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1. Multi-messenger Observations of a Binary Neutron Star Merger

Author: LIGO Scientific Collaboration, Virgo Collaboration, GBM, Fermi, INTEGRAL, Collaboration, IceCube, Team, AstroSat Cadmium Zinc Telluride Imager, Collaboration, IPN, Collaboration, The Insight-Hxmt, Collaboration, ANTARES, Collaboration, The Swift, Team, AGILE, Team, The 1M2H, Collaboration, The Dark Energy Camera GW-EM, Collaboration, the DES, Collaboration, The DLT40, GRAWITA, TeAm, GRAvitational Wave Inaf, Collaboration, The Fermi Large Area Telescope, ATCA, Array, Australia Telescope Compact, ASKAP, Pathfinder, Australian SKA, Group, Las Cumbres Observatory, OzGrav, DWF, AST3, Collaborations, CAASTRO, Collaboration, The VINROUGE, Collaboration, MASTER, J-GEM, GROWTH, JAGWAR, NRAO, Caltech, TTU-NRAO, Collaborations, NuSTAR, Pan-STARRS, Team, The MAXI, Consortium, TZAC, Collaboration, KU, Telescope, Nordic Optical, ePESSTO, GROND, University, Texas Tech, Group, SALT, TOROS, Collaboration, Transient Robotic Observatory of the South, Collaboration, The BOOTES, MWA, Array, Murchison Widefield, Collaboration, The CALET, Collaboration, IKI-GW Follow-up, Collaboration, H. E. S. S., Collaboration, LOFAR, LWA, Array, Long Wavelength, Collaboration, HAWC, Collaboration, The Pierre Auger, Collaboration, ALMA, Team, Euro VLBI, Collaboration, Pi of the Sky, University, The Chandra Team at McGill, DFN, Network, Desert Fireball, ATLAS, Survey, High Time Resolution Universe, RIMAS, RATIR, and Africa/MeerKAT, SKA South
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: On 2017 August 17 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 (GRB 170817A) with a time delay of $\sim$1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg$^2$ at a luminosity distance of $40^{+8}_{-8}$ 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 Msun. 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 AT 2017gfo) in NGC 4993 (at $\sim$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 $\sim$10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim$9 and $\sim$16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. (Abridged), Comment: This is a reproduction of the article published in the Astrophysical Journal Letters, under the terms of the Creative Commons Attribution 3.0 licence
Published: 2017
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2. Multi-messenger Observations of a Binary Neutron Star Merger

Author: Collaboration, LIGO Scientific, Collaboration, Virgo, Fermi, GBM, INTEGRAL, Collaboration, IceCube, Team, AstroSat Cadmium Zinc Telluride Imager, Collaboration, IPN, Collaboration, The Insight-Hxmt, Collaboration, ANTARES, Collaboration, The Swift, Team, AGILE, Team, The 1M2H, Collaboration, The Dark Energy Camera GW-EM, Collaboration, the DES, Collaboration, The DLT40, GRAWITA, TeAm, GRAvitational Wave Inaf, Collaboration, The Fermi Large Area Telescope, ATCA, Array, Australia Telescope Compact, ASKAP, Pathfinder, Australian SKA, Group, Las Cumbres Observatory, OzGrav, DWF, AST3, Collaborations, CAASTRO, Collaboration, The VINROUGE, Collaboration, MASTER, J-GEM, GROWTH, JAGWAR, Caltech-, NRAO, TTU-NRAO, Collaborations, NuSTAR, Pan-STARRS, Team, The MAXI, Consortium, TZAC, Collaboration, KU, Telescope, Nordic Optical, ePESSTO, GROND, University, Texas Tech, Group, SALT, TOROS, Collaboration, Transient Robotic Observatory of the South, Collaboration, The BOOTES, MWA, Array, Murchison Widefield, Collaboration, The CALET, Collaboration, IKI-GW Follow-up, Collaboration, H. E. S. S., Collaboration, LOFAR, LWA, Array, Long Wavelength, Collaboration, HAWC, Collaboration, The Pierre Auger, Collaboration, ALMA, Team, Euro VLBI, Collaboration, Pi of the Sky, University, The Chandra Team at McGill, DFN, Network, Desert Fireball, ATLAS, Survey, High Time Resolution Universe, RIMAS, RATIR, Africa/MeerKAT, SKA South, Van Eerten, Hendrik, Calloni, E., DE ROSA, Rosario, Garufi, F., De Laurentis, M., Di Girolamo, T., Milano, L., Barbato, F., Colalillo, R., Guarino, Fausto, Valore, L., Allocca, Annalisa, Fermi, Gbm, Integral, Icecube, Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, Ipn, Collaboration, The Insight-Hxmt Collaboration, Antares, Collaboration, The Swift Collaboration, Agile, Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, Ozgrav, Dwf, (Deeper, Wider, Faster, Program), Ast3, and CAASTRO Collaborations, The VINROUGE Collaboration, Master, Collaboration, J-GEM, Growth, Jagwar, Caltech-, Nrao, TTU-NRAO, and NuSTAR Collaborations, Pan-STARRS, The MAXI Team, Tzac, Consortium, Collaboration, Ku, Nordic Optical Telescope, Epessto, Grond, Texas Tech University, Salt, Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, Collaboration, H. E. S. S., Lofar, Collaboration, LWA: Long Wavelength Array, Hawc, Collaboration, The Pierre Auger Collaboration, Alma, Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, Atlas, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT, and Pinto, Innocenzo
Subjects: astro-ph.HE, Astrophysics::High Energy Astrophysical Phenomena, gr-qc, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: On 2017 August 17 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 (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with 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 of ${40}_{-8}^{+8}$ 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 $\,{M}_{\odot }$. 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 AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) 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 $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.
Published: 2017
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3. Multi-messenger Observations of a Binary Neutron Star Merger

Author: LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-HXMT Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF (Deeper, Wider, Faster Program), AST3, and CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, Caltech-NRAO, TTU-NRAO, and NuSTAR Collaborations, Pan-STARRS, The MAXI Team, TZAC Consortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H.E.S.S. Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT
Subjects: stars: neutron, gravitational waves
Abstract: 著者: 所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 海老沢, 研; 磯部, 直樹; 下向, 怜歩; 菅原, 泰晴; 冨田, 洋; 上野, 史郎; 桂川, 美穂; 中島, 真也; 小高, 裕和; 高橋, 忠幸, Author(s): Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Ebisawa, Ken; Isobe, Naoki; Shimomukai, Reiho; Sugawara, Yasuharu; Tomida,Hiroshi;Ueno, Shiro; Katsuragawa, Miho; Nakashima, Shinya; Odaka, Hirokazu; Takahashi, Tadayuki, Accepted: 2017-10-06, 資料番号: SA1170283000
Published: 2017

4. Gravitational Wave Constraints on Planetary-Mass Primordial Black Holes Using LIGO O3a Data.

Author: Miller AL, Aggarwal N, Clesse S, De Lillo F, Sachdev S, Astone P, Palomba C, Piccinni OJ, and Pierini L
Abstract: Gravitational waves from subsolar mass inspiraling compact objects would provide almost smoking-gun evidence for primordial black holes (PBHs). We perform the first search for inspiraling planetary-mass compact objects in equal-mass and highly asymmetric mass-ratio binaries using data from the first half of the LIGO-Virgo-KAGRA third observing run. Though we do not find any significant candidates, we determine the maximum luminosity distance reachable with our search to be of O(0.1-100) kpc, and corresponding model-independent upper limits on the merger rate densities to be O(10^{3}-10^{-7}) kpc^{-3} yr^{-1} for systems with chirp masses of O(10^{-4}-10^{-2})M_{⊙}, respectively. Furthermore, we interpret these rate densities as arising from PBH binaries and constrain the fraction of dark matter that such objects could comprise. For equal-mass PBH binaries, we find that these objects would compose less than 4%-100% of DM for PBH masses of 10^{-2}M_{⊙} to 2×10^{-3}M_{⊙}, respectively. For asymmetric binaries, assuming one black hole mass corresponds to a peak in the mass function at 2.5M_{⊙}, a PBH dark-matter fraction of 10% and a second, much lighter PBH, we constrain the mass function of the second PBH to be less than 1 for masses between 1.5×10^{-5}M_{⊙} and 2×10^{-4}M_{⊙}. Our constraints, recently released, are robust enough to be applied to any PBH or exotic compact object binary formation models, and complement existence microlensing results.
Published: 2024
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5. Quantum Enhanced Balanced Heterodyne Readout for Differential Interferometry.

Author: Gould DW, Adya VB, Chua SSY, Junker J, Wilken D, McRae TG, Slagmolen BJJ, Yap MJ, Ward RL, Heurs M, and McClelland DE
Abstract: Conventional heterodyne readout schemes are now under reconsideration due to the realization of techniques to evade its inherent 3 dB signal-to-noise penalty. The application of high-frequency, quadrature-entangled, two-mode squeezed states can further improve the readout sensitivity of audio-band signals. In this Letter, we experimentally demonstrate quantum-enhanced heterodyne readout of two spatially distinct interferometers with direct optical signal combination, circumventing the 3 dB heterodyne signal-to-noise penalty. Applying a high-frequency, quadrature-entangled, two-mode squeezed state, we show further signal-to-noise improvement of an injected audio band signal of 3.5 dB. This technique is applicable for quantum-limited high-precision experiments, with application to searches for quantum gravity, searches for dark matter, gravitational wave detection, and wavelength-multiplexed quantum communication.
Published: 2024
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6. Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243.

Author: Vigna-Gómez A, Willcox R, Tamborra I, Mandel I, Renzo M, Wagg T, Janka HT, Kresse D, Bodensteiner J, Shenar T, and Tauris TM
Abstract: The recently reported observation of VFTS 243 is the first example of a massive black-hole binary system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M_{⊙}) and near-circular orbit (e≈0.02) of VFTS 243 suggest that the progenitor star experienced complete collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence level, the natal kick velocity (mass decrement) is ≲10 km/s (≲1.0M_{⊙}), with a full probability distribution that peaks when ≈0.3M_{⊙} were ejected, presumably in neutrinos, and the black hole experienced a natal kick of 4 km/s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0-0.2%. Such a small neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Published: 2024
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7. Achieving the Fundamental Quantum Limit of Linear Waveform Estimation.

Author: Gardner JW, Gefen T, Haine SA, Hope JJ, and Chen Y
Abstract: Sensing a classical signal using a linear quantum device is a pervasive application of quantum-enhanced measurement. The fundamental precision limits of linear waveform estimation, however, are not fully understood. In certain cases, there is an unexplained gap between the known waveform-estimation quantum Cramér-Rao bound and the optimal sensitivity from quadrature measurement of the outgoing mode from the device. We resolve this gap by establishing the fundamental precision limit, the waveform-estimation Holevo Cramér-Rao bound, and how to achieve it using a nonstationary measurement. We apply our results to detuned gravitational-wave interferometry to accelerate the search for postmerger remnants from binary neutron-star mergers. If we have an unequal weighting between estimating the signal's power and phase, then we propose how to further improve the signal-to-noise ratio by a factor of sqrt[2] using this nonstationary measurement.
Published: 2024
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8. A case for a binary black hole system revealed via quasi-periodic outflows.

Author: Pasham DR, Tombesi F, Suková P, Zajaček M, Rakshit S, Coughlin E, Kosec P, Karas V, Masterson M, Mummery A, Holoien TW, Guolo M, Hinkle J, Ripperda B, Witzany V, Shappee B, Kara E, Horesh A, van Velzen S, Sfaradi I, Kaplan D, Burger N, Murphy T, Remillard R, Steiner JF, Wevers T, Arcodia R, Buchner J, Merloni A, Malyali A, Fabian A, Fausnaugh M, Daylan T, Altamirano D, Payne A, and Ferraraa EC
Abstract: Binaries containing a compact object orbiting a supermassive black hole are thought to be precursors of gravitational wave events, but their identification has been extremely challenging. Here, we report quasi-periodic variability in x-ray absorption, which we interpret as quasi-periodic outflows (QPOuts) from a previously low-luminosity active galactic nucleus after an outburst, likely caused by a stellar tidal disruption. We rule out several models based on observed properties and instead show using general relativistic magnetohydrodynamic simulations that QPOuts, separated by roughly 8.3 days, can be explained with an intermediate-mass black hole secondary on a mildly eccentric orbit at a mean distance of about 100 gravitational radii from the primary. Our work suggests that QPOuts could be a new way to identify intermediate/extreme-mass ratio binary candidates.
Published: 2024
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9. Heavy-element production in a compact object merger observed by JWST.

Author: Levan AJ, Gompertz BP, Salafia OS, Bulla M, Burns E, Hotokezaka K, Izzo L, Lamb GP, Malesani DB, Oates SR, Ravasio ME, Rouco Escorial A, Schneider B, Sarin N, Schulze S, Tanvir NR, Ackley K, Anderson G, Brammer GB, Christensen L, Dhillon VS, Evans PA, Fausnaugh M, Fong WF, Fruchter AS, Fryer C, Fynbo JPU, Gaspari N, Heintz KE, Hjorth J, Kennea JA, Kennedy MR, Laskar T, Leloudas G, Mandel I, Martin-Carrillo A, Metzger BD, Nicholl M, Nugent A, Palmerio JT, Pugliese G, Rastinejad J, Rhodes L, Rossi A, Saccardi A, Smartt SJ, Stevance HF, Tohuvavohu A, van der Horst A, Vergani SD, Watson D, Barclay T, Bhirombhakdi K, Breedt E, Breeveld AA, Brown AJ, Campana S, Chrimes AA, D'Avanzo P, D'Elia V, De Pasquale M, Dyer MJ, Galloway DK, Garbutt JA, Green MJ, Hartmann DH, Jakobsson P, Kerry P, Kouveliotou C, Langeroodi D, Le Floc'h E, Leung JK, Littlefair SP, Munday J, O'Brien P, Parsons SG, Pelisoli I, Sahman DI, Salvaterra R, Sbarufatti B, Steeghs D, Tagliaferri G, Thöne CC, de Ugarte Postigo A, and Kann DA
Abstract: The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs) 1 , sources of high-frequency gravitational waves (GWs) 2 and likely production sites for heavy-element nucleosynthesis by means of rapid neutron capture (the r-process) 3 . Here we present observations of the exceptionally bright GRB 230307A. We show that GRB 230307A belongs to the class of long-duration GRBs associated with compact object mergers 4-6 and contains a kilonova similar to AT2017gfo, associated with the GW merger GW170817 (refs. 7-12 ). We obtained James Webb Space Telescope (JWST) mid-infrared imaging and spectroscopy 29 and 61 days after the burst. The spectroscopy shows an emission line at 2.15 microns, which we interpret as tellurium (atomic mass A = 130) and a very red source, emitting most of its light in the mid-infrared owing to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy-element nucleosynthesis across the Universe., (© 2023. The Author(s).)
Published: 2024
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10. A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes.

Author: Barr ED, Dutta A, Freire PCC, Cadelano M, Gautam T, Kramer M, Pallanca C, Ransom SM, Ridolfi A, Stappers BW, Tauris TM, Venkatraman Krishnan V, Wex N, Bailes M, Behrend J, Buchner S, Burgay M, Chen W, Champion DJ, Chen CR, Corongiu A, Geyer M, Men YP, Padmanabh PV, and Possenti A
Abstract: Some compact objects observed in gravitational wave events have masses in the gap between known neutron stars (NSs) and black holes (BHs). The nature of these mass gap objects is unknown, as is the formation of their host binary systems. We report pulsar timing observations made with the Karoo Array Telescope (MeerKAT) of PSR J0514-4002E, an eccentric binary millisecond pulsar in the globular cluster NGC 1851. We found a total binary mass of 3.887 ± 0.004 solar masses ( M ⊙ ), and multiwavelength observations show that the pulsar's binary companion is also a compact object. The companion's mass (2.09 to 2.71 M ⊙ , 95% confidence interval) is in the mass gap, indicating either a very massive NS or a low-mass BH. We propose that the companion formed in a merger between two earlier NSs.
Published: 2024
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11. Roadmap on optical sensors.

Author: Ferreira MFS, Brambilla G, Thévenaz L, Feng X, Zhang L, Sumetsky M, Jones C, Pedireddy S, Vollmer F, Dragic PD, Henderson-Sapir O, Ottaway DJ, Strupiechonski E, Hernandez-Cardoso GG, Hernandez-Serrano AI, González FJ, Castro Camus E, Méndez A, Saccomandi P, Quan Q, Xie Z, Reinhard BM, and Diem M
Abstract: Optical sensors and sensing technologies are playing a more and more important role in our modern world. From micro-probes to large devices used in such diverse areas like medical diagnosis, defence, monitoring of industrial and environmental conditions, optics can be used in a variety of ways to achieve compact, low cost, stand-off sensing with extreme sensitivity and selectivity. Actually, the challenges to the design and functioning of an optical sensor for a particular application requires intimate knowledge of the optical, material, and environmental properties that can affect its performance. This roadmap on optical sensors addresses different technologies and application areas. It is constituted by twelve contributions authored by world-leading experts, providing insight into the current state-of-the-art and the challenges their respective fields face. Two articles address the area of optical fibre sensors, encompassing both conventional and specialty optical fibres. Several other articles are dedicated to laser-based sensors, micro- and nano-engineered sensors, whispering-gallery mode and plasmonic sensors. The use of optical sensors in chemical, biological and biomedical areas is discussed in some other papers. Different approaches required to satisfy applications at visible, infrared and THz spectral regions are also discussed., (© 2023 The Author(s). Published by IOP Publishing Ltd.)
Published: 2024
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12. Mitigating stimulated Brillouin scattering in multimode fibers with focused output via wavefront shaping.

Author: Chen CW, Nguyen LV, Wisal K, Wei S, Warren-Smith SC, Henderson-Sapir O, Schartner EP, Ahmadi P, Ebendorff-Heidepriem H, Stone AD, Ottaway DJ, and Cao H
Abstract: The key challenge for high-power delivery through optical fibers is overcoming nonlinear optical effects. To keep a smooth output beam, most techniques for mitigating optical nonlinearities are restricted to single-mode fibers. Moving out of the single-mode paradigm, we show experimentally that wavefront-shaping of coherent input light to a highly multimode fiber can increase the power threshold for stimulated Brillouin scattering (SBS) by an order of magnitude, whilst simultaneously controlling the output beam profile. The SBS suppression results from an effective broadening of the Brillouin spectrum under multimode excitation, without broadening of transmitted light. Strongest suppression is achieved with selective mode excitation that gives the broadest Brillouin spectrum. Our method is efficient, robust, and applicable to continuous waves and pulses. This work points toward a promising route for mitigating detrimental nonlinear effects in optical fibers, enabling further power scaling of high-power fiber systems for applications to directed energy, remote sensing, and gravitational-wave detection., (© 2023. The Author(s).)
Published: 2023
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13. Minutes-duration optical flares with supernova luminosities.

Author: Ho AYQ, Perley DA, Chen P, Schulze S, Dhillon V, Kumar H, Suresh A, Swain V, Bremer M, Smartt SJ, Anderson JP, Anupama GC, Awiphan S, Barway S, Bellm EC, Ben-Ami S, Bhalerao V, de Boer T, Brink TG, Burruss R, Chandra P, Chen TW, Chen WP, Cooke J, Coughlin MW, Das KK, Drake AJ, Filippenko AV, Freeburn J, Fremling C, Fulton MD, Gal-Yam A, Galbany L, Gao H, Graham MJ, Gromadzki M, Gutiérrez CP, Hinds KR, Inserra C, A J N, Karambelkar V, Kasliwal MM, Kulkarni S, Müller-Bravo TE, Magnier EA, Mahabal AA, Moore T, Ngeow CC, Nicholl M, Ofek EO, Omand CMB, Onori F, Pan YC, Pessi PJ, Petitpas G, Polishook D, Poshyachinda S, Pursiainen M, Riddle R, Rodriguez AC, Rusholme B, Segre E, Sharma Y, Smith KW, Sollerman J, Srivastav S, Strotjohann NL, Suhr M, Svinkin D, Wang Y, Wiseman P, Wold A, Yang S, Yang Y, Yao Y, Young DR, and Zheng W
Abstract: In recent years, certain luminous extragalactic optical transients have been observed to last only a few days 1 . Their short observed duration implies a different powering mechanism from the most common luminous extragalactic transients (supernovae), whose timescale is weeks 2 . Some short-duration transients, most notably AT2018cow (ref. 3 ), show blue optical colours and bright radio and X-ray emission 4 . Several AT2018cow-like transients have shown hints of a long-lived embedded energy source 5 , such as X-ray variability 6,7 , prolonged ultraviolet emission 8 , a tentative X-ray quasiperiodic oscillation 9,10 and large energies coupled to fast (but subrelativistic) radio-emitting ejecta 11,12 . Here we report observations of minutes-duration optical flares in the aftermath of an AT2018cow-like transient, AT2022tsd (the 'Tasmanian Devil'). The flares occur over a period of months, are highly energetic and are probably nonthermal, implying that they arise from a near-relativistic outflow or jet. Our observations confirm that, in some AT2018cow-like transients, the embedded energy source is a compact object, either a magnetar or an accreting black hole., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2023
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14. Black Hole Spectroscopy by Mode Cleaning.

