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  1. Article: Fast methods for training Gaussian processes on large datasets.

    Moore, C J / Chua, A J K / Berry, C P L / Gair, J R

    Royal Society open science

    2016  Volume 3, Issue 5, Page(s) 160125

    Abstract: Gaussian process regression (GPR) is a non-parametric Bayesian technique for interpolating or fitting data. The main barrier to further uptake of this powerful tool rests in the computational costs associated with the matrices which arise when dealing ... ...

    Abstract Gaussian process regression (GPR) is a non-parametric Bayesian technique for interpolating or fitting data. The main barrier to further uptake of this powerful tool rests in the computational costs associated with the matrices which arise when dealing with large datasets. Here, we derive some simple results which we have found useful for speeding up the learning stage in the GPR algorithm, and especially for performing Bayesian model comparison between different covariance functions. We apply our techniques to both synthetic and real data and quantify the speed-up relative to using nested sampling to numerically evaluate model evidences.
    Language English
    Publishing date 2016-05-11
    Publishing country England
    Document type Journal Article
    ZDB-ID 2787755-3
    ISSN 2054-5703
    ISSN 2054-5703
    DOI 10.1098/rsos.160125
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  2. Book ; Online: All correlations must die

    Taylor, S. R. / Lentati, L. / Babak, S. / Brem, P. / Gair, J. R. / Sesana, A. / Vecchio, A.

    Assessing the significance of a stochastic gravitational-wave background in pulsar-timing arrays

    2016  

    Abstract: We present two methods for determining the significance of a stochastic gravitational-wave (GW) background affecting a pulsar-timing array, where detection is based on evidence for quadrupolar spatial correlations between pulsars. Rather than ... ...

    Abstract We present two methods for determining the significance of a stochastic gravitational-wave (GW) background affecting a pulsar-timing array, where detection is based on evidence for quadrupolar spatial correlations between pulsars. Rather than constructing noise simulations, we eliminate the GWB spatial correlations in the true datasets to assess detection significance with all real data features intact. In our first method, we perform random phase shifts in the signal-model basis functions. This phase shifting eliminates signal phase coherence between pulsars, while keeping the statistical properties of the pulsar timing residuals intact. We then explore a method to null correlations between pulsars by using a "scrambled" overlap-reduction function in the signal model for the array. This scrambled function is orthogonal to what we expect of a real GW background signal. We demonstrate the efficacy of these methods using Bayesian model selection on a set of simulated datasets that contain a stochastic GW signal, timing noise, undiagnosed glitches, and uncertainties in the Solar system ephemeris. Finally, we introduce an overarching formalism under which these two techniques are naturally linked. These methods are immediately applicable to all current pulsar-timing array datasets, and should become standard tools for future analyses.

    Comment: 14 pages, 8 figures, 1 table. Updated to match published version
    Keywords Astrophysics - Instrumentation and Methods for Astrophysics ; General Relativity and Quantum Cosmology ; High Energy Physics - Experiment
    Subject code 612
    Publishing date 2016-06-29
    Publishing country us
    Document type Book ; Online
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  3. Article ; Online: Second Data Release from the European Pulsar Timing Array: Challenging the Ultralight Dark Matter Paradigm.

    Smarra, Clemente / Goncharov, Boris / Barausse, Enrico / Antoniadis, J / Babak, S / Nielsen, A-S Bak / Bassa, C G / Berthereau, A / Bonetti, M / Bortolas, E / Brook, P R / Burgay, M / Caballero, R N / Chalumeau, A / Champion, D J / Chanlaridis, S / Chen, S / Cognard, I / Desvignes, G /
    Falxa, M / Ferdman, R D / Franchini, A / Gair, J R / Graikou, E / Grießmeier, J-M / Guillemot, L / Guo, Y J / Hu, H / Iraci, F / Izquierdo-Villalba, D / Jang, J / Jawor, J / Janssen, G H / Jessner, A / Karuppusamy, R / Keane, E F / Keith, M J / Kramer, M / Krishnakumar, M A / Lackeos, K / Lee, K J / Liu, K / Liu, Y / Lyne, A G / McKee, J W / Main, R A / Mickaliger, M B / Niţu, I C / Parthasarathy, A / Perera, B B P / Perrodin, D / Petiteau, A / Porayko, N K / Possenti, A / Leclere, H Quelquejay / Samajdar, A / Sanidas, S A / Sesana, A / Shaifullah, G / Speri, L / Spiewak, R / Stappers, B W / Susarla, S C / Theureau, G / Tiburzi, C / van der Wateren, E / Vecchio, A / Krishnan, V Venkatraman / Wang, J / Wang, L / Wu, Z

