DOCSLIB.ORG

The Einstein Telescope

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Einstein Telescope Michele Punturo INFN Perugia and EGO ASPERA 2012: GW detectors 1 Talk Outline Introduction to the Gravitational Wave (GW) search Gravitational wave interferometric detectors Working principles Current status Advanced detectors 3rd generation of gravitational wave observatories The Einstein Telescope ASPERA 2012: GW detectors 2 General Relativity and GW GW are predicted by the Einstein General Relativity (GR) theory Formal treatment of the GW in GR is beyond the scope of this talk and only the aspects important for the GW detection will be considered Einstein field equation links c4 to the effect of the deformation the source of the space-time = − Tµν Gµν (Gµν the deformation tensor) deformation (Tµν Energy- 8πG impulse tensor) Far from the big masses Einstein field equation admits (linear approximation) wave solution (small perturbation of the background 1 ∂ 2 =η + << ⇒ ∇2 − = geometry) g h with hµν 1 2 2 hµν 0 c ∂t ASPERA 2012: GW detectors 3 Gravitational Waves Gravitational waves are a perturbation of the space-time 0 0 0 0 geometry 0 h+ h× 0 h(z,t) = ei(ωt−kz) 0 h − h 0 They present two polarizations × + 0 0 0 0 The effect of GWs on a mass distribution is the modulation of the reciprocal distance of the masses h× h+ ASPERA 2012: GW detectors 4 Quantify the “deformation” The amplitude of the space-time deformation is: 21G Where Qµν is the = ⋅ hQµν 4 µν quadrupolar moment cr of the GW source Let suppose to have a system of 2 and r is the distance coalescing neutron stars, located in between the detector the Virgo cluster (r~10Mpc): and the GW source h ≈10−21 −10−22 h δL ≈ ⋅ L −18 −19 2 0 ⇒ δL ≈10 −10 m 3 L0 ≈10 m Extremely challenging for the detectors ASPERA 2012: GW detectors 5 But, GWs really exist? Neutron star binary system: PSR1913+16 Pulsar bound to a “dark companion”, 7 kpc from Earth. -3 Relativistic clock: vmax/c ~10 GR predicts such a system to loose energy via GW emission: orbital period decrease Radiative prediction of general relativity verified at 0.2% level Nobel Prize 1993: HulseASPERA and 2012:Taylor GW detectors 6 GW interferometric initial detectors A network of detectors has been active in the World until few years ago GEO, Hannover, 600 m TAMA, Tokyo, 300 m Virgo, Pisa, 3 km (now CLIO) ASPERA 2012: GW detectors 7 VIRGO LAPP – Annecy LMA – Lyon INFN – Padova-Trento NIKHEF – Amsterdam INFN – Napoli INFN – Perugia RMKI - Budapest OCA – Nice INFN - Pisa INFN – Firenze-Urbino LAL – Orsay INFN – Roma 1 INFN – Genova APC – Paris INFN – Roma 2 INFN – LNF LKB - Paris POLGRAV - Warsaw ASPERA 2012: GW detectors 8 GEO600 ASPERA 2012: GW detectors 9 GW interferometric initial detectors A network of detectors has been active in the World until few years ago GEO, Hannover, 600 m LIGO Hanford, 4 km: 2 ITF on the same site! TAMA, Tokyo, 300 m Virgo, Cascina, 3 km (now CLIO) LIGO Livingston, 4 km ASPERA 2012: GW detectors 10 LIGO Scientific Collaboration GEO600, Hannover, Germany LIGO – Hanford, WA LIGO – Livingston, LA ASPERA 2012: GW detectors 11 GW interferometric initial detectors A network of detectors has been active in the World until few years ago GEO, Hannover, 600 m LIGO Hanford, 4 km: 2 ITF on the same site! TAMA, Tokyo, 300 m Virgo, Cascina, 3 km (now CLIO) LIGO Livingston, 4 km ASPERA 2012: GW detectors 12 Working principle The quadrupolar nature of the GW makes the Michelson interferometer a “natural” GW detector h δL ≈ ⋅ L 2 0 2 4 10 ≤L0 ≤10 m in terrestrial detectors Beam-splitter Mirror GW signal 4π φGW = L0 ⋅h λ Interference Photodetector 13 ASPERA 2012: GW detectors Real life: complex machine typical earth crust tidal strain: ~10-4 m Complex optical scheme ~ -14 Complex active control strategy allowed mirror