Author: Ma S, Sun L, and Chen Y
Abstract: We formulate a Bayesian framework to analyze ringdown gravitational waves from colliding binary black holes and test the no-hair theorem. The idea hinges on mode cleaning-revealing subdominant oscillation modes by removing dominant ones using newly proposed "rational filters." By incorporating the filter into Bayesian inference, we construct a likelihood function that depends only on the mass and spin of the remnant black hole (no dependence on mode amplitudes and phases) and implement an efficient pipeline to constrain the remnant mass and spin without Markov chain Monte Carlo. We test ringdown models by cleaning combinations of different modes and evaluating the consistency between the residual data and pure noise. The model evidence and Bayes factor are used to demonstrate the presence of a particular mode and to infer the mode starting time. In addition, we design a hybrid approach to estimate the remnant black hole properties exclusively from a single mode using Markov chain Monte Carlo after mode cleaning. We apply the framework to GW150914 and demonstrate more definitive evidence of the first overtone by cleaning the fundamental mode. This new framework provides a powerful tool for black hole spectroscopy in future gravitational-wave events.
Published: 2023
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15. A close quasar pair in a disk-disk galaxy merger at z = 2.17.

Author: Chen YC, Liu X, Foord A, Shen Y, Oguri M, Chen N, Di Matteo T, Holgado M, Hwang HC, and Zakamska N
Abstract: Galaxy mergers produce pairs of supermassive black holes (SMBHs), which may be witnessed as dual quasars if both SMBHs are rapidly accreting. The kiloparsec (kpc)-scale separation represents a physical regime sufficiently close for merger-induced effects to be important 1 yet wide enough to be directly resolvable with the facilities currently available. Whereas many kpc-scale, dual active galactic nuclei-the low-luminosity counterparts of quasars-have been observed in low-redshift mergers 2 , no unambiguous dual quasar is known at cosmic noon (z ≈ 2), the peak of global star formation and quasar activity 3,4 . Here we report multiwavelength observations of Sloan Digital Sky Survey (SDSS) J0749 + 2255 as a kpc-scale, dual-quasar system hosted by a galaxy merger at cosmic noon (z = 2.17). We discover extended host galaxies associated with the much brighter compact quasar nuclei (separated by 0.46″ or 3.8 kpc) and low-surface-brightness tidal features as evidence for galactic interactions. Unlike its low-redshift and low-luminosity counterparts, SDSS J0749 + 2255 is hosted by massive compact disk-dominated galaxies. The apparent lack of stellar bulges and the fact that SDSS J0749 + 2255 already follows the local SMBH mass-host stellar mass relation, suggest that at least some SMBHs may have formed before their host stellar bulges. While still at kpc-scale separations where the host-galaxy gravitational potential dominates, the two SMBHs may evolve into a gravitationally bound binary system in around 0.22 Gyr., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2023
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16. Magnetic Dynamo Caused by Axions in Neutron Stars.

Author: Anzuini F, Pons JA, Gómez-Bañón A, Lasky PD, Bianchini F, and Melatos A
Abstract: The coupling between axions and photons modifies Maxwell's equations, introducing a dynamo term in the magnetic induction equation. In neutron stars, for critical values of the axion decay constant and axion mass, the magnetic dynamo mechanism increases the total magnetic energy of the star. We show that this generates substantial internal heating due to enhanced dissipation of crustal electric currents. These mechanisms would lead magnetized neutron stars to increase their magnetic energy and thermal luminosity by several orders of magnitude, in contrast to observations of thermally emitting neutron stars. To prevent the activation of the dynamo, bounds on the allowed axion parameter space can be derived.
Published: 2023
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17. Publisher Correction: A very luminous jet from the disruption of a star by a massive black hole.

Author: Andreoni I, Coughlin MW, Perley DA, Yao Y, Lu W, Cenko SB, Kumar H, Anand S, Ho AYQ, Kasliwal MM, de Ugarte Postigo A, Sagués-Carracedo A, Schulze S, Kann DA, Kulkarni SR, Sollerman J, Tanvir N, Rest A, Izzo L, Somalwar JJ, Kaplan DL, Ahumada T, Anupama GC, Auchettl K, Barway S, Bellm EC, Bhalerao V, Bloom JS, Bremer M, Bulla M, Burns E, Campana S, Chandra P, Charalampopoulos P, Cooke J, D'Elia V, Das KK, Dobie D, Fernández JFA, Freeburn J, Fremling C, Gezari S, Goode S, Graham MJ, Hammerstein E, Karambelkar VR, Kilpatrick CD, Kool EC, Krips M, Laher RR, Leloudas G, Levan A, Lundquist MJ, Mahabal AA, Medford MS, Miller MC, Möller A, Mooley KP, Nayana AJ, Nir G, Pang PTH, Paraskeva E, Perley RA, Petitpas G, Pursiainen M, Ravi V, Ridden-Harper R, Riddle R, Rigault M, Rodriguez AC, Rusholme B, Sharma Y, Smith IA, Stein RD, Thöne C, Tohuvavohu A, Valdes F, van Roestel J, Vergani SD, Wang Q, and Zhang J
Published: 2023
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18. Neutron star mass estimates from gamma-ray eclipses in spider millisecond pulsar binaries.

Author: Clark CJ, Kerr M, Barr ED, Bhattacharyya B, Breton RP, Bruel P, Camilo F, Chen W, Cognard I, Cromartie HT, Deneva J, Dhillon VS, Guillemot L, Kennedy MR, Kramer M, Lyne AG, Sánchez DM, Nieder L, Phillips C, Ransom SM, Ray PS, Roberts MSE, Roy J, Smith DA, Spiewak R, Stappers BW, Tabassum S, Theureau G, and Voisin G
Abstract: Reliable neutron star mass measurements are key to determining the equation of state of cold nuclear matter, but such measurements are rare. Black widows and redbacks are compact binaries consisting of millisecond pulsars and semi-degenerate companion stars. Spectroscopy of the optically bright companions can determine their radial velocities, providing inclination-dependent pulsar mass estimates. Although inclinations can be inferred from subtle features in optical light curves, such estimates may be systematically biased due to incomplete heating models and poorly understood variability. Using data from the Fermi Large Area Telescope, we have searched for gamma-ray eclipses from 49 spider systems, discovering significant eclipses in 7 systems, including the prototypical black widow PSR B1957+20. Gamma-ray eclipses require direct occultation of the pulsar by the companion, and so the detection, or significant exclusion, of a gamma-ray eclipse strictly limits the binary inclination angle, providing new robust, model-independent pulsar mass constraints. For PSR B1957+20, the eclipse implies a much lighter pulsar (1.81 ± 0.07 solar masses) than inferred from optical light curve modelling., Competing Interests: Competing interestsThe authors declare no competing interests., (© The Author(s) 2023.)
Published: 2023
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19. A very luminous jet from the disruption of a star by a massive black hole.

Author: Andreoni I, Coughlin MW, Perley DA, Yao Y, Lu W, Cenko SB, Kumar H, Anand S, Ho AYQ, Kasliwal MM, de Ugarte Postigo A, Sagués-Carracedo A, Schulze S, Kann DA, Kulkarni SR, Sollerman J, Tanvir N, Rest A, Izzo L, Somalwar JJ, Kaplan DL, Ahumada T, Anupama GC, Auchettl K, Barway S, Bellm EC, Bhalerao V, Bloom JS, Bremer M, Bulla M, Burns E, Campana S, Chandra P, Charalampopoulos P, Cooke J, D'Elia V, Das KK, Dobie D, Fernández JFA, Freeburn J, Fremling C, Gezari S, Goode S, Graham MJ, Hammerstein E, Karambelkar VR, Kilpatrick CD, Kool EC, Krips M, Laher RR, Leloudas G, Levan A, Lundquist MJ, Mahabal AA, Medford MS, Miller MC, Möller A, Mooley KP, Nayana AJ, Nir G, Pang PTH, Paraskeva E, Perley RA, Petitpas G, Pursiainen M, Ravi V, Ridden-Harper R, Riddle R, Rigault M, Rodriguez AC, Rusholme B, Sharma Y, Smith IA, Stein RD, Thöne C, Tohuvavohu A, Valdes F, van Roestel J, Vergani SD, Wang Q, and Zhang J
Abstract: Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close 1 . TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet 2-9 , but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in γ-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z = 1.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron 'afterglow', probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility 10 survey data, we calculate a rate of [Formula: see text] per gigapascals cubed per year for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations 11 . Correcting for the beaming angle effects, this rate confirms that approximately 1 per cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2022
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20. General-relativistic precession in a black-hole binary.

Author: Hannam M, Hoy C, Thompson JE, Fairhurst S, Raymond V, Colleoni M, Davis D, Estellés H, Haster CJ, Helmling-Cornell A, Husa S, Keitel D, Massinger TJ, Menéndez-Vázquez A, Mogushi K, Ossokine S, Payne E, Pratten G, Romero-Shaw I, Sadiq J, Schmidt P, Tenorio R, Udall R, Veitch J, Williams D, Yelikar AB, and Zimmerman A
Abstract: The general-relativistic phenomenon of spin-induced orbital precession has not yet been observed in strong-field gravity. Gravitational-wave observations of binary black holes (BBHs) are prime candidates, as we expect the astrophysical binary population to contain precessing binaries 1,2 . Imprints of precession have been investigated in several signals 3-5 , but no definitive identification of orbital precession has been reported in any of the 84 BBH observations so far 5-7 by the Advanced LIGO and Virgo detectors 8,9 . Here we report the measurement of strong-field precession in the LIGO-Virgo-Kagra gravitational-wave signal GW200129. The binary's orbit precesses at a rate ten orders of magnitude faster than previous weak-field measurements from binary pulsars 10-13 . We also find that the primary black hole is probably highly spinning. According to current binary population estimates, a GW200129-like signal is extremely unlikely, and therefore presents a direct challenge to many current binary-formation models., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2022
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21. Common envelope binary interaction simulations between a thermally pulsating AGB star and a low mass companion.

Author: González-Bolívar M, De Marco O, Lau MYM, Hirai R, and Price DJ
Abstract: At least one in five of all planetary nebulae are the product of a common envelope (CE) interaction, where the companion in-spirals into the envelope of an asymptotic giant branch (AGB) star ejecting the nebula and leaving behind a compact binary. In this work we carry out 3D smoothed particle hydrodynamics simulations of the CE interaction between a 1.7 M ⊙ AGB star and a 0.6 M ⊙ companion. We model the AGB structure using a 1D stellar model taken at the seventh thermal pulse. The interaction takes place when the giant is on the expanding phase of the seventh thermal pulse and has a radius of 250 R ⊙ . The post-CE orbital separations varies between 20 and 31 R ⊙ , with the inclusion of recombination energy resulting in wider separations. Based on the observed short in-spiral time-scales, we suggest that thermal pulses can trigger CEs, extending the ability of AGB stars to capture companions into CEs, that would lead to the prediction of a larger population of post-AGB, post-CE binaries. Simulations that include a tabulated equation of state unbind a great deal more gas, likely unbinding the entire envelope on short time-scales. The shape of the CE after the in-spiral is more spherical for AGB than red giant branch stars, and even more so if recombination energy is included. We expect that the planetary nebula formed from this CE will have different features from those predicted by Zou et al. 2020., (© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.)
Published: 2022
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22. The role of the hadron-quark phase transition in core-collapse supernovae.

Author: Jakobus P, Müller B, Heger A, Motornenko A, Steinheimer J, and Stoecker H
Abstract: The hadron-quark phase transition in quantum chromodynamics has been suggested as an alternative explosion mechanism for core-collapse supernovae. We study the impact of three different hadron-quark equations of state (EoS) with first-order (DD2F_SF, STOS-B145) and second-order (CMF) phase transitions on supernova dynamics by performing 97 simulations for solar- and zero-metallicity progenitors in the range of [Formula: see text]. We find explosions only for two low-compactness models (14 and [Formula: see text]) with the DD2F_SF EoS, both with low explosion energies of [Formula: see text]. These weak explosions are characterized by a neutrino signal with several minibursts in the explosion phase due to complex reverse shock dynamics, in addition to the typical second neutrino burst for phase-transition-driven explosions. The nucleosynthesis shows significant overproduction of nuclei such as 90 Zr for the [Formula: see text] zero-metallicity model and 94 Zr for the [Formula: see text] solar-metallicity model, but the overproduction factors are not large enough to place constraints on the occurrence of such explosions. Several other low-compactness models using the DD2F_SF EoS and two high-compactness models using the STOS EoS end up as failed explosions and emit a second neutrino burst. For the CMF EoS, the phase transition never leads to a second bounce and explosion. For all three EoS, inverted convection occurs deep in the core of the protocompact star due to anomalous behaviour of thermodynamic derivatives in the mixed phase, which heats the core to entropies up to 4 k B /baryon and may have a distinctive gravitational-wave signature, also for a second-order phase transition., (© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.)
Published: 2022
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23. Search for Subsolar-Mass Binaries in the First Half of Advanced LIGO's and Advanced Virgo's Third Observing Run.

Author: Abbott R, Abbott TD, Acernese F, Ackley K, Adams C, Adhikari N, Adhikari RX, Adya VB, Affeldt C, Agarwal D, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Albanesi S, Allocca A, Altin PA, Amato A, Anand C, Anand S, Ananyeva A, Anderson SB, Anderson WG, Andrade T, Andres N, Andrić T, Angelova SV, Ansoldi S, Antelis JM, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Aronson SM, Arun KG, Asali Y, Ashton G, Assiduo M, Aston SM, Astone P, Aubin F, Austin C, Babak S, Badaracco F, Bader MKM, Badger C, Bae S, Baer AM, Bagnasco S, Bai Y, Baird J, Ball M, Ballardin G, Ballmer SW, Balsamo A, Baltus G, Banagiri S, Bankar D, Barayoga JC, Barbieri C, Barish BC, Barker D, Barneo P, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Barton MA, Bartos I, Bassiri R, Basti A, Bawaj M, Bayley JC, Baylor AC, Bazzan M, Bécsy B, Bedakihale VM, Bejger M, Belahcene I, Benedetto V, Beniwal D, Bennett TF, Bentley JD, BenYaala M, Bergamin F, Berger BK, Bernuzzi S, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Beveridge D, Bhandare R, Bhardwaj U, Bhattacharjee D, Bhaumik S, Bilenko IA, Billingsley G, Bini S, Birney R, Birnholtz O, Biscans S, Bischi M, Biscoveanu S, Bisht A, Biswas B, Bitossi M, Bizouard MA, Blackburn JK, Blair CD, Blair DG, Blair RM, Bobba F, Bode N, Boer M, Bogaert G, Boldrini M, Bonavena LD, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Bork R, Boschi V, Bose N, Bose S, Bossilkov V, Boudart V, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branch A, Branchesi M, Brau JE, Breschi M, Briant T, Briggs JH, Brillet A, Brinkmann M, Brockill P, Brooks AF, Brooks J, Brown DD, Brunett S, Bruno G, Bruntz R, Bryant J, Bulik T, Bulten HJ, Buonanno A, Buscicchio R, Buskulic D, Buy C, Byer RL, Cadonati L, Cagnoli G, Cahillane C, Bustillo JC, Callaghan JD, Callister TA, Calloni E, Cameron J, Camp JB, Canepa M, Canevarolo S, Cannavacciuolo M, Cannon KC, Cao H, Capote E, Carapella G, Carbognani F, 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Pereira A, Pereira T, Perez CJ, Périgois C, Perkins CC, Perreca A, Perriès S, Petermann J, Petterson D, Pfeiffer HP, Pham KA, Phukon KS, Piccinni OJ, Pichot M, Piendibene M, Piergiovanni F, Pierini L, Pierro V, Pillant G, Pillas M, Pilo F, Pinard L, Pinto IM, Pinto M, Piotrzkowski K, Pirello M, Pitkin MD, Placidi E, Planas L, Plastino W, Pluchar C, Poggiani R, Polini E, Pong DYT, Ponrathnam S, Popolizio P, Porter EK, Poulton R, Powell J, Pracchia M, Pradier T, Prajapati AK, Prasai K, Prasanna R, Pratten G, Principe M, Prodi GA, Prokhorov L, Prosposito P, Prudenzi L, Puecher A, Punturo M, Puosi F, Puppo P, Pürrer M, Qi H, Quetschke V, Quitzow-James R, Raab FJ, Raaijmakers G, Radkins H, Radulesco N, Raffai P, Rail SX, Raja S, Rajan C, Ramirez KE, Ramirez TD, Ramos-Buades A, Rana J, Rapagnani P, Rapol UD, Ray A, Raymond V, Raza N, Razzano M, Read J, Rees LA, Regimbau T, Rei L, Reid S, Reid SW, Reitze DH, Relton P, Renzini A, Rettegno P, Rezac M, Ricci F, Richards D, Richardson JW, Richardson L, Riemenschneider G, Riles K, Rinaldi S, Rink K, Rizzo M, Robertson NA, Robie R, Robinet F, Rocchi A, Rodriguez S, Rolland L, Rollins JG, Romanelli M, Romano R, Romel CL, Romero-Rodríguez A, Romero-Shaw IM, Romie JH, Ronchini S, Rosa L, Rose CA, Rosińska D, Ross MP, Rowan S, Rowlinson SJ, Roy S, Roy S, Roy S, Rozza D, Ruggi P, Ryan K, Sachdev S, Sadecki T, Sadiq J, Sakellariadou M, Salafia OS, Salconi L, Saleem M, Salemi F, Samajdar A, Sanchez EJ, Sanchez JH, Sanchez LE, Sanchis-Gual N, Sanders JR, Sanuy A, Saravanan TR, Sarin N, Sassolas B, Satari H, Sathyaprakash BS, Sauter O, Savage RL, Sawant D, Sawant HL, Sayah S, Schaetzl D, Scheel M, Scheuer J, Schiworski M, Schmidt P, Schmidt S, Schnabel R, Schneewind M, Schofield RMS, Schönbeck A, Schulte BW, Schutz BF, Schwartz E, Scott J, Scott SM, Seglar-Arroyo M, Sellers D, Sengupta AS, Sentenac D, Seo EG, Sequino V, Sergeev A, Setyawati Y, Shaffer T, Shahriar MS, Shams B, Sharma A, Sharma P, Shawhan P, Shcheblanov NS, Shikauchi M, Shoemaker DH, Shoemaker DM, ShyamSundar S, Sieniawska M, Sigg D, Singer LP, Singh D, Singh N, Singha A, Sintes AM, Sipala V, Skliris V, Slagmolen BJJ, Slaven-Blair TJ, Smetana J, Smith JR, Smith RJE, Soldateschi J, Somala SN, Son EJ, Soni K, Soni S, Sordini V, Sorrentino F, Sorrentino N, Soulard R, Souradeep T, Sowell E, Spagnuolo V, Spencer AP, Spera M, Srinivasan R, Srivastava AK, Srivastava V, Staats K, Stachie C, Steer DA, Steinlechner J, Steinlechner S, Stevenson S, Stops DJ, Stover M, Strain KA, Strang LC, Stratta G, Strunk A, Sturani R, Stuver AL, Sudhagar S, Sudhir V, Suh HG, Summerscales TZ, Sun H, Sun L, Sunil S, Sur A, Suresh J, Sutton PJ, Swinkels BL, Szczepańczyk MJ, Szewczyk P, Tacca M, Tait SC, Talbot CJ, Talbot C, Tanasijczuk AJ, Tanner DB, Tao D, Tao L, Martín ENTS, Taranto C, Tasson JD, Tenorio R, Terhune JE, Terkowski L, Thirugnanasambandam MP, Thomas M, Thomas P, Thompson JE, Thondapu SR, Thorne KA, Thrane E, Tiwari S, Tiwari S, Tiwari V, Toivonen AM, Toland K, Tolley AE, Tonelli M, Torres-Forné A, Torrie CI, E Melo IT, Töyrä D, Trapananti A, Travasso F, Traylor G, Trevor M, Tringali MC, Tripathee A, Troiano L, Trovato A, Trozzo L, Trudeau RJ, Tsai DS, Tsai D, Tsang KW, Tse M, Tso R, Tsukada L, Tsuna D, Tsutsui T, Turbang K, Turconi M, Ubhi AS, Udall RP, Ueno K, Unnikrishnan CS, Urban AL, Utina A, Vahlbruch H, Vajente G, Vajpeyi A, Valdes G, Valentini M, Valsan V, van Bakel N, van Beuzekom M, van den Brand JFJ, Van Den Broeck C, Vander-Hyde DC, van der Schaaf L, van Heijningen JV, Vanosky J, van Remortel N, Vardaro M, Vargas AF, Varma V, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venneberg J, Venugopalan G, Verkindt D, Verma P, Verma Y, Veske D, Vetrano F, Viceré A, Vidyant S, Viets AD, Vijaykumar A, Villa-Ortega V, Vinet JY, Virtuoso A, Vitale S, Vo T, Vocca H, von Reis ERG, von Wrangel JSA, Vorvick C, Vyatchanin SP, Wade LE, Wade M, Wagner KJ, Walet RC, Walker M, Wallace GS, Wallace L, Walsh S, Wang JZ, Wang WH, Ward RL, Warner J, Was M, Washington NY, Watchi J, Weaver B, Webster SA, Weinert M, Weinstein AJ, Weiss R, Weller CM, Wellmann F, Wen L, Weßels P, Wette K, Whelan JT, White DD, Whiting BF, Whittle C, Wilken D, Williams D, Williams MJ, Williamson AR, Willis JL, Willke B, Wilson DJ, Winkler W, Wipf CC, Wlodarczyk T, Woan G, Woehler J, Wofford JK, Wong ICF, Wu DS, Wysocki DM, Xiao L, Yamamoto H, Yang FW, Yang L, Yang Y, Yang Z, Yap MJ, Yeeles DW, Yelikar AB, Ying M, Yoo J, Yu H, Yu H, Zadrożny A, Zanolin M, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang T, Zhang Y, Zhao C, Zhao G, Zhao Y, Zhou R, Zhou Z, Zhu XJ, Zimmerman AB, Zucker ME, Zweizig J, Jeong D, and Shandera S
Abstract: We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 M_{⊙} and 1.0 M_{⊙} in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend our previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio q≥0.1. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14 yr^{-1}. This implies an upper limit on the merger rate of subsolar binaries in the range [220-24200] Gpc^{-3} yr^{-1}, depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes in the mass range 0.2 M_{⊙}
Published: 2022
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24. Enhancing the precision limits of interferometric satellite geodesy missions.

