602 The LIGO Collaboration
5
Louisiana State University, Baton Rouge, LA 70803, USA
6
University of Florida, Gainesville, FL 32611, USA
7
University of Birmingham, Birmingham, B15 2TT, United Kingdom
8
Leibniz Universit
¨
at Hannover, D-30167 Hannover, Germany
9
Albert-Einstein-Institut, Max-Planck-Institut f
¨
ur Gravitationsphysik, D-14476 Golm, Germany
10
Montana State University, Bozeman, MT 59717, USA
11
LIGO - Hanford Observatory, Richland, WA 99352, USA
12
University of Glasgow, Glasgow, G12 8QQ, United Kingdom
13
University of Western Australia, Crawley, WA 6009, Australia
14
LIGO - Massachusetts Institute of Technology, Cambridge, MA 02139, USA
15
Columbia University, New York, NY 10027, USA
16
The University of Texas at Brownsville and Texas Southmost College, Brownsville, TX 78520, USA
17
San Jose State University, San Jose, CA 95192, USA
18
Moscow State University, Moscow, 119992, Russia
19
LIGO - Livingston Observatory, Livingston, LA 70754, USA
20
Washington State University, Pullman, WA 99164, USA
21
University of Oregon, Eugene, OR 97403, USA
22
Syracuse University, Syracuse, NY 13244, USA
23
Rutherford Appleton Laboratory, HSIC, Chilton, Didcot, Oxon OX11 0QX, United Kingdom
24
University of Maryland, College Park, MD 20742 USA
25
University of Massachusetts - Amherst, MA 01003 USA
26
NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
27
University of Michigan, Ann Arbor, MI 48109, USA
28
University of Sannio at Benevento, I-82100 Benevento, Italy
29
The University of Mississippi, University, MS 38677, USA
30
Charles Sturt University, Wagga Wagga, NSW 2678, Australia
31
Caltech-CaRT, Pasadena, CA 91125, USA
32
Carleton College, Northfield, MN 55057, USA
33
The University of Melbourne, Parkville VIC 3010, Australia
34
Cardiff University, Cardiff, CF24 3AA, United Kingdom
35
E
¨
otv
¨
os University, ELTE 1053 Budapest, Hungary
36
University of Salerno, 84084 Fisciano (Salerno), Italy
37
The University of Sheffield, Sheffield S10 2TN, United Kingdom
38
The Pennsylvania State University, University Park, PA 16802, USA
39
Inter-University Centre for Astronomy and Astrophysics, Pune - 411007, India
40
Southern University and A&M College, Baton Rouge, LA 70813, USA
41
California Institute of Technology, Pasadena, CA 91125, USA
42
University of Rochester, Rochester, NY 14627, USA
43
The University of Texas at Austin, Austin, TX 78712, USA
44
Australian National University, Canberra, 0200, Australia
45
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
46
University of Minnesota, Minneapolis, MN 55455, USA
47
University of Adelaide, Adelaide, SA 5005, Australia
48
University of Southampton, Southampton, SO17 1BJ, United Kingdom
49
Northwestern University, Evanston, IL 60208, USA
50
National Astronomical Observatory of Japan, Tokyo 181-8588, Japan
51
Institute of Applied Physics, Nizhny Novgorod, 603950, Russia
52
University of Strathclyde, Glasgow, G1 1XQ, United Kingdom
53
Loyola University, New Orleans, LA 70118, USA
54
Hobart and William Smith Colleges, Geneva, NY 14456, USA
55
Louisiana Tech University, Ruston, LA 71272, USA
56
Andrews University, Berrien Springs, MI 49104, USA
57
Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain
3

Class. Quantum Grav. 27 (2010) 089602 The LIGO Collaboration
58
Sonoma State University, Rohnert Park, CA 94928, USA
59
Trinity University, San Antonio, TX 78212, USA
60
Rochester Institute of Technology, Rochester, NY 14623, USA
61
Southeastern Louisiana University, Hammond, LA 70402, USA
4

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Journal ArticleDOI
M. Punturo, M. R. Abernathy1, Fausto Acernese2, Benjamin William Allen3, Nils Andersson4, K. G. Arun5, Fabrizio Barone2, B. Barr1, M. Barsuglia6, M. G. Beker7, N. Beveridge1, S. Birindelli8, Suvadeep Bose9, L. Bosi, S. Braccini, C. Bradaschia, Tomasz Bulik10, Enrico Calloni, G. Cella, E. Chassande Mottin6, Simon Chelkowski11, Andrea Chincarini, John A. Clark12, E. Coccia13, C. N. Colacino, J. Colas, A. Cumming1, L. Cunningham1, E. Cuoco, S. L. Danilishin14, Karsten Danzmann3, G. De Luca, R. De Salvo15, T. Dent12, R. De Rosa, L. Di Fiore, A. Di Virgilio, M. Doets7, V. Fafone13, Paolo Falferi16, R. Flaminio17, J. Franc17, F. Frasconi, Andreas Freise11, Paul Fulda11, Jonathan R. Gair18, G. Gemme, A. Gennai11, A. Giazotto, Kostas Glampedakis19, M. Granata6, Hartmut Grote3, G. M. Guidi20, G. D. Hammond1, Mark Hannam21, Jan Harms22, D. Heinert23, Martin Hendry1, Ik Siong Heng1, Eric Hennes7, Stefan Hild1, J. H. Hough, Sascha Husa24, S. H. Huttner1, Gareth Jones12, F. Y. Khalili14, Keiko Kokeyama11, Kostas D. Kokkotas19, Badri Krishnan24, M. Lorenzini, Harald Lück3, Ettore Majorana, Ilya Mandel25, Vuk Mandic22, I. W. Martin1, C. Michel17, Y. Minenkov13, N. Morgado17, Simona Mosca, B. Mours26, H. Müller–Ebhardt3, P. G. Murray1, Ronny Nawrodt1, John Nelson1, Richard O'Shaughnessy27, Christian D. Ott15, C. Palomba, A. Paoli, G. Parguez, A. Pasqualetti, R. Passaquieti28, D. Passuello, L. Pinard17, Rosa Poggiani28, P. Popolizio, Mirko Prato, P. Puppo, D. S. Rabeling7, P. Rapagnani29, Jocelyn Read24, Tania Regimbau8, H. Rehbein3, Stuart Reid1, Luciano Rezzolla24, F. Ricci29, F. Richard, A. Rocchi, Sheila Rowan1, Albrecht Rüdiger3, Benoit Sassolas17, Bangalore Suryanarayana Sathyaprakash12, Roman Schnabel3, C. Schwarz, Paul Seidel, Alicia M. Sintes24, Kentaro Somiya15, Fiona C. Speirits1, Kenneth A. Strain1, S. E. Strigin14, P. J. Sutton12, S. P. Tarabrin14, Andre Thüring3, J. F. J. van den Brand7, C. van Leewen7, M. van Veggel1, C. Van Den Broeck12, Alberto Vecchio11, John Veitch11, F. Vetrano20, A. Viceré20, Sergey P. Vyatchanin14, Benno Willke3, Graham Woan1, P. Wolfango30, Kazuhiro Yamamoto3 
TL;DR: The third-generation ground-based observatory Einstein Telescope (ET) project as discussed by the authors is currently in its design study phase, and it can be seen as the first step in this direction.
Abstract: Advanced gravitational wave interferometers, currently under realization, will soon permit the detection of gravitational waves from astronomical sources. To open the era of precision gravitational wave astronomy, a further substantial improvement in sensitivity is required. The future space-based Laser Interferometer Space Antenna and the third-generation ground-based observatory Einstein Telescope (ET) promise to achieve the required sensitivity improvements in frequency ranges. The vastly improved sensitivity of the third generation of gravitational wave observatories could permit detailed measurements of the sources' physical parameters and could complement, in a multi-messenger approach, the observation of signals emitted by cosmological sources obtained through other kinds of telescopes. This paper describes the progress of the ET project which is currently in its design study phase.