rms motion: 10 m ASPERA 2012: GW detectors 14 Detector sensitivity The faint space-time deformation measurement must compete with a series of noise sources that are spoiling the detector sensitivity Seismic filtering: in Virgo pendulum chains to reduce seismic motion 14 Virgo nominal by a factor 10 sensitivity above 10 Hz ~ 8 m ASPERA 2012: GW detectors 15 Detector sensitivity The faint space-time deformation measurement must compete with a series of noise sources that are spoiling the detector sensitivity Optimization of the payload design to minimize the mechanical losses ASPERA 2012: GW detectors 16 Detector sensitivity The faint space-time deformation measurement must compete with a series of noise sources that are spoiling the detector sensitivity Maximization of the injected laser power, to minimize the shot noise ASPERA 2012: GW detectors 17 Noise budget: real life Virgo+ noise budget example ASPERA 2012: GW detectors 18 GW interferometer past evolution Evolution of the GW detectors (Virgo example): .) a.u Proof of the working principle Detection distance ( Infrastructu re 2012: GW ASPERA detectors realization Same and infrastructure detector assembling year 2003 2008 19 GW interferometer past evolution Evolution of the GW detectors (Virgo example): .) a.u Proof of the working principle Upper Limit physics Detection distance ( Infrastructu re 2012: GW ASPERA detectors realization Same and infrastructure detector assembling year 2003 2008 20 z GW sources: BS BH-BH r0 Binary systems of massive and compact stellar bodies: r NS-NS, NS-BH, BH-BH Source of crucial interest: We are able to model (roughly) the signal using the (post) Newtonian chirp physics ASPERA 2012: GW detectors 21 Network of GW detectors The search for GW signal emitted by a binary system (of neutron star) asks for a network of (distant) detectors Event reconstruction Source location in the sky Reconstruction of polarization components Reconstruction of amplitude at source and determination of source distance (BNS) Detection probability increase Detection confidence increase Larger uptime Better sky coverage ASPERA 2012: GW detectors 22 GW sources: BS z r0 Binary systems of massive and compact stellar bodies: r NS-NS, NS-BH, BH-BH 1ST GENERATION INTERFEROMETERS COULD DETECT A NS-NS COALESCENCE AS FAR AS VIRGO CLUSTER (15 MPc) LOW EXPECTED EVENT RATE: 0.01-0.1 ev/yr (NS-NS) ASPERA 2012: GW detectors 23 Scientific runs A series of runs have been performed by the GW network As expected, no BS detection so far! ’05 ’06 ’07 ’08 ’09 ’10 ’11 ’12 LIGO S4 S5 AstroWatch S6 GEO VSR1 VSR2 VSR3 Virgo But, upper limit physics explored! (PRD 85, 082002 – 2012, 24 Nature 460, 990-994 . 2009) ASPERA 2012: GW detectors GW source: Isolated NS Not-axisymmetric rotating neutron stars (pulsars) are expected to emit GW at frequency double of the spinning one 38 2 I zz ≈10 kg ⋅m G 2 h ≈ ε ⋅ I ⋅Ω I xx − I yy rc4 zz ε = I zz The periodicity of the signal allows to increase the SNR integrating for a long time But Doppler effect correction needed because of the Earth motion determines a computational obstacle to a full blind search Detection of GW from a NS gives info on the internal structure of the star (ε limit is related to the superfluid/strange matter nature of the star, to the magnetic field, …) ASPERA 2012: GW detectors 25 GW sources: isolated NS 713 671 Isolated NS are a possible source of GW if they have a non-null quadrupolar moment (ellipticity) Crab pulsar ApJ in the Crab nebula al. 2010 -22 Spin-down limit of known NS vs integrated sensitivities (2kpc) 10 et (tobs=1year, 1%FAP, 10%FDP) LIGO-S5 upper limit: -23 10 Know Pulsar spin down limit <1/4 of the SD limit Virgo nominal sensitivity iLIGO nominal sensitivity in h amplitude 10-24 B. P. Abbott B. P. 10-25 93 Vela pulsar in its -26 737 10 nebula (0.3kpc) -27 Space-time strain 10 Upper limit ApJ determined in the -28 2011 2011 10 Virgo VSR2 run: ~1/3 of the spin- -29 10 et al. 10 100 1000 down limit Frequency [Hz] Credits: C.Palomba ASPERA 2012: GW detectors 26 J. Abadie GW sources: GRB Gamma ray bursts are subdivided in 2 classes: Long (>2s duration): SNe generation mechanism Short (<2s): BNS coalescence mechanism → GW B.P. Abbot (LSC and Virgo coll), Astr. Jour. 715 (2010), 1438 GRB mainly detected by Swift satellite A series (137) of GRB occurred during the LIGO-S5/Virgo-VSR1 run No detection occurred, but lower limit for the distance of each GRB ASPERA 2012: GW detectors event 27 GW interferometer present evolution Evolution of the GW detectors (Virgo example): First detection .) a.u Initial astrophysics Proof of the working principle Upper Limit physics enhanced detectors Detection distance ( Infrastructu re 2012: GW ASPERA detectors realization Same Same Same and infrastructureinfrastructure infrastructure detector assembling year 2003 2008 2011 2017 28 Advanced detectors The upgrade to the advanced phase (2nd generation) is just started. The detectors should be back in commissioning in 2014 Advanced are promising roughly a factor 10 in sensitivity improvement: Enhanced LIGO/Virgo+ Virgo/LIGO 108 ly Adv. Virgo/Adv. LIGO Credit: R.Powell, B.Berger This allows a detection distance for coalescing BNS of about 130-200Mpc ASPERA 2012: GW detectors 29 Advanced detectors: BNS detection rates The detection rate follows the sight distance with a roughly cubic law: A BNS detection rate of few tens per year with a limited SNR: detection is assured et al. (LSC & Virgo), al. (LSC et arXiv:1003.2480; Virgo), & Abadie 173001 (2010) 27, CQG ASPERA 2012: GW detectors 30 Advanced detectors: pulsars Better sensitivities, especially at low frequency, will allow to beat the spin-down limit for many pulsars Credits: C.Palomba ASPERA 2012: GW detectors 31 Advanced detectors: technologies Advanced detectors
Load more

Recommended publications
  • Towards Gravitational Wave Astronomy: Commissioning and Characterization of GEO 600
    Journal of Physics: Conference Series Related content - Quantum measurements in gravitational- Towards gravitational wave astronomy: wave detectors F Ya Khalili Commissioning and characterization of GEO600 - Systematic survey for monitor signals to reduce fake burst events in a gravitational- wave detector To cite this article: S Hild et al 2006 J. Phys.: Conf. Ser. 32 66 Koji Ishidoshiro, Masaki Ando and Kimio Tsubono - Environmental Effects for Gravitational- wave Astrophysics Enrico Barausse, Vitor Cardoso and Paolo View the article online for updates and enhancements. Pani Recent citations - First joint search for gravitational-wave bursts in LIGO and GEO 600 data B Abbott et al - The status of GEO 600 H Grote (for the LIGO Scientific Collaboration) - Upper limits on gravitational wave emission from 78 radio pulsars W. G. Anderson et al This content was downloaded from IP address 194.95.159.70 on 30/01/2019 at 13:59 Institute of Physics Publishing Journal of Physics: Conference Series 32 (2006) 66–73 doi:10.1088/1742-6596/32/1/011 Sixth Edoardo Amaldi Conference on Gravitational Waves Towards gravitational wave astronomy: Commissioning and characterization of GEO 600 S. Hild1,H.Grote1,J.R.Smith1 and M. Hewitson1 for the GEO 600-team2 . 1 Max-Planck-Institut f¨ur Gravitationsphysik (Albert-Einstein-Institut) und Universit¨at Hannover, Callinstr. 38, D–30167 Hannover, Germany. 2 See GEO 600 status report paper for the author list of the GEO collaboration. E-mail: [email protected] Abstract. During the S4 LSC science run, the gravitational-wave detector GEO 600, the first large scale dual recycled interferometer, took 30 days of continuous√ data.
    [Show full text]
  • 5 Optical Design
    ET-0106A-10 issue :2 ET Design Study date :January27,2011 page :204of315 5 Optical design 5.1 Description Responsible: WP3 coordinator, A. Freise Put here the description of the content of the section . 5.2 Executive Summary Responsible: WP3 coordinator, A. Freise Put here a summary of the main achievement/statements of this section . 5.3 Review on the geometry of the observatory Author(s): Andreas Freise,StefanHild This section briefly reviews the reasoning behind the shape of current gravitational wave detectors and then discusses alternative geometries which can be of interest for third-generation detectors. We will use the ter- minology introduced in the review of a triangular configuration [220] and discriminate between the geometry, topology and configuration of a detector as follows: The geometry describes the position information of one or several interferometers, defined by the number of interferometers, their location and relative orientation. The topology describes the optical system formed by its core elements. The most common examples are the Michelson, Sagnac and Mach–Zehnder topologies. Finally the configuration describes the detail of the optical layout and the set of parameters that can be changed for a given topology, ranging from the specifications of the optical core elements to the control systems, including the operation point of the main interferometer. Please note that the addition of optical components to a given topology is often referred to as a change in configuration. 5.3.1 The L-shape Current gravitational wave detectors represent the most precise instruments for measuring length changes. They are laser interferometers with km-long arms and are operated differently from many precision instruments built for measuring an absolute length.
    [Show full text]
  • The Einstein Telescope (ET) Is a Proposed Underground Infrastructure to Host a Third- Generation, Gravitational-Wave Observatory
    The Einstein Telescope (ET) is a proposed underground infrastructure to host a third- generation, gravitational-wave observatory. It builds on the success of current, second-generation laser- interferometric detectors Advanced Virgo and Advanced LIGO, whose breakthrough discoveries of merging black holes (BHs) and neutron stars over the past 5 years have ushered scientists into the new era of gravitational-wave astronomy. The Einstein Telescope will achieve a greatly improved sensitivity by increasing the size of the interferometer from the 3km arm length of the Virgo detector to 10km, and by implementing a series of new technologies. These include a cryogenic system to cool some of the main optics to 10 – 20K, new quantum technologies to reduce the fluctuations of the light, and a set of infrastructural and active noise-mitigation measures to reduce environmental perturbations. The Einstein Telescope will make it possible, for the first time, to explore the Universe through gravitational waves along its cosmic history up to the cosmological dark ages, shedding light on open questions of fundamental physics and cosmology. It will probe the physics near black-hole horizons (from tests of general relativity to quantum gravity), help understanding the nature of dark matter (such as primordial BHs, axion clouds, dark matter accreting on compact objects), and the nature of dark energy and possible modifications of general relativity at cosmological scales. Exploiting the ET sensitivity and frequency band, the entire population of stellar and intermediate mass black holes will be accessible over the entire history of the Universe, enabling to understand their origin (stellar versus primordial), evolution, and demography.
    [Show full text]
  • Observing Gravitational Waves from Spinning Neutron Stars LIGO-G060662-00-Z Reinhard Prix (Albert-Einstein-Institut)
    Astrophysical Motivation Detecting Gravitational Waves from NS Observing Gravitational Waves from Spinning Neutron Stars LIGO-G060662-00-Z Reinhard Prix (Albert-Einstein-Institut) for the LIGO Scientific Collaboration Toulouse, 6 July 2006 R. Prix Gravitational Waves from Neutron Stars Astrophysical Motivation Detecting Gravitational Waves from NS Outline 1 Astrophysical Motivation Gravitational Waves from Neutron Stars? Emission Mechanisms (Mountains, Precession, Oscillations, Accretion) Gravitational Wave Astronomy of NS 2 Detecting Gravitational Waves from NS Status of LIGO (+GEO600) Data-analysis of continous waves Observational Results R. Prix Gravitational Waves from Neutron Stars Gravitational Waves from Neutron Stars? Astrophysical Motivation Emission Mechanisms Detecting Gravitational Waves from NS Gravitational Wave Astronomy of NS Orders of Magnitude Quadrupole formula (Einstein 1916). GW luminosity (: deviation from axisymmetry): 2 G MV 3 O(10−53) L ∼ 2 GW c5 R c5 R 2 V 6 O(1059) erg = 2 s s G R c 2 Schwarzschild radius Rs = 2GM/c Need compact objects in relativistic motion: Black Holes, Neutron Stars, White Dwarfs R. Prix Gravitational Waves from Neutron Stars Gravitational Waves from Neutron Stars? Astrophysical Motivation Emission Mechanisms Detecting Gravitational Waves from NS Gravitational Wave Astronomy of NS What is a neutron star? −1 Mass: M ∼ 1.4 M Rotation: ν . 700 s Radius: R ∼ 10 km Magnetic field: B ∼ 1012 − 1014 G =⇒ density: ρ¯ & ρnucl =⇒ Rs = 2GM ∼ . relativistic: R c2R 0 4 R. Prix Gravitational Waves from Neutron Stars Gravitational Waves from Neutron Stars? Astrophysical Motivation Emission Mechanisms Detecting Gravitational Waves from NS Gravitational Wave Astronomy of NS Gravitational Wave Strain h(t) + Plane gravitational wave hµν along z-direction: Lx −Ly Strain h(t) ≡ 2L : y Ly Lx x h(t) t R.
    [Show full text]
  • Holographic Noise in Interferometers a New Experimental Probe of Planck Scale Unification
    Holographic Noise in Interferometers A new experimental probe of Planck scale unification FCPA planning retreat, April 2010 1 Planck scale seconds The physics of this “minimum time” is unknown 1.616 ×10−35 m Black hole radius particle energy ~1016 TeV € Quantum particle energy size Particle confined to Planck volume makes its own black hole FCPA planning retreat, April 2010 2 Interferometers might probe Planck scale physics One interpretation of the Planck frequency/bandwidth limit predicts a new kind of uncertainty leading to a new detectable effect: "holographic noise” Different from gravitational waves or quantum field fluctuations Predicts Planck-amplitude noise spectrum with no parameters We are developing an experiment to test this hypothesis FCPA planning retreat, April 2010 3 Quantum limits on measuring event positions Spacelike-separated event intervals can be defined with clocks and light But transverse position measured with frequency-bounded waves is uncertain by the diffraction limit, Lλ0 This is much larger than the wavelength € Lλ0 L λ0 Add second€ dimension: small phase difference of events over Wigner (1957): quantum limits large transverse patch with one spacelike dimension FCPA planning€ retreat, April 2010 4 € Nonlocal comparison of event positions: phases of frequency-bounded wavepackets λ0 Wavepacket of phase: relative positions of null-field reflections off massive bodies € Δf = c /2πΔx Separation L € ΔxL = L(Δf / f0 ) = cL /2πf0 Uncertainty depends only on L, f0 € FCPA planning retreat, April 2010 5 € Physics Outcomes
    [Show full text]
  • Seismic Characterization of the Euregio Meuse-Rhine in View of Einstein Telescope
    SEISMIC CHARACTERIZATION OF THE EUREGIO MEUSE-RHINE IN VIEW OF EINSTEIN TELESCOPE 13 September 2019 First results of seismic studies of the Belgian-Dutch-German site for Einstein Telescope Soumen Koley1, Maria Bader1, Alessandro Bertolini1, Jo van den Brand1,2, Henk Jan Bulten1,3, Stefan Hild1,2, Frank Linde1,4, Bas Swinkels1, Bjorn Vink5 1. Nikhef, National Institute for Subatomic Physics, Amsterdam, The Netherlands 2. Maastricht University, Maastricht, The Netherlands 3. VU University Amsterdam, Amsterdam, The Netherlands 4. University of Amsterdam, Amsterdam, The Netherlands 5. Antea Group, Maastricht, The Netherlands CONFIDENTIAL Figure 1: Artist impression of the Einstein Telescope gravitational wave observatory situated at a depth of 200-300 meters in the Euregio Meuse-Rhine landscape. The triangular topology with 10 kilometers long arms allows for the installation of multiple so-called laser interferometers. Each of which can detect ripples in the fabric of space-time – the unique signature of a gravitational wave – as minute relative movements of the mirrors hanging at the bottom of the red and white towers indicated in the illustration at the corners of the triangle. 1 SEISMIC CHARACTERIZATION OF THE EUREGIO MEUSE-RHINE IN VIEW OF EINSTEIN TELESCOPE Figure 2: Drill rig for the 2018-2019 campaign used for the completion of the 260 meters deep borehole near Terziet on the Dutch-Belgian border in South Limburg. Two broadband seismic sensors were installed: one at a depth of 250 meters and one just below the surface. Both sensors are accessible via the KNMI portal: http://rdsa.knmi.nl/dataportal/. 2 SEISMIC CHARACTERIZATION OF THE EUREGIO MEUSE-RHINE IN VIEW OF EINSTEIN TELESCOPE Executive summary The European 2011 Conceptual Design Report for Einstein Telescope identified the Euregio Meuse-Rhine and in particular the South Limburg border region as one of the prospective sites for this next generation gravitational wave observatory.
    [Show full text]
  • Stochastic Gravitational Wave Backgrounds
    Stochastic Gravitational Wave Backgrounds Nelson Christensen1;2 z 1ARTEMIS, Universit´eC^oted'Azur, Observatoire C^oted'Azur, CNRS, 06304 Nice, France 2Physics and Astronomy, Carleton College, Northfield, MN 55057, USA Abstract. A stochastic background of gravitational waves can be created by the superposition of a large number of independent sources. The physical processes occurring at the earliest moments of the universe certainly created a stochastic background that exists, at some level, today. This is analogous to the cosmic microwave background, which is an electromagnetic record of the early universe. The recent observations of gravitational waves by the Advanced LIGO and Advanced Virgo detectors imply that there is also a stochastic background that has been created by binary black hole and binary neutron star mergers over the history of the universe. Whether the stochastic background is observed directly, or upper limits placed on it in specific frequency bands, important astrophysical and cosmological statements about it can be made. This review will summarize the current state of research of the stochastic background, from the sources of these gravitational waves, to the current methods used to observe them. Keywords: stochastic gravitational wave background, cosmology, gravitational waves 1. Introduction Gravitational waves are a prediction of Albert Einstein from 1916 [1,2], a consequence of general relativity [3]. Just as an accelerated electric charge will create electromagnetic waves (light), accelerating mass will create gravitational waves. And almost exactly arXiv:1811.08797v1 [gr-qc] 21 Nov 2018 a century after their prediction, gravitational waves were directly observed [4] for the first time by Advanced LIGO [5, 6].
    [Show full text]
  • Multi-Messenger Observations of a Binary Neutron Star Merger
    DRAFT VERSION OCTOBER 6, 2017 Typeset using LATEX twocolumn style in AASTeX61 MULTI-MESSENGER OBSERVATIONS OF A BINARY NEUTRON STAR MERGER LIGO SCIENTIFIC COLLABORATION,VIRGO COLLABORATION AND PARTNER ASTRONOMY GROUPS (Dated: October 6, 2017) ABSTRACT On August 17, 2017 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB170817A) with a time-delay of 1.7swith respect to the merger ⇠ time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance +8 of 40 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range− 0.86 to 2.26 M . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT2017gfo) in NGC 4993 (at 40 Mpc) less ⇠ than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1-m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over 10 days. Following early non-detections, X-ray and radio emission were discovered at the ⇠ transient’s position 9 and 16 days, respectively, after the merger.
    [Show full text]
  • First Low-Frequency Einstein@Home All-Sky Search for Continuous Gravitational Waves in Advanced LIGO Data
    First low-frequency Einstein@Home all-sky search for continuous gravitational waves in Advanced LIGO data The LIGO Scientific Collaboration and The Virgo Collaboration et al. We report results of a deep all-sky search for periodic gravitational waves from isolated neutron stars in data from the first Advanced LIGO observing run. This search investigates the low frequency range of Advanced LIGO data, between 20 and 100 Hz, much of which was not explored in initial LIGO. The search was made possible by the computing power provided by the volunteers of the Einstein@Home project. We find no significant signal candidate and set the most stringent upper limits to date on the amplitude of gravitationalp wave signals from the target population, corresponding to a sensitivity depth of 48:7 [1/ Hz]. At the frequency of best strain sensitivity, near 100 Hz, we set 90% confidence upper limits of 1:8×10−25. At the low end of our frequency range, 20 Hz, we achieve upper limits of 3:9×10−24. At 55 Hz we can exclude sources with ellipticities greater than 10−5 within 100 pc of Earth with fiducial value of the principal moment of inertia of 1038kg m2. I. INTRODUCTION ≈ 20 at 50 Hz. For this reason all-sky searches did not include frequencies below 50 Hz on initial LIGO data. In this paper we report the results of a deep all-sky Ein- Since interferometers sporadically fall out of operation stein@Home [1] search for continuous, nearly monochro- (\lose lock") due to environmental or instrumental dis- matic gravitational waves (GWs) in data from the first turbances or for scheduled maintenance periods, the data Advanced LIGO observing run (O1).
    [Show full text]
  • Model Comparison from LIGO–Virgo Data on GW170817's Binary Components and Consequences for the Merger Remnant
    University of Rhode Island DigitalCommons@URI Physics Faculty Publications Physics 1-16-2020 Model comparison from LIGO–Virgo data on GW170817's binary components and consequences for the merger remnant Robert Coyne Et Al Follow this and additional works at: https://digitalcommons.uri.edu/phys_facpubs Classical and Quantum Gravity PAPER • OPEN ACCESS Recent citations Model comparison from LIGO–Virgo data on - Numerical-relativity simulations of long- lived remnants of binary neutron star GW170817’s binary components and mergers consequences for the merger remnant Roberto De Pietri et al - Stringent constraints on neutron-star radii from multimessenger observations and To cite this article: B P Abbott et al 2020 Class. Quantum Grav. 37 045006 nuclear theory Collin D. Capano et al - Nonparametric inference of neutron star composition, equation of state, and maximum mass with GW170817 View the article online for updates and enhancements. Reed Essick et al This content was downloaded from IP address 132.174.254.155 on 02/04/2020 at 18:13 IOP Classical and Quantum Gravity Class. Quantum Grav. Classical and Quantum Gravity Class. Quantum Grav. 37 (2020) 045006 (43pp) https://doi.org/10.1088/1361-6382/ab5f7c 37 2020 © 2020 IOP Publishing Ltd Model comparison from LIGO–Virgo data on GW170817’s binary components and CQGRDG consequences for the merger remnant 045006 B P Abbott1, R Abbott1, T D Abbott2, S Abraham3, 4,5 6 7 8 9,10 B P Abbott et al F Acernese , K Ackley , C Adams , V B Adya , C Affeldt , M Agathos11,12, K Agatsuma13, N Aggarwal14,
    [Show full text]
  • LIGO SCIENTIFIC COLLABORATION LIGO Scientific Collaboration
    LIGO SCIENTIFIC COLLABORATION Document Type LIGO-M-1900084 LIGO Scientific Collaboration Program 2019-2020 The LSC Program Committee: Gabriela Gonzalez,´ Stephen Fairhurst, P. Ajith, Patrick Brady, Alessandra Buonanno, Alessandra Corsi, Peter Fritschel, Bala Iyer, Joey Key, Sergey Klimenko, Brian Lantz, Albert Lazzarini, David McClelland, David Reitze, Keith Riles, Sheila Rowan, Alicia Sintes, Josh Smith WWW: http://www.ligo.org/ Processed with LATEX on 2019/05/30 LIGO Scientific Collaboration Program 2019-2020 Contents 1 Overview 3 1.1 The LIGO Scientific Collaboration’s Scientific Mission . .3 1.2 LSC Science Goals: Gravitational Wave Targets . .4 1.3 LSC Science Goals: Gravitational Wave Astronomy . .5 2 LIGO Scientific Operations and Scientific Results 7 2.1 LIGO Observatory Operations . .7 2.2 LSC Detector Commissioning and Detector Improvement activities . .8 2.3 Detector Calibration and Data Timing . .8 2.4 Operating computing systems and services for modeling, analysis, and interpretation . .9 2.5 Detector Characterization . 10 2.6 The operations of data analysis search, simulation and interpretation pipelines . 10 2.7 LSC Fellows Program . 11 2.8 Development of data analysis tools to search and interpret the gravitational wave data . 12 2.9 Dissemination of LIGO data and scientific results . 13 2.10 Outreach to the public and the scientific community . 14 2.11 A+ Upgrade Project . 15 2.12 LIGO-India . 15 2.13 Roles in LSC organization . 15 3 Advancing frontiers of Gravitational-Wave Astrophysics, Astronomy and Fundamental Physics: Improved Gravitational Wave Detectors 17 3.1 Substrates . 17 3.2 Suspensions and seismic isolation . 18 3.3 Optical Coatings . 18 3.4 Cryogenics .
    [Show full text]
  • Towards Simulations of Binary Neutron Star Mergers and Core- Collapse Supernovae with Genasis
    University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 8-2010 Towards Simulations of Binary Neutron Star Mergers and Core- Collapse Supernovae with GenASiS Reuben Donald Budiardja University of Tennessee - Knoxville, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the Fluid Dynamics Commons, Numerical Analysis and Scientific Computing Commons, and the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Budiardja, Reuben Donald, "Towards Simulations of Binary Neutron Star Mergers and Core-Collapse Supernovae with GenASiS. " PhD diss., University of Tennessee, 2010. https://trace.tennessee.edu/utk_graddiss/781 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Reuben Donald Budiardja entitled "Towards Simulations of Binary Neutron Star Mergers and Core-Collapse Supernovae with GenASiS." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Physics. Michael W. Guidry, Major Professor We have
    [Show full text]