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1. Comutations and KRASG12C Inhibitor Efficacy in Advanced NSCLC.

Author

Negrao, Marcelo, Negrao, Marcelo, Araujo, Haniel, Lamberti, Giuseppe, Cooper, Alissa, Akhave, Neal, Zhou, Teng, Delasos, Lukas, Hicks, J, Aldea, Mihaela, Minuti, Gabriele, Hines, Jacobi, Aredo, Jacqueline, Dennis, Michael, Scott, Susan, Bironzo, Paolo, Scheffler, Matthias, Christopoulos, Petros, Stenzinger, Albrecht, Riess, Jonathan, Kim, So, Goldberg, Sarah, Li, Mingjia, Wang, Qi, Qing, Yun, Ni, Ying, Do, Minh, Lee, Richard, Ricciuti, Biagio, Alessi, Joao, Wang, Jing, Resuli, Blerina, Landi, Lorenza, Tseng, Shu-Chi, Nishino, Mizuki, Digumarthy, Subba, Rinsurongkawong, Waree, Rinsurongkawong, Vadeerat, Vaporciyan, Ara, Blumenschein, George, Zhang, Jianjun, Owen, Dwight, Mountzios, Giannis, Shu, Catherine, Bestvina, Christine, Garassino, Marina, Marrone, Kristen, Gray, Jhanelle, Patel, Sandip, Cummings, Amy, Wakelee, Heather, Wolf, Juergen, Scagliotti, Giorgio, Cappuzzo, Federico, Barlesi, Fabrice, Patil, Pradnya, Drusbosky, Leylah, Gibbons, Don, Meric-Bernstam, Funda, Lee, J, Heymach, John, Hong, David, Heist, Rebecca, Awad, Mark, Skoulidis, Ferdinandos, Blakely, Collin, Chakrabarti, Turja, Negrao, Marcelo, Negrao, Marcelo, Araujo, Haniel, Lamberti, Giuseppe, Cooper, Alissa, Akhave, Neal, Zhou, Teng, Delasos, Lukas, Hicks, J, Aldea, Mihaela, Minuti, Gabriele, Hines, Jacobi, Aredo, Jacqueline, Dennis, Michael, Scott, Susan, Bironzo, Paolo, Scheffler, Matthias, Christopoulos, Petros, Stenzinger, Albrecht, Riess, Jonathan, Kim, So, Goldberg, Sarah, Li, Mingjia, Wang, Qi, Qing, Yun, Ni, Ying, Do, Minh, Lee, Richard, Ricciuti, Biagio, Alessi, Joao, Wang, Jing, Resuli, Blerina, Landi, Lorenza, Tseng, Shu-Chi, Nishino, Mizuki, Digumarthy, Subba, Rinsurongkawong, Waree, Rinsurongkawong, Vadeerat, Vaporciyan, Ara, Blumenschein, George, Zhang, Jianjun, Owen, Dwight, Mountzios, Giannis, Shu, Catherine, Bestvina, Christine, Garassino, Marina, Marrone, Kristen, Gray, Jhanelle, Patel, Sandip, Cummings, Amy, Wakelee, Heather, Wolf, Juergen, Scagliotti, Giorgio, Cappuzzo, Federico, Barlesi, Fabrice, Patil, Pradnya, Drusbosky, Leylah, Gibbons, Don, Meric-Bernstam, Funda, Lee, J, Heymach, John, Hong, David, Heist, Rebecca, Awad, Mark, Skoulidis, Ferdinandos, Blakely, Collin, and Chakrabarti, Turja

Abstract

UNLABELLED: Molecular modifiers of KRASG12C inhibitor (KRASG12Ci) efficacy in advanced KRASG12C-mutant NSCLC are poorly defined. In a large unbiased clinicogenomic analysis of 424 patients with non-small cell lung cancer (NSCLC), we identified and validated coalterations in KEAP1, SMARCA4, and CDKN2A as major independent determinants of inferior clinical outcomes with KRASG12Ci monotherapy. Collectively, comutations in these three tumor suppressor genes segregated patients into distinct prognostic subgroups and captured ∼50% of those with early disease progression (progression-free survival ≤3 months) with KRASG12Ci. Pathway-level integration of less prevalent coalterations in functionally related genes nominated PI3K/AKT/MTOR pathway and additional baseline RAS gene alterations, including amplifications, as candidate drivers of inferior outcomes with KRASG12Ci, and revealed a possible association between defective DNA damage response/repair and improved KRASG12Ci efficacy. Our findings propose a framework for patient stratification and clinical outcome prediction in KRASG12C-mutant NSCLC that can inform rational selection and appropriate tailoring of emerging combination therapies. SIGNIFICANCE: In this work, we identify co-occurring genomic alterations in KEAP1, SMARCA4, and CDKN2A as independent determinants of poor clinical outcomes with KRASG12Ci monotherapy in advanced NSCLC, and we propose a framework for patient stratification and treatment personalization based on the comutational status of individual tumors. See related commentary by Heng et al., p. 1513. This article is highlighted in the In This Issue feature, p. 1501.

Published
2023

2. Methods and prospects for gravitational wave searches targeting ultralight vector boson clouds around known black holes

Author

Jones, Dana, Sun, Ling, Siemonsen, Nils, East, William E., Scott, Susan M., Wette, Karl, Jones, Dana, Sun, Ling, Siemonsen, Nils, East, William E., Scott, Susan M., and Wette, Karl

Abstract

Ultralight bosons are predicted in many extensions to the Standard Model and are popular dark matter candidates. The black hole superradiance mechanism allows for these particles to be probed using only their gravitational interaction. In this scenario, an ultralight boson cloud may form spontaneously around a spinning black hole and extract a non-negligible fraction of the black hole's mass. These oscillating clouds produce quasi-monochromatic, long-duration gravitational waves that may be detectable by ground-based or space-based gravitational wave detectors. We discuss the capability of a new long-duration signal tracking method, based on a hidden Markov model, to detect gravitational wave signals generated by ultralight vector boson clouds, including cases where the signal frequency evolution timescale is much shorter than that of a typical continuous wave signal. We quantify the detection horizon distances for vector boson clouds with current- and next-generation ground-based detectors. We demonstrate that vector clouds hosted by black holes with mass $\gtrsim 60 M_{\odot}$ and spin $\gtrsim 0.6$ are within the reach of current-generation detectors up to a luminosity distance of $\sim 1$ Gpc. This search method enables one to target vector boson clouds around remnant black holes from compact binary mergers detected by gravitational-wave detectors. We discuss the impact of the sky localization of the merger events and demonstrate that a typical remnant black hole reasonably well-localized by the current generation detector network is accessible in a follow-up search., Comment: 21 pages, 12 figures

Published
2023

3. Developing and implementing an Einsteinian science curriculum from Years 3 to 10:Part B: Teacher upskilling: response to training and teacher's classroom experience

Author

Kaur, Tejinder, Kersting, Magdalena, Adams, Kyla, Blair, David G., Treagust, David, Popkova, Anastasia, Boublil, Shon, Santoso, Jesse, Ju, Li, Zadnik, Marjan, Wood, David, Horne, Elaine, McGoran, Darren, Scott, Susan, Venville, Grady, Kaur, Tejinder, Kersting, Magdalena, Adams, Kyla, Blair, David G., Treagust, David, Popkova, Anastasia, Boublil, Shon, Santoso, Jesse, Ju, Li, Zadnik, Marjan, Wood, David, Horne, Elaine, McGoran, Darren, Scott, Susan, and Venville, Grady

Abstract

Recent years have seen a growing interest in modernizing physics and science curricula around the world. While many science educators and curriculum developers design instructional resources to successfully introduce topics of Einsteinian physics to young learners, it is clear that successful curriculum development needs to rest on successful teacher professional development.Teachers with or without science backgrounds were trained in short professional learning workshops or completed micro-credential courses. The courses enabled teachers to gain knowledge and confidence to deliver the Einstein-First program. Detailed lesson plans and instructional videos for teachers define the lessons. Questionnaires were used to collect data, and teacher interviews were conducted following the various teacher training programs. The research results show that teachers effectively deliver the Einsteinian physics programs and that their subject matter and pedagogical content knowledge increased. In addition, teacher attitudes were favorable towards modernizing the physics curriculum. We conclude that it is feasible to upskill teachers from diverse backgrounds in Einsteinian physics and break the cycle that has inhibited the modernization of school curricula.

Published
2023

4. Piecewise frequency model for searches for long-transient gravitational waves from young neutron stars

Author

Grace, Benjamin, Wette, Karl, Scott, Susan M., Sun, Ling, Grace, Benjamin, Wette, Karl, Scott, Susan M., and Sun, Ling

Abstract

In this work we characterise the performance of a new search technique designed to be sensitive to the remnants of binary neutron star systems. Sensitivity estimates of the new method on simulated data are competitive against those of other work. Previous searches for a gravitational-wave signal from a possible neutron star remnant of the binary neutron star merger event GW170817 have focused on short ($<500$~s) and long duration (2.5~hr -- 8~day) signals. To date, no such post-merger signal has been detected. We introduce a new piecewise model which has the flexibility to accurately follow gravitational-wave signals which are rapidly evolving in frequency, such as those which may be emitted from young neutron stars born from binary neutron star mergers or supernovae. We investigate the sensitivity and computational cost of this piecewise model when used in a fully coherent 1800-second $\mathcal{F}$-statistic search on simulated data containing possible signals from the GW170817 remnant. The sensitivity of the search using the piecewise model is determined using simulated data, with noise consistent with the LIGO second observing run. Across a 100--2000~Hz frequency band, the model achieves a peak sensitivity of $h_{\text{rss}}^{50\%} = 4.4 \times 10^{-23} \text{Hz}^{-1/2}$ at 200~Hz, competitive with other methods. The computational cost of conducting the search, over a bank of $1.1 \times 10^{12}$ templates, is estimated at 10 days running on 100 CPU's., Comment: 16 pages, 11 figures, 2 tables

Published
2023
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5. What are neutron stars made of? Gravitational waves may reveal the answer

Author

Lu, Neil, Scott, Susan M., Wette, Karl, Lu, Neil, Scott, Susan M., and Wette, Karl

Abstract

Neutron stars are one of the most mysterious wonders in the Universe. Their extreme densities hint at new and exotic physics at work within. Gravitational waves could be the key to unlocking their secrets. In particular, a first detection of gravitational waves from rapidly-spinning, deformed neutron stars could yield new insights into the physics of matter at extreme densities and under strong gravity. Once a first detection is made, a critical challenge will be to robustly extract physically interesting information from the detected signals. In this essay, we describe initial research towards answering this challenge, and thereby unleashing the full power of gravitational waves as an engine for the discovery of new physics., Comment: 14 pages, 2 figures. This essay was awarded 5th Place in the Gravity Research Foundation 2023 Awards for Essays on Gravitation. To appear in International Journal of Modern Physics D

Published
2023
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6. Methods and prospects for gravitational wave searches targeting ultralight vector boson clouds around known black holes

Author

Jones, Dana, Sun, Ling, Siemonsen, Nils, East, William E., Scott, Susan M., Wette, Karl, Jones, Dana, Sun, Ling, Siemonsen, Nils, East, William E., Scott, Susan M., and Wette, Karl