    Physical review letters

    2023  Volume 131, Issue 17, Page(s) 171001

    Abstract: Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar ... ...

    Abstract Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results show that ultralight particles with masses 10^{-24.0}  eV≲m≲10^{-23.3}  eV cannot constitute 100% of the measured local dark matter density, but can have at most local density ρ≲0.3  GeV/cm^{3}.
    Language English
    Publishing date 2023-11-13
    Publishing country United States
    Document type Journal Article
    ZDB-ID 208853-8
    ISSN 1079-7114 ; 0031-9007
    ISSN (online) 1079-7114
    ISSN 0031-9007
    DOI 10.1103/PhysRevLett.131.171001
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  4. Book ; Online: The second data release from the European Pulsar Timing Array II. Customised pulsar noise models for spatially correlated gravitational waves

    Antoniadis, J. / Arumugam, P. / Arumugam, S. / Babak, S. / Bagchi, M. / Nielsen, A. S. Bak / Bassa, C. G. / Bathula, A. / Berthereau, A. / Bonetti, M. / Bortolas, E. / Brook, P. R. / Burgay, M. / Caballero, R. N. / Chalumeau, A. / Champion, D. J. / Chanlaridis, S. / Chen, S. / Cognard, I. /
    Dandapat, S. / Deb, D. / Desai, S. / Desvignes, G. / Dhanda-Batra, N. / Dwivedi, C. / Falxa, M. / Ferdman, R. D. / Franchini, A. / Gair, J. R. / Goncharov, B. / Gopakumar, A. / Graikou, E. / Grießmeier, J. -M. / Guillemot, L. / Guo, Y. J. / Gupta, Y. / Hisano, S. / Hu, H. / Iraci, F. / Izquierdo-Villalba, D. / Jang, J. / Jawor, J. / Janssen, G. H. / Jessner, A. / Joshi, B. C. / Kareem, F. / Karuppusamy, R. / Keane, E. F. / Keith, M. J. / Kharbanda, D. / Kikunaga, T. / Kolhe, N. / Kramer, M. / Krishnakumar, M. A. / Lackeos, K. / Lee, K. J. / Liu, K. / Liu, Y. / Lyne, A. G. / McKee, J. W. / Maan, Y. / Main, R. A. / Mickaliger, M. B. / Niţu, I. C. / Nobleson, K. / Paladi, A. K. / Parthasarathy, A. / Perera, B. B. P. / Perrodin, D. / Petiteau, A. / Porayko, N. K. / Possenti, A. / Prabu, T. / Leclere, H. Quelquejay / Rana, P. / Samajdar, A. / Sanidas, S. A. / Sesana, A. / Shaifullah, G. / Singha, J. / Speri, L. / Spiewak, R. / Srivastava, A. / Stappers, B. W. / Surnis, M. / Susarla, S. C. / Susobhanan, A. / Takahashi, K. / Tarafdar, P. / Theureau, G. / Tiburzi, C. / van der Wateren, E. / Vecchio, A. / Krishnan, V. Venkatraman / Verbiest, J. P. W. / Wang, J. / Wang, L. / Wu, Z.

    2023  

    Abstract: The nanohertz gravitational wave background (GWB) is expected to be an aggregate signal of an ensemble of gravitational waves emitted predominantly by a large population of coalescing supermassive black hole binaries in the centres of merging galaxies. ... ...

