24 research outputs found
Eenergiebesparingen in de ammoniakfabricage: Voorstudie G-opdracht 1983
No full textDocument uit de collectie Chemische ProcestechnologieDelftChemTechApplied Science
Veiligheidsstudie van de ammoniakfabriek
No full textDocument uit de collectie Chemische ProcestechnologieDelftChemTechApplied Science
Quantum correlations between light and the kilogram-mass mirrors of LIGO
No full textThe measurement of minuscule forces and displacements with ever greater precision is inhibited by the Heisenberg uncertainty principle, which imposes a limit to the precision with which the position of an object can be measured continuously, known as the standard quantum limit1,2,3,4. When light is used as the probe, the standard quantum limit arises from the balance between the uncertainties of the photon radiation pressure applied to the object and of the photon number in the photoelectric detection. The only way to surpass the standard quantum limit is by introducing correlations between the position/momentum uncertainty of the object and the photon number/phase uncertainty of the light that it reflects5. Here we confirm experimentally the theoretical prediction5 that this type of quantum correlation is naturally produced in the Laser Interferometer Gravitational-wave Observatory (LIGO). We characterize and compare noise spectra taken without squeezing and with squeezed vacuum states injected at varying quadrature angles. After subtracting classical noise, our measurements show that the quantum mechanical uncertainties in the phases of the 200-kilowatt laser beams and in the positions of the 40-kilogram mirrors of the Advanced LIGO detectors yield a joint quantum uncertainty that is a factor of 1.4 (3 decibels) below the standard quantum limit. We anticipate that the use of quantum correlations will improve not only the observation of gravitational waves, but also more broadly future quantum noise-limited measurements
Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO
No full textThe global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages. © 2023. The Author(s). Published by the American Astronomical Society
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
No full textOn April 1st, 2019, the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), joined by the Advanced Virgo detector, began the third observing run, a year-long dedicated search for gravitational radiation. The LIGO detectors have achieved a higher duty cycle and greater sensitivity to gravitational waves than ever before, with LIGO Hanford achieving angle-averaged sensitivity to binary neutron star coalescences to a distance of 111 Mpc, and LIGO Livingston to 134 Mpc with duty factors of 74.6% and 77.0% respectively. The improvement in sensitivity and stability is a result of several upgrades to the detectors, including doubled intracavity power, the addition of an in-vacuum optical parametric oscillator for squeezed-light injection, replacement of core optics and end reaction masses, and installation of acoustic mode dampers. This paper explores the purposes behind these upgrades, and explains to the best of our knowledge the noise currently limiting the sensitivity of each detector
Quantum-enhanced advanced LIGO detectors in the era of gravitational-wave astronomy
No full textThe Laser Interferometer Gravitational Wave Observatory (LIGO) has been directly detecting gravitational waves from compact binary mergers since 2015. We report on the first use of squeezed vacuum states in the direct measurement of gravitational waves with the Advanced LIGO H1 and L1 detectors. This achievement is the culmination of decades of research to implement squeezed states in gravitational-wave detectors. During the ongoing O3 observation run, squeezed states are improving the sensitivity of the LIGO interferometers to signals above 50 Hz by up to 3 dB, thereby increasing the expected detection rate by 40% (H1) and 50% (L1)
A Standard Siren Measurement of the Hubble Constant from GW170817 without the Electromagnetic Counterpart