Author: Conlon LO, Michel T, Guccione G, McKenzie K, Assad SM, and Lam PK
Abstract: Satellite geodesy uses the measurement of the motion of one or more satellites to infer precise information about the Earth's gravitational field. In this work, we consider the achievable precision limits on such measurements by examining approximate models for the three main noise sources in the measurement process of the current Gravitational Recovery and Climate Experiment (GRACE) Follow-On mission: laser phase noise, accelerometer noise and quantum noise. We show that, through time-delay interferometry, it is possible to remove the laser phase noise from the measurement, allowing for almost three orders of magnitude improvement in the signal-to-noise ratio. Several differential mass satellite formations are presented which can further enhance the signal-to-noise ratio through the removal of accelerometer noise. Finally, techniques from quantum optics have been studied, and found to have great promise for reducing quantum noise in other alternative mission configurations. We model the spectral noise performance using an intuitive 1D model and verify that our proposals have the potential to greatly enhance the performance of near-future satellite geodesy missions., (© 2022. The Author(s).)
Published: 2022
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25. Constraining Cosmological Phase Transitions with the Parkes Pulsar Timing Array.

Author: Xue X, Bian L, Shu J, Yuan Q, Zhu X, Bhat NDR, Dai S, Feng Y, Goncharov B, Hobbs G, Howard E, Manchester RN, Russell CJ, Reardon DJ, Shannon RM, Spiewak R, Thyagarajan N, and Wang J
Abstract: A cosmological first-order phase transition is expected to produce a stochastic gravitational wave background. If the phase transition temperature is on the MeV scale, the power spectrum of the induced stochastic gravitational waves peaks around nanohertz frequencies, and can thus be probed with high-precision pulsar timing observations. We search for such a stochastic gravitational wave background with the latest data set of the Parkes Pulsar Timing Array. We find no evidence for a Hellings-Downs spatial correlation as expected for a stochastic gravitational wave background. Therefore, we present constraints on first-order phase transition model parameters. Our analysis shows that pulsar timing is particularly sensitive to the low-temperature (T∼1-100 MeV) phase transition with a duration (β/H_{*})^{-1}∼10^{-2}-10^{-1} and therefore can be used to constrain the dark and QCD phase transitions.
Published: 2021
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26. Point Absorber Limits to Future Gravitational-Wave Detectors.

Author: Jia W, Yamamoto H, Kuns K, Effler A, Evans M, Fritschel P, Abbott R, Adams C, Adhikari RX, Ananyeva A, Appert S, Arai K, Areeda JS, Asali Y, Aston SM, Austin C, Baer AM, Ball M, Ballmer SW, Banagiri S, Barker D, Barsotti L, Bartlett J, Berger BK, Betzwieser J, Bhattacharjee D, Billingsley G, Biscans S, Blair CD, Blair RM, Bode N, Booker P, Bork R, Bramley A, Brooks AF, Brown DD, Buikema A, Cahillane C, Cannon KC, Chen X, Ciobanu AA, Clara F, Compton CM, Cooper SJ, Corley KR, Countryman ST, Covas PB, Coyne DC, Datrier LEH, Davis D, Di Fronzo C, Dooley KL, Driggers JC, Dupej P, Dwyer SE, Etzel T, Evans TM, Feicht J, Fernandez-Galiana A, Frolov VV, Fulda P, Fyffe M, Giaime JA, Giardina KD, Godwin P, Goetz E, Gras S, Gray C, Gray R, Green AC, Gustafson EK, Gustafson R, Hall ED, Hanks J, Hanson J, Hardwick T, Hasskew RK, Heintze MC, Helmling-Cornell AF, Holland NA, Jones JD, Kandhasamy S, Karki S, Kasprzack M, Kawabe K, Kijbunchoo N, King PJ, Kissel JS, Kumar R, Landry M, Lane BB, Lantz B, Laxen M, Lecoeuche YK, Leviton J, Liu J, Lormand M, Lundgren AP, Macas R, MacInnis M, Macleod DM, Mansell GL, Márka S, Márka Z, Martynov DV, Mason K, Massinger TJ, Matichard F, Mavalvala N, McCarthy R, McClelland DE, McCormick S, McCuller L, McIver J, McRae T, Mendell G, Merfeld K, Merilh EL, Meylahn F, Mistry T, Mittleman R, Moreno G, Mow-Lowry CM, Mozzon S, Mullavey A, Nelson TJN, Nguyen P, Nuttall LK, Oberling J, Oram RJ, Osthelder C, Ottaway DJ, Overmier H, Palamos JR, Parker W, Payne E, Pele A, Penhorwood R, Perez CJ, Pirello M, Radkins H, Ramirez KE, Richardson JW, Riles K, Robertson NA, Rollins JG, Romel CL, Romie JH, Ross MP, Ryan K, Sadecki T, Sanchez EJ, Sanchez LE, Saravanan TR, Savage RL, Schaetzl D, Schnabel R, Schofield RMS, Schwartz E, Sellers D, Shaffer T, Sigg D, Slagmolen BJJ, Smith JR, Soni S, Sorazu B, Spencer AP, Strain KA, Sun L, Szczepańczyk MJ, Thomas M, Thomas P, Thorne KA, Toland K, Torrie CI, Traylor G, Tse M, Urban AL, Vajente G, Valdes G, Vander-Hyde DC, Veitch PJ, Venkateswara K, Venugopalan G, Viets AD, Vo T, Vorvick C, Wade M, Ward RL, Warner J, Weaver B, Weiss R, Whittle C, Willke B, Wipf CC, Xiao L, Yu H, Yu H, Zhang L, Zucker ME, and Zweizig J
Abstract: High-quality optical resonant cavities require low optical loss, typically on the scale of parts per million. However, unintended micron-scale contaminants on the resonator mirrors that absorb the light circulating in the cavity can deform the surface thermoelastically and thus increase losses by scattering light out of the resonant mode. The point absorber effect is a limiting factor in some high-power cavity experiments, for example, the Advanced LIGO gravitational-wave detector. In this Letter, we present a general approach to the point absorber effect from first principles and simulate its contribution to the increased scattering. The achievable circulating power in current and future gravitational-wave detectors is calculated statistically given different point absorber configurations. Our formulation is further confirmed experimentally in comparison with the scattered power in the arm cavity of Advanced LIGO measured by in situ photodiodes. The understanding presented here provides an important tool in the global effort to design future gravitational-wave detectors that support high optical power and thus reduce quantum noise.
Published: 2021
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27. Advancement of Photospheric Radius Expansion and Clocked Type-I X-Ray Burst Models with the New ^{22}Mg(α,p)^{25}Al Reaction Rate Determined at the Gamow Energy.

Author: Hu J, Yamaguchi H, Lam YH, Heger A, Kahl D, Jacobs AM, Johnston Z, Xu SW, Zhang NT, Ma SB, Ru LH, Liu EQ, Liu T, Hayakawa S, Yang L, Shimizu H, Hamill CB, Murphy ASJ, Su J, Fang X, Chae KY, Kwag MS, Cha SM, Duy NN, Uyen NK, Kim DH, Pizzone RG, La Cognata M, Cherubini S, Romano S, Tumino A, Liang J, Psaltis A, Sferrazza M, Kim D, Li YY, and Kubono S
Abstract: We report the first (in)elastic scattering measurement of ^{25}Al+p with the capability to select and measure in a broad energy range the proton resonances in ^{26}Si contributing to the ^{22}Mg(α,p) reaction at type I x-ray burst energies. We measured spin-parities of four resonances above the α threshold of ^{26}Si that are found to strongly impact the ^{22}Mg(α,p) rate. The new rate advances a state-of-the-art model to remarkably reproduce light curves of the GS 1826-24 clocked burster with mean deviation <9% and permits us to discover a strong correlation between the He abundance in the accreting envelope of the photospheric radius expansion burster and the dominance of ^{22}Mg(α,p) branch.
Published: 2021
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28. Bayesian Inference for Gravitational Waves from Binary Neutron Star Mergers in Third Generation Observatories.

Author: Smith R, Borhanian S, Sathyaprakash B, Hernandez Vivanco F, Field SE, Lasky P, Mandel I, Morisaki S, Ottaway D, Slagmolen BJJ, Thrane E, Töyrä D, and Vitale S
Abstract: Third generation (3G) gravitational-wave detectors will observe thousands of coalescing neutron star binaries with unprecedented fidelity. Extracting the highest precision science from these signals is expected to be challenging owing to both high signal-to-noise ratios and long-duration signals. We demonstrate that current Bayesian inference paradigms can be extended to the analysis of binary neutron star signals without breaking the computational bank. We construct reduced-order models for ∼90-min-long gravitational-wave signals covering the observing band (5-2048 Hz), speeding up inference by a factor of ∼1.3×10^{4} compared to the calculation times without reduced-order models. The reduced-order models incorporate key physics including the effects of tidal deformability, amplitude modulation due to Earth's rotation, and spin-induced orbital precession. We show how reduced-order modeling can accelerate inference on data containing multiple overlapping gravitational-wave signals, and determine the speedup as a function of the number of overlapping signals. Thus, we conclude that Bayesian inference is computationally tractable for the long-lived, overlapping, high signal-to-noise-ratio events present in 3G observatories.
Published: 2021
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29. Constraints on Cosmic Strings Using Data from the Third Advanced LIGO-Virgo Observing Run.

Author: Abbott R, Abbott TD, Abraham S, Acernese F, Ackley K, Adams A, Adams C, Adhikari RX, Adya VB, Affeldt C, Agarwal D, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Akutsu T, Aleman KM, Allen G, Allocca A, Altin PA, Amato A, Anand S, Ananyeva A, Anderson SB, Anderson WG, Ando M, Angelova SV, Ansoldi S, Antelis JM, Antier S, Appert S, Arai K, Arai K, Arai Y, Araki S, Araya A, Araya MC, Areeda JS, Arène M, Aritomi N, Arnaud N, Aronson SM, Asada H, Asali Y, Ashton G, Aso Y, Aston SM, Astone P, Aubin F, Auclair P, Aufmuth P, AultONeal K, Austin C, Babak S, Badaracco F, Bader MKM, Bae S, Bae Y, Baer AM, Bagnasco S, Bai Y, Baiotti L, Baird J, Bajpai R, Ball M, Ballardin G, Ballmer SW, Bals M, Balsamo A, Baltus G, Banagiri S, Bankar D, Bankar RS, Barayoga JC, Barbieri C, Barish BC, Barker D, Barneo P, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Barton MA, Bartos I, Bassiri R, Basti A, Bawaj M, Bayley JC, Baylor AC, Bazzan M, Bécsy B, Bedakihale VM, Bejger M, Belahcene I, Benedetto V, Beniwal D, Benjamin MG, Bennett TF, Bentley JD, BenYaala M, Bergamin F, Berger BK, Bernuzzi S, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bhandari AV, Bhattacharjee D, Bhaumik S, Bidler J, Bilenko IA, Billingsley G, Birney R, Birnholtz O, Biscans S, Bischi M, Biscoveanu S, Bisht A, Biswas B, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bobba F, Bode N, Boer M, Bogaert G, Boldrini M, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Bork R, Boschi V, Bose N, Bose S, Bossilkov V, Boudart V, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branch A, Branchesi M, Breschi M, Briant T, Briggs JH, Brillet A, Brinkmann M, Brockill P, Brooks AF, Brooks J, Brown DD, Brunett S, Bruno G, Bruntz R, Bryant J, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buscicchio R, Buskulic D, Cadonati L, Caesar M, Cagnoli G, Cahillane C, Cain HW, Calderón Bustillo J, Callaghan JD, Callister TA, Calloni E, Camp JB, Canepa M, Cannavacciuolo M, Cannon KC, Cao H, Cao J, Cao Z, Capocasa E, Capote E, Carapella G, Carbognani F, Carlin JB, Carney MF, Carpinelli M, Carullo G, Carver TL, Casanueva Diaz J, Casentini C, Castaldi G, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cerdá-Durán P, Cesarini E, Chaibi W, Chakravarti K, Champion B, Chan CH, Chan C, Chan CL, Chan M, Chandra K, Chanial P, Chao S, Charlton P, Chase EA, Chassande-Mottin E, Chatterjee D, Chaturvedi M, Chatziioannou K, Chen A, Chen C, Chen HY, Chen J, Chen K, Chen X, Chen YB, Chen YR, Chen Z, Cheng H, Cheong CK, Cheung HY, Chia HY, Chiadini F, Chiang CY, Chierici R, Chincarini A, Chiofalo ML, Chiummo A, Cho G, Cho HS, Choate S, Choudhary RK, Choudhary S, Christensen N, Chu H, Chu Q, Chu YK, Chua S, Chung KW, Ciani G, Ciecielag P, Cieślar M, Cifaldi M, Ciobanu AA, Ciolfi R, Cipriano F, Cirone A, Clara F, Clark EN, Clark JA, Clarke L, Clearwater P, Clesse S, Cleva F, Coccia E, Cohadon PF, Cohen DE, Cohen L, Colleoni M, Collette CG, Colpi M, Compton CM, Constancio M, Conti L, Cooper SJ, Corban P, Corbitt TR, Cordero-Carrión I, Corezzi S, Corley KR, Cornish N, Corre D, Corsi A, Cortese S, Costa CA, Cotesta R, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Cousins B, Couvares P, Covas PB, Coward DM, Cowart MJ, Coyne DC, Coyne R, Creighton JDE, Creighton TD, Criswell AW, Croquette M, Crowder SG, Cudell JR, Cullen TJ, Cumming A, Cummings R, Cuoco E, Curyło M, Canton TD, Dálya G, Dana A, DaneshgaranBajastani LM, D'Angelo B, Danilishin SL, D'Antonio S, Danzmann K, Darsow-Fromm C, Dasgupta A, Datrier LEH, Dattilo V, Dave I, Davier M, Davies GS, Davis D, Daw EJ, Dean R, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Del Favero V, De Lillo F, De Lillo N, Del Pozzo W, DeMarchi LM, De Matteis F, D'Emilio V, Demos N, Dent T, Depasse A, De Pietri R, De Rosa R, De Rossi C, DeSalvo R, De Simone R, Dhurandhar S, Díaz MC, Diaz-Ortiz M, Didio NA, Dietrich T, Di Fiore L, Di Fronzo C, Di Giorgio C, Di Giovanni F, Di Girolamo T, Di Lieto A, Ding B, Di Pace S, Di Palma I, Di Renzo F, Divakarla AK, Dmitriev A, Doctor Z, D'Onofrio L, Donovan F, Dooley KL, Doravari S, Dorrington I, Drago M, Driggers JC, Drori Y, Du Z, Ducoin JG, Dupej P, Durante O, D'Urso D, Duverne PA, Dwyer SE, Easter PJ, Ebersold M, Eddolls G, Edelman B, Edo TB, Edy O, Effler A, Eguchi S, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Ejlli A, Enomoto Y, Errico L, Essick RC, Estellés H, Estevez D, Etienne Z, Etzel T, Evans M, Evans TM, Ewing BE, Fafone V, Fair H, Fairhurst S, Fan X, Farah AM, Farinon S, Farr B, Farr WM, Farrow NW, Fauchon-Jones EJ, Favata M, Fays M, Fazio M, Feicht J, Fejer MM, Feng F, Fenyvesi E, Ferguson DL, Fernandez-Galiana A, Ferrante I, Ferreira TA, Fidecaro F, Figura P, Fiori I, Fishbach M, Fisher RP, Fishner JM, Fittipaldi R, Fiumara V, Flaminio R, Floden E, Flynn E, Fong H, Font JA, Fornal B, Forsyth PWF, Franke A, Frasca S, Frasconi F, Frederick C, Frei Z, Freise A, Frey R, Fritschel P, Frolov VV, Fronzé GG, Fujii Y, Fujikawa Y, Fukunaga M, Fukushima M, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Gais J, Galaudage S, Gamba R, Ganapathy D, Ganguly A, Gao D, Gaonkar SG, Garaventa B, García-Núñez C, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gayathri V, Ge G, Gemme G, Gennai A, George J, Gergely L, Gewecke P, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Ghosh S, Ghosh S, Giacomazzo B, Giacoppo L, Giaime JA, Giardina KD, Gibson DR, Gier C, Giesler M, Giri P, Gissi F, Glanzer J, Gleckl AE, Godwin P, Goetz E, Goetz R, Gohlke N, Goncharov B, González G, Gopakumar A, Gosselin M, Gouaty R, Grace B, Grado A, Granata M, Granata V, Grant A, Gras S, Grassia P, Gray C, Gray R, Greco G, Green AC, Green R, Gretarsson AM, Gretarsson EM, Griffith D, Griffiths W, Griggs HL, Grignani G, Grimaldi A, Grimes E, Grimm SJ, Grote H, Grunewald S, Gruning P, Guerrero JG, Guidi GM, Guimaraes AR, Guixé G, Gulati HK, Guo HK, Guo Y, Gupta A, Gupta A, Gupta P, Gustafson EK, Gustafson R, Guzman F, Ha S, Haegel L, Hagiwara A, Haino S, Halim O, Hall ED, Hamilton EZ, Hammond G, Han WB, Haney M, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hansen H, Hansen TJ, Hanson J, Harder T, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hartwig D, Hasegawa K, Haskell B, Hasskew RK, Haster CJ, Hattori K, Haughian K, Hayakawa H, Hayama K, Hayes FJ, Healy J, Heidmann A, Heintze MC, Heinze J, Heinzel J, Heitmann H, Hellman F, Hello P, Helmling-Cornell AF, Hemming G, Hendry M, Heng IS, Hennes E, Hennig J, Hennig MH, Hernandez Vivanco F, Heurs M, Hild S, Hill P, Himemoto Y, Hines AS, Hiranuma Y, Hirata N, Hirose E, Hochheim S, Hofman D, Hohmann JN, Holgado AM, Holland NA, Hollows IJ, Holmes ZJ, Holt K, Holz DE, Hong Z, Hopkins P, Hough J, Howell EJ, Hoy CG, Hoyland D, Hreibi A, Hsieh B, Hsu Y, Huang GZ, Huang HY, Huang P, Huang YC, Huang YJ, Huang YW, Hübner MT, Huddart AD, Huerta EA, Hughey B, Hui DCY, Hui V, Husa S, Huttner SH, Huxford R, Huynh-Dinh T, Ide S, Idzkowski B, Iess A, Ikenoue B, Imam S, Inayoshi K, Inchauspe H, Ingram C, Inoue Y, Intini G, Ioka K, Isi M, Isleif K, Ito K, Itoh Y, Iyer BR, Izumi K, JaberianHamedan V, Jacqmin T, Jadhav SJ, Jadhav SP, James AL, Jan AZ, Jani K, Janssens K, Janthalur NN, Jaranowski P, Jariwala D, Jaume R, Jenkins AC, Jeon C, Jeunon M, Jia W, Jiang J, Jin HB, Johns GR, Jones AW, Jones DI, Jones JD, Jones P, Jones R, Jonker RJG, Ju L, Jung K, Jung P, Junker J, Kaihotsu K, Kajita T, Kakizaki M, Kalaghatgi CV, Kalogera V, Kamai B, Kamiizumi M, Kanda N, Kandhasamy S, Kang G, Kanner JB, Kao Y, Kapadia SJ, Kapasi DP, Karathanasis C, Karki S, Kashyap R, Kasprzack M, Kastaun W, Katsanevas S, Katsavounidis E, Katzman W, Kaur T, Kawabe K, Kawaguchi K, Kawai N, Kawasaki T, Kéfélian F, Keitel D, Key JS, Khadka S, Khalili FY, Khan I, Khan S, Khazanov EA, Khetan N, Khursheed M, Kijbunchoo N, Kim C, Kim JC, Kim J, Kim K, Kim WS, Kim YM, Kimball C, Kimura N, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kita N, Kitazawa H, Kleybolte L, Klimenko S, Knee AM, Knowles TD, Knyazev E, Koch P, Koekoek G, Kojima Y, Kokeyama K, Koley S, Kolitsidou P, Kolstein M, Komori K, Kondrashov V, Kong AKH, Kontos A, Koper N, Korobko M, Kotake K, Kovalam M, Kozak DB, Kozakai C, Kozu R, Kringel V, Krishnendu NV, Królak A, Kuehn G, Kuei F, Kumar A, Kumar P, Kumar R, Kumar R, Kume J, Kuns K, Kuo C, Kuo HS, Kuromiya Y, Kuroyanagi S, Kusayanagi K, Kwak K, Kwang S, Laghi D, Lalande E, Lam TL, Lamberts A, Landry M, Lane BB, Lang RN, Lange J, Lantz B, La Rosa I, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lecoeuche YK, Lee HK, Lee HM, Lee HW, Lee J, Lee K, Lee R, Lehmann J, Lemaître A, Leon E, Leonardi M, Leroy N, Letendre N, Levin Y, Leviton JN, Li AKY, Li B, Li J, Li KL, Li TGF, Li X, Lin CY, Lin FK, Lin FL, Lin HL, Lin LC, Linde F, Linker SD, Linley JN, Littenberg TB, Liu GC, Liu J, Liu K, Liu X, Llorens-Monteagudo M, Lo RKL, Lockwood A, Lollie ML, London LT, Longo A, Lopez D, Lorenzini M, Loriette V, 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Rodriguez-Soto RD, Rolland L, Rollins JG, Roma VJ, Romanelli M, Romano R, Romel CL, Romero A, Romero-Shaw IM, Romie JH, Rose CA, Rosińska D, Rosofsky SG, Ross MP, Rowan S, Rowlinson SJ, Roy S, Roy S, Rozza D, Ruggi P, Ryan K, Sachdev S, Sadecki T, Sadiq J, Sago N, Saito S, Saito Y, Sakai K, Sakai Y, Sakellariadou M, Sakuno Y, Salafia OS, Salconi L, Saleem M, Salemi F, Samajdar A, Sanchez EJ, Sanchez JH, Sanchez LE, Sanchis-Gual N, Sanders JR, Sanuy A, Saravanan TR, Sarin N, Sassolas B, Satari H, Sato S, Sato T, Sauter O, Savage RL, Savant V, Sawada T, Sawant D, Sawant HL, Sayah S, Schaetzl D, Scheel M, Scheuer J, Schindler-Tyka A, Schmidt P, Schnabel R, Schneewind M, Schofield RMS, Schönbeck A, Schulte BW, Schutz BF, Schwartz E, Scott J, Scott SM, Seglar-Arroyo M, Seidel E, Sekiguchi T, Sekiguchi Y, Sellers D, Sengupta AS, Sennett N, Sentenac D, Seo EG, Sequino V, Setyawati Y, Shaffer T, Shahriar MS, Shams B, Shao L, Sharifi S, Sharma A, Sharma P, Shawhan P, Shcheblanov NS, Shen H, 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Tanasijczuk AJ, Tanioka S, Tanner DB, Tao D, Tapia A, Tapia San Martin EN, Tapia San Martin EN, Tasson JD, Telada S, Tenorio R, Terkowski L, Test M, Thirugnanasambandam MP, Thomas M, Thomas P, Thompson JE, Thondapu SR, Thorne KA, Thrane E, Tiwari S, Tiwari S, Tiwari V, Toland K, Tolley AE, Tomaru T, Tomigami Y, Tomura T, Tonelli M, Torres-Forné A, Torrie CI, Tosta E Melo I, Töyrä D, Trapananti A, Travasso F, Traylor G, Tringali MC, Tripathee A, Troiano L, Trovato A, Trozzo L, Trudeau RJ, Tsai DS, Tsai D, Tsang KW, Tsang T, Tsao JS, Tse M, Tso R, Tsubono K, Tsuchida S, Tsukada L, Tsuna D, Tsutsui T, Tsuzuki T, Turconi M, Tuyenbayev D, Ubhi AS, Uchikata N, Uchiyama T, Udall RP, Ueda A, Uehara T, Ueno K, Ueshima G, Ugolini D, Unnikrishnan CS, Uraguchi F, Urban AL, Ushiba T, Usman SA, Utina AC, Vahlbruch H, Vajente G, Vajpeyi A, Valdes G, Valentini M, Valsan V, van Bakel N, van Beuzekom M, van den Brand JFJ, Van Den Broeck C, Vander-Hyde DC, van der Schaaf L, van Heijningen JV, van Putten MHPM, van Remortel N, Vardaro M, Vargas AF, Varma V, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Venneberg J, Venugopalan G, Verkindt D, Verma Y, Veske D, Vetrano F, Viceré A, Viets AD, Villa-Ortega V, Vinet JY, Vitale S, Vo T, Vocca H, von Reis ERG, Vorvick C, Vyatchanin SP, Wade LE, Wade M, Wagner KJ, Walet RC, Walker M, Wallace GS, Wallace L, Walsh S, Wang J, Wang JZ, Wang WH, Ward RL, Warner J, Was M, Washimi T, Washington NY, Watchi J, Weaver B, Wei L, Weinert M, Weinstein AJ, Weiss R, Weller CM, Wellmann F, Wen L, Weßels P, Westhouse JW, Wette K, Whelan JT, White DD, Whiting BF, Whittle C, Wilken D, Williams D, Williams MJ, Williamson AR, Willis JL, Willke B, Wilson DJ, Winkler W, Wipf CC, Wlodarczyk T, Woan G, Woehler J, Wofford JK, Wong ICF, Wrangel J, Wu C, Wu DS, Wu H, Wu S, Wysocki DM, Xiao L, Xu WR, Yamada T, Yamamoto H, Yamamoto K, Yamamoto K, Yamamoto T, Yamashita K, Yamazaki R, Yang FW, Yang L, Yang Y, Yang Y, Yang Z, Yap MJ, Yeeles DW, Yelikar AB, Ying M, Yokogawa K, Yokoyama J, Yokozawa T, Yoon A, Yoshioka T, Yu H, Yu H, Yuzurihara H, Zadrożny A, Zanolin M, Zeidler S, Zelenova T, Zendri JP, Zevin M, Zhan M, Zhang H, Zhang J, Zhang L, Zhang R, Zhang T, Zhao C, Zhao G, Zhao Y, Zhao Y, Zhou Z, Zhu XJ, Zhu ZH, Zucker ME, and Zweizig J
Abstract: We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks, and, for the first time, kink-kink collisions. A template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension Gμ as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models. Additionally, we develop and test a third model that interpolates between these two models. Our results improve upon the previous LIGO-Virgo constraints on Gμ by 1 to 2 orders of magnitude depending on the model that is tested. In particular, for the one-loop distribution model, we set the most competitive constraints to date: Gμ≲4×10^{-15}. In the case of cosmic strings formed at the end of inflation in the context of grand unified theories, these results challenge simple inflationary models.
Published: 2021
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30. Approaching the motional ground state of a 10-kg object.