    Abstract The nanohertz gravitational wave background (GWB) is expected to be an aggregate signal of an ensemble of gravitational waves emitted predominantly by a large population of coalescing supermassive black hole binaries in the centres of merging galaxies. Pulsar timing arrays, ensembles of extremely stable pulsars, are the most precise experiments capable of detecting this background. However, the subtle imprints that the GWB induces on pulsar timing data are obscured by many sources of noise. These must be carefully characterized to increase the sensitivity to the GWB. In this paper, we present a novel technique to estimate the optimal number of frequency coefficients for modelling achromatic and chromatic noise and perform model selection. We also incorporate a new model to fit for scattering variations in the pulsar timing package temponest and created realistic simulations of the European Pulsar Timing Array (EPTA) datasets that allowed us to test the efficacy of our noise modelling algorithms. We present an in-depth analysis of the noise properties of 25 millisecond pulsars (MSPs) that form the second data release (DR2) of the EPTA and investigate the effect of incorporating low-frequency data from the Indian PTA collaboration. We use enterprise and temponest packages to compare noise models with those reported with the EPTA DR1. We find that, while in some pulsars we can successfully disentangle chromatic from achromatic noise owing to the wider frequency coverage in DR2, in others the noise models evolve in a more complicated way. We also find evidence of long-term scattering variations in PSR J1600$-$3053. Through our simulations, we identify intrinsic biases in our current noise analysis techniques and discuss their effect on GWB searches. The results presented here directly help improve sensitivity to the GWB and are already being used as part of global PTA efforts.

    Comment: 20 pages, 6 figures, 9 tables
    Keywords Astrophysics - High Energy Astrophysical Phenomena ; Astrophysics - Instrumentation and Methods for Astrophysics
    Subject code 612
    Publishing date 2023-06-28
    Publishing country us
    Document type Book ; Online
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  5. Article ; Online: Limits on Anisotropy in the Nanohertz Stochastic Gravitational Wave Background.

    Taylor, S R / Mingarelli, C M F / Gair, J R / Sesana, A / Theureau, G / Babak, S / Bassa, C G / Brem, P / Burgay, M / Caballero, R N / Champion, D J / Cognard, I / Desvignes, G / Guillemot, L / Hessels, J W T / Janssen, G H / Karuppusamy, R / Kramer, M / Lassus, A /
    Lazarus, P / Lentati, L / Liu, K / Osłowski, S / Perrodin, D / Petiteau, A / Possenti, A / Purver, M B / Rosado, P A / Sanidas, S A / Smits, R / Stappers, B / Tiburzi, C / van Haasteren, R / Vecchio, A / Verbiest, J P W

    Physical review letters

    2015  Volume 115, Issue 4, Page(s) 41101

    Abstract: The paucity of observed supermassive black hole binaries (SMBHBs) may imply that the gravitational wave background (GWB) from this population is anisotropic, rendering existing analyses suboptimal. We present the first constraints on the angular ... ...

    Abstract The paucity of observed supermassive black hole binaries (SMBHBs) may imply that the gravitational wave background (GWB) from this population is anisotropic, rendering existing analyses suboptimal. We present the first constraints on the angular distribution of a nanohertz stochastic GWB from circular, inspiral-driven SMBHBs using the 2015 European Pulsar Timing Array data. Our analysis of the GWB in the ~2-90 nHz band shows consistency with isotropy, with the strain amplitude in l>0 spherical harmonic multipoles ≲40% of the monopole value. We expect that these more general techniques will become standard tools to probe the angular distribution of source populations.
    Language English
    Publishing date 2015-07-24
    Publishing country United States
    Document type Journal Article
    ZDB-ID 208853-8
    ISSN 1079-7114 ; 0031-9007
    ISSN (online) 1079-7114
    ISSN 0031-9007
    DOI 10.1103/PhysRevLett.115.041101
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  6. Book ; Online: Comparing recent PTA results on the nanohertz stochastic gravitational wave background

