A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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The Advanced LIGO gravitational wave detectors are second generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA. 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 isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid- and high- frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.
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- abstract The Advanced LIGO gravitational wave detectors are second generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA. 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 regi
- background Sherman Fairchild Foundation at Caltech and Cornell. This material is based upon work supported by NSF's LIGO Laboratory which is a major facility fully funded by the NSF. REFERENCES [1] B. P. Abbottet al.(LIGO Scientific, Virgo), "Observation of Gravitational Waves from a Binary Black Hole Merger," Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [2] J. Aasiet al.(LIGO Scientific), "Advanced LIGO," Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [3] F. Acerneseet al.
- background posteriors for essentially all of them. These considerations should be useful to inform the development of the XG detector network. I. INTRODUCTION In the past decade, the observation of the gravitational- wave (GW) signal emitted by compact binary coalescences (CBCs) gave us a new tool to study the Universe. With more than 200 event candidates observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) detectors, the GWs give us insight into the demography of masses, redshifts, and spins of compac
- background 545) σg (0.333) µg (0.100) Figure 2. P-P plot for 2500 simulated catalogs with random sizes N∼ U (25, 1000). Gray bands show 1-, 2-, and 3- σ intervals under perfect calibration; Kolmogorov-Smirnov p- values are listed in the legend (combinedp-value: 0.20). noise. We assume a two-detector configuration of LIGO Hanford and Livingston at O3 sensitivity [ 3, 54-56]. We use a signal-to-noise ratio of 12 as our detection thresh- old. In total, the population model is described by nine hyperparameters
- background source properties from there derived are naturally suited to astrophysical interpretation and catalog statistics, such as identification of exceptional events from previous and ongoing observing runs. Using the latest LIGO-Virgo-KAGRA data, we thus demonstrate that population inference is not optional to interpret gravitational-wave observations. Pitfalls of parameter estimation-Gravitational- wave (GW) signals observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) interferometers are used to
- background Wang, S. Kastha, S. Wu, M. Sch¨ afer, R. Dhurkunde, and C. D. Capano, Astrophys. J.946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]. [6] R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]. [7] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [8] J. Aasiet al.(LIGO Scientific), Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [9] F. Acerneseet al.(VIRGO), Class. Quant. Grav.32
- background improved sensitivity will allow the detection of additional subdominant modes. To address these challenges, we adopt the semiana- lytic method based on orthonormalized QNMs, which reduces parameter degeneracies and accelerates compu- tations [76]. In this paper, we apply this approach to the event GW250114 082203, henceforth GW250114 [15]. This event was detected by the LIGO detectors [77] on January 14, 2025, and has the largest network signal-to- noise ratio (SNR) to date, with a value of appr
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GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$
A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.
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AI-enabled gravitational-waves searches for binary neutron stars at optimal sensitivity
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Population Properties of Binary Black Holes with Eccentricity
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Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries
All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.
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Constraints on Line-of-Sight Acceleration from O1-O4
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Effective description of lensed gravitational waves diffracted by stellar fields
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Measuring a Black Hole's Area Immediately after Merger: A Direct-Wave Test of Hawking's Area Law
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Fast gravitational waveform models for quasi-circular coalescences of neutron star--black hole binaries
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Model-Independent Search Discards Faint Lensed-Pairs of Gravitational Wave Events in the Sub-Threshold Candidates of GWTC-4
A cross-correlation search of ~11,000 event pairs in GWTC-4 including sub-threshold candidates finds no lensed GW pairs above 3σ, setting an upper bound of ≤1.5/yr on the lensing rate.
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\texttt{calypso}: a Parameter-Conditioned Stochastic Surrogate Model for Circumbinary Accretion Time-Series
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Contrastive self-supervised convolutional autoencoder for core-collapse supernova gravitational-wave detection
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End-to-End Population Inference from Gravitational-Wave Strain using Transformers
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How lonely are the Binary Compact Objects Detected by the LIGO-Virgo-KAGRA Collaboration?
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Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries
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Gravitational-wave astronomy requires population-informed parameter estimation
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Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries
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Measurement prospects for the pair-instability mass cutoff with gravitational waves
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