Abstract

Ultralight bosons are predicted in many extensions to the Standard Model and are popular dark matter candidates. The black hole superradiance mechanism allows for these particles to be probed using only their gravitational interaction. In this scenario, an ultralight boson cloud may form spontaneously around a spinning black hole and extract a non-negligible fraction of the black hole's mass. These oscillating clouds produce quasi-monochromatic, long-duration gravitational waves that may be detectable by ground-based or space-based gravitational wave detectors. We discuss the capability of a new long-duration signal tracking method, based on a hidden Markov model, to detect gravitational wave signals generated by ultralight vector boson clouds, including cases where the signal frequency evolution timescale is much shorter than that of a typical continuous wave signal. We quantify the detection horizon distances for vector boson clouds with current- and next-generation ground-based detectors. We demonstrate that vector clouds hosted by black holes with mass $\gtrsim 60 M_{\odot}$ and spin $\gtrsim 0.6$ are within the reach of current-generation detectors up to a luminosity distance of $\sim 1$ Gpc. This search method enables one to target vector boson clouds around remnant black holes from compact binary mergers detected by gravitational-wave detectors. We discuss the impact of the sky localization of the merger events and demonstrate that a typical remnant black hole reasonably well-localized by the current generation detector network is accessible in a follow-up search., Comment: 21 pages, 12 figures

Published
2023
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7. Developing and implementing an Einsteinian science curriculum from Years 3 to 10:Part B: Teacher upskilling: response to training and teacher's classroom experience

Author

Kaur, Tejinder, Kersting, Magdalena, Adams, Kyla, Blair, David G., Treagust, David, Popkova, Anastasia, Boublil, Shon, Santoso, Jesse, Ju, Li, Zadnik, Marjan, Wood, David, Horne, Elaine, McGoran, Darren, Scott, Susan, Venville, Grady, Kaur, Tejinder, Kersting, Magdalena, Adams, Kyla, Blair, David G., Treagust, David, Popkova, Anastasia, Boublil, Shon, Santoso, Jesse, Ju, Li, Zadnik, Marjan, Wood, David, Horne, Elaine, McGoran, Darren, Scott, Susan, and Venville, Grady

Abstract

Recent years have seen a growing interest in modernizing physics and science curricula around the world. While many science educators and curriculum developers design instructional resources to successfully introduce topics of Einsteinian physics to young learners, it is clear that successful curriculum development needs to rest on successful teacher professional development.Teachers with or without science backgrounds were trained in short professional learning workshops or completed micro-credential courses. The courses enabled teachers to gain knowledge and confidence to deliver the Einstein-First program. Detailed lesson plans and instructional videos for teachers define the lessons. Questionnaires were used to collect data, and teacher interviews were conducted following the various teacher training programs. The research results show that teachers effectively deliver the Einsteinian physics programs and that their subject matter and pedagogical content knowledge increased. In addition, teacher attitudes were favorable towards modernizing the physics curriculum. We conclude that it is feasible to upskill teachers from diverse backgrounds in Einsteinian physics and break the cycle that has inhibited the modernization of school curricula.

Published
2023

8. Liminal innovation in practice: Understanding the reconfiguration of digital work in crisis

Author

Sloan School of Management, Orlikowski, Wanda J, Scott, Susan V, Sloan School of Management, Orlikowski, Wanda J, and Scott, Susan V

Abstract

© 2021 Elsevier Ltd As conditions of crisis disrupt established practices, existing ways of doing things are interrupted and called into question. The suspension of routine sociomaterial enactments produces openings for liminal innovation, a process entailing iterative experimentation and implementation that explores novel or alternative materializations of established work practices. We draw attention to three distinct tensions on the ground that arise in conditions of crisis — pragmatic, tactical, and existential — and show how these may be leveraged to produce liminal innovations in practice. While the process of liminal innovation can be challenging, it can also be generative, creating opportunities for the reconfiguration of digital work in conditions of crisis.

Published
2022

9. The Digital Undertow: How the Corollary Effects of Digital Transformation Affect Industry Standards

Author

Sloan School of Management, Scott, Susan, Orlikowski, Wanda, Sloan School of Management, Scott, Susan, and Orlikowski, Wanda

Abstract

Digital transformation research shows how waves of digitalization produce strategic changes within and across firms, enabling new forms of value creation. We argue that different but no less important processes of digital transformation are generated by the undertow produced by these waves. Digital undertow, a corollary effect of waves of digitalization, profoundly influences how firms operate by transforming the industry standards that coordinate and regulate their core business activities. This is producing what we refer to as digital displacement, a process that is significantly challenging the capacity of standards to effectively manage industry operations in the digital age.

Published
2022

10. Crowd-Based Accountability: Examining How Social Media Commentary Reconfigures Organizational Accountability

Author

Sloan School of Management, Karunakaran, Arvind, Orlikowski, Wanda J, Scott, Susan V, Sloan School of Management, Karunakaran, Arvind, Orlikowski, Wanda J, and Scott, Susan V

Abstract

Organizational accountability is considered critical to organizations’ sustained performance and survival. Prior research examines the structural and rhetorical responses that organizations use to manage accountability pressures from different constituents. With the emergence of social media, accountability pressures shift from the relatively clear and well-specified demands of identifiable stakeholders to the unclear and unspecified concerns of a pseudonymous crowd. This is further exacerbated by the public visibility of social media, materializing as a stream of online commentary for a distributed audience. In such conditions, the established structural and rhetorical responses of organizations become less effective for addressing accountability pressures. We conducted a multisite comparative study to examine how organizations in two service sectors (emergency response and hospitality) respond to accountability pressures manifesting as social media commentary on two platforms (Twitter and TripAdvisor). We find organizations responding online to social media commentary while also enacting changes to their practices that recalibrate risk, redeploy resources, and redefine service. These changes produce a diffractive reactivity that reconfigures the meanings, activities, relations, and outcomes of service work as well as the boundaries of organizational accountability. We synthesize these findings in a model of crowd-based accountability and discuss the contributions of this study to research on accountability and organizing in the social media era.

Published
2022

11. SkyMapper Optical Follow-up of Gravitational Wave Triggers: Alert Science Data Pipeline and LIGO/Virgo O3 Run

Author

Chang, Seo-Won, Onken, Christopher A., Wolf, Christian, Luvaul, Lance, Möller, Anais, Scalzo, Richard, Schmidt, Brian P., Scott, Susan M., Sura, Nikunj, Yuan, Fang, Chang, Seo-Won, Onken, Christopher A., Wolf, Christian, Luvaul, Lance, Möller, Anais, Scalzo, Richard, Schmidt, Brian P., Scott, Susan M., Sura, Nikunj, and Yuan, Fang

Abstract

We present an overview of the SkyMapper optical follow-up program for gravitational-wave event triggers from the LIGO/Virgo observatories, which aims at identifying early GW170817-like kilonovae out to $\sim 200$ Mpc distance. We describe our robotic facility for rapid transient follow-up, which can target most of the sky at $\delta<+10\deg $ to a depth of $i_\mathrm{AB}\approx 20$ mag. We have implemented a new software pipeline to receive LIGO/Virgo alerts, schedule observations and examine the incoming real-time data stream for transient candidates. We adopt a real-bogus classifier using ensemble-based machine learning techniques, attaining high completeness ($\sim$98%) and purity ($\sim$91%) over our whole magnitude range. Applying further filtering to remove common image artefacts and known sources of transients, such as asteroids and variable stars, reduces the number of candidates by a factor of more than 10. We demonstrate the system performance with data obtained for GW190425, a binary neutron star merger detected during the LIGO/Virgo O3 observing campaign. In time for the LIGO/Virgo O4 run, we will have deeper reference images allowing transient detection to $i_\mathrm{AB}\approx $21 mag., Comment: 13 pages, 6 figures, Accepted for publication in PASA

Published
2021
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12. Targeted Treatment of Non-Small Cell Lung Cancer: Focus on Capmatinib with Companion Diagnostics

Author

Guo,Matthew Z, Marrone,Kristen A, Spira,Alexander, Waterhouse,David M, Scott,Susan C, Guo,Matthew Z, Marrone,Kristen A, Spira,Alexander, Waterhouse,David M, and Scott,Susan C

Abstract

Matthew Z Guo,1 Kristen A Marrone,1 Alexander Spira,1– 3 David M Waterhouse,3,4 Susan C Scott1 1Johns Hopkins University School of Medicine, Sidney Kimmel Comprehensive Cancer Center, Baltimore, MD, USA; 2Virginia Cancer Specialists Research Institute, Fairfax, VA, USA; 3US Oncology, The Woodlands, TX, USA; 4Oncology Hematology Care, Cincinnati, OH, UsaCorrespondence: Susan C ScottJohns Hopkins University School of Medicine, Sidney Kimmel Comprehensive Cancer Center, 201 N Broadway, Baltimore, MD, 21287, USATel +1410-955-8893Fax +1410-367-2194Email sscott89@jhmi.eduAbstract: MET dysregulation promoting tumorigenesis in non-small cell lung cancer (NSCLC) is associated with worse outcomes following chemotherapy as compared to non-driver mutated NSCLC and occurs either through mutations causing MET exon 14 skipping (METex14) or gene amplification and overexpression that result in enhanced receptor signaling. Capmatinib is the first FDA-approved targeted therapy for NSCLC with METex14 skipping mutations, approved in 2020. FoundationOne® CDx, a comprehensive genomic profiling test for solid tumors, was concurrently approved as a companion diagnostic for capmatinib use. The GEOMETRY mono-1 phase II trial of capmatinib monotherapy demonstrated an overall response rate (ORR) of 68% in treatment naïve (n=28) and 41% in pre-treated (n=69) METex14 skipping advanced NSCLC; in MET amplified advanced NSCLC (gene copy number ≥ 10) ORRs of 40% in treatment naïve and 29% in pre-treated disease was seen. This review outlines the clinical data supporting capmatinib approval in the treatment of NSCLC and FoundationOne® CDx approval as a companion diagnostic. We detail the practical clinical administration of capmatinib, including dosing and toxicity management, compare capmatinib to other approved and investigational MET-targeted therapies, discuss limitations of capmatinib, and highlight ongoing trials of capmatinib in combinatorial approaches.Keywords: capmatinib, MET exon 14

Published
2021

13. GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object

Author

Abbott, R., Abbott, T. D., Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adhikari, Rana X, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Toyra, Daniel, Wade, Andrew, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, R., Abbott, T. D., Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adhikari, Rana X, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Toyra, Daniel, Wade, Andrew, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We report the observation of a compact binary coalescence involving a 22.2–24.3 Me black hole and a compact object with a mass of 2.50–2.67 Me (all measurements quoted at the 90% credible level). The gravitational-wave signal, GW190814, was observed during LIGO’s and Virgo’s third observing run on 2019 August 14 at 21:10:39 UTC and has a signal-to-noise ratio of 25 in the three-detector network. The source was localized to 18.5 deg2 at a distance of - + 241 45 41 Mpc; no electromagnetic counterpart has been confirmed to date. The source has the most unequal mass ratio yet measured with gravitational waves, - + 0.112 0.009 0.008, and its secondary component is either the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system. The dimensionless spin of the primary black hole is tightly constrained to 0.07. Tests of general relativity reveal no measurable deviations from the theory, and its prediction of higher-multipole emission is confirmed at high confidence. We estimate a merger rate density of 1–23 Gpc−3 yr−1 for the new class of binary coalescence sources that GW190814 represents. Astrophysical models predict that binaries with mass ratios similar to this event can form through several channels, but are unlikely to have formed in globular clusters. However, the combination of mass ratio, component masses, and the inferred merger rate for this event challenges all current models of the formation and mass distribution of compact-object binaries.

Published
2020

14. GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Author

Abbott, R., Abbott, T. D., Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, Rana X, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Toyra, Daniel, Wade, Andrew, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, R., Abbott, T. D., Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, Rana X, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Toyra, Daniel, Wade, Andrew, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ~ 30Mo black hole merged with a ~ 8Mo black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein's general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs.

Published
2020

15. Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adya, Vaishali, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Grace, Benjamin, Holland, Nathan, Kijbunchoo, Nutsinee, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. The sources with neutrino-driven explosions are detectable at the distances approaching 5 kpc, and for magnetorotationally driven explosions the distances are up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes, we constrained the gravitational-wave energy emitted during core collapse at the levels of 4.27×10⁻⁴ M⊙c2 and 1.28×10⁻¹ M⊙c² for emissions at 235 and 1304 Hz, respectively. These constraints are 2 orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo, and GEO 600 data.