    The International Pulsar Timing Array Collaboration / Agazie, G. / Antoniadis, J. / Anumarlapudi, A. / Archibald, A. M. / Arumugam, P. / Arumugam, S. / Arzoumanian, Z. / Askew, J. / Babak, S. / Bagchi, M. / Bailes, M. / Nielsen, A. -S. Bak / Baker, P. T. / Bassa, C. G. / Bathula, A. / Bécsy, B. / Berthereau, A. / Bhat, N. D. R. /
    Blecha, L. / Bonetti, M. / Bortolas, E. / Brazier, A. / Brook, P. R. / Burgay, M. / Burke-Spolaor, S. / Burnette, R. / Caballero, R. N. / Cameron, A. / Case, R. / Chalumeau, A. / Champion, D. J. / Chanlaridis, S. / Charisi, M. / Chatterjee, S. / Chatziioannou, K. / Cheeseboro, B. D. / Chen, S. / Chen, Z. -C. / Cognard, I. / Cohen, T. / Coles, W. A. / Cordes, J. M. / Cornish, N. J. / Crawford, F. / Cromartie, H. T. / Crowter, K. / Curyło, M. / Cutler, C. J. / Dai, S. / Dandapat, S. / Deb, D. / DeCesar, M. E. / DeGan, D. / Demorest, P. B. / Deng, H. / Desai, S. / Desvignes, G. / Dey, L. / Dhanda-Batra, N. / Di Marco, V. / Dolch, T. / Drachler, B. / Dwivedi, C. / Ellis, J. A. / Falxa, M. / Feng, Y. / Ferdman, R. D. / Ferrara, E. C. / Fiore, W. / Fonseca, E. / Franchini, A. / Freedman, G. E. / Gair, J. R. / Garver-Daniels, N. / Gentile, P. A. / Gersbach, K. A. / Glaser, J. / Good, D. C. / Goncharov, B. / Gopakumar, A. / Graikou, E. / Grießmeier, J. -M. / Guillemot, L. / Gültekin, K. / Guo, Y. J. / Gupta, Y. / Grunthal, K. / Hazboun, J. S. / Hisano, S. / Hobbs, G. B. / Hourihane, S. / Hu, H. / Iraci, F. / Islo, K. / Izquierdo-Villalba, D. / Jang, J. / Jawor, J. / Janssen, G. H. / Jennings, R. J. / Jessner, A. / Johnson, A. D. / Jones, M. L. / Joshi, B. C. / Kaiser, A. R. / Kaplan, D. L. / Kapur, A. / Kareem, F. / Karuppusamy, R. / Keane, E. F. / Keith, M. J. / Kelley, L. Z. / Kerr, M. / Key, J. S. / Kharbanda, D. / Kikunaga, T. / Klein, T. C. / Kolhe, N. / Kramer, M. / Krishnakumar, M. A. / Kulkarni, A. / Laal, N. / Lackeos, K. / Lam, M. T. / Lamb, W. G. / Larsen, B. B. / Lazio, T. J. W. / Lee, K. J. / Levin, Y. / Lewandowska, N. / Littenberg, T. B. / Liu, K. / Liu, T. / Liu, Y. / Lommen, A. / Lorimer, D. R. / Lower, M. E. / Luo, J. / Luo, R. / Lynch, R. S. / Lyne, A. G. / Ma, C. -P. / Maan, Y. / Madison, D. R. / Main, R. A. / Manchester, R. N. / Mandow, R. / Mattson, M. A. / McEwen, A. / McKee, J. W. / McLaughlin, M. A. / McMann, N. / Meyers, B. W. / Meyers, P. M. / Mickaliger, M. B. / Miles, M. / Mingarelli, C. M. F. / Mitridate, A. / Natarajan, P. / Nathan, R. S. / Ng, C. / Nice, D. J. / Niţu, I. C. / Nobleson, K. / Ocker, S. K. / Olum, K. D. / Osłowski, S. / Paladi, A. K. / Parthasarathy, A. / Pennucci, T. T. / Perera, B. B. P. / Perrodin, D. / Petiteau, A. / Petrov, P. / Pol, N. S. / Porayko, N. K. / Possenti, A. / Prabu, T. / Leclere, H. Quelquejay / Radovan, H. A. / Rana, P. / Ransom, S. M. / Ray, P. S. / Reardon, D. J. / Rogers, A. F. / Romano, J. D. / Russell, C. J. / Samajdar, A. / Sanidas, S. A. / Sardesai, S. C. / Schmiedekamp, A. / Schmiedekamp, C. / Schmitz, K. / Schult, L. / Sesana, A. / Shaifullah, G. / Shannon, R. M. / Shapiro-Albert, B. J. / Siemens, X. / Simon, J. / Singha, J. / Siwek, M. S. / Speri, L. / Spiewak, R. / Srivastava, A. / Stairs, I. H. / Stappers, B. W. / Stinebring, D. R. / Stovall, K. / Sun, J. P. / Surnis, M. / Susarla, S. C. / Susobhanan, A. / Swiggum, J. K. / Takahashi, K. / Tarafdar, P. / Taylor, J. / Taylor, S. R. / Theureau, G. / Thrane, E. / Thyagarajan, N. / Tiburzi, C. / Toomey, L. / Turner, J. E. / Unal, C. / Vallisneri, M. / van der Wateren, E. / van Haasteren, R. / Vecchio, A. / Krishnan, V. Venkatraman / Verbiest, J. P. W. / Vigeland, S. J. / Wahl, H. M. / Wang, S. / Wang, Q. / Witt, C. A. / Wang, J. / Wang, L. / Wayt, K. E. / Wu, Z. / Young, O. / Zhang, L. / Zhang, S. / Zhu, X. -J. / Zic, A.

    2023  

    Abstract: The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different ... ...

    Abstract The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTAs that constitute the International Pulsar Timing Array (IPTA). We show that despite making different modeling choices, there is no significant difference in the GWB parameters that are measured by the different PTAs, agreeing within $1\sigma$. The pulsar noise parameters are also consistent between different PTAs for the majority of the pulsars included in these analyses. We bridge the differences in modeling choices by adopting a standardized noise model for all pulsars and PTAs, finding that under this model there is a reduction in the tension in the pulsar noise parameters. As part of this reanalysis, we "extended" each PTA's data set by adding extra pulsars that were not timed by that PTA. Under these extensions, we find better constraints on the GWB amplitude and a higher signal-to-noise ratio for the Hellings and Downs correlations. These extensions serve as a prelude to the benefits offered by a full combination of data across all pulsars in the IPTA, i.e., the IPTA's Data Release 3, which will involve not just adding in additional pulsars, but also including data from all three PTAs where any given pulsar is timed by more than as single PTA.

    Comment: 21 pages, 9 figures, submitted to ApJ
    Keywords Astrophysics - High Energy Astrophysical Phenomena ; General Relativity and Quantum Cosmology
    Subject code 551
    Publishing date 2023-09-01
    Publishing country us
    Document type Book ; Online
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  7. Book ; Online: The International Pulsar Timing Array

    Verbiest, J. P. W. / Lentati, L. / Hobbs, G. / van Haasteren, R. / Demorest, P. B. / Janssen, G. H. / Wang, J. -B. / Desvignes, G. / Caballero, R. N. / Keith, M. J. / Champion, D. J. / Arzoumanian, Z. / Babak, S. / Bassa, C. G. / Bhat, N. D. R. / Brazier, A. / Brem, P. / Burgay, M. / Burke-Spolaor, S. /
    Chamberlin, S. J. / Chatterjee, S. / Christy, B. / Cognard, I. / Cordes, J. M. / Dai, S. / Dolch, T. / Ellis, J. A. / Ferdman, R. D. / Fonseca, E. / Gair, J. R. / Garver-Daniels, N. E. / Gentile, P. / Gonzalez, M. E. / Graikou, E. / Guillemot, L. / Hessels, J. W. T. / Jones, G. / Karuppusamy, R. / Kerr, M. / Kramer, M. / Lam, M. T. / Lasky, P. D. / Lassus, A. / Lazarus, P. / Lazio, T. J. W. / Lee, K. J. / Levin, L. / Liu, K. / Lynch, R. S. / Lyne, A. G. / Mckee, J. / McLaughlin, M. A. / McWilliams, S. T. / Madison, D. R. / Manchester, R. N. / Mingarelli, C. M. F. / Nice, D. J. / Oslowski, S. / Palliyaguru, N. T. / Pennucci, T. T. / Perera, B. B. P. / Perrodin, D. / Possenti, A. / Petiteau, A. / Ransom, S. M. / Reardon, D. / Rosado, P. A. / Sanidas, S. A. / Sesana, A. / Shaifullah, G. / Shannon, R. M. / Siemens, X. / Simon, J. / Smits, R. / Spiewak, R. / Stairs, I. H. / Stappers, B. W. / Stinebring, D. R. / Stovall, K. / Swiggum, J. K. / Taylor, S. R. / Theureau, G. / Tiburzi, C. / Toomey, L. / Vallisneri, M. / van Straten, W. / Vecchio, A. / Wang, Y. / Wen, L. / You, X. P. / Zhu, W. W. / Zhu, X. -J.

    First Data Release

    2016  

    Abstract: The highly stable spin of neutron stars can be exploited for a variety of (astro-)physical investigations. In particular arrays of pulsars with rotational periods of the order of milliseconds can be used to detect correlated signals such as those caused ... ...

    Abstract The highly stable spin of neutron stars can be exploited for a variety of (astro-)physical investigations. In particular arrays of pulsars with rotational periods of the order of milliseconds can be used to detect correlated signals such as those caused by gravitational waves. Three such "Pulsar Timing Arrays" (PTAs) have been set up around the world over the past decades and collectively form the "International" PTA (IPTA). In this paper, we describe the first joint analysis of the data from the three regional PTAs, i.e. of the first IPTA data set. We describe the available PTA data, the approach presently followed for its combination and suggest improvements for future PTA research. Particular attention is paid to subtle details (such as underestimation of measurement uncertainty and long-period noise) that have often been ignored but which become important in this unprecedentedly large and inhomogeneous data set. We identify and describe in detail several factors that complicate IPTA research and provide recommendations for future pulsar timing efforts. The first IPTA data release presented here (and available online) is used to demonstrate the IPTA's potential of improving upon gravitational-wave limits placed by individual PTAs by a factor of ~2 and provides a 2-sigma limit on the dimensionless amplitude of a stochastic GWB of 1.7x10^{-15} at a frequency of 1 yr^{-1}. This is 1.7 times less constraining than the limit placed by (Shannon et al. 2015), due mostly to the more recent, high-quality data they used.

    Comment: 25 pages, 6 tables, 5 figures. Accepted for publication in MNRAS
    Keywords Astrophysics - Instrumentation and Methods for Astrophysics
    Subject code 333
    Publishing date 2016-02-11
    Publishing country us
    Document type Book ; Online
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  8. Article ; Online: Search for Subsolar-Mass Binaries in the First Half of Advanced LIGO's and Advanced Virgo's Third Observing Run.

    Abbott, R / Abbott, T D / Acernese, F / Ackley, K / Adams, C / Adhikari, N / Adhikari, R X / Adya, V B / Affeldt, C / Agarwal, D / Agathos, M / Agatsuma, K / Aggarwal, N / Aguiar, O D / Aiello, L / Ain, A / Ajith, P / Albanesi, S / Allocca, A /
    Altin, P A / Amato, A / Anand, C / Anand, S / Ananyeva, A / Anderson, S B / Anderson, W G / Andrade, T / Andres, N / Andrić, T / Angelova, S V / Ansoldi, S / Antelis, J M / Antier, S / Appert, S / Arai, K / Araya, M C / Areeda, J S / Arène, M / Arnaud, N / Aronson, S M / Arun, K G / Asali, Y / Ashton, G / Assiduo, M / Aston, S M / Astone, P / Aubin, F / Austin, C / Babak, S / Badaracco, F / Bader, M K M / Badger, C / Bae, S / Baer, A M / Bagnasco, S / Bai, Y / Baird, J / Ball, M / Ballardin, G / Ballmer, S W / Balsamo, A / Baltus, G / Banagiri, S / Bankar, D / Barayoga, J C / Barbieri, C / Barish, B C / Barker, D / Barneo, P / Barone, F / Barr, B / Barsotti, L / Barsuglia, M / Barta, D / Bartlett, J / Barton, M A / Bartos, I / Bassiri, R / Basti, A / Bawaj, M / Bayley, J C / Baylor, A C / Bazzan, M / Bécsy, B / Bedakihale, V M / Bejger, M / Belahcene, I / Benedetto, V / Beniwal, D / Bennett, T F / Bentley, J D / BenYaala, M / Bergamin, F / Berger, B K / Bernuzzi, S / Berry, C P L / Bersanetti, D / Bertolini, A / Betzwieser, J / Beveridge, D / Bhandare, R / Bhardwaj, U / Bhattacharjee, D / Bhaumik, S / Bilenko, I A / Billingsley, G / Bini, S / Birney, R / Birnholtz, O / Biscans, S / Bischi, M / Biscoveanu, S / Bisht, A / Biswas, B / Bitossi, M / Bizouard, M-A / Blackburn, J K / Blair, C D / Blair, D G / Blair, R M / Bobba, F / Bode, N / Boer, M / Bogaert, G / Boldrini, M / Bonavena, L D / Bondu, F / Bonilla, E / Bonnand, R / Booker, P / Boom, B A / Bork, R / Boschi, V / Bose, N / Bose, S / Bossilkov, V / Boudart, V / Bouffanais, Y / Bozzi, A / Bradaschia, C / Brady, P R / Bramley, A / Branch, A / Branchesi, M / Brau, J E / Breschi, M / Briant, T / Briggs, J H / Brillet, A / Brinkmann, M / Brockill, P / Brooks, A F / Brooks, J / Brown, D D / Brunett, S / Bruno, G / Bruntz, R / Bryant, J / Bulik, T / Bulten, H J / Buonanno, A / Buscicchio, R / Buskulic, D / Buy, C / Byer, R L / Cadonati, L / Cagnoli, G / Cahillane, C / Bustillo, J Calderón / Callaghan, J D / Callister, T A / Calloni, E / Cameron, J / Camp, J B / Canepa, M / Canevarolo, S / Cannavacciuolo, M / Cannon, K C / Cao, H / Capote, E / Carapella, G / Carbognani, F / Carlin, J B / Carney, M F / Carpinelli, M / Carrillo, G / Carullo, G / Carver, T L / Diaz, J Casanueva / Casentini, C / Castaldi, G / Caudill, S / Cavaglià, M / Cavalier, F / Cavalieri, R / Ceasar, M / Cella, G / Cerdá-Durán, P / Cesarini, E / Chaibi, W / Chakravarti, K / Subrahmanya, S Chalathadka / Champion, E / Chan, C-H / Chan, C / Chan, C L / Chan, K / Chandra, K / Chanial, P / Chao, S / Charlton, P / Chase, E A / Chassande-Mottin, E / Chatterjee, C / Chatterjee, Debarati / Chatterjee, Deep / Chaturvedi, M / Chaty, S / Chatziioannou, K / Chen, H Y / Chen, J / Chen, X / Chen, Y / Chen, Z / Cheng, H / Cheong, C K / Cheung, H Y / Chia, H Y / Chiadini, F / Chiarini, G / Chierici, R / Chincarini, A / Chiofalo, M L / Chiummo, A / Cho, G / Cho, H S / Choudhary, R K / Choudhary, S / Christensen, N / Chu, Q / Chua, S / Chung, K W / Ciani, G / Ciecielag, P / Cieślar, M / Cifaldi, M / Ciobanu, A A / Ciolfi, R / Cipriano, F / Cirone, A / Clara, F / Clark, E N / Clark, J A / Clarke, L / Clearwater, P / Clesse, S / Cleva, F / Coccia, E / Codazzo, E / Cohadon, P-F / Cohen, D E / Cohen, L / Colleoni, M / Collette, C G / Colombo, A / Colpi, M / Compton, C M / Constancio, M / Conti, L / Cooper, S J / Corban, P / Corbitt, T R / Cordero-Carrión, I / Corezzi, S / Corley, K R / Cornish, N / Corre, D / Corsi, A / Cortese, S / Costa, C A / Cotesta, R / Coughlin, M W / Coulon, J-P / Countryman, S T / Cousins, B / Couvares, P / Coward, D M / Cowart, M J / Coyne, D C / Coyne, R / Creighton, J D E / Creighton, T D / Criswell, A W / Croquette, M / Crowder, S G / Cudell, J R / Cullen, T J / Cumming, A / Cummings, R / Cunningham, L / Cuoco, E / Curyło, M / Dabadie, P / Canton, T Dal / Dall'Osso, S / Dálya, G / Dana, A / DaneshgaranBajastani, L M / D'Angelo, B / Danilishin, S / D'Antonio, S / Danzmann, K / Darsow-Fromm, C / Dasgupta, A / Datrier, L E H / Datta, S / Dattilo, V / Dave, I / Davier, M / Davies, G S / Davis, D / Davis, M C / Daw, E J / Dean, R / DeBra, D / Deenadayalan, M / Degallaix, J / De Laurentis, M / Deléglise, S / Del Favero, V / De Lillo, F / De Lillo, N / Del Pozzo, W / DeMarchi, L M / De Matteis, F / D'Emilio, V / Demos, N / Dent, T / Depasse, A / De Pietri, R / De Rosa, R / De Rossi, C / DeSalvo, R / De Simone, R / Dhurandhar, S / Díaz, M C / Diaz-Ortiz, M / Didio, N A / Dietrich, T / Di Fiore, L / Di Fronzo, C / Di Giorgio, C / Di Giovanni, F / Di Giovanni, M / Di Girolamo, T / Di Lieto, A / Ding, B / Di Pace, S / Di Palma, I / Di Renzo, F / Divakarla, A K / Dmitriev, A / Doctor, Z / D'Onofrio, L / Donovan, F / Dooley, K L / Doravari, S / Dorrington, I / Drago, M / Driggers, J C / Drori, Y / Ducoin, J-G / Dupej, P / Durante, O / D'Urso, D / Duverne, P-A / Dwyer, S E / Eassa, C / Easter, P J / Ebersold, M / Eckhardt, T / Eddolls, G / Edelman, B / Edo, T B / Edy, O / Effler, A / Eichholz, J / Eikenberry, S S / Eisenmann, M / Eisenstein, R A / Ejlli, A / Engelby, E / Errico, L / Essick, R C / Estellés, H / Estevez, D / Etienne, Z / Etzel, T / Evans, M / Evans, T M / Ewing, B E / Fafone, V / Fair, H / Fairhurst, S / Farah, A M / Farinon, S / Farr, B / Farr, W M / Farrow, N W / Fauchon-Jones, E J / Favaro, G / Favata, M / Fays, M / Fazio, M / Feicht, J / Fejer, M M / Fekecs, B / Fenyvesi, E / Ferguson, D L / Fernandez-Galiana, A / Ferrante, I / Ferreira, T A / Fidecaro, F / Figura, P / Fiori, I / Fishbach, M / Fisher, R P / Fittipaldi, R / Fiumara, V / Flaminio, R / Floden, E / Fong, H / Font, J A / Fornal, B / Forsyth, P W F / Franke, A / Frasca, S / Frasconi, F / Frederick, C / Freed, J P / Frei, Z / Freise, A / Frey, R / Fritschel, P / Frolov, V V / Fronzé, G G / Fulda, P / Fyffe, M / Gabbard, H A / