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      Quasi-monolithic mirror suspensions in ground-based gravitational-wave detectors: an overview and look to the future

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          There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.

          Abstract

          At the commencement of a new era in astrophysics, with added information from direct detections of gravitational-wave (GW) signals, this paper is a testament to the quasi-monolithic suspensions of the test masses of the GW detectors that have enabled the opening of a new window on the universe. The quasi-monolithic suspensions are the final stages in the seismic isolation of the test masses in GW detectors, and are specifically designed to introduce as little thermal noise as possible. The history of the development of the fused-silica quasi-monolithic suspensions, which have been so essential for the first detections of GWs, is outlined and a glimpse into the status of research towards quasi-monolithic suspensions made of sapphire and silicon is given.

          This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

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          Observation of Gravitational Waves from a Binary Black Hole Merger

          B. Abbott, R. Abbott, T. D. Abbott … (2016)
          On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160)  Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
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            Die Grundlage der allgemeinen Relativitätstheorie

            Danielle A Einstein (1916)
            Article 0 comments Cited 371 times – based on 0 reviews     Review now
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              GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

              B. Abbott, R. Abbott, T. D. Abbott … (2016)
              We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4_{-0.9}^{+0.7}×10^{-22}. The inferred source-frame initial black hole masses are 14.2_{-3.7}^{+8.3}M_{⊙} and 7.5_{-2.3}^{+2.3}M_{⊙}, and the final black hole mass is 20.8_{-1.7}^{+6.1}M_{⊙}. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440_{-190}^{+180}  Mpc corresponding to a redshift of 0.09_{-0.04}^{+0.03}. All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
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                Author and article information

                Contributors
                Anna-Maria A. van Veggel:
                ORCID: http://orcid.org/0000-0002-5634-5169
                On behalf of : (on behalf of the LIGO Scientific Collaboration)
                Journal
                Journal ID (nlm-ta): Philos Trans A Math Phys Eng Sci
                Journal ID (iso-abbrev): Philos Trans A Math Phys Eng Sci
                Journal ID (publisher-id): RSTA
                Journal ID (hwp): roypta
                Title: Philosophical transactions. Series A, Mathematical, physical, and engineering sciences
                Publisher: The Royal Society Publishing
                ISSN (Print): 1364-503X
                ISSN (Electronic): 1471-2962
                Publication date (Print): 28 May 2018
                Publication date (Electronic): 16 April 2018
                Publication date PMC-release: 16 April 2018
                Volume: 376
                Issue: 2120 , Discussion meeting issue ‘The promises of gravitational-wave astronomy’ organised and edited by Iain Martin, Nils Andersson, Carole Mundell and James Hough
                Electronic Location Identifier: 20170281
                Affiliations
                SUPA School of Physics and Astronomy, University of Glasgow , Kelvin Building, Glasgow G12 8 QQ, UK
                Author notes

                One contribution of 11 to a discussion meeting issue ‘ The promises of gravitational-wave astronomy’.

                Author information
                http://orcid.org/0000-0002-5634-5169
                Article
                Publisher ID: rsta20170281
                DOI: 10.1098/rsta.2017.0281
                PMC ID: 5915646
                PubMed ID: 29661973
                SO-VID: 88dce188-2b17-439b-bbb4-4c2da45c1705
                Copyright © © 2018 The Authors.
                License:

                Published by the Royal Society under the terms of the Creative Commons Attribution License http://creativecommons.org/licenses/by/4.0/, which permits unrestricted use, provided the original author and source are credited.

                History
                Date accepted : 8 February 2018
                Funding
                Funded by: Dorothy Hodgkin Research;
                Award ID: DH120021
                Funded by: STFC;
                Award ID: ST/N005422/1, ST/L000946/1
                Categories
                Subject: 1000
                Subject: 10
                Subject: 1006
                Subject: 117
                Subject: Articles
                Subject: Review Article
                Custom metadata
                cover-date May 28, 2018

                Keywords: mirror,suspensions,quasi-monolithic,silica,sapphire,silicon
                Data availability:
                Keywords: mirror, suspensions, quasi-monolithic, silica, sapphire, silicon

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