Published
2020

16. The long-term effect of digital innovation on bank performance: An empirical study of SWIFT adoption in financial services

Author

Sloan School of Management, Massachusetts Institute of Technology. Department of Economics, Scott, Susan V., Van Reenen, John Michael, Zachariadis, Markos, Sloan School of Management, Massachusetts Institute of Technology. Department of Economics, Scott, Susan V., Van Reenen, John Michael, and Zachariadis, Markos

Abstract

We examine the impact on bank performance of the adoption of SWIFT, a network-based technological infrastructure and set of standards for worldwide interbank telecommunication. We construct a new longitudinal dataset of 6848 banks in 29 countries in Europe and the Americas with the full history of adoption since SWIFT's initial operations in 1977. Our results suggest that the adoption of SWIFT (i) has large effects on profitability in the long-term; (ii) these profitability effects are greater for small than for large banks; and (iii) exhibits significant network effects on performance. We use an in-depth field study to better understand the mechanisms underlying the effects on profitability.

Published
2020

17. Ground-Based Gravitational-Wave Astronomy in Australia: 2019 White Paper

Author

Bailes, Matthew, McClelland, David, Thrane, Eric, Blair, David, Cooke, Jeffrey, Coward, David, Evans, Robin, Fenner, Yeshe, Galloway, Duncan, Hurley, Jarrod, Ju, Li, Lasky, Paul, Mandel, Ilya, McKenzie, Kirk, Melatos, Andrew, Ottaway, David, Scott, Susan, Slagmolen, Bram, Veitch, Peter, Wen, Linqing, Zhao, Chunnong, Bailes, Matthew, McClelland, David, Thrane, Eric, Blair, David, Cooke, Jeffrey, Coward, David, Evans, Robin, Fenner, Yeshe, Galloway, Duncan, Hurley, Jarrod, Ju, Li, Lasky, Paul, Mandel, Ilya, McKenzie, Kirk, Melatos, Andrew, Ottaway, David, Scott, Susan, Slagmolen, Bram, Veitch, Peter, Wen, Linqing, and Zhao, Chunnong

Abstract

The past four years have seen a scientific revolution through the birth of a new field: gravitational-wave astronomy. The first detection of gravitational waves---recognised by the 2017 Nobel Prize in Physics---provided unprecedented tests of general relativity while unveiling a previously unknown class of massive black holes, thirty times more massive than the Sun. The subsequent detection of gravitational waves from a merging binary neutron star confirmed the hypothesised connection between binary neutron stars and short gamma-ray bursts while providing an independent measurement of the expansion of the Universe. The discovery enabled precision measurement of the speed of gravity while shedding light on the origin of heavy elements. At the time of writing, the Laser Interferometer Gravitational-wave Observatory (LIGO) and its European partner, Virgo, have published the detection of eleven gravitational-wave events. New, not-yet-published detections are announced on a nearly weekly basis. This fast-growing catalogue of gravitational-wave transients is expected to yield insights into a number of topics, from the equation of state of matter at supra-nuclear densities to the fate of massive stars. The science potential of 3G observatories is enormous, enabling measurements of gravitational waves from the edge of the Universe and precise determination of the neutron star equation of state. Australia is well-positioned to help develop the required technology. The Mid-term Review for the Decadal plan for Australian astronomy 2016-2025 should consider investment in a scoping study for an Australian Gravitational-Wave Pathfinder that develops and validates core technologies required for the global 3G detector network., Comment: 8 pages, 7 figures

Published
2019

18. A contemporary, nationwide analysis of surgery and radiotherapy treatment for prostate cancer

Author

Roberts, Matthew J., Papa, Nathan, Perera, Marlon, Scott, Susan, Teloken, Patrick E., Joshi, Andre, Vela, Ian, Pryor, David, Martin, Jarad, Woo, Henry, Roberts, Matthew J., Papa, Nathan, Perera, Marlon, Scott, Susan, Teloken, Patrick E., Joshi, Andre, Vela, Ian, Pryor, David, Martin, Jarad, and Woo, Henry

Abstract

Objective: To characterize national clinical practice trends in the treatment of prostate cancer (PCa) in Australia. Patients and Methods: Population-level data were extracted from existing Medicare Benefits Schedule data for radical prostatectomy (RP) and brachytherapy (2002–2016), as well as external beam radiotherapy (EBRT; 2012–2016). Treatment rates were calculated relative to whole and PCa populations among privately treated patients. Overall age-related and geographical trends were analysed. Results: The use of RP and low-dose-rate (LDR) brachytherapy increased between 2002 and 2009, but subsequently decreased to 124 and 6.9 per 100 000 men, respectively, in 2016. More dramatic decreases were observed for men aged <65 years. From 2012, rates of RP (15% drop) and LDR brachytherapy (58% drop) decreased, while the use of EBRT remained steady, falling by 5% to 42 per 100 000 men in 2016. Overall treatment increased in the age group 75–84 years, with the rate of RP increasing by 108%. Conclusion: National claims data indicate there has been a reduction in PCa treatment since 2009, which is mostly attributable to a reduction in the treatment of younger patients and reduced use of brachytherapy. RP is most commonly used and its use is rising in men aged >65 years.Special Issue: Urological Society of Australia and New Zealand

Published
2019

19. Searches for Continuous Gravitational Waves from 15 Supernova Remnants and Fomalhaut b with Advanced LIGO

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We describe directed searches for continuous gravitational waves (GWs) from 16 well-localized candidate neutron stars, assuming none of the stars has a binary companion. The searches were directed toward 15 supernova remnants and Fomalhaut b, a directly imaged extrasolar planet candidate that has been suggested to be a nearby old neutron star. Each search covered a broad band of frequencies and first and second time derivatives. After coherently integrating spans of data from the first Advanced LIGO observing run of 3.5–53.7 days per search, applying data-based vetoes, and discounting known instrumental artifacts, we found no astrophysical signals. We set upper limits on intrinsic GW strain as strict as 1 × 10−25, fiducial neutron star ellipticity as strict as 2 × 10−9, and fiducial r-mode amplitude as strict as 3 × 10−8.

Published
2019

20. Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, Benjamin P., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.

Published
2019

21. Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data

Author

Abbott, Benjamin P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, Fausto, Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, Fausto, Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We present a search for gravitational waves from 222 pulsars with rotation frequencies gsim10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015–2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711−6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 1038 kg m2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2 × 10−8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars.

Published
2019

22. Tests of General Relativity with GW170817

Author

Abbott, Benjamin P., Abbott, R., Abbott, T. D., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thien, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, R., Abbott, T. D., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thien, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

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

23. Search for Multimessenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during Its First Observing Run, ANTARES, and IceCube

Author

Albert, A., Andre, M., Anghinolfi, M., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Ardid, M., Aubert, J. J., Aublin, J., Avgitas, T., Baret, B., Bourret, S., Bouwhuis, M. C., Albert, A., Andre, M., Anghinolfi, M., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Ardid, M., Aubert, J. J., Aublin, J., Avgitas, T., Baret, B., Bourret, S., and Bouwhuis, M. C.

Abstract

Astrophysical sources of gravitational waves, such as binary neutron star and black hole mergers or core-collapse supernovae, can drive relativistic outflows, giving rise to non-thermal high-energy emission. High-energy neutrinos are signatures of such outflows. The detection of gravitational waves and high-energy neutrinos from common sources could help establish the connection between the dynamics of the progenitor and the properties of the outflow. We searched for associated emission of gravitational waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the Antares and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origins could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational-wave and neutrino emission processes.

Published
2019

24. Search for Transient Gravitational-wave Signals Associated with Magnetar Bursts during Advanced LIGO's Second Observing Run

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana, Adya, V., Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana, Adya, V., Affeldt, C., Altin, Paul, Forsyth, Perry, Holland, Nathan, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

We present the results of a search for short- and intermediate-duration gravitational-wave signals from four magnetar bursts in Advanced LIGO's second observing run. We find no evidence of a signal and set upper bounds on the root sum squared of the total dimensionless strain (h rss ) from incoming intermediate-duration gravitational waves ranging from 1.1×10 -22 at 150 Hz to 4.4×10 -22 at 1550 Hz at 50% detection efficiency. From the known distance to the magnetar SGR 1806-20 (8.7 kpc), we can place upper bounds on the isotropic gravitational-wave energy of 3.4 ×10 44 erg at 150 Hz assuming optimal orientation. This represents an improvement of about a factor of 10 in strain sensitivity from the previous search for such signals, conducted during initial LIGO's sixth science run. The short-duration search yielded upper limits of 2.1 ×10 44 erg for short white noise bursts, and 2.3×10 47 erg for 100 ms long ringdowns at 1500 Hz, both at 50% detection efficiency.

Published
2019

25. Low-latency Gravitational-wave Alerts for Multimessenger Astronomy during the Second Advanced LIGO and Virgo Observing Run

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C, Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C, Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

Advanced LIGO's second observing run (O2), conducted from 2016 November 30 to 2017 August 25, combined with Advanced Virgo's first observations in 2017 August, witnessed the birth of gravitational-wave multimessenger astronomy. The first ever gravitational-wave detection from the coalescence of two neutron stars, GW170817, and its gamma-ray counterpart, GRB 170817A, led to an electromagnetic follow-up of the event at an unprecedented scale. Several teams from across the world searched for EM/neutrino counterparts to GW170817, paving the way for the discovery of optical, X-ray, and radio counterparts. In this article, we describe the online identification of gravitational-wave transients and the distribution of gravitational-wave alerts by the LIGO and Virgo collaborations during O2. We also describe the gravitational-wave observables that were sent in the alerts to enable searches for their counterparts. Finally, we give an overview of the online candidate alerts shared with observing partners during O2. Alerts were issued for 14 candidates, 6 of which have been confirmed as gravitational-wave events associated with the merger of black holes or neutron stars. Of the 14 alerts, 8 were issued less than an hour after data acquisition.

Published
2019

26. Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T. D., Abraham, S., Acernese, Fausto, Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, Benjamin P., Abbott, Richard, Abbott, T. D., Abraham, S., Acernese, Fausto, Ackley, K., Adams, C., Adhikari, Rana X., Adya, Vaishali, Affeldt, C., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrowband algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400 − 6325, J1813 − 1246, J1833 − 1034, J1952 þ 3252, and for new targets such as J0940 − 5428 and J1747 − 2809. For J1400 − 6325, J1833 − 1034, and J1747 − 2809, this is the first time the spin-down limit is surpassed.

Published
2019

27. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814

Author

Soares-Santos, M, Palmese, A, Hartley, W, Annis, James, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E., Lin, H, Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Soares-Santos, M, Palmese, A, Hartley, W, Annis, James, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E., Lin, H, Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

We present a multi-messenger measurement of the Hubble constant H 0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s-1 Mpc-1, and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s-1 Mpc-1, we find (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H 0.

Published
2019

28. All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO O2 data

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, Catherine Anne, Adhikari, Rana, Adya, V., Affeldt, C., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, Benjamin P., Abbott, Richard, Abbott, T., Abraham, S., Acernese, F., Ackley, K., Adams, Catherine Anne, Adhikari, Rana, Adya, V., Affeldt, C., Altin, Paul, Forsyth, Perry, Kijbunchoo, Nutsinee, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. Three different semicoherent methods are used to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from −1 × 10−8 to 2 × 10−9 Hz=s. None of these searches has found clear evidence for a CW signal, so upper limits on the gravitational-wave strain amplitude are calculated, which for this broad range in parameter space are the most sensitive ever achieved.