No full textWe perform a statistical standard siren analysis of GW170817. Our analysis does not utilize knowledge of NGC 4993 as the unique host galaxy of the optical counterpart to GW170817. Instead, we consider each galaxy within the GW170817 localization region as a potential host; combining the redshifts from all of the galaxies with the distance estimate from GW170817 provides an estimate of the Hubble constant, H 0 . Considering all galaxies brighter than as equally likely to host a binary neutron star merger, we find km s -1 Mpc -1 (maximum a posteriori and 68.3% highest density posterior interval; assuming a flat H 0 prior in the range km s -1 Mpc -1 ). We explore the dependence of our results on the thresholds by which galaxies are included in our sample, and we show that weighting the host galaxies by stellar mass or star formation rate provides entirely consistent results with potentially tighter constraints. By applying the method to simulated gravitational-wave events and a realistic galaxy catalog we show that, because of the small localization volume, this statistical standard siren analysis of GW170817 provides an unusually informative (top 10%) constraint. Under optimistic assumptions for galaxy completeness and redshift uncertainty, we find that dark binary neutron star measurements of H 0 will converge as , where N is the number of sources. While these statistical estimates are inferior to the value from the counterpart standard siren measurement utilizing NGC 4993 as the unique host, km s -1 Mpc -1 (determined from the same publicly available data), our analysis is a proof-of-principle demonstration of the statistical approach first proposed by Bernard Schutz over 30 yr ago
GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run
No full textThe second gravitational-wave transient catalog, GWTC-2, reported on 39compact binary coalescences observed by the Advanced LIGO and Advanced Virgodetectors between 1 April 2019 15:00 UTC and 1 October 2019 15:00 UTC. Here, wepresent GWTC-2.1, which reports on a deeper list of candidate events observedover the same period. We analyze the final version of the strain data over thisperiod, which is now publicly released. We employ three matched-filter searchpipelines for candidate identification, and estimate the probability ofastrophysical origin for each candidate event. While GWTC-2 used a false alarmrate threshold of 2 per year, we include in GWTC-2.1, 1201 candidates that passa false alarm rate threshold of 2 per day. We calculate the source propertiesof a subset of 44 high-significance candidates that have a probability ofastrophysical origin greater than 0.5, using the default priors. Of thesecandidates, 36 have been reported in GWTC-2. If the 8 additionalhigh-significance candidates presented here are astrophysical, the mass rangeof candidate events that are unambiguously identified as binary black holes(both objects ) is increased compared to GWTC-2, with totalmasses from for GW190924_021846 to forGW190426_190642. The primary components of two new candidate events(GW190403_051519 and GW190426_190642) fall in the mass gap predicted bypair-instability supernova theory. We also expand the population of binarieswith significantly asymmetric mass ratios reported in GWTC-2 by an additionaltwo events ( and at credibility forGW190403_051519 and GW190917_114630 respectively), and find that 2 of the 8 newevents have effective inspiral spins (at credibility), while no binary is consistent with atthe same significance.<br
Search for subsolar-mass black hole binaries in the second part of Advanced LIGO's and Advanced Virgo's third observing run
No full textWe describe a search for gravitational waves from compact binaries with at least one component with mass 0.2 M⊙–1.0 M⊙ and mass ratio q ≥ 0.1 in Advanced LIGO and Advanced Virgo data collected between 1 November 2019, 15:00 UTC and 27 March 2020, 17:00 UTC. No signals were detected. The most significant candidate has a false alarm rate of 0.2yr−1. We estimate the sensitivity of our search over the entirety of Advanced LIGO’s and Advanced Virgo’s third observing run, and present the most stringent limits to date on the merger rate of binary black holes with at least one subsolar-mass component. We use the upper limits to constrain two fiducial scenarios that could produce subsolar-mass black holes: primordial black holes (PBH) and a model of dissipative dark matter. The PBH model uses recent prescriptions for the merger rate of PBH binaries that include a rate suppression factor to effectively account for PBH early binary disruptions. If the PBHs are monochromatically distributed, we can exclude a dark matter fraction in PBHs fPBH ≳ 0.6 (at 90% confidence) in the probed subsolar-mass range. However, if we allow for broad PBH mass distributions we are unable to rule out fPBH = 1. For the dissipative model, where the dark matter has chemistry that allows a small fraction to cool and collapse into black holes, we find an upper bound fDBH < 10−5 on the fraction of atomic dark matter collapsed into black holes
Erratum: "A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo" (2021, ApJ, 909, 218)
No full text[no abstract available