1,497 citations

Journal ArticleDOI
TL;DR: In this article, a Theta vacua of gauge theories is proposed for cosmologists. But the authors do not consider the cosmological perturbation theory of axions in string theory.
Abstract: 1 Introduction 2 Models: the QCD axion; the strong CP problem; PQWW, KSVZ, DFSZ; anomalies, instantons and the potential; couplings; axions in string theory 3 Production and IC's: SSB and non-perturbative physics; the axion field during inflation and PQ SSB; cosmological populations - decay of parent, topological defects, thermal production, vacuum realignment 4 The Cosmological Field: action; background evolution; misalignment for QCD axion and ALPs; cosmological perturbation theory - ic's, early time treatment, axion sound speed and Jeans scale, transfer functions and WDM; the Schrodinger picture; simualting axions; BEC 5 CMB and LSS: Primary anisotropies; matter power; combined constraints; Isocurvature and inflation 6 Galaxy Formation; halo mass function; high-z and the EOR; density profiles; the CDM small-scale crises 7 Accelerated expansion: the cc problem; axion inflation (natural and monodromy) 8 Gravitational interactions with black holes and pulsars 9 Non-gravitational interactions: stellar astrophysics; LSW; vacuum birefringence; axion forces; direct detection with ADMX and CASPEr; Axion decays; dark radiation; astrophysical magnetic fields; cosmological birefringence 10 Conclusions A Theta vacua of gauge theories B EFT for cosmologists C Friedmann equations D Cosmological fluids E Bayes Theorem and priors F Degeneracies and sampling G Sheth-Tormen HMF

1,282 citations

Journal ArticleDOI
J. Aasi1, J. Abadie1, B. P. Abbott1, Richard J. Abbott1  +884 moreInstitutions (98)
TL;DR: In this paper, the authors review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of the detectors to a variety of astrophysical sources.
Abstract: In 2009–2010, the Laser Interferometer Gravitational-Wave Observatory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves (GWs) of astrophysical origin. The sensitivity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the GW readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the detectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources.

1,266 citations


Cites background or methods from "Advanced LIGO: the next generation ..."

  • ...For S6 a number of new systems were implemented to improve sensitivity and to prototype upgrades for the second-generation aLIGO detectors [21, 23]....

    [...]

  • ...The first-generation LIGO instruments were decommissioned shortly following the end of the science run (although immediately after S6 shot noise reduction was demonstrated in the H1 interferometer by using squeezed states of light [57]), and installation and early testing of aLIGO systems is now under way [23]....

    [...]

Journal ArticleDOI
Edo Berger1
TL;DR: A review of nearly a decade of short gamma-ray bursts and their afterglow and host-galaxy observations is presented in this article, where the authors use this information to shed light on the nature and properties of their progenitors, the energy scale and collimation of the relativistic outflow, and the properties of the circumburst environments.
Abstract: Gamma-ray bursts (GRBs) display a bimodal duration distribution with a separation between the short- and long-duration bursts at about 2 s. The progenitors of long GRBs have been identified as massive stars based on their association with Type Ic core-collapse supernovae (SNe), their exclusive location in star-forming galaxies, and their strong correlation with bright UV regions within their host galaxies. Short GRBs have long been suspected on theoretical grounds to arise from compact object binary mergers (neutron star–neutron star or neutron star–black hole). The discovery of short GRB afterglows in 2005 provided the first insight into their energy scale and environments, as well as established a cosmological origin, a mix of host-galaxy types, and an absence of associated SNe. In this review, I summarize nearly a decade of short GRB afterglow and host-galaxy observations and use this information to shed light on the nature and properties of their progenitors, the energy scale and collimation of the relativistic outflow, and the properties of the circumburst environments. The preponderance of the evidence points to compact object binary progenitors, although some open questions remain. On the basis of this association, observations of short GRBs and their afterglows can shed light on the on- and off-axis electromagnetic counterparts of gravitational wave sources from the Advanced LIGO/Virgo experiments.