Published
2019

29. All-sky search for short gravitational-wave bursts in the second Advanced LIGO and Advanced Virgo run

Author

Abbott, B. P., Abbott, Richard, Abbott, T, Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adhikari, Rana X, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Kijbunchoo, Nutsinee, McClelland, David, McRae, Terry, McManus, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Adya, Vaishali, Holland, Nathan, Grace, Benjamin, Abbott, B. P., Abbott, Richard, Abbott, T, Abraham, S, Acernese, Fausto, Ackley, K, Adams, C, Adhikari, Rana X, Affeldt, C, Agathos, M., Agatsuma, K., Altin, Paul, Eichholz, Johannes, Forsyth, Perry, Kijbunchoo, Nutsinee, McClelland, David, McRae, Terry, McManus, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Adya, Vaishali, Holland, Nathan, and Grace, Benjamin

Abstract

We present the results of a search for short-duration gravitational-wave transients in the data from the second observing run of Advanced LIGO and Advanced Virgo. We search for gravitational-wave transients with a duration of milliseconds to approximately one second in the 32–4096 Hz frequency band with minimal assumptions about the signal properties, thus targeting a wide variety of sources. We also perform a matched-filter search for gravitational-wave transients from cosmic string cusps for which the waveform is well modeled. The unmodeled search detected gravitational waves from several binary black hole mergers which have been identified by previous analyses. No other significant events have been found by either the unmodeled search or the cosmic string search. We thus present the search sensitivities for a variety of signal waveforms and report upper limits on the source rate density as a function of the characteristic frequency of the signal. These upper limits are a factor of 3 lower than the first observing run, with a 50% detection probability for gravitational-wave emissions with energies of ∼10−9 M⊙c2 at 153 Hz. For the search dedicated to cosmic string cusps we consider several loop distribution models, and present updated constraints from the same search done in the first observing run.

Published
2019

30. Constraining the p-Mode-g-Mode Tidal Instability with GW170817

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, B. P., Abbott, R., Abbott, T. D., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

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!pgpg) 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!pgpg=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!pgpg even when p-g effects are absent. We find that the p-g amplitude for 1.4 MâŠneutron 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 a103 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 a1051 erg over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves.

Published
2019

31. Ground-Based Gravitational-Wave Astronomy in Australia: 2019 White Paper

Author

Bailes, Matthew, McClelland, David, Thrane, Eric, Blair, David, Cooke, Jeffrey, Coward, David, Evans, Robin, Fenner, Yeshe, Galloway, Duncan, Hurley, Jarrod, Ju, Li, Lasky, Paul, Mandel, Ilya, McKenzie, Kirk, Melatos, Andrew, Ottaway, David, Scott, Susan, Slagmolen, Bram, Veitch, Peter, Wen, Linqing, Zhao, Chunnong, Bailes, Matthew, McClelland, David, Thrane, Eric, Blair, David, Cooke, Jeffrey, Coward, David, Evans, Robin, Fenner, Yeshe, Galloway, Duncan, Hurley, Jarrod, Ju, Li, Lasky, Paul, Mandel, Ilya, McKenzie, Kirk, Melatos, Andrew, Ottaway, David, Scott, Susan, Slagmolen, Bram, Veitch, Peter, Wen, Linqing, and Zhao, Chunnong

Abstract

The past four years have seen a scientific revolution through the birth of a new field: gravitational-wave astronomy. The first detection of gravitational waves---recognised by the 2017 Nobel Prize in Physics---provided unprecedented tests of general relativity while unveiling a previously unknown class of massive black holes, thirty times more massive than the Sun. The subsequent detection of gravitational waves from a merging binary neutron star confirmed the hypothesised connection between binary neutron stars and short gamma-ray bursts while providing an independent measurement of the expansion of the Universe. The discovery enabled precision measurement of the speed of gravity while shedding light on the origin of heavy elements. At the time of writing, the Laser Interferometer Gravitational-wave Observatory (LIGO) and its European partner, Virgo, have published the detection of eleven gravitational-wave events. New, not-yet-published detections are announced on a nearly weekly basis. This fast-growing catalogue of gravitational-wave transients is expected to yield insights into a number of topics, from the equation of state of matter at supra-nuclear densities to the fate of massive stars. The science potential of 3G observatories is enormous, enabling measurements of gravitational waves from the edge of the Universe and precise determination of the neutron star equation of state. Australia is well-positioned to help develop the required technology. The Mid-term Review for the Decadal plan for Australian astronomy 2016-2025 should consider investment in a scoping study for an Australian Gravitational-Wave Pathfinder that develops and validates core technologies required for the global 3G detector network., Comment: 8 pages, 7 figures

Published
2019

32. Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Yap, Min Jet, Abernathy, M., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana, Abbott, B. P., Abbott, R., Abbott, T. D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Yap, Min Jet, Abernathy, M., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., and Adhikari, Rana

Abstract

We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90% credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5– 20 deg2 requires at least three detectors of sensitivity within a factor of ∼2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

Published
2018

33. Search for Subsolar-Mass Ultracompact Binaries in Advanced LIGO's First Observing Run

Author

Abbott, B., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, B., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

We present the first Advanced LIGO and Advanced Virgo search for ultracompact binary systems with component masses between 0.2 M-circle dot-1.0 M-circle dot using data taken between September 12, 2015 and January 19, 2016. We find no viable gravitational wave candidates. Our null result constrains the coalescence rate of monochromatic (delta function) distributions of nonspinning (0.2 M-circle dot, 0.2 M-circle dot) ultracompact binaries to be less than 1.0 x 10(6) Gpc(-3) yr(-1) and the coalescence rate of a similar distribution of (1.0 M-circle dot, 1.0 M-circle dot) ultracompact binaries to be less than 1.9 x Gpc(-3) yr(-1) (at 90% confidence). Neither black holes nor neutron stars are expected to form below similar to 1 M-circle dot through conventional stellar evolution, though it has been proposed that similarly low mass black holes could be formed primordially through density fluctuations in the early Universe and contribute to the dark matter density. The interpretation of our constraints in the primordial black hole dark matter paradigm is highly model dependent; however, under a particular primordial black hole binary formation scenario we constrain monochromatic primordial black hole populations of 0.2 M-circle dot to be less than 33% of the total dark matter density and monochromatic populations of 1.0 M-circle dot to be less than 5% of the dark matter density. The latter strengthens the presently placed bounds from microlensing surveys of massive compact halo objects (MACHOs) provided by the MACHO and EROS Collaborations.

Published
2018

34. Effects of data quality vetoes on a search for compact binary coalescences in Advanced LIGO's first observing run

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, Thomas D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Wade, Andrew, Ward, Robert, Abernathy, M., Acernese, Fausto, Ackley, K., Adams, Catherine Anne, Adams, T., Addesso, P., Adhikari, Rana, Adya, V., Abbott, Benjamin P., Abbott, Richard, Abbott, Thomas D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Wade, Andrew, Ward, Robert, Abernathy, M., Acernese, Fausto, Ackley, K., Adams, Catherine Anne, Adams, T., Addesso, P., Adhikari, Rana, and Adya, V.

Abstract

The first observing run of Advanced LIGO spanned 4 months, from 12 September 2015 to 19 January 2016, during which gravitational waves were directly detected from two binary black hole systems, namely GW150914 and GW151226. Confident detection of gravitational waves requires an understanding of instrumental transients and artifacts that can reduce the sensitivity of a search. Studies of the quality of the detector data yield insights into the cause of instrumental artifacts and data quality vetoes specific to a search are produced to mitigate the effects of problematic data. In this paper, the systematic removal of noisy data from analysis time is shown to improve the sensitivity of searches for compact binary coalescences. The output of the PyCBC pipeline, which is a python-based code package used to search for gravitational wave signals from compact binary coalescences, is used as a metric for improvement. GW150914 was a loud enough signal that removing noisy data did not improve its significance. However, the removal of data with excess noise decreased the false alarm rate of GW151226 by more than two orders of magnitude, from 1 in 770 yr to less than 1 in 186 000 yr.

Published
2018

35. Full band all-sky search for periodic gravitational waves in the O1 LIGO data

Author

Abbott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Kijbunchoo, Nutsinee, Manske, Michael, Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, V., Abbott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Kijbunchoo, Nutsinee, Manske, Michael, Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., and Adya, V.

Abstract

We report on a new all-sky search for periodic gravitational waves in the frequency band 475–2000 Hz and with a frequency time derivative in the range of ½−1.0; þ0.1 × 10−8 Hz=s. Potential signals could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the data from Advanced LIGO’s first observational run O1. No gravitational-wave signals were observed, and upper limits were placed on their strengths. For completeness, results from the separately published low-frequency search 20–475 Hz are included as well. Our lowest upper limit on worst-case (linearly polarized) strain amplitude h0 is ∼4 × 10−25 near 170 Hz, while at the high end of our frequency range, we achieve a worst-case upper limit of 1.3 × 10−24. For a circularly polarized source (most favorable orientation), the smallest upper limit obtained is ∼1.5 × 10−25.

Published
2018

36. First Search for Nontensorial Gravitational Waves from Known Pulsars

Author

Abott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Acernese, Fausto, Ackley, K., Adams, T., Addesso, P., Adhikari, Rana X., Adya, V., Affeldt, C., Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Yap, Min Jet, Abott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Acernese, Fausto, Ackley, K., Adams, T., Addesso, P., Adhikari, Rana X., Adya, V., Affeldt, C., Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, and Yap, Min Jet

Abstract

We present results from the first directed search for nontensorial gravitational waves. While general relativity allows for tensorial (plus and cross) modes only, a generic metric theory may, in principle, predict waves with up to six different polarizations. This analysis is sensitive to continuous signals of scalar, vector, or tensor polarizations, and does not rely on any specific theory of gravity. After searching data from the first observation run of the advanced LIGO detectors for signals at twice the rotational frequency of 200 known pulsars, we find no evidence of gravitational waves of any polarization. We report the first upper limits for scalar and vector strains, finding values comparable in magnitude to previously published limits for tensor strain. Our results may be translated into constraints on specific alternative theories of gravity.

Published
2018

37. All-sky search for long-duration gravitational wave transients in the first Advanced LIGO observing run

Author

Abbott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Yap, Min Jet, Yu, Hang, Yu, Haocun, Yvert, M., Zadrozny, A., Zangrando, L., Zanolin, M., Zendri, J-P., Abbott, Benjamin P., Abbott, Robert, Abbott, Thomas D., Altin, Paul, Chow, Jong, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Yap, Min Jet, Yu, Hang, Yu, Haocun, Yvert, M., Zadrozny, A., Zangrando, L., Zanolin, M., and Zendri, J-P.

Abstract

We present the results of a search for long-duration gravitational wave transients in the data of the LIGO Hanford and LIGO Livingston second generation detectors between September 2015 and January 2016, with a total observational time of 49 d. The search targets gravitational wave transients of 10–500 s duration in a frequency band of 24–2048 Hz, with minimal assumptions about the signal waveform, polarization, source direction, or time of occurrence. No significant events were observed. As a result we set 90% confidence upper limits on the rate of long-duration gravitational wave transients for different types of gravitational wave signals. We also show that the search is sensitive to sources in the Galaxy emitting at least ∼10−8 M c2 in gravitational waves.

Published
2018

38. GW170817: Measurements of Neutron Star Radii and Equation of State

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Holland, Nicole, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Holland, Nathan, Abbott, Benjamin P., Abbott, Richard, Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, Vaishali, Altin, Paul, Chow, Jong, Forsyth, Perry, Holland, Nicole, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Holland, Nathan

Abstract

On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parametrization of the defining function p(rho) of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as R-1 = 10.8(-1.7)(+2.0) km for the heavier star and R-2 = 10.7(-1.5)(+2.1) km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than 1.97 M-circle dot as required from electromagnetic observations and employ the equation-of-state parametrization, we further constrain R-1 = 11.9(-1.4)(+1.4) km and R-2 = 11.9(-1.4)(+1.4) km at the 90% credible level. Finally, we obtain constraints on p(rho) at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5(-1.7)(+2.7) x 10(34) dyn cm(-2) at the 90% level.

Published
2018

39. Full band all-sky search for periodic gravitational waves in the O1 LIGO data

Author

Abbott, Benjamin P., Abbott, Rich, Abbott, Thomas D., Acernese, Fausto, Ackley, Kendall, Adams, Carl, Adams, Thomas, Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali B., Affeldt, Christoph, Afrough, Mohammad, Agarwal, Bhanu, Agathos, Michalis, Agatsuma, Kazuhiro, Aggarwal, Nancy, Aguiar, Odylio D., Aiello, Lorenzo, Ain, Anirban, Allen, Bruce, Allen, Gabrielle, Allocca, Annalisa, Altin, Paul A., Amato, Alex, Ananyeva, Alena, Anderson, Stuart B., Anderson, Warren G., Angelova, Svetoslava V., Antier, Sarah, Appert, Stephen, Arai, Koji, Araya, Melody C., Areeda, Joseph S., Arnaud, Nicolas, Ascenzi, Stefano, Ashton, Gregory, Ast, M., Aston, Stuart M., Astone, Pia, Atallah, Dany V., Aufmuth, Peter, Aulbert, Carsten, AultONeal, K., Austin, Corey, Avila-Alvarez, A., Babak, Stanislav, Bacon, Philippe, Bader, Maria K.M., Bae, Sangwook, Baker, Paul T., Baldaccini, Francesca, Ballardin, Giulio, Ballmer, Stefan W., Banagiri, Sharan, Barayoga, Juan C., Barclay, Sheena E., Barish, Barry C., Barker, David, Barkett, Kevin, Barone, Fabrizio, Barr, Bryan, Barsotti, Lisa, Barsuglia, Matteo, Barta, Daniel, Bartlett, Jeffrey, Bartos, Imre, Bassiri, Riccardo, Basti, Andrea, Batch, James C., Bawaj, Mateusz, Bayley, Joseph C., Bazzan, Marco, Bécsy, Bence, Beer, Christian, Bejger, Michal, Belahcene, Imene, Bell, Angus S., Berger, Beverly K., Bergmann, Gerald, Bero, John J., Berry, Christopher P.L., Bersanetti, Diego, Bertolini, Alessandro, Betzwieser, Joseph, Bhagwat, Swetha, Bhandare, Rohan, Bilenko, Igor A., Billingsley, Garilynn, Billman, Chris R., Birch, Jeremy, Birney, Ross, Birnholtz, Ofek, Biscans, Sebastien, Biscoveanu, Sylvia, Bisht, Aparna, Bitossi, Massimiliano, Biwer, Christopher, Bizouard, Marieanne A., Blackburn, J.K., Blackman, Jonathan, Blair, Carl D., Blair, David G., Blair, Ryan M., Bloemen, Steven, Bock, Oliver, Bode, Nina, Boer, Michel, Bogaert, Gilles, Bohe, Alejandro, Bondu, Francois, Bonilla, Edgard, Bonnand, Romain, Boom, Boris A., Bork, Rolf, Boschi, Valerio, Bose, Sukanta, Bossie, Ken, Bouffanais, Yann, Bozzi, Antonella, Bradaschia, Carlo, Brady, Patrick R., Branchesi, Marica, Brau, Jim E., Briant, Tristan, Brillet, Alain, Brinkmann, Marc, Brisson, Violette, Brockill, Patrick, Broida, Jacob E., Brooks, Aidan F., Brown, Duncan A., Brown, Daniel D., Brunett, Sharon, Buchanan, Christopher C., Buikema, Aaron, Bulik, Tomasz, Bulten, Henk J., Buonanno, Alessandra, Buskulic, Damir, Buy, Christelle, Byer, Robert L., Cabero, Miriam, Cadonati, Laura, Cagnoli, Giampietro, Cahillane, Craig, Calderón Bustillo, J., Callister, Thomas A., Calloni, Enrico, Camp, Jordan B., Canepa, Maurizio, Canizares, Priscilla, Cannon, Kipp C., Cao, H., Cao, Junwei, Capano, Collin D., Capocasa, Eleonora, Carbognani, Franco, Caride, Santiago, Carney, Matthew F., Casanueva Diaz, J., Casentini, Claudio, Caudill, Sarah, Cavaglià, Marco, Cavalier, Fabien, Cavalieri, Roberto, Cella, Giancarlo, Cepeda, Christian B., Cerdá-Durán, P., Cerretani, Giovanni, Cesarini, Elisabetta, Chamberlin, Sydney J., Chan, Manleong, Chao, Shiuh, Charlton, Philip, Chase, Eve, Chassande-Mottin, E., Chatterjee, Deep, Cheeseboro, Belinda D., Chen, H.Y., Chen, Xu, Chen, Yanbei, Cheng, H.-P., Chia, Hanyu Y., Chincarini, Andrea, Chiummo, Antonino, Chmiel, Theresa, Cho, Heesuk S., Cho, M., Chow, Jong H., Christensen, Nelson, Chu, Qi, Chua, Alvin J.K., Chua, Sheon, Chung, A.K.W., Chung, Shinkee, Ciani, Giacomo, Ciecielag, P., Ciolfi, Riccardo, Cirelli, Carissa E., Cirone, Alessio, Clara, Filiberto, Clark, James A., Clearwater, Patrick, Cleva, Frederic, Cocchieri, Camillo, Coccia, Eugenio, Cohadon, P.-F., Cohen, David, Colla, Alberto, Collette, Christophe G., Cominsky, Lynn R., Constancio, M., Conti, Livia, Cooper, Sam J., Corban, Paul, Corbitt, Thomas R., Cordero-Carrión, I., Corley, Kenneth R., Cornish, Neil, Corsi, Alessandra, Cortese, Stefano, Costa, Cesar A., Coughlin, Eric T., Coughlin, Michael W., Coughlin, Scott B., Coulon, J.-P., Countryman, Stefan T., Couvares, Peter, Covas, Pep B., Cowan, Erika E., Coward, David M., Cowart, Matthew J., Coyne, Dennis C., Coyne, Robert, Creighton, Jolien D.E., Creighton, Teviet D., Cripe, Jonathan, Crowder, Sgwynne G., Cullen, Torrey J., Cumming, Alan, Cunningham, Liam, Cuoco, Elena, Dal Canton, Tito, Dálya, Gergely, Danilishin, Stefan L., D'Antonio, S., Danzmann, Karsten, Dasgupta, Arnab, Da Silva Costa, C.F., Dattilo, Vincenzo, Dave, Ishant, Davier, Michel, Davis, Derek, Daw, Edward J., Day, Brian, De, Soumi, Debra, D., Degallaix, Jerome, De Laurentis, M., Deléglise, Samuel, Del Pozzo, W., Demos, Nicholas, Denker, Timo, Dent, Thomas, De Pietri, R., Dergachev, Vladimir, De Rosa, R., DeRosa, R.T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, Jan, Dhurandhar, Sanjeev, Díaz, Mario C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Zoheyr, Dolique, Vincent, Donovan, Fred, Dooley, Katherine L., Doravari, Suresh, Dorosh, O., Dorrington, Iain, Douglas, Rebecca, Dovale Álvarez, M., Downes, Thomas P., Drago, Marco, Dreissigacker, Christoph, Driggers, Jenne C., Du, Zhihui, Ducrot, Marine, Dupej, Peter, Dwyer, Sheila E., Edo, Tega B., Edwards, Matthew C., Effler, Anamaria, Eggenstein, H.-B., Ehrens, Phil, Eichholz, Johannes, Eikenberry, Stephen S., Eisenstein, Robert A., Essick, Reed C., Estevez, Dimitri, Etienne, Zachariah B., Etzel, Todd, Evans, Matthew, Evans, Tom M., Factourovich, Maxim, Fafone, Viviana, Fair, Hannah, Fairhurst, Stephen, Fan, Xilong, Farinon, Stefania, Farr, Benjamin, Farr, Will M., Fauchon-Jones, E.J., Favata, Marc, Fays, Maxime, Fee, Campbell, Fehrmann, Henning, Feicht, Jon, Fejer, Martin M., Fernandez-Galiana, A., Ferrante, Isidoro, Ferreira, Elvis C., Ferrini, Federico, Fidecaro, Francesco, Finstad, Daniel, Fiori, Irene, Fiorucci, Donatella, Fishbach, Maya, Fisher, Ryan P., Fitz-Axen, M., Flaminio, Raffaele, Fletcher, Mark, Fong, Heather, Font, J.A., Forsyth, Perry W.F., Forsyth, Steven S., Fournier, J.-D., Frasca, Sergio, Frasconi, Franco, Frei, Zsolt, Freise, Andreas, Frey, Raymond, Frey, Valentin, Fries, Eric M., Fritschel, Peter, Frolov, Valery V., Fulda, Paul, Fyffe, Michael, Gabbard, Hunter, Gadre, Bhooshan U., Gaebel, Sebastian M., Gair, Jonathan R., Gammaitoni, Luca, Ganija, Miftar R., Gaonkar, Sharad G., Garcia-Quiros, C., Garufi, Fabio, Gateley, B., Gaudio, Sergio, Gaur, Gurudatt, Gayathri, V., Gehrels, Neil, Gemme, Gianluca, Genin, Eric, Gennai, Alberto, George, Daniel, George, Jogy, Gergely, Laszlo, Germain, Vincent, Ghonge, Sudarshan, Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Giaime, Joe A., Giardina, K.D., Giazotto, Adalberto, Gill, Kiranjyot, Glover, Lamar, Goetz, Evan, Goetz, Ryan, Gomes, Sandra, Goncharov, Boris, González, Gabriela, Gonzalez Castro, J.M., Gopakumar, A., Gorodetsky, Michael L., Gossan, Sarah E., GOSSELIN, Matthieu, Gouaty, Romain, Grado, Aniello, Graef, Christian, Granata, Massimo, Grant, Alastair, Gras, Slawomir, Gray, Corey, Greco, Giuseppe, Green, Anna C., Gretarsson, Elizabeth M., Groot, Paul, Grote, Hartmut, Grunewald, Steffen, Gruning, Pierre, Guidi, Gianluca M., Guo, Xiangyu, Gupta, Anuradha, Gupta, Manojipr K., Gushwa, Kaitlin E., Gustafson, Eric K., Gustafson, R., Halim, O., Hall, Bernard R., Hall, Evan D., Hamilton, Eleanor Z., Hammond, Giles, Haney, Maria, Hanke, Manuela M., Hanks, Jonathan, Hanna, Chad, Hannam, Mark D., Hannuksela, Otto A., Hanson, Joe, Hardwick, Terra, Harms, Jan, Harry, Gregg M., Harry, Ian W., Hart, Martin J., Haster, C.-J., Haughian, Karen, Healy, James, Heidmann, Antoine, Heintze, Matthew C., Heitmann, Henrich, Hello, Patrice, Hemming, Gary, Hendry, Martin, Heng, I.S., Hennig, J., Heptonstall, Alastair W., Heurs, Michele, Hild, Stefan, Hinderer, Tanja, Hoak, Daniel, Hofman, David, Holt, Kathy, Holz, Daniel E., Hopkins, Paul, Horst, Christian, Hough, James, Houston, Ewan A., Howell, Eric J., Hreibi, A., Hu, Yiming M., Huerta, Eliu A., Huet, Dominique, Hughey, Brennan, Husa, Sascha, Huttner, Sabina H., Huynh-Dinh, T., Indik, Nathaniel, Inta, Ra, Intini, Giuseppe, Isa, Hafizah N., Isac, J.-M., Isi, Max, Iyer, Bala R., Izumi, Kiwamu, Jacqmin, Thibaut, Jani, Karan, Jaranowski, Piotr, Jawahar, Sharat, Jiménez-Forteza, F., Johnson, Warren W., Jones, D.I., Jones, Russell, Jonker, Reinier J.G., Ju, L., Junker, Jonas, Kalaghatgi, Chinmay V., Kalogera, Vassiliki, Kamai, Brittany, Kandhasamy, Shivaraj, Kang, Gungwon, Kanner, Jonah B., Kapadia, Shasvath J., Karki, Sudarshan, Karvinen, Kai S., Kasprzack, Marie, Katolik, Michael, Katsavounidis, Erik, Katzman, William, Kaufer, Steffen, Kawabe, Keita, Kéfélian, Fabien, Keitel, David, Kemball, Athol J., Kennedy, Ross, Kent, Christopher, Key, Joey S., Khalili, Farit Y., Khan, I., Khan, Sebastian, Khan, Ziauddin, Khazanov, Efim A., Kijbunchoo, Nutsinee, Kim, Chunglee, Kim, Jeongcho C., Kim, Kyungmin, Kim, Won, Kim, Whansun S., Kim, Y.-M., Kimbrell, Seth J., King, Eleanor J., King, Peter J., Kinley-Hanlon, M., Kirchhoff, Robin, Kissel, Jeffrey S., Kleybolte, Lisa, Klimenko, Sergei, Knowles, Tyler D., Koch, Philip, Koehlenbeck, Sina M., Koley, Soumen, Kondrashov, Veronica, Kontos, Antonios, Korobko, Mikhail, Korth, William Z., Kowalska, Izabela, Kozak, Dan B., Krämer, Christina, Kringel, Volker, Krishnan, Badri, Królak, Andrzej, Kuehn, Gerrit, Kumar, Prayush, Kumar, Rakesh, Kumar, Sumit, Kuo, L., Kutynia, Adam, Kwang, Shawn, Lackey, Benjamin D., Lai, K.H., Landry, Michael, Lang, Ryan N., Lange, Jacob, Lantz, Brian, Lanza, Robert K., Lartaux-Vollard, A., Lasky, Paul D., Laxen, Michael, Lazzarini, Albert, Lazzaro, Claudia, Leaci, Paola, Leavey, Sean, Lee, C.H., Lee, Hyunkyu K., Lee, H.M., Lee, Hyungwon W., Lee, K., Lehmann, Johannes, Lenon, Amber, Leonardi, Matteo, Leroy, Nicolas, Letendre, Nicolas, Levin, Yuri, Li, Tjonnie G.F., Linker, Seth D., Littenberg, Tyson B., Liu, J., Lo, R.K.L., Lockerbie, Nick A., London, Lionel T., Lord, Jaysin E., Lorenzini, Matteo, Loriette, Vincent, Lormand, Marc, Losurdo, Giovanni, Lough, James D., 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Jaranowski, Piotr, Jawahar, Sharat, Jiménez-Forteza, F., Johnson, Warren W., Jones, D.I., Jones, Russell, Jonker, Reinier J.G., Ju, L., Junker, Jonas, Kalaghatgi, Chinmay V., Kalogera, Vassiliki, Kamai, Brittany, Kandhasamy, Shivaraj, Kang, Gungwon, Kanner, Jonah B., Kapadia, Shasvath J., Karki, Sudarshan, Karvinen, Kai S., Kasprzack, Marie, Katolik, Michael, Katsavounidis, Erik, Katzman, William, Kaufer, Steffen, Kawabe, Keita, Kéfélian, Fabien, Keitel, David, Kemball, Athol J., Kennedy, Ross, Kent, Christopher, Key, Joey S., Khalili, Farit Y., Khan, I., Khan, Sebastian, Khan, Ziauddin, Khazanov, Efim A., Kijbunchoo, Nutsinee, Kim, Chunglee, Kim, Jeongcho C., Kim, Kyungmin, Kim, Won, Kim, Whansun S., Kim, Y.-M., Kimbrell, Seth J., King, Eleanor J., King, Peter J., Kinley-Hanlon, M., Kirchhoff, Robin, Kissel, Jeffrey S., Kleybolte, Lisa, Klimenko, Sergei, Knowles, Tyler D., Koch, Philip, Koehlenbeck, Sina M., Koley, Soumen, Kondrashov, Veronica, Kontos, Antonios, Korobko, Mikhail, Korth, William Z., Kowalska, Izabela, Kozak, Dan B., Krämer, Christina, Kringel, Volker, Krishnan, Badri, Królak, Andrzej, Kuehn, Gerrit, Kumar, Prayush, Kumar, Rakesh, Kumar, Sumit, Kuo, L., Kutynia, Adam, Kwang, Shawn, Lackey, Benjamin D., Lai, K.H., Landry, Michael, Lang, Ryan N., Lange, Jacob, Lantz, Brian, Lanza, Robert K., Lartaux-Vollard, A., Lasky, Paul D., Laxen, Michael, Lazzarini, Albert, Lazzaro, Claudia, Leaci, Paola, Leavey, Sean, Lee, C.H., Lee, Hyunkyu K., Lee, H.M., Lee, Hyungwon W., Lee, K., Lehmann, Johannes, Lenon, Amber, Leonardi, Matteo, Leroy, Nicolas, Letendre, Nicolas, Levin, Yuri, Li, Tjonnie G.F., Linker, Seth D., Littenberg, Tyson B., Liu, J., Lo, R.K.L., Lockerbie, Nick A., London, Lionel T., Lord, Jaysin E., Lorenzini, Matteo, Loriette, Vincent, Lormand, Marc, Losurdo, Giovanni, Lough, James D., Lovelace, Geoffrey, Lück, Harald, Lumaca, Diana, Lundgren, Andrew P., Lynch, Ryan, Ma, Y., Macas, Ronaldas, Macfoy, Sean, Machenschalk, Bernd, Macinnis, M., Macleod, Duncan M., Magaña Hernandez, I., Magaña-Sandoval, F., Magaña Zertuche, L., Magee, Ryan M., Majorana, Ettore, Maksimovic, Ivan, Man, N., Mandic, Vuk, Mangano, Valentina, Mansell, Georgia L., Manske, Michael, Mantovani, Maddalena, Marchesoni, Fabio, Marion, Frederique, Márka, Szabolcs, Márka, Zsuzsanna, Markakis, Charalampos, Markosyan, Ashot S., Markowitz, Aaron, Maros, E., Marquina, Antonio, Martelli, Filippo, Martellini, Lionel, Martin, Ian W., Martin, Rodica M., Martynov, Denis V., Mason, Ken, Massera, Elena, Masserot, Alain, Massinger, Thomas J., Masso-Reid, M., Mastrogiovanni, Simone, Matas, Andrew, Matichard, Fabrice, Matone, Luca, Mavalvala, Nergis, Mazumder, Nairwita, McCarthy, R., Mcclelland, D.E., Mccormick, S., McCuller, L., McGuire, S.C., Mcintyre, G., Mciver, J., McManus, David J., McNeill, L., McRae, T., McWilliams, S.T., Meacher, Duncan, Meadors, Grant D., Mehmet, Moritz, Meidam, Jeroen, Mejuto-Villa, E., Melatos, Andrew, Mendell, Gregory, Mercer, R.A., Merilh, Edmond L., Merzougui, Mourad, Meshkov, Syd, Messenger, Chris, Messick, Cody, Metzdorff, R., Meyers, Patrick M., Miao, Haixing, Michel, Christophe, Middleton, Hannah, Mikhailov, Eugeniy E., Milano, Leopoldo, Miller, Andrewlawrence L., Miller, Brandon B., Miller, John, Millhouse, Meg, Milovich-Goff, M.C., Minazzoli, Olivier, Minenkov, Yuri, Ming, Jing, Mishra, Chandra, Mitra, Sanjit, Mitrofanov, Valery P., Mitselmakher, Guenakh, Mittleman, Richard, Moffa, Donald, Moggi, Andrea, Mogushi, Kentaro, Mohan, Martin, Mohapatra, S.R.P., Montani, Matteo, Moore, Christopher J., Moraru, Dan, Moreno, Gerardo, Morriss, Sean R., Mours, Benoit, Mow-Lowry, C.M., Mueller, Guido, Muir, Alistair W., Mukherjee, Arunava, Mukherjee, Debnandini, Mukherjee, Soma, Mukund, Nikhil, Mullavey, Adam, Munch, Jesper, Muñiz, Erik A., Muratore, Martina, Murray, Peter G., Napier, Kate, Nardecchia, Ilaria, Naticchioni, Luca, Nayak, Rajesh K., Neilson, Joshua, Nelemans, Gijs, Nelson, Timothy J.N., Nery, Marina, Neunzert, Ansel, Nevin, Lydia, Newport, Jonathan M., Newton, Gavin, Ng, K.Y., Nguyen, Thanh T., Nichols, David, Nielsen, Alex B., Nissanke, Samaya, Nitz, Alex, Noack, Andreas, Nocera, Flavio, Nolting, David, North, Chris, Nuttall, Laura K., Oberling, Jason, O'Dea, G.D., Ogin, Greg H., Oh, John J., Oh, Sanghoon H., Ohme, Frank, Okada, Marcos A., Oliver, Miquel, Oppermann, Patrick, Oram, Richard J., O'Reilly, B., Ormiston, Rich, Ortega, Luis F., O'Shaughnessy, R., Ossokine, Serguei, Ottaway, David J., Overmier, Harry, Owen, Ben J., Pace, Alexander E., Page, Jessica, Page, Michael A., Pai, Archana, Pai, Siddhesh A., Palamos, Jordan R., Palashov, Oleg, Palomba, Cristiano, Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, Belinda, Pang, P.T.H., Pankow, Chris, Pannarale, Francesco, Pant, Brijesh C., Paoletti, Federico, PAOLI, Andrea, Papa, Maria A., Parida, Abhishek, Parker, William, Pascucci, Daniela, Pasqualetti, Antonio, Passaquieti, Roberto, Passuello, Diego, Patil, M., Patricelli, Barbara, Pearlstone, Brynley L., Pedraza, Mike, Pedurand, Richard, Pekowsky, L., Pele, Arnaud, Penn, Steven, Perez, Carlos J., Perreca, Antonio, Perri, Leah M., Pfeiffer, Harald P., Phelps, Margot, Piccinni, Ornella J., Pichot, Mikhael, Piergiovanni, Francesco, Pierro, Vincenzo, Pillant, Gabriel, Pinard, Laurent, Pinto, Innocenzo M., Pirello, Marc, Pisarski, A., Pitkin, Matthew, Poe, Mark, Poggiani, Rosa, Popolizio, Pasquale, Porter, K., Post, Alexander, Powell, Jade, Prasad, Jayanti, Pratt, James W.W., Pratten, Geraint, Predoi, Valeriu, Prestegard, Tanner, Prijatelj, Mirko, Principe, Maria, Privitera, Stephen, Prodi, Giovanni A., Prokhorov, Leonid G., Puncken, Oliver, Punturo, Michele, Puppo, Paola, Pürrer, Michael, Qi, Hong, Quetschke, Volker, Quintero, Eric A., Quitzow-James, R., Raab, Fred J., Rabeling, David S., Radkins, Hugh, Raffai, Peter, Raja, Sendhil, Rajan, C., Rajbhandari, Binod, Rakhmanov, Malik, Ramirez, Karla E., Ramos-Buades, A., Rapagnani, Piero, Raymond, Vivien, Razzano, Massimiliano, Read, Jocelyn, Regimbau, Tania, Rei, Luca, Reid, Stuart, Reitze, David H., Ren, Wei, Reyes, Steven D., Ricci, Fulvio, Ricker, Paul M., Rieger, Sascha, Riles, Keith, Rizzo, Monica, Robertson, Norna A., Robie, Raymond, Robinet, Florent, Rocchi, Alessio, ROLLAND, Loic, Rollins, Jameson G., Roma, Vincent J., Romano, Rocco, Romel, Chandra L., Romie, Janeen H., Rosińska, Dorota, Ross, Michael P., Rowan, Sheila, Rüdiger, Albrecht, Ruggi, Paolo, Rutins, Guntis, Ryan, Kyle, Sachdev, Surabhi, Sadecki, Travis, Sadeghian, Laleh, Sakellariadou, Mairi, Salconi, Livio, Saleem, Muhammed, Salemi, Francesco, Samajdar, Anuradha, Sammut, Letizia, Sampson, Laura M., Sanchez, Eduardo J., Sanchez, Luis E., Sanchis-Gual, N., Sandberg, Vernon, Sanders, Jaclyn R., Sassolas, Benoit, Saulson, Peter R., Sauter, Orion, Savage, Richard L., Sawadsky, Andreas, Schale, Paul, Scheel, Mark, Scheuer, Jacob, Schmidt, Justus, Schmidt, Patricia, Schnabel, Roman, Schofield, Robert M.S., Schönbeck, Axel, Schreiber, Emil, Schuette, Dirk, Schulte, Bernd W., Schutz, Bernard F., Schwalbe, Sophia G., Scott, Jamie, Scott, Susan M., Seidel, E., Sellers, Danny, Sengupta, Anand S., Sentenac, Daniel, Sequino, Valeria, Sergeev, Alexander, Shaddock, Daniel A., Shaffer, Thomas J., Shah, Ankur A., Shahriar, M.S., Shaner, Morgan B., Shao, Lijing, Shapiro, Brett, Shawhan, Peter, Sheperd, Alec, Shoemaker, David H., Shoemaker, Deirdre M., Siellez, Karelle, Siemens, Xavier, Sieniawska, Magdalena, Sigg, Daniel, Silva, Allan D., Singer, Leo P., Singh, Avneet, Singhal, Akshat, Sintes, Alicia M., Slagmolen, Bram J.J., Smith, Bryan, Smith, Joshua R., Smith, Rory J.E., Somala, Surendranadh, Son, Edwin J., Sonnenberg, Jacob A., Sorazu, Borja, Sorrentino, Fiodor, Souradeep, Tarun, Spencer, Andrew P., Srivastava, Amit K., Staats, Kai, Staley, Alexan, Steinke, Michael, Steinlechner, Jessica, Steinlechner, Sebastian, Steinmeyer, Daniel, Stevenson, Simon P., Stone, Robert, Stops, David J., Strain, Ken A., Stratta, Giulia, Strigin, Sergey E., Strunk, A., Sturani, Riccardo, Stuver, Amber L., Summerscales, Tiffany Z., Sun, Ling, Sunil, S., Suresh, Jishnu, Sutton, Patrick J., Swinkels, Bas L., Szczepańczyk, Marek J., Tacca, Matteo, Tait, Simon C., Talbot, Colm, Talukder, Dipongkar, Tanner, David B., Tao, Duo, Tápai, Marton, Taracchini, Andrea, Tasson, Jay D., Taylor, Jordan A., Taylor, Robert, Tewari, Shivam V., Theeg, Thomas, Thies, Fabian, Thomas, E.G., Thomas, Michael, Thomas, Patrick, Thorne, Keith A., Thrane, Eric, Tiwari, Shubhanshu, Tiwari, Vaibhav, Tokmakov, Kirill V., Toland, Karl, Tonelli, Mauro, Tornasi, Zeno, Torres-Forné, A., Torrie, Calum I., Töyrä, Daniel, Travasso, Flavio, Traylor, Gary, Trinastic, Jonathan, Tringali, Maria C., Trozzo, Lucia, Tsang, K.W., Tse, Maggie, Tso, Rhondale, Tsukada, Leo, Tsuna, Daichi, Tuyenbayev, Darkhan, Ueno, Koh, Ugolini, Dennis, Unnikrishnan, Cs S., Urban, Alexander L., Usman, Samantha A., Vahlbruch, Henning, Vajente, Gabriele, Valdes, Guillermo, Van Bakel, N., van Beuzekom, Martin, Van Den Brand, J.F.J., Van Den Broeck, C., Vander-Hyde, D.C., van der Schaaf, L., van Heijningen, J.V., van Veggel, A.A., Vardaro, Marco, Varma, Vijay, Vass, Steve, Vasúth, Matyas, Vecchio, Alberto, Vedovato, Gabriele, Veitch, John, Veitch, Peter J., Venkateswara, Krishna, Venugopalan, Gautam, Verkindt, Didier, Vetrano, Flavio, Viceré, Andrea, Viets, Aaron D., Vinciguerra, Serena, Vine, David J., Vinet, J.-Y., Vitale, Salvatore, Vo, Thomas, Vocca, Helios, Vorvick, Cheryl, Vyatchanin, Sergey P., Wade, Andrew R., Wade, Leslie E., Wade, Madeline, Walet, Rob, Walker, Marissa, Wallace, Larry, Walsh, Sinead, Wang, Gang, Wang, Haoyu, Wang, Jonathan Z., Wang, Wenhui H., Wang, Yifan F., Ward, Robert L., Warner, Jim, Was, Michal, Watchi, Jennifer, Weaver, Betsy, Wei, L.-W., Weinert, Michael, Weinstein, Alan J., Weiss, Rainer, Wen, Linqing, Wessel, Erik K., Weßels, Peter, Westerweck, Julian, Westphal, Tobias, Wette, Karl, Whelan, John T., Whiting, Bernard F., Whittle, Chris, Wilken, D., Williams, Daniel, Williams, Roy D., Williamson, Andrew R., Willis, Joshua L., Willke, Benno, Wimmer, Maximilian H., Winkler, Walter, Wipf, Christopher C., Wittel, Holger, Woan, Graham, Woehler, Janis, Wofford, Jared, Wong, W.K., Worden, John, Wright, Jennifer L., Wu, David S., Wysocki, Daniel M., Xiao, Sophia, Yamamoto, Hiro, Yancey, Cregg C., Yang, Le, Yap, M.J., Yazback, Maher, Yu, Hang, Yu, Haocun, Yvert, Michel, Zadrożny, Adam, Zanolin, Michele, Zelenova, Tatiana, Zendri, J.-P., Zevin, Michael, Zhang, Liyuan, Zhang, Mi, Zhang, Teng, Zhang, Y.-H., Zhao, Chunnong, Zhou, Minchuan, Zhou, Zifan, Zhu, Sylvia J., Zhu, Xingjiang J., Zucker, Michael E., and Zweizig, J.