Author: Whittle C, Hall ED, Dwyer S, Mavalvala N, Sudhir V, Abbott R, Ananyeva A, Austin C, Barsotti L, Betzwieser J, Blair CD, Brooks AF, Brown DD, Buikema A, Cahillane C, Driggers JC, Effler A, Fernandez-Galiana A, Fritschel P, Frolov VV, Hardwick T, Kasprzack M, Kawabe K, Kijbunchoo N, Kissel JS, Mansell GL, Matichard F, McCuller L, McRae T, Mullavey A, Pele A, Schofield RMS, Sigg D, Tse M, Vajente G, Vander-Hyde DC, Yu H, Yu H, Adams C, Adhikari RX, Appert S, Arai K, Areeda JS, Asali Y, Aston SM, Baer AM, Ball M, Ballmer SW, Banagiri S, Barker D, Bartlett J, Berger BK, Bhattacharjee D, Billingsley G, Biscans S, Blair RM, Bode N, Booker P, Bork R, Bramley A, Cannon KC, Chen X, Ciobanu AA, Clara F, Compton CM, Cooper SJ, Corley KR, Countryman ST, Covas PB, Coyne DC, Datrier LEH, Davis D, Di Fronzo C, Dooley KL, Dupej P, Etzel T, Evans M, Evans TM, Feicht J, Fulda P, Fyffe M, Giaime JA, Giardina KD, Godwin P, Goetz E, Gras S, Gray C, Gray R, Green AC, Gustafson EK, Gustafson R, Hanks J, Hanson J, Hasskew RK, Heintze MC, Helmling-Cornell AF, Holland NA, Jones JD, Kandhasamy S, Karki S, King PJ, Kumar R, Landry M, Lane BB, Lantz B, Laxen M, Lecoeuche YK, Leviton J, Liu J, Lormand M, Lundgren AP, Macas R, MacInnis M, Macleod DM, Márka S, Márka Z, Martynov DV, Mason K, Massinger TJ, McCarthy R, McClelland DE, McCormick S, McIver J, Mendell G, Merfeld K, Merilh EL, Meylahn F, Mistry T, Mittleman R, Moreno G, Mow-Lowry CM, Mozzon S, Nelson TJN, Nguyen P, Nuttall LK, Oberling J, Oram RJ, Osthelder C, Ottaway DJ, Overmier H, Palamos JR, Parker W, Payne E, Penhorwood R, Perez CJ, Pirello M, Radkins H, Ramirez KE, Richardson JW, Riles K, Robertson NA, Rollins JG, Romel CL, Romie JH, Ross MP, Ryan K, Sadecki T, Sanchez EJ, Sanchez LE, Saravanan TR, Savage RL, Schaetz D, Schnabel R, Schwartz E, Sellers D, Shaffer T, Slagmolen BJJ, Smith JR, Soni S, Sorazu B, Spencer AP, Strain KA, Sun L, Szczepańczyk MJ, Thomas M, Thomas P, Thorne KA, Toland K, Torrie CI, Traylor G, Urban AL, Valdes G, Veitch PJ, Venkateswara K, Venugopalan G, Viets AD, Vo T, Vorvick C, Wade M, Ward RL, Warner J, Weaver B, Weiss R, Willke B, Wipf CC, Xiao L, Yamamoto H, Zhang L, Zucker ME, and Zweizig J
Abstract: The motion of a mechanical object, even a human-sized object, should be governed by the rules of quantum mechanics. Coaxing them into a quantum state is, however, difficult because the thermal environment masks any quantum signature of the object's motion. The thermal environment also masks the effects of proposed modifications of quantum mechanics at large mass scales. We prepared the center-of-mass motion of a 10-kilogram mechanical oscillator in a state with an average phonon occupation of 10.8. The reduction in temperature, from room temperature to 77 nanokelvin, is commensurate with an 11 orders-of-magnitude suppression of quantum back-action by feedback and a 13 orders-of-magnitude increase in the mass of an object prepared close to its motional ground state. Our approach will enable the possibility of probing gravity on massive quantum systems., (Copyright © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)
Published: 2021
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31. A multi-orientation low-frequency rotational accelerometer.

Author: McCann JJ, Winterflood J, Ju L, and Zhao C
Abstract: We present a low frequency rotational accelerometer coined ALFRA with a few nrad/Hz readout sensitivity above 20 mHz and 0.1 nrad/Hz above 50 mHz. The ALFRA is a beam-balance style rotation sensor, which pivots about a cross flexure designed to allow mounting with any orientation, the axis of the pivot determining which rotational component is measured. The high sensitivity is achieved through the use of a walk-off sensor readout used in a feedback loop with an electromagnetic coil to keep the beam dynamically locked. The ALFRA is relatively compact for a ground rotation sensor, measuring at 780 × 240 × 55 mm 3 .
Published: 2021
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32. Upconversion Fluorescence in Naturally Occurring Calcium Fluoride.

Author: Moffatt JE, Payten TB, Tsiminis G, de Prinse TJ, Da Silva Teixeira L, Klantsataya E, Ottaway DJ, Smith BW, and Spooner NA
Abstract: Fluorine can negatively interfere with leach and smelting processes during mineral processing. Real-time knowledge of the concentration and mineral hosts of fluorine in a mineral processing ore stream is important to protect process line equipment and product. Currently only offline methods of detection are available. Online sensors that determine specific fluorine-bearing mineral concentration in real-time would enable improved efficiency in processing decisions during mine production. Common excitation wavelengths used for fluorescence studies in minerals frequently provide signals that are not clearly host-specific, and hence of limited utility for mineral identification. We show that upconversion fluorescence, a process in which two or more photons are absorbed and one higher-energy photon is emitted, provides a more host-specific fluorescence output, minimizing spurious signals in complex environments and therefore greatly improving detection thresholds. Natural samples of fluorite (CaF 2 ), a major fluorine host at many mine sites, have been analyzed by near-infrared excitation and have revealed upconversion fluorescence from rare earth inclusions. Upconversion fluorescence was detected in samples with rare earth concentrations as low as one part per million and is therefore considered a potential new sensing modality for real-time fluorite monitoring.
Published: 2021
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33. Confusing Head-On Collisions with Precessing Intermediate-Mass Binary Black Hole Mergers.

Author: Bustillo JC, Sanchis-Gual N, Torres-Forné A, and Font JA
Abstract: We report a degeneracy between the gravitational-wave signals from quasicircular precessing black-hole mergers and those from extremely eccentric mergers, namely, head-on collisions. Performing model selection on numerically simulated signals of head-on collisions using models for quasicircular binaries, we find that, for signal-to-noise ratios of 15 and 25, typical of Advanced LIGO observations, head-on mergers with respective total masses of M∈(125,300)M_{⊙} and M∈(200,440)M_{⊙} would be identified as precessing quasicircular intermediate-mass black-hole binaries located at a much larger distance. Ruling out the head-on scenario would require us to perform model selection using currently nonexistent waveform models for head-on collisions, together with the application of astrophysically motivated priors on the (rare) occurrence of those events. We show that in situations where standard parameter inference of compact binaries may report component masses inside (outside) the pair-instability supernova gap, the true object may be a head-on merger with masses outside (inside) this gap. We briefly discuss the potential implications of these findings for GW190521, which we analyze in detail in J. Calderón Bustillo et al., Phys. Rev. Lett. 126, 081101 (2021)PRLTAO0031-900710.1103/PhysRevLett.126.081101.
Published: 2021
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34. A low-frequency torsion pendulum with interferometric readout.

Author: Ross MP, Venkateswara K, Hagedorn CA, Leupold CJ, Forsyth PWF, Wegner JD, Shaw EA, Lee JG, and Gundlach JH
Abstract: We describe a torsion pendulum with a large mass-quadrupole moment and a resonant frequency of 2.8 mHz, whose angle is measured using a Michelson interferometer. The system achieved noise levels of ∼200prad/Hz between 0.2 and 30 Hz and ∼10prad/Hz above 100 Hz. Such a system can be applied to a broad range of fields from the study of rotational seismic motion and elastogravity signals to gravitational wave observation and tests of gravity.
Published: 2021
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35. Cygnus X-1 contains a 21-solar mass black hole-Implications for massive star winds.

Author: Miller-Jones JCA, Bahramian A, Orosz JA, Mandel I, Gou L, Maccarone TJ, Neijssel CJ, Zhao X, Ziółkowski J, Reid MJ, Uttley P, Zheng X, Byun DY, Dodson R, Grinberg V, Jung T, Kim JS, Marcote B, Markoff S, Rioja MJ, Rushton AP, Russell DM, Sivakoff GR, Tetarenko AJ, Tudose V, and Wilms J
Abstract: The evolution of massive stars is influenced by the mass lost to stellar winds over their lifetimes. These winds limit the masses of the stellar remnants (such as black holes) that the stars ultimately produce. We used radio astrometry to refine the distance to the black hole x-ray binary Cygnus X-1, which we found to be [Formula: see text] kiloparsecs. When combined with archival optical data, this implies a black hole mass of 21.2 ± 2.2 solar masses, which is higher than previous measurements. The formation of such a high-mass black hole in a high-metallicity system (within the Milky Way) constrains wind mass loss from massive stars., (Copyright © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)
Published: 2021
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36. GW190521 as a Merger of Proca Stars: A Potential New Vector Boson of 8.7×10^{-13} eV.

Author: Bustillo JC, Sanchis-Gual N, Torres-Forné A, Font JA, Vajpeyi A, Smith R, Herdeiro C, Radu E, and Leong SHW
Abstract: Advanced LIGO-Virgo have reported a short gravitational-wave signal (GW190521) interpreted as a quasicircular merger of black holes, one at least populating the pair-instability supernova gap, that formed a remnant black hole of M_{f}∼142 M_{⊙} at a luminosity distance of d_{L}∼5.3 Gpc. With barely visible pre-merger emission, however, GW190521 merits further investigation of the pre-merger dynamics and even of the very nature of the colliding objects. We show that GW190521 is consistent with numerically simulated signals from head-on collisions of two (equal mass and spin) horizonless vector boson stars (aka Proca stars), forming a final black hole with M_{f}=231_{-17}^{+13} M_{⊙}, located at a distance of d_{L}=571_{-181}^{+348} Mpc. This provides the first demonstration of close degeneracy between these two theoretical models, for a real gravitational-wave event. The favored mass for the ultralight vector boson constituent of the Proca stars is μ_{V}=8.72_{-0.82}^{+0.73}×10^{-13} eV. Confirmation of the Proca star interpretation, which we find statistically slightly preferred, would provide the first evidence for a long sought dark matter particle.
Published: 2021
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37. Measuring the Primordial Gravitational-Wave Background in the Presence of Astrophysical Foregrounds.

Author: Biscoveanu S, Talbot C, Thrane E, and Smith R
Abstract: Primordial gravitational waves are expected to create a stochastic background encoding information about the early Universe that may not be accessible by other means. However, the primordial background is obscured by an astrophysical foreground consisting of gravitational waves from compact binaries. We demonstrate a Bayesian method for estimating the primordial background in the presence of an astrophysical foreground. Since the background and foreground signal parameters are estimated simultaneously, there is no subtraction step, and therefore we avoid astrophysical contamination of the primordial measurement, sometimes referred to as "residuals." Additionally, since we include the non-Gaussianity of the astrophysical foreground in our model, this method represents the statistically optimal approach to the simultaneous detection of a multicomponent stochastic background.
Published: 2020
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38. GW190521: A Binary Black Hole Merger with a Total Mass of 150 M_{⊙}.

Author: Abbott R, Abbott TD, Abraham S, Acernese F, Ackley K, Adams C, Adhikari RX, Adya VB, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aich A, Aiello L, Ain A, Ajith P, Akcay S, Allen G, Allocca A, Altin PA, Amato A, Anand S, Ananyeva A, Anderson SB, Anderson WG, Angelova SV, Ansoldi S, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Aronson SM, Arun KG, Asali Y, Ascenzi S, Ashton G, Aston SM, Astone P, Aubin F, Aufmuth P, AultONeal K, Austin C, Avendano V, Babak S, Bacon P, Badaracco F, Bader MKM, Bae S, Baer AM, Baird J, Baldaccini F, Ballardin G, Ballmer SW, Bals A, Balsamo A, Baltus G, Banagiri S, Bankar D, Bankar RS, Barayoga JC, Barbieri C, Barish BC, Barker D, Barkett K, Barneo P, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Bejger M, Belahcene I, Bell AS, Beniwal D, Benjamin MG, Bentley JD, Bergamin F, Berger BK, Bergmann G, Bernuzzi S, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bhandari AV, Bidler J, Biggs E, Bilenko IA, Billingsley G, Birney R, Birnholtz O, Biscans S, Bischi M, Biscoveanu S, Bisht A, Bissenbayeva G, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bobba F, Bode N, Boer M, Boetzel Y, Bogaert G, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Bork R, Boschi V, Bose S, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Breschi M, Briant T, Briggs JH, Brighenti F, Brillet A, Brinkmann M, Brockill P, Brooks AF, Brooks J, Brown DD, Brunett S, Bruno G, Bruntz R, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buscicchio R, Buskulic D, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Calderón Bustillo J, Callaghan JD, Callister TA, Calloni E, Camp JB, Canepa M, Cannon KC, Cao H, Cao J, Carapella G, Carbognani F, Caride S, Carney MF, Carullo G, Casanueva Diaz J, Casentini C, Castañeda J, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cerdá-Durán P, Cesarini E, Chaibi O, Chakravarti K, Chan C, Chan M, Chandra K, Chao S, Charlton P, Chase EA, Chassande-Mottin E, Chatterjee D, Chaturvedi M, Chatziioannou K, Chen HY, Chen X, Chen Y, Cheng HP, Cheong CK, Chia HY, Chiadini F, Chierici R, Chincarini A, Chiummo A, Cho G, Cho HS, Cho M, Christensen N, Chu Q, Chua S, Chung KW, Chung S, Ciani G, Ciecielag P, Cieślar M, Ciobanu AA, Ciolfi R, Cipriano F, Cirone A, Clara F, Clark JA, Clearwater P, Clesse S, Cleva F, Coccia E, Cohadon PF, Cohen D, Colleoni M, Collette CG, Collins C, Colpi M, Constancio M, Conti L, Cooper SJ, Corban P, Corbitt TR, Cordero-Carrión I, Corezzi S, Corley KR, Cornish N, Corre D, Corsi A, Cortese S, Costa CA, Cotesta R, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Covas PB, Coward DM, Cowart MJ, Coyne DC, Coyne R, Creighton JDE, Creighton TD, Cripe J, Croquette M, Crowder SG, Cudell JR, Cullen TJ, Cumming A, Cummings R, Cunningham L, Cuoco E, Curylo M, Canton TD, Dálya G, Dana A, Daneshgaran-Bajastani LM, D'Angelo B, Danilishin SL, D'Antonio S, Danzmann K, Darsow-Fromm C, Dasgupta A, Datrier LEH, Dattilo V, Dave I, Davier M, Davies GS, Davis D, Daw EJ, DeBra D, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Delfavero M, De Lillo N, Del Pozzo W, DeMarchi LM, D'Emilio V, Demos N, Dent T, De Pietri R, De Rosa R, De Rossi C, DeSalvo R, de Varona O, Dhurandhar S, Díaz MC, Diaz-Ortiz M, Dietrich T, Di Fiore L, Di Fronzo C, Di Giorgio C, Di Giovanni F, Di Giovanni M, Di Girolamo T, Di Lieto A, Ding B, Di Pace S, Di Palma I, Di Renzo F, Divakarla AK, Dmitriev A, Doctor Z, Donovan F, Dooley KL, Doravari S, Dorrington I, Downes TP, Drago M, Driggers JC, Du Z, Ducoin JG, Dupej P, Durante O, D'Urso D, Dwyer SE, Easter PJ, Eddolls G, Edelman B, Edo TB, Edy O, Effler A, Ehrens P, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Ejlli A, Errico L, Essick RC, Estelles H, Estevez D, Etienne ZB, Etzel T, Evans M, Evans TM, Ewing BE, Fafone V, Fairhurst S, Fan X, Farinon S, Farr B, Farr WM, Fauchon-Jones EJ, Favata M, Fays M, Fazio M, Feicht J, Fejer MM, Feng F, Fenyvesi E, Ferguson DL, Fernandez-Galiana A, Ferrante I, Ferreira EC, Ferreira TA, Fidecaro F, Fiori I, Fiorucci D, Fishbach M, Fisher RP, Fittipaldi R, Fitz-Axen M, Fiumara V, Flaminio R, Floden E, Flynn E, Fong H, Font JA, Forsyth PWF, Fournier JD, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fritschel P, Frolov VV, Fronzè G, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Galaudage S, Ganapathy D, Ganguly A, Gaonkar SG, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gayathri V, Gemme G, Genin E, Gennai A, George D, George J, Gergely L, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Giacomazzo B, Giaime JA, Giardina KD, Gibson DR, Gier C, Gill K, Glanzer J, Gniesmer J, Godwin P, Goetz E, Goetz R, Gohlke N, Goncharov B, González G, Gopakumar A, Gossan SE, Gosselin M, Gouaty R, Grace B, Grado A, Granata M, Grant A, Gras S, Grassia P, Gray C, Gray R, Greco G, Green AC, Green R, Gretarsson EM, Griggs HL, Grignani G, Grimaldi A, Grimm SJ, Grote H, Grunewald S, Gruning P, Guidi GM, Guimaraes AR, Guixé G, Gulati HK, Guo Y, Gupta A, Gupta A, Gupta P, Gustafson EK, Gustafson R, Haegel L, Halim O, Hall ED, Hamilton EZ, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hansen TJ, Hanson J, Harder T, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hasskew RK, Haster CJ, Haughian K, Hayes FJ, Healy J, Heidmann A, Heintze MC, Heinze J, Heitmann H, Hellman F, Hello P, Hemming G, Hendry M, Heng IS, Hennes E, Hennig J, Heurs M, Hild S, Hinderer T, Hoback SY, Hochheim S, Hofgard E, Hofman D, Holgado AM, Holland NA, Holt K, Holz DE, Hopkins P, Horst C, Hough J, Howell EJ, Hoy CG, Huang Y, Hübner MT, Huerta EA, Huet D, Hughey B, Hui V, Husa S, Huttner SH, Huxford R, Huynh-Dinh T, Idzkowski B, Iess A, Inchauspe H, Ingram C, Intini G, Isac JM, Isi M, Iyer BR, Jacqmin T, Jadhav SJ, Jadhav SP, James AL, Jani K, Janthalur NN, Jaranowski P, Jariwala D, Jaume R, Jenkins AC, Jiang J, Johns GR, Johnson-McDaniel NK, Jones AW, Jones DI, Jones JD, Jones P, Jones R, Jonker RJG, Ju L, Junker J, Kalaghatgi CV, Kalogera V, Kamai B, Kandhasamy S, Kang G, Kanner JB, Kapadia SJ, Karki S, Kashyap R, Kasprzack M, Kastaun W, Katsanevas S, Katsavounidis E, Katzman W, Kaufer S, Kawabe K, Kéfélian F, Keitel D, Keivani A, Kennedy R, Key JS, Khadka S, Khalili FY, Khan I, Khan S, Khan ZA, Khazanov EA, Khetan N, Khursheed M, Kijbunchoo N, Kim C, Kim GJ, Kim JC, Kim K, Kim W, Kim WS, Kim YM, Kimball C, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kleybolte L, Klimenko S, Knowles TD, Knyazev E, Koch P, Koehlenbeck SM, Koekoek G, Koley S, Kondrashov V, Kontos A, Koper N, Korobko M, Korth WZ, Kovalam M, Kozak DB, Kringel V, Krishnendu NV, Królak A, Krupinski N, Kuehn G, Kumar A, Kumar P, Kumar R, Kumar R, Kumar S, Kuo L, Kutynia A, Lackey BD, Laghi D, Lalande E, Lam TL, Lamberts A, Landry M, Lane BB, Lang RN, Lange J, Lantz B, Lanza RK, La Rosa I, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lecoeuche YK, Lee CH, Lee HM, Lee HW, Lee J, Lee K, Lehmann J, Leroy N, Letendre N, Levin Y, Li AKY, Li J, Li K, Li TGF, Li X, Linde F, Linker SD, Linley JN, Littenberg TB, Liu J, Liu X, Llorens-Monteagudo M, Lo RKL, Lockwood A, London LT, Longo A, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Lousto CO, Lovelace G, Lück H, Lumaca D, Lundgren AP, Ma Y, Macas R, Macfoy S, MacInnis M, Macleod DM, MacMillan IAO, Macquet A, Magaña Hernandez I, Magaña-Sandoval F, Magee RM, Majorana E, Maksimovic I, Malik A, Man N, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Mapelli M, Marchesoni F, Marion F, Márka S, Márka Z, Markakis C, Markosyan AS, Markowitz A, Maros E, Marquina A, Marsat S, Martelli F, Martin IW, Martin RM, Martinez V, Martynov DV, Masalehdan H, Mason K, Massera E, Masserot A, Massinger TJ, Masso-Reid M, Mastrogiovanni S, Matas A, Matichard F, Mavalvala N, Maynard E, McCann JJ, McCarthy R, McClelland DE, McCormick S, McCuller L, McGuire SC, McIsaac C, McIver J, McManus DJ, McRae T, McWilliams ST, Meacher D, Meadors GD, Mehmet M, Mehta AK, Mejuto Villa E, Melatos A, Mendell G, Mercer RA, Mereni L, Merfeld K, Merilh EL, Merritt JD, Merzougui M, Meshkov S, Messenger C, Messick C, Metzdorff R, Meyers PM, Meylahn F, Mhaske A, Miani A, Miao H, Michaloliakos I, Michel C, Middleton H, Milano L, Miller AL, Millhouse M, Mills JC, Milotti E, Milovich-Goff MC, Minazzoli O, Minenkov Y, Mishkin A, Mishra C, Mistry T, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Mo G, Mogushi K, Mohapatra SRP, Mohite SR, Molina-Ruiz M, Mondin M, Montani M, Moore CJ, Moraru D, Morawski F, Moreno G, Morisaki S, Mours B, Mow-Lowry CM, Mozzon S, Muciaccia F, Mukherjee A, Mukherjee D, Mukherjee S, Mukherjee S, Mukund N, Mullavey A, Munch J, Muñiz EA, Murray PG, Nagar A, Nardecchia I, Naticchioni L, Nayak RK, Neil BF, Neilson J, Nelemans G, Nelson TJN, Nery M, Neunzert A, Ng KY, Ng S, Nguyen C, Nguyen P, Nichols D, Nichols SA, Nissanke S, Nitz A, Nocera F, Noh M, North C, Nothard D, Nuttall LK, Oberling J, O'Brien BD, Oganesyan G, Ogin GH, Oh JJ, Oh SH, Ohme F, Ohta H, Okada MA, Oliver M, Olivetto C, Oppermann P, Oram RJ, O'Reilly B, Ormiston RG, Ortega LF, O'Shaughnessy R, Ossokine S, Osthelder C, Ottaway DJ, Overmier H, Owen BJ, Pace AE, Pagano G, Page MA, Pagliaroli G, Pai A, Pai SA, Palamos JR, Palashov O, Palomba C, Pan H, Panda PK, Pang PTH, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Parida A, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patricelli B, Payne E, Pearlstone BL, Pechsiri TC, Pedersen AJ, Pedraza M, Pele A, Penn S, Perego A, Perez CJ, Périgois C, Perreca A, Perriès S, Petermann J, Pfeiffer HP, Phelps M, Phukon KS, Piccinni OJ, Pichot M, Piendibene M, Piergiovanni F, Pierro V, Pillant G, Pinard L, Pinto IM, Piotrzkowski K, Pirello M, Pitkin M, Plastino W, Poggiani R, Pong DYT, Ponrathnam S, Popolizio P, Porter EK, Powell J, Prajapati AK, Prasai K, Prasanna R, Pratten G, Prestegard T, Principe M, Prodi GA, Prokhorov L, Punturo M, Puppo P, Pürrer M, Qi H, Quetschke V, Quinonez PJ, Raab FJ, Raaijmakers G, Radkins H, Radulesco N, Raffai P, Rafferty H, Raja S, Rajan C, Rajbhandari B, Rakhmanov M, Ramirez KE, Ramos-Buades A, Rana J, Rao K, Rapagnani P, Raymond V, Razzano M, Read J, Regimbau T, Rei L, Reid S, Reitze DH, Rettegno P, Ricci F, Richardson CJ, Richardson JW, Ricker PM, Riemenschneider G, Riles K, Rizzo M, Robertson NA, Robinet F, Rocchi A, Rodriguez-Soto RD, Rolland L, Rollins JG, Roma VJ, Romanelli M, Romano R, Romel CL, Romero-Shaw IM, Romie JH, Rose CA, Rose D, Rose K, Rosińska D, Rosofsky SG, Ross MP, Rowan S, Rowlinson SJ, Roy PK, Roy S, Roy S, Ruggi P, Rutins G, Ryan K, Sachdev S, Sadecki T, Sakellariadou M, Salafia OS, Salconi L, Saleem M, Salemi F, Samajdar A, Sanchez EJ, Sanchez LE, Sanchis-Gual N, Sanders JR, Santiago KA, Santos E, Sarin N, Sassolas B, Sathyaprakash BS, Sauter O, Savage RL, Savant V, Sawant D, Sayah S, Schaetzl D, Schale P, Scheel M, Scheuer J, Schmidt P, Schnabel R, Schofield RMS, Schönbeck A, Schreiber E, Schulte BW, Schutz BF, Schwarm O, Schwartz E, Scott J, Scott SM, Seidel E, Sellers D, Sengupta AS, Sennett N, Sentenac D, Sequino V, Sergeev A, Setyawati Y, Shaddock DA, Shaffer T, Sharifi S, Shahriar MS, Sharma A, Sharma P, Shawhan P, Shen H, Shikauchi M, Shink R, Shoemaker DH, Shoemaker DM, Shukla K, ShyamSundar S, Siellez K, Sieniawska M, Sigg D, Singer LP, Singh D, Singh N, Singha A, Singhal A, Sintes AM, Sipala V, Skliris V, Slagmolen BJJ, Slaven-Blair TJ, Smetana J, Smith JR, Smith RJE, Somala S, Son EJ, Soni S, Sorazu B, Sordini V, Sorrentino F, Souradeep T, Sowell E, Spencer AP, Spera M, Srivastava AK, Srivastava V, Staats K, Stachie C, Standke M, Steer DA, Steinke M, Steinlechner J, Steinlechner S, Steinmeyer D, Stevenson S, Stocks D, Stops DJ, Stover M, Strain KA, Stratta G, Strunk A, Sturani R, Stuver AL, Sudhagar S, Sudhir V, Summerscales TZ, Sun L, Sunil S, Sur A, Suresh J, Sutton PJ, Swinkels BL, Szczepańczyk MJ, Tacca M, Tait SC, Talbot C, Tanasijczuk AJ, Tanner DB, Tao D, Tápai M, Tapia A, Tapia San Martin EN, Tasson JD, Taylor R, Tenorio R, Terkowski L, Thirugnanasambandam MP, Thomas M, Thomas P, Thompson JE, Thondapu SR, Thorne KA, Thrane E, Tinsman CL, Saravanan TR, Tiwari S, Tiwari S, Tiwari V, Toland K, Tonelli M, Tornasi Z, Torres-Forné A, Torrie CI, Tosta E Melo I, Töyrä D, Travasso F, Traylor G, Tringali MC, Tripathee A, Trovato A, Trudeau RJ, Tsang KW, Tse M, Tso R, Tsukada L, Tsuna D, Tsutsui T, Turconi M, Ubhi AS, Udall R, Ueno K, Ugolini D, Unnikrishnan CS, Urban AL, Usman SA, Utina AC, Vahlbruch H, Vajente G, Valdes G, Valentini M, van Bakel N, van Beuzekom M, van den Brand JFJ, Van Den Broeck C, Vander-Hyde DC, van der Schaaf L, Van Heijningen JV, van Veggel AA, Vardaro M, Varma V, Vass S, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Venugopalan G, Verkindt D, Veske D, Vetrano F, Viceré A, Viets AD, Vinciguerra S, Vine DJ, Vinet JY, Vitale S, Vivanco FH, Vo T, Vocca H, Vorvick C, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walet R, Walker M, Wallace GS, Wallace L, Walsh S, Wang JZ, Wang S, Wang WH, Ward RL, Warden ZA, Warner J, Was M, Watchi J, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Wellmann F, Wen L, Weßels P, Westhouse JW, Wette K, Whelan JT, Whiting BF, Whittle C, Wilken DM, Williams D, Willis JL, Willke B, Winkler W, Wipf CC, Wittel H, Woan G, Woehler J, Wofford JK, Wong ICF, Wright JL, Wu DS, Wysocki DM, Xiao L, Yamamoto H, Yang L, Yang Y, Yang Z, Yap MJ, Yazback M, Yeeles DW, Yu H, Yu H, Yuen SHR, Zadrożny AK, Zadrożny A, Zanolin M, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang T, Zhao C, Zhao G, Zhou M, Zhou Z, Zhu XJ, Zimmerman AB, Zucker ME, and Zweizig J
Abstract: On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85_{-14}^{+21} M_{⊙} and 66_{-18}^{+17} M_{⊙} (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 M_{⊙}. We calculate the mass of the remnant to be 142_{-16}^{+28} M_{⊙}, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3_{-2.6}^{+2.4} Gpc, corresponding to a redshift of 0.82_{-0.34}^{+0.28}. The inferred rate of mergers similar to GW190521 is 0.13_{-0.11}^{+0.30} Gpc^{-3} yr^{-1}.
Published: 2020
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39. Site-selection criteria for the Einstein Telescope.

Author: Amann F, Bonsignorio F, Bulik T, Bulten HJ, Cuccuru S, Dassargues A, DeSalvo R, Fenyvesi E, Fidecaro F, Fiori I, Giunchi C, Grado A, Harms J, Koley S, Kovács L, Losurdo G, Mandic V, Meyers P, Naticchioni L, Nguyen F, Oggiano G, Olivieri M, Paoletti F, Paoli A, Plastino W, Razzano M, Ruggi P, Saccorotti G, Sintes AM, Somlai L, Ván P, and Vasúth M
Abstract: The Einstein Telescope (ET) is a proposed next-generation, underground gravitational-wave detector to be based in Europe. It will provide about an order of magnitude sensitivity increase with respect to the currently operating detectors and, also extend the observation band targeting frequencies as low as 3 Hz. One of the first decisions that needs to be made is about the future ET site following an in-depth site characterization. Site evaluation and selection is a complicated process, which takes into account science, financial, political, and socio-economic criteria. In this paper, we provide an overview of the site-selection criteria for ET, provide a formalism to evaluate the direct impact of environmental noise on ET sensitivity, and outline the necessary elements of a site-characterization campaign.
Published: 2020
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40. Quantum correlations between light and the kilogram-mass mirrors of LIGO.

Author: Yu H, McCuller L, Tse M, Kijbunchoo N, Barsotti L, and Mavalvala N
Abstract: The 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 limit 1-4 . 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 reflects 5 . Here we confirm experimentally the theoretical prediction 5 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.
Published: 2020
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41. Lense-Thirring frame dragging induced by a fast-rotating white dwarf in a binary pulsar system.

Author: Krishnan VV, Bailes M, van Straten W, Wex N, Freire PCC, Keane EF, Tauris TM, Rosado PA, Bhat NDR, Flynn C, Jameson A, and Osłowski S
Abstract: Radio pulsars in short-period eccentric binary orbits can be used to study both gravitational dynamics and binary evolution. The binary system containing PSR J1141-6545 includes a massive white dwarf (WD) companion that formed before the gravitationally bound young radio pulsar. We observed a temporal evolution of the orbital inclination of this pulsar that we infer is caused by a combination of a Newtonian quadrupole moment and Lense-Thirring (LT) precession of the orbit resulting from rapid rotation of the WD. LT precession, an effect of relativistic frame dragging, is a prediction of general relativity. This detection is consistent with an evolutionary scenario in which the WD accreted matter from the pulsar progenitor, spinning up the WD to a period of <200 seconds., (Copyright © 2020 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)
Published: 2020
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42. Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA.

Author: Abbott BP, Abbott R, Abbott TD, Abraham S, Acernese F, Ackley K, Adams C, Adya VB, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Akutsu T, Allen G, Allocca A, Aloy MA, Altin PA, Amato A, Ananyeva A, Anderson SB, Anderson WG, Ando M, Angelova SV, Antier S, Appert S, Arai K, Arai K, Arai Y, Araki S, Araya A, Araya MC, Areeda JS, Arène M, Aritomi N, Arnaud N, Arun KG, Ascenzi S, Ashton G, Aso Y, Aston SM, Astone P, Aubin F, Aufmuth P, AultONeal K, Austin C, Avendano V, Avila-Alvarez A, Babak S, Bacon P, Badaracco F, Bader MKM, Bae SW, Bae YB, Baiotti L, Bajpai R, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Banagiri S, Barayoga JC, Barclay SE, Barish BC, Barker D, Barkett K, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Barton MA, Bartos I, Bassiri R, Basti A, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Bejger M, Belahcene I, Bell AS, Beniwal D, Berger BK, Bergmann G, Bernuzzi S, Bero JJ, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bidler J, Bilenko IA, Bilgili SA, Billingsley G, Birch J, Birney R, Birnholtz O, Biscans S, Biscoveanu S, Bisht A, Bitossi M, Bizouard MA, Blackburn JK, Blair CD, Blair DG, Blair RM, Bloemen S, Bode N, Boer M, Boetzel Y, Bogaert G, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Booth CD, Bork R, Boschi V, Bose S, Bossie K, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Briant T, Briggs JH, Brighenti F, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DA, Brown DD, Brunett S, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Bustillo JC, Callister TA, Calloni E, Camp JB, Campbell WA, Canepa M, Cannon K, Cannon KC, Cao H, Cao J, Capocasa E, Carbognani F, Caride S, Carney MF, Carullo G, Diaz JC, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cerdá-Durán P, Cerretani G, Cesarini E, Chaibi O, Chakravarti K, Chamberlin SJ, Chan M, Chan ML, Chao S, Charlton P, Chase EA, Chassande-Mottin E, Chatterjee D, Chaturvedi M, Chatziioannou K, Cheeseboro BD, Chen CS, Chen HY, Chen KH, Chen X, Chen Y, Chen YR, Cheng HP, Cheong CK, Chia HY, Chincarini A, Chiummo A, Cho G, Cho HS, Cho M, Christensen N, Chu HY, Chu Q, Chu YK, Chua S, Chung KW, Chung S, Ciani G, Ciobanu AA, Ciolfi R, Cipriano F, Cirone A, Clara F, Clark JA, Clearwater P, Cleva F, Cocchieri C, Coccia E, Cohadon PF, Cohen D, Colgan R, Colleoni M, Collette CG, Collins C, Cominsky LR, Constancio M Jr, Conti L, Cooper SJ, Corban P, Corbitt TR, Cordero-Carrión I, Corley KR, Cornish N, Corsi A, Cortese S, Costa CA, Cotesta R, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Covas PB, Cowan EE, Coward DM, Cowart MJ, Coyne DC, Coyne R, Creighton JDE, Creighton TD, Cripe J, Croquette M, Crowder SG, Cullen TJ, Cumming A, Cunningham L, Cuoco E, Canton TD, Dálya G, Danilishin SL, D'Antonio S, Danzmann K, Dasgupta A, Da Silva Costa CF, Datrier LEH, Dattilo V, Dave I, Davier M, Davis D, Daw EJ, DeBra D, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Pozzo WD, DeMarchi LM, Demos N, Dent T, De Pietri R, Derby J, De Rosa R, De Rossi C, DeSalvo R, de Varona O, Dhurandhar S, Díaz MC, Dietrich T, Fiore LD, Giovanni MD, Girolamo TD, Lieto AD, Ding B, Pace SD, Palma ID, Renzo FD, Dmitriev A, Doctor Z, Doi K, Donovan F, Dooley KL, Doravari S, Dorrington I, Downes TP, Drago M, Driggers JC, Du Z, Ducoin JG, Dupej P, Dwyer SE, Easter PJ, Edo TB, Edwards MC, Effler A, Eguchi S, Ehrens P, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Enomoto Y, Essick RC, Estelles H, Estevez D, Etienne ZB, Etzel T, Evans M, Evans TM, Fafone V, Fair H, Fairhurst S, Fan X, Farinon S, Farr B, Farr WM, Fauchon-Jones EJ, Favata M, Fays M, Fazio M, Fee C, Feicht J, Fejer MM, Feng F, Fernandez-Galiana A, Ferrante I, Ferreira EC, Ferreira TA, Ferrini F, Fidecaro F, Fiori I, Fiorucci D, Fishbach M, Fisher RP, Fishner JM, Fitz-Axen M, Flaminio R, Fletcher M, Flynn E, Fong H, Font JA, Forsyth PWF, Fournier JD, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fritschel P, Frolov VV, Fujii Y, Fukunaga M, Fukushima M, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Gammaitoni L, Ganija MR, Gaonkar SG, Garcia A, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gaur G, Gayathri V, Ge GG, Gemme G, Genin E, Gennai A, George D, George J, Gergely L, Germain V, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Giacomazzo B, Giaime JA, Giardina KD, Giazotto A, Gill K, Giordano G, Glover L, Godwin P, Goetz E, Goetz R, Goncharov B, González G, Castro JMG, Gopakumar A, Gorodetsky ML, Gossan SE, Gosselin M, Gouaty R, Grado A, Graef C, Granata M, Grant A, Gras S, Grassia P, Gray C, Gray R, Greco G, Green AC, Green R, Gretarsson EM, Groot P, Grote H, Grunewald S, Gruning P, Guidi GM, Gulati HK, Guo Y, Gupta A, Gupta MK, Gustafson EK, Gustafson R, Haegel L, Hagiwara A, Haino S, Halim O, Hall BR, Hall ED, Hamilton EZ, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hanson J, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hasegawa K, Haster CJ, Haughian K, Hayakawa H, Hayama K, Hayes FJ, Healy J, Heidmann A, Heintze MC, Heitmann H, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heptonstall AW, Heurs M, Hild S, Himemoto Y, Hinderer T, Hiranuma Y, Hirata N, Hirose E, Hoak D, Hochheim S, Hofman D, Holgado AM, Holland NA, Holt K, Holz DE, Hong Z, Hopkins P, Horst C, Hough J, Howell EJ, Hoy CG, Hreibi A, Hsieh BH, Huang GZ, Huang PW, Huang YJ, Huerta EA, Huet D, Hughey B, Hulko M, Husa S, Huttner SH, Huynh-Dinh T, Idzkowski B, Iess A, Ikenoue B, Imam S, Inayoshi K, Ingram C, Inoue Y, Inta R, Intini G, Ioka K, Irwin B, Isa HN, Isac JM, Isi M, Itoh Y, Iyer BR, Izumi K, Jacqmin T, Jadhav SJ, Jani K, Janthalur NN, Jaranowski P, Jenkins AC, Jiang J, Johnson DS, Jones AW, Jones DI, Jones R, Jonker RJG, Ju L, Jung K, Jung P, Junker J, Kajita T, Kalaghatgi CV, Kalogera V, Kamai B, Kamiizumi M, Kanda N, Kandhasamy S, Kang GW, Kanner JB, Kapadia SJ, Karki S, Karvinen KS, Kashyap R, Kasprzack M, Katsanevas S, Katsavounidis E, Katzman W, Kaufer S, Kawabe K, Kawaguchi K, Kawai N, Kawasaki T, Keerthana NV, Kéfélian F, Keitel D, Kennedy R, Key JS, Khalili FY, Khan H, Khan I, Khan S, Khan Z, Khazanov EA, Khursheed M, Kijbunchoo N, Kim C, Kim C, Kim JC, Kim J, Kim K, Kim W, Kim WS, Kim YM, Kimball C, Kimura N, King EJ, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kita N, Kitazawa H, Kleybolte L, Klika JH, Klimenko S, Knowles TD, Knyazev E, Koch P, Koehlenbeck SM, Koekoek G, Kojima Y, Kokeyama K, Koley S, Komori K, Kondrashov V, Kong AKH, Kontos A, Koper N, Korobko M, Korth WZ, Kotake K, Kowalska I, Kozak DB, Kozakai C, Kozu R, Kringel V, Krishnendu N, Królak A, Kuehn G, Kumar A, Kumar P, Kumar R, Kumar R, Kumar S, Kume J, Kuo CM, Kuo HS, Kuo L, Kuroyanagi S, Kusayanagi K, Kutynia A, Kwak K, Kwang S, Lackey BD, Lai KH, Lam TL, Landry M, Lane BB, Lang RN, Lange J, Lantz B, Lanza RK, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lecoeuche YK, Lee CH, Lee HK, Lee HM, Lee HW, Lee J, Lee K, Lee RK, Lehmann J, Lenon A, Leonardi M, Leroy N, Letendre N, Levin Y, Li J, Li KJL, Li TGF, Li X, Lin CY, Lin F, Lin FL, Lin LCC, Linde F, Linker SD, Littenberg TB, Liu GC, Liu J, Liu X, Lo RKL, Lockerbie NA, London LT, Longo A, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Lousto CO, Lovelace G, Lower ME, Lück H, Lumaca D, Lundgren AP, Luo LW, Lynch R, Ma Y, Macas R, Macfoy S, MacInnis M, Macleod DM, Macquet A, Magaña-Sandoval F, Zertuche LM, Magee RM, Majorana E, Maksimovic I, Malik A, Man N, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Marchesoni F, Marchio M, Marion F, Márka S, Márka Z, Markakis C, Markosyan AS, Markowitz A, Maros E, Marquina A, Marsat S, Martelli F, Martin IW, Martin RM, Martynov DV, Mason K, Massera E, Masserot A, Massinger TJ, Masso-Reid M, Mastrogiovanni S, Matas A, Matichard F, Matone L, Mavalvala N, Mazumder N, McCann JJ, McCarthy R, McClelland DE, McCormick S, McCuller L, McGuire SC, McIver J, McManus DJ, McRae T, McWilliams ST, Meacher D, Meadors GD, Mehmet M, Mehta AK, Meidam J, Melatos A, Mendell G, Mercer RA, Mereni L, Merilh EL, Merzougui M, Meshkov S, Messenger C, Messick C, Metzdorff R, Meyers PM, Miao H, Michel C, Michimura Y, Middleton H, Mikhailov EE, Milano L, Miller AL, Miller A, Millhouse M, Mills JC, Milovich-Goff MC, Minazzoli O, Minenkov Y, Mio N, Mishkin A, Mishra C, Mistry T, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Miyakawa O, Miyamoto A, Miyazaki Y, Miyo K, Miyoki S, Mo G, Moffa D, Mogushi K, Mohapatra SRP, Montani M, Moore CJ, Moraru D, Moreno G, Morisaki S, Moriwaki Y, Mours B, Mow-Lowry CM, Mukherjee A, Mukherjee D, Mukherjee S, Mukund N, Mullavey A, Munch J, Muñiz EA, Muratore M, Murray PG, Nagano K, Nagano S, Nagar A, Nakamura K, Nakano H, Nakano M, Nakashima R, Nardecchia I, Narikawa T, Naticchioni L, Nayak RK, Negishi R, Neilson J, Nelemans G, Nelson TJN, Nery M, Neunzert A, Ng KY, Ng S, Nguyen P, Ni WT, Nichols D, Nishizawa A, Nissanke S, Nocera F, North C, Nuttall LK, Obergaulinger M, Oberling J, O'Brien BD, Obuchi Y, O'Dea GD, Ogaki W, Ogin GH, Oh JJ, Oh SH, Ohashi M, Ohishi N, Ohkawa M, Ohme F, Ohta H, Okada MA, Okutomi K, Oliver M, Oohara K, Ooi CP, Oppermann P, Oram RJ, O'Reilly B, Ormiston RG, Ortega LF, O'Shaughnessy R, Oshino S, Ossokine S, Ottaway DJ, Overmier H, Owen BJ, Pace AE, Pagano G, Page MA, Pai A, Pai SA, Palamos JR, Palashov O, Palomba C, Pal-Singh A, Pan HW, Pan KC, Pang B, Pang HF, Pang PTH, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Papa MA, Parida A, Park J, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patil M, Patricelli B, Pearlstone BL, Pedersen C, Pedraza M, Pedurand R, Pele A, Arellano FEP, Penn S, Perez CJ, Perreca A, Pfeiffer HP, Phelps M, Phukon KS, Piccinni OJ, Pichot M, Piergiovanni F, Pillant G, Pinard L, Pinto I, Pirello M, Pitkin M, Poggiani R, Pong DYT, Ponrathnam S, Popolizio P, Porter EK, Powell J, Prajapati AK, Prasad J, Prasai K, Prasanna R, Pratten G, Prestegard T, Privitera S, Prodi GA, Prokhorov LG, Puncken O, Punturo M, Puppo P, Pürrer M, Qi H, Quetschke V, Quinonez PJ, Quintero EA, Quitzow-James R, Raab FJ, Radkins H, Radulescu N, Raffai P, Raja S, Rajan C, Rajbhandari B, Rakhmanov M, Ramirez KE, Ramos-Buades A, Rana J, Rao K, Rapagnani P, Raymond V, Razzano M, Read J, Regimbau T, Rei L, Reid S, Reitze DH, Ren W, Ricci F, Richardson CJ, Richardson JW, Ricker PM, Riles K, Rizzo M, Robertson NA, Robie R, Robinet F, Rocchi A, Rolland L, Rollins JG, Roma VJ, Romanelli M, Romano R, Romel CL, Romie JH, Rose K, Rosińska D, Rosofsky SG, Ross MP, Rowan S, Rüdiger A, Ruggi P, Rutins G, Ryan K, Sachdev S, Sadecki T, Sago N, Saito S, Saito Y, Sakai K, Sakai Y, Sakamoto H, Sakellariadou M, Sakuno Y, Salconi L, Saleem M, Samajdar A, Sammut L, Sanchez EJ, Sanchez LE, Sanchis-Gual N, Sandberg V, Sanders JR, Santiago KA, Sarin N, Sassolas B, Sathyaprakash BS, Sato S, Sato T, Sauter O, Savage RL, Sawada T, Schale P, Scheel M, Scheuer J, Schmidt P, Schnabel R, Schofield RMS, Schönbeck A, Schreiber E, Schulte BW, Schutz BF, Schwalbe SG, Scott J, Scott SM, Seidel E, Sekiguchi T, Sekiguchi Y, Sellers D, Sengupta AS, Sennett N, Sentenac D, Sequino V, Sergeev A, Setyawati Y, Shaddock DA, Shaffer T, Shahriar MS, Shaner MB, Shao L, Sharma P, Shawhan P, Shen H, Shibagaki S, Shimizu R, Shimoda T, Shimode K, Shink R, Shinkai H, Shishido T, Shoda A, Shoemaker DH, Shoemaker DM, ShyamSundar S, Siellez K, Sieniawska M, Sigg D, Silva AD, Singer LP, Singh N, Singhal A, Sintes AM, Sitmukhambetov S, Skliris V, Slagmolen BJJ, Slaven-Blair TJ, Smith JR, Smith RJE, Somala S, Somiya K, Son EJ, Sorazu B, Sorrentino F, Sotani H, Souradeep T, Sowell E, Spencer AP, Srivastava AK, Srivastava V, Staats K, Stachie C, Standke M, Steer DA, Steinke M, Steinlechner J, Steinlechner S, Steinmeyer D, Stevenson SP, Stocks D, Stone R, Stops DJ, Strain KA, Stratta G, Strigin SE, Strunk A, Sturani R, Stuver AL, Sudhir V, Sugimoto R, Summerscales TZ, Sun L, Sunil S, Suresh J, Sutton PJ, Suzuki T, Suzuki T, Swinkels BL, Szczepańczyk MJ, Tacca M, Tagoshi H, Tait SC, Takahashi H, Takahashi R, Takamori A, Takano S, Takeda H, Takeda M, Talbot C, Talukder D, Tanaka H, Tanaka K, Tanaka K, Tanaka T, Tanaka T, Tanioka S, Tanner DB, Tápai M, Martin ENTS, Taracchini A, Tasson JD, Taylor R, Telada S, Thies F, Thomas M, Thomas P, Thondapu SR, Thorne KA, Thrane E, Tiwari S, Tiwari S, Tiwari V, Toland K, Tomaru T, Tomigami Y, Tomura T, Tonelli M, Tornasi Z, Torres-Forné A, Torrie CI, Töyrä D, Travasso F, Traylor G, Tringali MC, Trovato A, Trozzo L, Trudeau R, Tsang KW, Tsang TTL, Tse M, Tso R, Tsubono K, Tsuchida S, Tsukada L, Tsuna D, Tsuzuki T, Tuyenbayev D, Uchikata N, Uchiyama T, Ueda A, Uehara T, Ueno K, Ueshima G, Ugolini D, Unnikrishnan CS, Uraguchi F, Urban AL, Ushiba T, Usman SA, Vahlbruch H, Vajente G, Valdes G, Bakel NV, Beuzekom MV, Brand JFJVD, Broeck CVD, Vander-Hyde DC, Schaaf LV, Heijningen JVV, Putten MHPMV, Veggel AAV, Vardaro M, Varma V, Vass S, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Venugopalan G, Verkindt D, Vetrano F, Viceré A, Viets AD, Vine DJ, Vinet JY, Vitale S, Vivanco FH, Vo T, Vocca H, Vorvick C, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walet R, Walker M, Wallace L, Walsh S, Wang G, Wang H, Wang J, Wang JZ, Wang WH, Wang YF, Ward RL, Warden ZA, Warner J, Was M, Watchi J, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Wellmann F, Wen L, Wessel EK, Weßels P, Westhouse JW, Wette K, Whelan JT, Whiting BF, Whittle C, Wilken DM, Williams D, Williamson AR, Willis JL, Willke B, Wimmer MH, Winkler W, Wipf CC, Wittel H, Woan G, Woehler J, Wofford JK, Worden J, Wright JL, Wu CM, Wu DS, Wu HC, Wu SR, Wysocki DM, Xiao L, Xu WR, Yamada T, Yamamoto H, Yamamoto K, Yamamoto K, Yamamoto T, Yancey CC, Yang L, Yap MJ, Yazback M, Yeeles DW, Yokogawa K, Yokoyama J, Yokozawa T, Yoshioka T, Yu H, Yu H, Yuen SHR, Yuzurihara H, Yvert M, Zadrożny AK, Zanolin M, Zeidler S, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang T, Zhao C, Zhao Y, Zhou M, Zhou Z, Zhu XJ, Zhu ZH, Zimmerman AB, Zucker ME, and Zweizig J
Abstract: We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star-black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of 10 5 , 10 6 , 10 7 Mpc 3 for binary neutron star, neutron star-black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of 1 - 1 + 12 ( 10 - 10 + 52 ) for binary neutron star mergers, of 0 - 0 + 19 ( 1 - 1 + 91 ) for neutron star-black hole mergers, and 17 - 11 + 22 ( 79 - 44 + 89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers., (© The Author(s) 2020.)
Published: 2020
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43. Author Correction: Superluminal motion of a relativistic jet in the neutron-star merger GW170817.

Author: Mooley KP, Deller AT, Gottlieb O, Nakar E, Hallinan G, Bourke S, Frail DA, Horesh A, Corsi A, and Hotokezaka K
Abstract: An Amendment to this paper has been published and can be accessed via a link at the top of the paper.
Published: 2020
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44. Quantum-Enhanced Advanced LIGO Detectors in the Era of Gravitational-Wave Astronomy.

Author: Tse M, Yu H, Kijbunchoo N, Fernandez-Galiana A, Dupej P, Barsotti L, Blair CD, Brown DD, Dwyer SE, Effler A, Evans M, Fritschel P, Frolov VV, Green AC, Mansell GL, Matichard F, Mavalvala N, McClelland DE, McCuller L, McRae T, Miller J, Mullavey A, Oelker E, Phinney IY, Sigg D, Slagmolen BJJ, Vo T, Ward RL, Whittle C, Abbott R, Adams C, Adhikari RX, Ananyeva A, Appert S, Arai K, Areeda JS, Asali Y, Aston SM, Austin C, Baer AM, Ball M, Ballmer SW, Banagiri S, Barker D, Bartlett J, Berger BK, Betzwieser J, Bhattacharjee D, Billingsley G, Biscans S, Blair RM, Bode N, Booker P, Bork R, Bramley A, Brooks AF, Buikema A, Cahillane C, Cannon KC, Chen X, Ciobanu AA, Clara F, Cooper SJ, Corley KR, Countryman ST, Covas PB, Coyne DC, Datrier LEH, Davis D, Di Fronzo C, Driggers JC, Etzel T, Evans TM, Feicht J, Fulda P, Fyffe M, Giaime JA, Giardina KD, Godwin P, Goetz E, Gras S, Gray C, Gray R, Gupta A, Gustafson EK, Gustafson R, Hanks J, Hanson J, Hardwick T, Hasskew RK, Heintze MC, Helmling-Cornell AF, Holland NA, Jones JD, Kandhasamy S, Karki S, Kasprzack M, Kawabe K, King PJ, Kissel JS, Kumar R, Landry M, Lane BB, Lantz B, Laxen M, Lecoeuche YK, Leviton J, Liu J, Lormand M, Lundgren AP, Macas R, MacInnis M, Macleod DM, Márka S, Márka Z, Martynov DV, Mason K, Massinger TJ, McCarthy R, McCormick S, McIver J, Mendell G, Merfeld K, Merilh EL, Meylahn F, Mistry T, Mittleman R, Moreno G, Mow-Lowry CM, Mozzon S, Nelson TJN, Nguyen P, Nuttall LK, Oberling J, Oram RJ, O'Reilly B, Osthelder C, Ottaway DJ, Overmier H, Palamos JR, Parker W, Payne E, Pele A, Perez CJ, Pirello M, Radkins H, Ramirez KE, Richardson JW, Riles K, Robertson NA, Rollins JG, Romel CL, Romie JH, Ross MP, Ryan K, Sadecki T, Sanchez EJ, Sanchez LE, Saravanan TR, Savage RL, Schaetzl D, Schnabel R, Schofield RMS, Schwartz E, Sellers D, Shaffer TJ, Smith JR, Soni S, Sorazu B, Spencer AP, Strain KA, Sun L, Szczepańczyk MJ, Thomas M, Thomas P, Thorne KA, Toland K, Torrie CI, Traylor G, Urban AL, Vajente G, Valdes G, Vander-Hyde DC, Veitch PJ, Venkateswara K, Venugopalan G, Viets AD, Vorvick C, Wade M, Warner J, Weaver B, Weiss R, Willke B, Wipf CC, Xiao L, Yamamoto H, Yap MJ, Yu H, Zhang L, Zucker ME, and Zweizig J
Abstract: The 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).
Published: 2019
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45. Search for Subsolar Mass Ultracompact Binaries in Advanced LIGO's Second Observing Run.

Author: Abbott BP, Abbott R, Abbott TD, Abraham S, Acernese F, Ackley K, Adams C, Adhikari RX, Adya VB, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen G, Allocca A, Aloy MA, Altin PA, Amato A, Anand S, Ananyeva A, Anderson SB, Anderson WG, Angelova SV, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Aronson SM, Arun KG, Ascenzi S, Ashton G, Aston SM, Astone P, Aubin F, Aufmuth P, AultONeal K, Austin C, Avendano V, Avila-Alvarez A, Babak S, Bacon P, Badaracco F, Bader MKM, Bae S, Baird J, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Bals A, Banagiri S, Barayoga JC, Barbieri C, Barclay SE, Barish BC, Barker D, Barkett K, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Bejger M, Belahcene I, Bell AS, Beniwal D, Benjamin MG, Berger BK, Bergmann G, Bernuzzi S, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bidler J, Biggs E, Bilenko IA, Bilgili SA, Billingsley G, Birney R, Birnholtz O, Biscans S, Bischi M, Biscoveanu S, Bisht A, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bloemen S, Bobba F, Bode N, Boer M, Boetzel Y, Bogaert G, Bondu F, Bonnand R, Booker P, Boom BA, Bork R, Boschi V, Bose S, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Breschi M, Briant T, Briggs JH, Brighenti F, Brillet A, Brinkmann M, Brockill P, Brooks AF, Brooks J, Brown DD, Brunett S, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Calderón Bustillo J, Callister TA, Calloni E, Camp JB, Campbell WA, Cannon KC, Cao H, Cao J, Carapella G, Carbognani F, Caride S, Carney MF, Carullo G, Casanueva Diaz J, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cerdá-Durán P, Cesarini E, Chaibi O, Chakravarti K, Chamberlin SJ, Chan M, Chao S, Charlton P, Chase EA, Chassande-Mottin E, Chatterjee D, Chaturvedi M, Chatziioannou K, Cheeseboro BD, Chen HY, Chen X, Chen Y, Cheng HP, Cheong CK, Chia HY, Chiadini F, Chincarini A, Chiummo A, Cho G, Cho HS, Cho M, Christensen N, Chu Q, Chua S, Chung KW, Chung S, Ciani G, Cieślar M, Ciobanu AA, Ciolfi R, Cipriano F, Cirone A, Clara F, Clark JA, Clearwater P, Cleva F, Coccia E, Cohadon PF, Cohen D, Colleoni M, Collette CG, Collins C, Colpi M, Cominsky LR, Constancio M, Conti L, Cooper SJ, Corban P, Corbitt TR, Cordero-Carrión I, Corezzi S, Corley KR, Cornish N, Corre D, Corsi A, Cortese S, Costa CA, Cotesta R, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Covas PB, Cowan EE, Coward DM, Cowart MJ, Coyne DC, Coyne R, Creighton JDE, Creighton TD, Cripe J, Croquette M, Crowder SG, Cullen TJ, Cumming A, Cunningham L, Cuoco E, Canton TD, Dálya G, D'Angelo B, Danilishin SL, D'Antonio S, Danzmann K, Dasgupta A, Da Silva Costa CF, Datrier LEH, Dattilo V, Dave I, Davier M, Davis D, Daw EJ, DeBra D, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Del Pozzo W, DeMarchi LM, Demos N, Dent T, De Pietri R, De Rosa R, De Rossi C, DeSalvo R, de Varona O, Dhurandhar S, Díaz MC, Dietrich T, Di Fiore L, DiFronzo C, Di Giorgio C, Di Giovanni F, Di Giovanni M, Di Girolamo T, Di Lieto A, Ding B, Di Pace S, Di Palma I, Di Renzo F, Divakarla AK, Dmitriev A, Doctor Z, Donovan F, Dooley KL, Doravari S, Dorrington I, Downes TP, Drago M, Driggers JC, Du Z, Ducoin JG, Dupej P, Durante O, Dwyer SE, Easter PJ, Eddolls G, Edo TB, Effler A, Ehrens P, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Errico L, Essick RC, Estelles H, Estevez D, Etienne ZB, Etzel T, Evans M, Evans TM, Fafone V, Fairhurst S, Fan X, Farinon S, Farr B, Farr WM, Fauchon-Jones EJ, Favata M, Fays M, Fazio M, Fee C, Feicht J, Fejer MM, Feng F, Fernandez-Galiana A, Ferrante I, Ferreira EC, Ferreira TA, Fidecaro F, Fiori I, Fiorucci D, Fishbach M, Fisher RP, Fishner JM, Fittipaldi R, Fitz-Axen M, Fiumara V, Flaminio R, Fletcher M, Floden E, Flynn E, Fong H, Font JA, Forsyth PWF, Fournier JD, Vivanco FH, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fritschel P, Frolov VV, Fronzè G, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Gammaitoni L, Gaonkar SG, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gaur G, Gayathri V, Gemme G, Genin E, Gennai A, George D, George J, Gergely L, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Giacomazzo B, Giaime JA, Giardina KD, Gibson DR, Gill K, Glover L, Gniesmer J, Godwin P, Goetz E, Goetz R, Goncharov B, González G, Gonzalez Castro JM, Gopakumar A, Gossan SE, Gosselin M, Gouaty R, Grace B, Grado A, Granata M, Grant A, Gras S, Grassia P, Gray C, Gray R, Greco G, Green AC, Green R, Gretarsson EM, Grimaldi A, Grimm SJ, Groot P, Grote H, Grunewald S, Gruning P, Guidi GM, Gulati HK, Guo Y, Gupta A, Gupta A, Gupta P, Gustafson EK, Gustafson R, Haegel L, Halim O, Hall BR, Hall ED, Hamilton EZ, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hansen TJ, Hanson J, Harder T, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hasskew RK, Haster CJ, Haughian K, Hayes FJ, Healy J, Heidmann A, Heintze MC, Heitmann H, Hellman F, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heurs M, Hild S, Hinderer T, Hochheim S, Hofman D, Holgado AM, Holland NA, Holt K, Holz DE, Hopkins P, Horst C, Hough J, Howell EJ, Hoy CG, Huang Y, Hübner MT, Huerta EA, Huet D, Hughey B, Hui V, Husa S, Huttner SH, Huynh-Dinh T, Idzkowski B, Iess A, Inchauspe H, Ingram C, Inta R, Intini G, Irwin B, Isa HN, Isac JM, Isi M, Iyer BR, Jacqmin T, Jadhav SJ, Jani K, Janthalur NN, Jaranowski P, Jariwala D, Jenkins AC, Jiang J, Johnson DS, Jones AW, Jones DI, Jones JD, Jones R, Jonker RJG, Ju L, Junker J, Kalaghatgi CV, Kalogera V, Kamai B, Kandhasamy S, Kang G, Kanner JB, Kapadia SJ, Karki S, Kashyap R, Kasprzack M, Katsanevas S, Katsavounidis E, Katzman W, Kaufer S, Kawabe K, Keerthana NV, Kéfélian F, Keitel D, Kennedy R, Key JS, Khalili FY, Khan I, Khan S, Khazanov EA, Khetan N, Khursheed M, Kijbunchoo N, Kim C, Kim JC, Kim K, Kim W, Kim WS, Kim YM, Kimball C, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kleybolte L, Klika JH, Klimenko S, Knowles TD, Koch P, Koehlenbeck SM, Koekoek G, Koley S, Kondrashov V, Kontos A, Koper N, Korobko M, Korth WZ, Kovalam M, Kozak DB, Krämer C, Kringel V, Krishnendu N, Królak A, Krupinski N, Kuehn G, Kumar A, Kumar P, Kumar R, Kumar R, Kuo L, Kutynia A, Kwang S, Lackey BD, Laghi D, Lai KH, Lam TL, Landry M, Lane BB, Lang RN, Lange J, Lantz B, Lanza RK, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lecoeuche YK, Lee CH, Lee HK, Lee HM, Lee HW, Lee J, Lee K, Lehmann J, Lenon AK, Leroy N, Letendre N, Levin Y, Li A, Li J, Li KJL, Li TGF, Li X, Lin F, Linde F, Linker SD, Littenberg TB, Liu J, Liu X, Llorens-Monteagudo M, Lo RKL, London LT, Longo A, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Lousto CO, Lovelace G, Lower ME, Lück H, Lumaca D, Lundgren AP, Lynch R, Ma Y, Macas R, Macfoy S, MacInnis M, Macleod DM, Macquet A, Magaña Hernandez I, Magaña-Sandoval F, Magee RM, Majorana E, Maksimovic I, Malik A, Man N, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Mapelli M, Marchesoni F, Marion F, Márka S, Márka Z, Markakis C, Markosyan AS, Markowitz A, Maros E, Marquina A, Marsat S, Martelli F, Martin IW, Martin RM, Martinez V, Martynov DV, Masalehdan H, Mason K, Massera E, Masserot A, Massinger TJ, Masso-Reid M, Mastrogiovanni S, Matas A, Matichard F, Matone L, Mavalvala N, McCann JJ, McCarthy R, McClelland DE, McClincy P, McCormick S, McCuller L, McGuire SC, McIsaac C, McIver J, McManus DJ, McRae T, McWilliams ST, Meacher D, Meadors GD, Mehmet M, Mehta AK, Meidam J, Mejuto Villa E, Melatos A, Mendell G, Mercer RA, Mereni L, Merfeld K, Merilh EL, Merzougui M, Meshkov S, Messenger C, Messick C, Messina F, Metzdorff R, Meyers PM, Meylahn F, Miani A, Miao H, Michel C, Middleton H, Milano L, Miller AL, Millhouse M, Mills JC, Milovich-Goff MC, Minazzoli O, Minenkov Y, Mishkin A, Mishra C, Mistry T, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Mo G, Moffa D, Mogushi K, Mohapatra SRP, Molina-Ruiz M, Mondin M, Montani M, Moore CJ, Moraru D, Morawski F, Moreno G, Morisaki S, Mours B, Mow-Lowry CM, Muciaccia F, Mukherjee A, Mukherjee D, Mukherjee S, Mukherjee S, Mukund N, Mullavey A, Munch J, Muñiz EA, Muratore M, Murray PG, Nardecchia I, Naticchioni L, Nayak RK, Neil BF, Neilson J, Nelemans G, Nelson TJN, Nery M, Neunzert A, Nevin L, Ng KY, Ng S, Nguyen C, Nguyen P, Nichols D, Nichols SA, Nissanke S, Nocera F, North C, Nuttall LK, Obergaulinger M, Oberling J, O'Brien BD, Oganesyan G, Ogin GH, Oh JJ, Oh SH, Ohme F, Ohta H, Okada MA, Oliver M, Oppermann P, Oram RJ, O'Reilly B, Ormiston RG, Ortega LF, O'Shaughnessy R, Ossokine S, Ottaway DJ, Overmier H, Owen BJ, Pace AE, Pagano G, Page MA, Pagliaroli G, Pai A, Pai SA, Palamos JR, Palashov O, Palomba C, Pan H, Panda PK, Pang PTH, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Parida A, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patil M, Patricelli B, Payne E, Pearlstone BL, Pechsiri TC, Pedersen AJ, Pedraza M, Pedurand R, Pele A, Penn S, Perego A, Perez CJ, Périgois C, Perreca A, Petermann J, Pfeiffer HP, Phelps M, Phukon KS, Piccinni OJ, Pichot M, Piergiovanni F, Pierro V, Pillant G, Pinard L, Pinto IM, Pirello M, Pitkin M, Plastino W, Poggiani R, Pong DYT, Ponrathnam S, Popolizio P, Porter EK, Powell J, Prajapati AK, Prasad J, Prasai K, Prasanna R, Pratten G, Prestegard T, Principe M, Prodi GA, Prokhorov L, Punturo M, Puppo P, Pürrer M, Qi H, Quetschke V, Quinonez PJ, Raab FJ, Raaijmakers G, Radkins H, Radulesco N, Raffai P, Raja S, Rajan C, Rajbhandari B, Rakhmanov M, Ramirez KE, Ramos-Buades A, Rana J, Rao K, Rapagnani P, Raymond V, Razzano M, Read J, Regimbau T, Rei L, Reid S, Reitze DH, Rettegno P, Ricci F, Richardson CJ, Richardson JW, Ricker PM, Riemenschneider G, Riles K, Rizzo M, Robertson NA, Robinet F, Rocchi A, Rolland L, Rollins JG, Roma VJ, Romanelli M, Romano R, Romel CL, Romie JH, Rose CA, Rose D, Rose K, Rosińska D, Rosofsky SG, Ross MP, Rowan S, Rüdiger A, Ruggi P, Rutins G, Ryan K, Sachdev S, Sadecki T, Sakellariadou M, Salafia OS, Salconi L, Saleem M, Samajdar A, Sammut L, Sanchez EJ, Sanchez LE, Sanchis-Gual N, Sanders JR, Santiago KA, Santos E, Sarin N, Sassolas B, Sathyaprakash BS, Sauter O, Savage RL, Schale P, Scheel M, Scheuer J, Schmidt P, Schnabel R, Schofield RMS, Schönbeck A, Schreiber E, Schulte BW, Schutz BF, Scott J, Scott SM, Seidel E, Sellers D, Sengupta AS, Sennett N, Sentenac D, Sequino V, Sergeev A, Setyawati Y, Shaddock DA, Shaffer T, Shahriar MS, Shaner MB, Sharma A, Sharma P, Shawhan P, Shen H, Shink R, Shoemaker DH, Shoemaker DM, Shukla K, ShyamSundar S, Siellez K, Sieniawska M, Sigg D, Singer LP, Singh D, Singh N, Singhal A, Sintes AM, Sitmukhambetov S, Skliris V, Slagmolen BJJ, Slaven-Blair TJ, Smith JR, Smith RJE, Somala S, Son EJ, Soni S, Sorazu B, Sorrentino F, Souradeep T, Sowell E, Spencer AP, Spera M, Srivastava AK, Srivastava V, Staats K, Stachie C, Standke M, Steer DA, Steinke M, Steinlechner J, Steinlechner S, Steinmeyer D, Stevenson SP, Stocks D, Stone R, Stops DJ, Strain KA, Stratta G, Strigin SE, Strunk A, Sturani R, Stuver AL, Sudhir V, Summerscales TZ, Sun L, Sunil S, Sur A, Suresh J, Sutton PJ, Swinkels BL, Szczepańczyk MJ, Tacca M, Tait SC, Talbot C, Tanner DB, Tao D, Tápai M, Tapia A, Tasson JD, Taylor R, Tenorio R, Terkowski L, Thomas M, Thomas P, Thondapu SR, Thorne KA, Thrane E, Tiwari S, Tiwari S, Tiwari V, Toland K, Tonelli M, Tornasi Z, Torres-Forné A, Torrie CI, Töyrä D, Travasso F, Traylor G, Tringali MC, Tripathee A, Trovato A, Trozzo L, Tsang KW, Tse M, Tso R, Tsukada L, Tsuna D, Tsutsui T, Tuyenbayev D, Ueno K, Ugolini D, Unnikrishnan CS, Urban AL, Usman SA, Vahlbruch H, Vajente G, Valdes G, Valentini M, van Bakel N, van Beuzekom M, van den Brand JFJ, Van Den Broeck C, Vander-Hyde DC, van der Schaaf L, VanHeijningen JV, van Veggel AA, Vardaro M, Varma V, Vass S, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Venugopalan G, Verkindt D, Vetrano F, Viceré A, Viets AD, Vinciguerra S, Vine DJ, Vinet JY, Vitale S, Vo T, Vocca H, Vorvick C, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walet R, Walker M, Wallace L, Walsh S, Wang H, Wang JZ, Wang S, Wang WH, Wang YF, Ward RL, Warden ZA, Warner J, Was M, Watchi J, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Wellmann F, Wen L, Wessel EK, Weßels P, Westhouse JW, Wette K, Whelan JT, Whiting BF, Whittle C, Wilken DM, Williams D, Williamson AR, Willis JL, Willke B, Winkler W, Wipf CC, Wittel H, Woan G, Woehler J, Wofford JK, Wright JL, Wu DS, Wysocki DM, Xiao S, Xu R, Yamamoto H, Yancey CC, Yang L, Yang Y, Yang Z, Yap MJ, Yazback M, Yeeles DW, Yu H, Yu H, Yuen SHR, Zadrożny AK, Zadrożny A, Zanolin M, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang T, Zhao C, Zhao G, Zhou M, Zhou Z, Zhu XJ, Zimmerman AB, Zucker ME, Zweizig J, and Shandera S
Abstract: We present a search for subsolar mass ultracompact objects in data obtained during Advanced LIGO's second observing run. In contrast to a previous search of Advanced LIGO data from the first observing run, this search includes the effects of component spin on the gravitational waveform. We identify no viable gravitational-wave candidates consistent with subsolar mass ultracompact binaries with at least one component between 0.2 M_{⊙}-1.0 M_{⊙}. We use the null result to constrain the binary merger rate of (0.2 M_{⊙}, 0.2 M_{⊙}) binaries to be less than 3.7×10^{5} Gpc^{-3} yr^{-1} and the binary merger rate of (1.0 M_{⊙}, 1.0 M_{⊙}) binaries to be less than 5.2×10^{3} Gpc^{-3} yr^{-1}. Subsolar mass ultracompact objects are not expected to form via known stellar evolution channels, though it has been suggested that primordial density fluctuations or particle dark matter with cooling mechanisms and/or nuclear interactions could form black holes with subsolar masses. Assuming a particular primordial black hole (PBH) formation model, we constrain a population of merging 0.2 M_{⊙} black holes to account for less than 16% of the dark matter density and a population of merging 1.0 M_{⊙} black holes to account for less than 2% of the dark matter density. We discuss how constraints on the merger rate and dark matter fraction may be extended to arbitrary black hole population models that predict subsolar mass binaries.
Published: 2019
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46. Measuring Spin of the Remnant Black Hole from Maximum Amplitude.

Author: Ferguson D, Ghonge S, Clark JA, Calderon Bustillo J, Laguna P, and Shoemaker D
Abstract: Gravitational waves emitted during the merger of two black holes carry information about the remnant black hole, namely its mass and spin. This information is typically found from the ringdown radiation as the black hole settles to a final state. We find that the remnant black hole spin is already known at the peak amplitude of the gravitational wave strain. Using this knowledge, we present a new method for measuring the final spin that is template independent, using only the chirp mass, the instantaneous frequency of the strain, and its derivative at maximum amplitude, all template independent.
Published: 2019
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47. Non-invasive in vivo hyperspectral imaging of the retina for potential biomarker use in Alzheimer's disease.

Author: Hadoux X, Hui F, Lim JKH, Masters CL, Pébay A, Chevalier S, Ha J, Loi S, Fowler CJ, Rowe C, Villemagne VL, Taylor EN, Fluke C, Soucy JP, Lesage F, Sylvestre JP, Rosa-Neto P, Mathotaarachchi S, Gauthier S, Nasreddine ZS, Arbour JD, Rhéaume MA, Beaulieu S, Dirani M, Nguyen CTO, Bui BV, Williamson R, Crowston JG, and van Wijngaarden P
Subjects: Aged, Alzheimer Disease metabolism, Amyloid beta-Peptides metabolism, Animals, Biomarkers metabolism, Brain diagnostic imaging, Brain metabolism, Cohort Studies, Female, Humans, Male, Mice, Mice, Inbred C57BL, Mice, Transgenic, Middle Aged, Positron-Emission Tomography, Retina metabolism, Alzheimer Disease diagnostic imaging, Amyloid beta-Peptides chemistry, Biomarkers chemistry, Retina diagnostic imaging, Tomography, Optical Coherence methods
Abstract: Studies of rodent models of Alzheimer's disease (AD) and of human tissues suggest that the retinal changes that occur in AD, including the accumulation of amyloid beta (Aβ), may serve as surrogate markers of brain Aβ levels. As Aβ has a wavelength-dependent effect on light scatter, we investigate the potential for in vivo retinal hyperspectral imaging to serve as a biomarker of brain Aβ. Significant differences in the retinal reflectance spectra are found between individuals with high Aβ burden on brain PET imaging and mild cognitive impairment (n = 15), and age-matched PET-negative controls (n = 20). Retinal imaging scores are correlated with brain Aβ loads. The findings are validated in an independent cohort, using a second hyperspectral camera. A similar spectral difference is found between control and 5xFAD transgenic mice that accumulate Aβ in the brain and retina. These findings indicate that retinal hyperspectral imaging may predict brain Aβ load.
Published: 2019
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48. Tests of General Relativity with GW170817.