1,061 citations

Journal ArticleDOI
TL;DR: In this paper, the authors review the performance of the LIGO instruments during this epoch, the work done to characterize the de- tectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of the detectors to a variety of astrophysical sources.
Abstract: In 2009-2010, the Laser Interferometer Gravitational-wave Observa- tory (LIGO) operated together with international partners Virgo and GEO600 as a network to search for gravitational waves of astrophysical origin. The sensitiv- ity of these detectors was limited by a combination of noise sources inherent to the instrumental design and its environment, often localized in time or frequency, that couple into the gravitational-wave readout. Here we review the performance of the LIGO instruments during this epoch, the work done to characterize the de- tectors and their data, and the effect that transient and continuous noise artefacts have on the sensitivity of LIGO to a variety of astrophysical sources.

973 citations

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40,330 citations


"Advanced LIGO: the next generation ..." refers background in this paper

  • ...At low frequencies, building an interferometer underground as a way to reduce gravity gradient noise is being explored [35]....

    [...]

Journal ArticleDOI
TL;DR: Laser Interferometric Gravitational-Wave Observatory (LIGO) as discussed by the authors is a project to detect and study gravitational waves of astrophysical origin, which holds the promise of testing general relativity in the strong-field regime, providing a new probe of exotic objects such as black hole and neutron stars, and uncovering unanticipated new astrophysics.
Abstract: The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves of astrophysical origin. Direct detection of gravitational waves holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black hole and neutron stars, and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech-MIT project supported by the National Science Foundation, operates three multi-kilometer interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction, and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than 1 part in 1E21. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on gravitational waves from a variety of potential astrophysical sources.

844 citations

Journal ArticleDOI
21 May 2006
TL;DR: LIGO as discussed by the authors is a trio of extremely sensitive Michelson interferometers built to detect gravitational waves from space, and the results of their recent observations are described in detail.
Abstract: LIGO is a trio of extremely sensitive Michelson interferometers built to detect gravitational waves from space. We describe predicted sources of gravitational waves, our detectors, and the results of our recent observations.

839 citations

Journal ArticleDOI
TL;DR: In this article, a phase detected output control signal is filtered and utilized to provide greater stability in a phase-locked loop, where an adder adds the phase detected control signal to a signal corresponding to the preceding filtered control signal multiplied by a constant factor which is less than unity (<1).
Abstract: The invention relates to a novel filtering circuit whereby a phase detected output control signal is filtered and utilized to provide greater stability in a phase-locked loop. The filtering circuit is placed in the connecting path between a phase detector and an oscillator; the oscillator supplies output signals, having a repetition rate which depends on the instantaneous values of the filtered control signal. The filtering circuit comprises an adder which adds the phase detected control signal to a signal corresponding to the preceding filtered control signal multiplied by a constant factor which is less than unity (<1).

388 citations

Journal ArticleDOI
B. P. Abbott1, Richard J. Abbott1, Fausto Acernese, Rana X. Adhikari1  +664 moreInstitutions (60)
20 Aug 2009-Nature
TL;DR: In this paper, the authors reported limits on the amplitude of the stochastic gravitational-wave background using the data from a two-year science run of the Laser Interferometer Gravitational-wave Observatory (LIGO).
Abstract: A stochastic background of gravitational waves is expected to arise from a superposition of a large number of unresolved gravitational-wave sources of astrophysical and cosmological origin. It should carry unique signatures from the earliest epochs in the evolution of the Universe, inaccessible to standard astrophysical observations. Direct measurements of the amplitude of this background are therefore of fundamental importance for understanding the evolution of the Universe when it was younger than one minute. Here we report limits on the amplitude of the stochastic gravitational-wave background using the data from a two-year science run of the Laser Interferometer Gravitational-wave Observatory (LIGO). Our result constrains the energy density of the stochastic gravitational-wave background normalized by the critical energy density of the Universe, in the frequency band around 100 Hz, to be <6.9 times 10-6 at 95% confidence. The data rule out models of early Universe evolution with relatively large equation-of-state parameter, as well as cosmic (super)string models with relatively small string tension that are favoured in some string theory models. This search for the stochastic background improves on the indirect limits from Big Bang nucleosynthesis and cosmic microwave background at 100 Hz.

364 citations