Abstract

We report on a new all-sky search for periodic gravitational waves in the frequency band 475-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Potential signals could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the data from Advanced LIGO's first observational run O1. No gravitational-wave signals were observed, and upper limits were placed on their strengths. For completeness, results from the separately published low-frequency search 20-475 Hz are included as well. Our lowest upper limit on worst-case (linearly polarized) strain amplitude h0 is ∼4×10-25 near 170 Hz, while at the high end of our frequency range, we achieve a worst-case upper limit of 1.3×10-24. For a circularly polarized source (most favorable orientation), the smallest upper limit obtained is ∼1.5×10-25. © 2018 American Physical Society.

Published
2018

40. Reconfiguring relations of accountability: Materialization of social media in the travel sector

Author

Orlikowski, Wanda J, Scott, Susan V., Orlikowski, Wanda J, and Scott, Susan V.

Abstract

Expanding use of Web 2.0 technologies has generated complex information dynamics that are propelling organizations in unexpected directions, redrawing boundaries and shifting relationships. Using research on user-generated content, we examine online rating and ranking mechanisms and analyze how their performance reconfigures relations of accountability. Our specific interest is in the use of so-called “social media” such as TripAdvisor, where participant reviews are used to rank the popularity of services provided by the travel sector. Although ranking mechanisms are not new, they become “power-charged”—to use Donna Haraway’s term—when enacted through Web 2.0 technologies. As such, they perform a substantial redistribution of accountability. We draw on data from an on-going field study of small businesses in a remote geographical area for whom TripAdvisor has changed ‘the rules of the game,’ and we explore the moral and strategic implication of this transformation.

Published
2017

41. Search for intermediate mass black hole binaries in the first observing run of Advanced LIGO

Author

Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Abbott, B., Abbott, Robert, Adhikari, Rana, Arai, Koji, Barayoga, J. C. B., Barish, Barry, Berger, B. K., Billingsley, G., Blackburn, James Kent, Bork, R., Ehrens, P., Etzel, T., Heptonstall, A., Korth, W. Zach, Kozak, D., Lazzarini, A., Maros, E., Meshkov, S., Pedraza, M., Altin, Paul, Chow, Jong, Forsyth, Perry, Mansell, Georgia, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Abbott, B., Abbott, Robert, Adhikari, Rana, Arai, Koji, Barayoga, J. C. B., Barish, Barry, Berger, B. K., Billingsley, G., Blackburn, James Kent, Bork, R., Ehrens, P., Etzel, T., Heptonstall, A., Korth, W. Zach, Kozak, D., Lazzarini, A., Maros, E., Meshkov, S., and Pedraza, M.

Abstract

During their first observational run, the two Advanced LIGO detectors attained an unprecedented sensitivity, resulting in the first direct detections of gravitational-wave signals produced by stellar-mass binary black hole systems. This paper reports on an all-sky search for gravitational waves (GWs) from merging intermediate mass black hole binaries (IMBHBs). The combined results from two independent search techniques were used in this study: the first employs a matched-filter algorithm that uses a bank of filters covering the GW signal parameter space, while the second is a generic search for GW transients (bursts). No GWs from IMBHBs were detected; therefore, we constrain the rate of several classes of IMBHB mergers. The most stringent limit is obtained for black holes of individual mass 100 M⊙, with spins aligned with the binary orbital angular momentum. For such systems, the merger rate is constrained to be less than 0.93 Gpc−3 yr−1 in comoving units at the 90% confidence level, an improvement of nearly 2 orders of magnitude over previous upper limits.

Published
2017

42. Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

Author

Abbott, Robert, Abbott, B., Abbott, T. D., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, V., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Robert, Abbott, B., Abbott, T. D., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana X., Adya, V., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

The first observation of a binary neutron star (NS) coalescence by the Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors offers an unprecedented opportunity to study matter under the most extreme conditions. After such a merger, a compact remnant is left over whose nature depends primarily on the masses of the inspiraling objects and on the equation of state of nuclear matter. This could be either a black hole (BH) or an NS, with the latter being either long-lived or too massive for stability implying delayed collapse to a BH. Here, we present a search for GWs from the remnant of the binary NS merger GW170817 using data from Advanced LIGO and Advanced Virgo. We search for short- (lesssim1 s) and intermediate-duration (lesssim500 s) signals, which include GW emission from a hypermassive NS or supramassive NS, respectively. We find no signal from the post-merger remnant. Our derived strain upper limits are more than an order of magnitude larger than those predicted by most models. For short signals, our best upper limit on the root sum square of the GW strain emitted from 1–4 kHz is ${h}_{\mathrm{rss}}^{50 \% }=2.1\times {10}^{-22}\,{\mathrm{Hz}}^{-1/2}$ at 50% detection efficiency. For intermediate-duration signals, our best upper limit at 50% detection efficiency is ${h}_{\mathrm{rss}}^{50 \% }=8.4\times {10}^{-22}\,{\mathrm{Hz}}^{-1/2}$ for a millisecond magnetar model, and ${h}_{\mathrm{rss}}^{50 \% }=5.9\times {10}^{-22}\,{\mathrm{Hz}}^{-1/2}$ for a bar-mode model. These results indicate that post-merger emission from a similar event may be detectable when advanced detectors reach design sensitivity or with next-generation detectors.

Published
2017

43. GW170608: Observation of a 19 Solar-mass Binary Black Hole Coalescence

Author

Abbott, Benjamin P., Abbott, R., Abbott, T. D., Acernese, Fausto, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, R., Abbott, T. D., Acernese, Fausto, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

On 2017 June 8 at 02:01:16.49 UTC, a gravitational-wave (GW) signal from the merger of two stellar-mass blackholes was observed by the two Advanced Laser Interferometer Gravitational-Wave Observatory detectors with anetwork signal-to-noise ratio of 13. This system is the lightest black hole binary so far observed, with componentmasses of 12+7-2M⊙7+2-2 (90% credible intervals). These lie in the range of measured black hole masses inlow-mass X-ray binaries, thus allowing us to compare black holes detected through GWs with electromagneticobservations. The source's luminosity distance is 340+140-140corresponding to redshift -0.07+0.03003. We verify thatthe signal waveform is consistent with the predictions of general relativity.

Published
2017

44. GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral

Author

Abbott, B, Abbott, Robert, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Affeldt, C, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Altin, Paul, Abbott, B, Abbott, Robert, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Affeldt, C, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, and Altin, Paul

Abstract

On August 17, 2017 at 12:41:04 UTC the Advanced LIGO and Advanced Virgo gravitational-wave detectors made their first observation of a binary neutron star inspiral. The signal, GW170817, was detected with a combined signal-to-noise ratio of 32.4 and a false-alarm-rate estimate of less than one per 8.0 x 10(4) years. We infer the component masses of the binary to be between 0.86 and 2.26 M-circle dot, in agreement with masses of known neutron stars. Restricting the component spins to the range inferred in binary neutron stars, we find the component masses to be in the range 1.17-1.60 M-circle dot, with the total mass of the system 2.74(-0.01)(+0.04) M-circle dot. The source was localized within a sky region of 28 deg(2) (90% probability) and had a luminosity distance of 40(-14)(+8) Mpc, the closest and most precisely localized gravitational-wave signal yet. The association with the gamma-ray burst GRB 170817A, detected by Fermi-GBM 1.7 s after the coalescence, corroborates the hypothesis of a neutron star merger and provides the first direct evidence of a link between these mergers and short gamma-ray bursts. Subsequent identification of transient counterparts across the electromagnetic spectrum in the same location further supports the interpretation of this event as a neutron star merger. This unprecedented joint gravitational and electromagnetic observation provides insight into astrophysics, dense matter, gravitation, and cosmology.

Published
2017

45. Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory

Author

Albert, A., Andre, M., Anghinolfi, M., Ardid, M, Aubert, J. J., Aublin, J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Albert, A., Andre, M., Anghinolfi, M., Ardid, M, Aubert, J. J., Aublin, J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for high-energy neutrinos from the merger in the GeV-EeV energy range using the ANTARES, IceCube, and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within +/- 500 s around the merger time. Additionally, no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for high-energy neutrinos within the 14 day period following the merger, but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The non-detection is consistent with model predictions of short GRBs observed at a large off-axis angle.

Published
2017

46. Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A

Author

Abbott, B, Abbott, Robert, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, B, Abbott, Robert, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

On 2017 August 17, the gravitational-wave event GW170817 was observed by the Advanced LIGO and Virgo detectors, and the gamma-ray burst (GRB) GRB 170817A was observed independently by the Fermi Gamma-ray Burst Monitor, and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory. The probability of the near-simultaneous temporal and spatial observation of GRB 170817A and GW170817 occurring by chance is $5.0\times {10}^{-8}$. We therefore confirm binary neutron star mergers as a progenitor of short GRBs. The association of GW170817 and GRB 170817A provides new insight into fundamental physics and the origin of short GRBs. We use the observed time delay of $(+1.74\pm 0.05)\,{\rm{s}}$ between GRB 170817A and GW170817 to: (i) constrain the difference between the speed of gravity and the speed of light to be between $-3\times {10}^{-15}$ and $+7\times {10}^{-16}$ times the speed of light, (ii) place new bounds on the violation of Lorentz invariance, (iii) present a new test of the equivalence principle by constraining the Shapiro delay between gravitational and electromagnetic radiation. We also use the time delay to constrain the size and bulk Lorentz factor of the region emitting the gamma-rays. GRB 170817A is the closest short GRB with a known distance, but is between 2 and 6 orders of magnitude less energetic than other bursts with measured redshift. A new generation of gamma-ray detectors, and subthreshold searches in existing detectors, will be essential to detect similar short bursts at greater distances. Finally, we predict a joint detection rate for the Fermi Gamma-ray Burst Monitor and the Advanced LIGO and Virgo detectors of 0.1–1.4 per year during the 2018–2019 observing run and 0.3–1.7 per year at design sensitivity.

Published
2017

47. First narrow-band search for continuous gravitational waves from known pulsars in advanced detector data

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana X, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, Richard, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana X, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

Spinning neutron stars asymmetric with respect to their rotation axis are potential sources of continuous gravitational waves for ground-based interferometric detectors. In the case of known pulsars a fully coherent search, based on matched filtering, which uses the position and rotational parameters obtained from electromagnetic observations, can be carried out. Matched filtering maximizes the signal-to-noise (SNR) ratio, but a large sensitivity loss is expected in case of even a very small mismatch between the assumed and the true signal parameters. For this reason, narrow-band analysis methods have been developed, allowing a fully coherent search for gravitational waves from known pulsars over a fraction of a hertz and several spin-down values. In this paper we describe a narrow-band search of 11 pulsars using data from Advanced LIGO's first observing run. Although we have found several initial outliers, further studies show no significant evidence for the presence of a gravitational wave signal. Finally, we have placed upper limits on the signal strain amplitude lower than the spin-down limit for 5 of the 11 targets over the bands searched; in the case of J1813-1749 the spin-down limit has been beaten for the first time. For an additional 3 targets, the median upper limit across the search bands is below the spin-down limit. This is the most sensitive narrow-band search for continuous gravitational waves carried out so far.

Published
2017

48. Estimating the Contribution of Dynamical Ejecta in the Kilonova Associated with GW170817

Author

Abbott, B., Abbott, Robert, Abbott, T., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana, Adya, V., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, B., Abbott, Robert, Abbott, T., Acernese, Fausto, Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, Rana, Adya, V., Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M., Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

The source of the gravitational-wave (GW) signal GW170817, very likely a binary neutron star merger, was also observed electromagnetically, providing the first multi-messenger observations of this type. The two-week-long electromagnetic (EM) counterpart had a signature indicative of an r-process-induced optical transient known as a kilonova. This Letter examines how the mass of the dynamical ejecta can be estimated without a direct electromagnetic observation of the kilonova, using GW measurements and a phenomenological model calibrated to numerical simulations of mergers with dynamical ejecta. Specifically, we apply the model to the binary masses inferred from the GW measurements, and use the resulting mass of the dynamical ejecta to estimate its contribution (without the effects of wind ejecta) to the corresponding kilonova light curves from various models. The distributions of dynamical ejecta mass range between M-ej = 10(-3) - 10(-2) M-circle dot for various equations of state, assuming that the neutron stars are rotating slowly. In addition, we use our estimates of the dynamical ejecta mass and the neutron star merger rates inferred from GW170817 to constrain the contribution of events like this to the r-process element abundance in the Galaxy when ejecta mass from post-merger winds is neglected. We find that if greater than or similar to 10% of the matter dynamically ejected from binary neutron star (BNS) mergers is converted to r-process elements, GW170817-like BNS mergers could fully account for the amount of r-process material observed in the Milky Way.

Published
2017

49. GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence

Author

Abbott, Benjamin P., Abbott, Richard, Abbott, T. D., Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana X, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, Yap, Min Jet, Abbott, Benjamin P., Abbott, Richard, Abbott, T. D., Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, Rana X, Adya, V, Altin, Paul, Chow, Jong, Forsyth, Perry, Kijbunchoo, Nutsinee, Mansell, Georgia, Manske, Michael, McClelland, David, McManus, David, McRae, Terry, Nguyen, Thanh, Rabeling, David, Scott, Susan M, Shaddock, Daniel, Slagmolen, Bram, Ward, Robert, Wette, Karl, and Yap, Min Jet

Abstract

On August 14, 2017 at 10:30:43 UTC, the Advanced Virgo detector and the two Advanced LIGO detectors coherently observed a transient gravitational-wave signal produced by the coalescence of two stellar mass black holes, with a false-alarm rate of less than or similar to 1 in 27 000 years. The signal was observed with a three-detector network matched-filter signal-to-noise ratio of 18. The inferred masses of the initial black holes are 30.5(-3.0)(+5.7)M(circle dot) and 25.3(-4.2)(+2.8) M-circle dot (at the 90% credible level). The luminosity distance of the source is 540(-210)(+130) Mpc, corresponding to a redshift of z = 0.11(-0.04)(+0.03). A network of three detectors improves the sky localization of the source, reducing the area of the 90% credible region from 1160 deg(2) using only the two LIGO detectors to 60 deg(2) using all three detectors. For the first time, we can test the nature of gravitational-wave polarizations from the antenna response of the LIGO-Virgo network, thus enabling a new class of phenomenological tests of gravity.

Published
2017

50. The Southern 1958-02-14

Author

Byington, Charles, Anderson, Cortland, Yates, Janet, Wille, Paul, Schwartz, Carolyn, Foy, M. J., Layton, Sandra, Fox, Jane, Nolen, Mike, Hughes, Tom, Adkins, Curt, Akins, Ron, Shipp, Connie, Auld, Marilyn, Withee, Lianne, Scott, Susan, Hamilton, Leon, Kayser, Ann, Rule, Robert W., Harpole, Leon, Hussey, Bill, Byington, Charles, Anderson, Cortland, Yates, Janet, Wille, Paul, Schwartz, Carolyn, Foy, M. J., Layton, Sandra, Fox, Jane, Nolen, Mike, Hughes, Tom, Adkins, Curt, Akins, Ron, Shipp, Connie, Auld, Marilyn, Withee, Lianne, Scott, Susan, Hamilton, Leon, Kayser, Ann, Rule, Robert W., Harpole, Leon, and Hussey, Bill

Abstract

vol. 71 no. 16, MISS LAKELAND--Mary Jane Blake, Miss Lakeland of 1957, is shown as she places the crown on the new queen, Judith Ann Bradley, who won the title in a recent contest. (p. 1) -- HONORED--Five students were chosen to Florida Southern's Hall of Fame following a stringent screening in which the students were judged on leadership, scholarship, and extra-curricular activities. Left to right are: Richard Kamerling, Amityville, N. Y.; Beverly Tresca, Jacksonville; Sheila Stephen, Mundelein, Ill.; Arlene Levine, Hopatong, N. J.; and Natale Naccarato, Miami Beach. (p. 1). Jane (p. 3) -- 15 MINUTE POSE . . . By Norton Foster (p. 3). FSC 78-YEAR OLD FRESHMAN--Robert Orr, a new freshman although now in his 78th year, poses with two younger members of his class, Nancy Cupp, of Clearwater, left, and Mary Anna Ahrendt, of Bradenton. Orr plans to study food and nutrition, a subject that he has already spend 14 years on in research. Orr is believed to hold the distinction of being one of the oldest college freshmen, if not the oldest, in the United States. (p. 4). LEN RILEY . . . Top freshman (p. 5) -- HAL SMELTZLY . . . Handles baseball (p. 5). JON JOYCE . . . Magazine honeymoon (p. 6)., 1-6

Published
2017

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