Author: Abbott BP, Abbott R, Abbott TD, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari RX, Adya VB, Affeldt C, Agarwal B, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen B, Allen G, Allocca A, Aloy MA, Altin PA, Amato A, Ananyeva A, Anderson SB, Anderson WG, Angelova SV, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Arun KG, Ascenzi S, Ashton G, Ast M, Aston SM, Astone P, Atallah DV, Aubin F, Aufmuth P, Aulbert C, AultONeal K, Austin C, Avila-Alvarez A, Babak S, Bacon P, Badaracco F, Bader MKM, Bae S, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Banagiri S, Barayoga JC, Barclay SE, Barish BC, Barker D, Barkett K, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Batch JC, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Beer C, Bejger M, Belahcene I, Bell AS, Beniwal D, Bensch M, Berger BK, Bergmann G, Bernuzzi S, Bero JJ, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bilenko IA, Bilgili SA, Billingsley G, Billman CR, Birch J, Birney R, Birnholtz O, Biscans S, Biscoveanu S, Bisht A, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bloemen S, Bock O, Bode N, Boer M, Boetzel Y, Bogaert G, Bohe A, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Booth CD, Bork R, Boschi V, Bose S, Bossie K, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Briant T, Brighenti F, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DD, Brunett S, Buchanan CC, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Bustillo JC, Callister TA, Calloni E, Camp JB, Canepa M, Canizares P, Cannon KC, Cao H, Cao J, Capano CD, Capocasa E, Carbognani F, Caride S, Carney MF, Carullo G, Diaz JC, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cepeda CB, Cerdá-Durán P, Cerretani G, Cesarini E, Chaibi O, Chamberlin SJ, Chan M, Chao S, Charlton P, Chase E, Chassande-Mottin E, Chatterjee D, Chatziioannou K, Cheeseboro BD, Chen HY, Chen X, Chen Y, Cheng HP, Chia HY, Chincarini A, Chiummo A, Chmiel T, Cho HS, Cho M, Chow JH, Christensen N, Chu Q, Chua AJK, Chua S, Chung KW, Chung S, Ciani G, Ciobanu AA, Ciolfi R, Cipriano F, Cirelli CE, Cirone A, Clara F, Clark JA, Clearwater P, Cleva F, Cocchieri C, Coccia E, Cohadon PF, Cohen D, Colla A, Collette CG, Collins C, Cominsky LR, Constancio M, Conti L, Cooper SJ, Corban P, Corbitt TR, Cordero-Carrión I, Corley KR, Cornish N, Corsi A, Cortese S, Costa CA, Cotesta R, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Covas PB, Cowan EE, Coward DM, Cowart MJ, Coyne DC, Coyne R, Creighton JDE, Creighton TD, Cripe J, Crowder SG, Cullen TJ, Cumming A, Cunningham L, Cuoco E, Canton TD, Dálya G, Danilishin SL, D'Antonio S, Danzmann K, Dasgupta A, Costa CFDS, Dattilo V, Dave I, Davier M, Davis D, Daw EJ, Day B, DeBra D, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Del Pozzo W, Demos N, Denker T, Dent T, De Pietri R, Derby J, Dergachev V, De Rosa R, De Rossi C, DeSalvo R, de Varona O, Dhurandhar S, Díaz MC, Dietrich T, Di Fiore L, Di Giovanni M, Di Girolamo T, Di Lieto A, Ding B, Di Pace S, Di Palma I, Di Renzo F, Dmitriev A, Doctor Z, Dolique V, Donovan F, Dooley KL, Doravari S, Dorrington I, Álvarez MD, Downes TP, Drago M, Dreissigacker C, Driggers JC, Du Z, Dupej P, Dwyer SE, Easter PJ, Edo TB, Edwards MC, Effler A, Eggenstein HB, Ehrens P, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Essick RC, Estelles H, Estevez D, Etienne ZB, Etzel T, Evans M, Evans TM, Fafone V, Fair H, Fairhurst S, Fan X, Farinon S, Farr B, Farr WM, Fauchon-Jones EJ, Favata M, Fays M, Fee C, Fehrmann H, Feicht J, Fejer MM, Feng F, Fernandez-Galiana A, Ferrante I, Ferreira EC, Ferrini F, Fidecaro F, Fiori I, Fiorucci D, Fishbach M, Fisher RP, Fishner JM, Fitz-Axen M, Flaminio R, Fletcher M, Fong H, Font JA, Forsyth PWF, Forsyth SS, Fournier JD, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fritschel P, Frolov VV, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Gammaitoni L, Ganija MR, Gaonkar SG, Garcia A, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gaur G, Gayathri V, Gemme G, Genin E, Gennai A, George D, George J, Gergely L, Germain V, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Giacomazzo B, Giaime JA, Giardina KD, Giazotto A, Gill K, Giordano G, Glover L, Goetz E, Goetz R, Goncharov B, González G, Castro JMG, Gopakumar A, Gorodetsky ML, Gossan SE, Gosselin M, Gouaty R, Grado A, Graef C, Granata M, Grant A, Gras S, Gray C, Greco G, Green AC, Green R, Gretarsson EM, Groot P, Grote H, Grunewald S, Gruning P, Guidi GM, Gulati HK, Guo X, Gupta A, Gupta MK, Gushwa KE, Gustafson EK, Gustafson R, Halim O, Hall BR, Hall ED, Hamilton EZ, Hamilton HF, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hanson J, Hardwick T, Harms J, Harry GM, Harry IW, Hart MJ, Haster CJ, Haughian K, Healy J, Heidmann A, Heintze MC, Heitmann H, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heptonstall AW, Hernandez FJ, Heurs M, Hild S, Hinderer T, Hoak D, Hochheim S, Hofman D, Holland NA, Holt K, Holz DE, Hopkins P, Horst C, Hough J, Houston EA, Howell EJ, Hreibi A, Huerta EA, Huet D, Hughey B, Hulko M, Husa S, Huttner SH, Huynh-Dinh T, Iess A, Indik N, Ingram C, Inta R, Intini G, Isa HN, Isac JM, Isi M, Iyer BR, Izumi K, Jacqmin T, Jani K, Jaranowski P, Johnson DS, Johnson WW, Jones DI, Jones R, Jonker RJG, Ju L, Junker J, Kalaghatgi CV, Kalogera V, Kamai B, Kandhasamy S, Kang G, Kanner JB, Kapadia SJ, Karki S, Karvinen KS, Kasprzack M, Katolik M, Katsanevas S, Katsavounidis E, Katzman W, Kaufer S, Kawabe K, Keerthana NV, Kéfélian F, Keitel D, Kemball AJ, Kennedy R, Key JS, Khalili FY, Khamesra B, Khan H, Khan I, Khan S, Khan Z, Khazanov EA, Kijbunchoo N, Kim C, Kim JC, Kim K, Kim W, Kim WS, Kim YM, King EJ, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kleybolte L, Klimenko S, Knowles TD, Koch P, Koehlenbeck SM, Koley S, Kondrashov V, Kontos A, Korobko M, Korth WZ, Kowalska I, Kozak DB, Krämer C, Kringel V, Krishnan B, Królak A, Kuehn G, Kumar P, Kumar R, Kumar S, Kuo L, Kutynia A, Kwang S, Lackey BD, Lai KH, Landry M, Lang RN, Lange J, Lantz B, Lanza RK, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lee CH, Lee HK, Lee HM, Lee HW, Lee K, Lehmann J, Lenon A, Leonardi M, Leroy N, Letendre N, Levin Y, Li J, Li TGF, Li X, Linker SD, Littenberg TB, Liu J, Liu X, Lo RKL, Lockerbie NA, London LT, Longo A, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Lousto CO, Lovelace G, Lück H, Lumaca D, Lundgren AP, Lynch R, Ma Y, Macas R, Macfoy S, Machenschalk B, MacInnis M, Macleod DM, Hernandez IM, Magaña-Sandoval F, Zertuche LM, Magee RM, Majorana E, Maksimovic I, Man N, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Marchesoni F, Marion F, Márka S, Márka Z, Markakis C, 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Mullavey A, Munch J, Muñiz EA, Muratore M, Murray PG, Nagar A, Napier K, Nardecchia I, Naticchioni L, Nayak RK, Neilson J, Nelemans G, Nelson TJN, Nery M, Neunzert A, Nevin L, Newport JM, Ng KY, Ng S, Nguyen P, Nguyen TT, Nichols D, Nielsen AB, Nissanke S, Nitz A, Nocera F, Nolting D, North C, Nuttall LK, Obergaulinger M, Oberling J, O'Brien BD, O'Dea GD, Ogin GH, Oh JJ, Oh SH, Ohme F, Ohta H, Okada MA, Oliver M, Oppermann P, Oram RJ, O'Reilly B, Ormiston R, Ortega LF, O'Shaughnessy R, Ossokine S, Ottaway DJ, Overmier H, Owen BJ, Pace AE, Pagano G, Page J, Page MA, Pai A, Pai SA, Palamos JR, Palashov O, Palomba C, Pal-Singh A, Pan H, Pan HW, Pang B, Pang PTH, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Papa MA, Parida A, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patil M, Patricelli B, Pearlstone BL, Pedersen C, Pedraza M, Pedurand R, Pekowsky L, Pele A, Penn S, Perez CJ, Perreca A, Perri LM, Pfeiffer HP, Phelps M, Phukon KS, Piccinni OJ, Pichot M, 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Tanner DB, Tápai M, Taracchini A, Tasson JD, Taylor JA, Taylor R, Tewari SV, Theeg T, Thies F, Thomas EG, Thomas M, Thomas P, Thorne KA, Thrane E, Tiwari S, Tiwari V, Tokmakov KV, Toland K, Tonelli M, Tornasi Z, Torres-Forné A, Torrie CI, Töyrä D, Travasso F, Traylor G, Trinastic J, Tringali MC, Trozzo L, Tsang KW, Tse M, Tso R, Tsukada L, Tsuna D, Tuyenbayev D, Ueno K, Ugolini D, Urban AL, Usman SA, Vahlbruch H, Vajente G, Valdes G, van Bakel N, van Beuzekom M, van den Brand JFJ, Van Den Broeck C, Vander-Hyde DC, van der Schaaf L, van Heijningen JV, van Veggel AA, Vardaro M, Varma V, Vass S, Vasúth M, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Venugopalan G, Verkindt D, Vetrano F, Viceré A, Viets AD, Vinciguerra S, Vine DJ, Vinet JY, Vitale S, Vo T, Vocca H, Vorvick C, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walet R, Walker M, Wallace L, Walsh S, Wang G, Wang H, Wang JZ, Wang WH, Wang YF, Ward RL, Warner J, Was M, Watchi J, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Wellmann F, Wen L, Wessel EK, Weßels P, Westerweck J, Wette K, Whelan JT, Whiting BF, Whittle C, Wilken D, Williams D, Williams RD, Williamson AR, Willis JL, Willke B, Wimmer MH, Winkler W, Wipf CC, Wittel H, Woan G, Woehler J, Wofford JK, Wong WK, Worden J, Wright JL, Wu DS, Wysocki DM, Xiao S, Yam W, Yamamoto H, Yancey CC, Yang L, Yap MJ, Yazback M, Yu H, Yu H, Yvert M, Zadrożny A, Zanolin M, Zelenova T, Zendri JP, Zevin M, Zhang J, Zhang L, Zhang M, Zhang T, Zhang YH, Zhao C, Zhou M, Zhou Z, Zhu SJ, Zhu XJ, Zimmerman AB, Zucker ME, and Zweizig J
Abstract: The recent discovery by Advanced LIGO and Advanced Virgo of a gravitational wave signal from a binary neutron star inspiral has enabled tests of general relativity (GR) with this new type of source. This source, for the first time, permits tests of strong-field dynamics of compact binaries in the presence of matter. In this Letter, we place constraints on the dipole radiation and possible deviations from GR in the post-Newtonian coefficients that govern the inspiral regime. Bounds on modified dispersion of gravitational waves are obtained; in combination with information from the observed electromagnetic counterpart we can also constrain effects due to large extra dimensions. Finally, the polarization content of the gravitational wave signal is studied. The results of all tests performed here show good agreement with GR.
Published: 2019
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49. A laser walk-off sensor for high-precision low-frequency rotation measurements.

Author: McCann JJ, Winterflood J, Ju L, and Zhao C
Abstract: We present an optical walk-off sensor with an angular sensitivity of a few nrad/Hz above 1 mHz and 0.4 nrad/Hz above 100 mHz. This experiment furthers previous research into the walk-off sensor capabilities through an improved input laser, reduction in air optical travel length, and position control on photo-diodes. The angle change measured in this walk-off scheme features a knife edge to split the beam into two separate fiber coupled photo-diodes to minimize power dissipation in the thermally sensitive region. Using this photo-diode power differential as an error signal, a simple control scheme is used to maintain the balance position, increasing common mode rejection and improving dynamic range by mitigating thermal drift. The in-vacuum component of the optical readout takes up a volume less than 100 mm × 100 mm × 50 mm. This experiment shows that the walk-off sensor provides a simple and compact readout scheme with nanoradian sensitivity for angle sensing at low frequencies.
Published: 2019
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50. Constraining the p-Mode-g-Mode Tidal Instability with GW170817.

Author: Abbott BP, Abbott R, Abbott TD, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari RX, Adya VB, Affeldt C, Agarwal B, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen B, Allen G, Allocca A, Aloy MA, Altin PA, Amato A, Ananyeva A, Anderson SB, Anderson WG, Angelova SV, Antier S, Appert S, Arai K, Araya MC, Areeda JS, Arène M, Arnaud N, Arun KG, Ascenzi S, Ashton G, Ast M, Aston SM, Astone P, Atallah DV, Aubin F, Aufmuth P, Aulbert C, AultONeal K, Austin C, Avila-Alvarez A, Babak S, Bacon P, Badaracco F, Bader MKM, Bae S, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Banagiri S, Barayoga JC, Barclay SE, Barish BC, Barker D, Barkett K, Barnum S, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Bartlett J, Bartos I, Bassiri R, Basti A, Batch JC, Bawaj M, Bayley JC, Bazzan M, Bécsy B, Beer C, Bejger M, Belahcene I, Bell AS, Beniwal D, Bensch M, Berger BK, Bergmann G, Bernuzzi S, Bero JJ, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhandare R, Bilenko IA, Bilgili SA, Billingsley G, Billman CR, Birch J, Birney R, Birnholtz O, Biscans S, Biscoveanu S, Bisht A, Bitossi M, Bizouard MA, Blackburn JK, Blackman J, Blair CD, Blair DG, Blair RM, Bloemen S, Bock O, Bode N, Boer M, Boetzel Y, Bogaert G, Bohe A, Bondu F, Bonilla E, Bonnand R, Booker P, Boom BA, Booth CD, Bork R, Boschi V, Bose S, Bossie K, Bossilkov V, Bosveld J, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Bramley A, Branchesi M, Brau JE, Briant T, Brighenti F, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DD, Brunett S, Buchanan CC, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cabero M, Cadonati L, Cagnoli G, Cahillane C, Calderón Bustillo J, Callister TA, Calloni E, Camp JB, Canepa M, Canizares P, Cannon KC, Cao H, Cao J, Capano CD, Capocasa E, Carbognani F, Caride S, Carney MF, Casanueva Diaz J, Casentini C, Caudill S, Cavaglià M, Cavalier F, Cavalieri R, Cella G, Cepeda CB, Cerdá-Durán P, Cerretani G, 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D, Deenadayalan M, Degallaix J, De Laurentis M, Deléglise S, Del Pozzo W, Demos N, Denker T, Dent T, De Pietri R, Derby J, Dergachev V, De Rosa R, De Rossi C, DeSalvo R, de Varona O, Dhurandhar S, Díaz MC, Di Fiore L, Di Giovanni M, Di Girolamo T, Di Lieto A, Ding B, Di Pace S, Di Palma I, Di Renzo F, Dmitriev A, Doctor Z, Dolique V, Donovan F, Dooley KL, Doravari S, Dorrington I, Dovale Álvarez M, Downes TP, Drago M, Dreissigacker C, Driggers JC, Du Z, Dupej P, Dwyer SE, Easter PJ, Edo TB, Edwards MC, Effler A, Eggenstein HB, Ehrens P, Eichholz J, Eikenberry SS, Eisenmann M, Eisenstein RA, Essick RC, Estelles H, Estevez D, Etienne ZB, Etzel T, Evans M, Evans TM, Fafone V, Fair H, Fairhurst S, Fan X, Farinon S, Farr B, Farr WM, Fauchon-Jones EJ, Favata M, Fays M, Fee C, Fehrmann H, Feicht J, Fejer MM, Feng F, Fernandez-Galiana A, Ferrante I, Ferreira EC, Ferrini F, Fidecaro F, Fiori I, Fiorucci D, Fishbach M, Fisher RP, Fishner JM, Fitz-Axen M, Flaminio R, Fletcher M, Fong H, Font JA, Forsyth PWF, Forsyth SS, Fournier JD, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fritschel P, Frolov VV, Fulda P, Fyffe M, Gabbard HA, Gadre BU, Gaebel SM, Gair JR, Gammaitoni L, Ganija MR, Gaonkar SG, Garcia A, García-Quirós C, Garufi F, Gateley B, Gaudio S, Gaur G, Gayathri V, Gemme G, Genin E, Gennai A, George D, George J, Gergely L, Germain V, Ghonge S, Ghosh A, Ghosh A, Ghosh S, Giacomazzo B, Giaime JA, Giardina KD, Giazotto A, Gill K, Giordano G, Glover L, Goetz E, Goetz R, Goncharov B, González G, Gonzalez Castro JM, Gopakumar A, Gorodetsky ML, Gossan SE, Gosselin M, Gouaty R, Grado A, Graef C, Granata M, Grant A, Gras S, Gray C, Greco G, Green AC, Green R, Gretarsson EM, Groot P, Grote H, Grunewald S, Gruning P, Guidi GM, Gulati HK, Guo X, Gupta A, Gupta MK, Gushwa KE, Gustafson EK, Gustafson R, Halim O, Hall BR, Hall ED, Hamilton EZ, Hamilton HF, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hannuksela OA, Hanson J, Hardwick T, Harms J, Harry GM, Harry IW, Hart MJ, Haster CJ, Haughian K, Healy J, Heidmann A, Heintze MC, Heitmann H, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heptonstall AW, Hernandez FJ, Heurs M, Hild S, Hinderer T, Hoak D, Hochheim S, Hofman D, Holland NA, Holt K, Holz DE, Hopkins P, Horst C, Hough J, Houston EA, Howell EJ, Hreibi A, Huerta EA, Huet D, Hughey B, Hulko M, Husa S, Huttner SH, Huynh-Dinh T, Iess A, Indik N, Ingram C, Inta R, Intini G, Isa HN, Isac JM, Isi M, Iyer BR, Izumi K, Jacqmin T, Jani K, Jaranowski P, Johnson DS, Johnson WW, Jones DI, Jones R, Jonker RJG, Ju L, Junker J, Kalaghatgi CV, Kalogera V, Kamai B, Kandhasamy S, Kang G, Kanner JB, Kapadia SJ, Karki S, Karvinen KS, Kasprzack M, Katolik M, Katsanevas S, Katsavounidis E, Katzman W, Kaufer S, Kawabe K, Keerthana NV, Kéfélian F, Keitel D, Kemball AJ, Kennedy R, Key JS, Khalili FY, Khamesra B, Khan H, Khan I, Khan S, Khan Z, Khazanov EA, Kijbunchoo N, Kim C, Kim JC, Kim K, Kim W, Kim WS, Kim YM, King EJ, King PJ, Kinley-Hanlon M, Kirchhoff R, Kissel JS, Kleybolte L, Klimenko S, Knowles TD, Koch P, Koehlenbeck SM, Koley S, Kondrashov V, Kontos A, Korobko M, Korth WZ, Kowalska I, Kozak DB, Krämer C, Kringel V, Krishnan B, Królak A, Kuehn G, Kumar P, Kumar R, Kumar S, Kuo L, Kutynia A, Kwang S, Lackey BD, Lai KH, Landry M, Lang RN, Lange J, Lantz B, Lanza RK, Lartaux-Vollard A, Lasky PD, Laxen M, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lee CH, Lee HK, Lee HM, Lee HW, Lee K, Lehmann J, Lenon A, Leonardi M, Leroy N, Letendre N, Levin Y, Li J, Li TGF, Li X, Linker SD, Littenberg TB, Liu J, Liu X, Lo RKL, Lockerbie NA, London LT, Longo A, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Lovelace G, Lück H, Lumaca D, Lundgren AP, Lynch R, Ma Y, Macas R, Macfoy S, Machenschalk B, MacInnis M, Macleod DM, Magaña Hernandez I, Magaña-Sandoval F, Magaña Zertuche L, Magee RM, Majorana E, Maksimovic I, Man N, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Marchesoni F, Marion F, Márka S, Márka Z, Markakis C, Markosyan AS, Markowitz A, Maros E, Marquina A, Martelli F, Martellini L, Martin IW, Martin RM, Martynov DV, Mason K, Massera E, Masserot A, Massinger TJ, Masso-Reid M, Mastrogiovanni S, Matas A, Matichard F, Matone L, Mavalvala N, Mazumder N, McCann JJ, McCarthy R, McClelland DE, McCormick S, McCuller L, McGuire SC, McIver J, McManus DJ, McRae T, McWilliams ST, Meacher D, Meadors GD, Mehmet M, Meidam J, Mejuto-Villa E, Melatos A, Mendell G, Mendoza-Gandara D, Mercer RA, Mereni L, Merilh EL, Merzougui M, Meshkov S, Messenger C, Messick C, Metzdorff R, Meyers PM, Miao H, Michel C, Middleton H, Mikhailov EE, Milano L, Miller AL, Miller A, Miller BB, Miller J, Millhouse M, Mills J, Milovich-Goff MC, Minazzoli O, Minenkov Y, Ming J, Mishra C, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Moffa D, Mogushi K, Mohan M, Mohapatra SRP, Montani M, Moore CJ, Moraru D, Moreno G, Morisaki S, Mours B, Mow-Lowry CM, Mueller G, Muir AW, Mukherjee A, Mukherjee D, Mukherjee S, Mukund N, 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Abstract: We analyze the impact of a proposed tidal instability coupling p modes and g modes within neutron stars on GW170817. This nonresonant instability transfers energy from the orbit of the binary to internal modes of the stars, accelerating the gravitational-wave driven inspiral. We model the impact of this instability on the phasing of the gravitational wave signal using three parameters per star: an overall amplitude, a saturation frequency, and a spectral index. Incorporating these additional parameters, we compute the Bayes factor (lnB_{!pg}^{pg}) comparing our p-g model to a standard one. We find that the observed signal is consistent with waveform models that neglect p-g effects, with lnB_{!pg}^{pg}=0.03_{-0.58}^{+0.70} (maximum a posteriori and 90% credible region). By injecting simulated signals that do not include p-g effects and recovering them with the p-g model, we show that there is a ≃50% probability of obtaining similar lnB_{!pg}^{pg} even when p-g effects are absent. We find that the p-g amplitude for 1.4 M_{⊙} neutron stars is constrained to less than a few tenths of the theoretical maximum, with maxima a posteriori near one-tenth this maximum and p-g saturation frequency ∼70 Hz. This suggests that there are less than a few hundred excited modes, assuming they all saturate by wave breaking. For comparison, theoretical upper bounds suggest ≲10^{3} modes saturate by wave breaking. Thus, the measured constraints only rule out extreme values of the p-g parameters. They also imply that the instability dissipates ≲10^{51} erg over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves.
Published: 2019
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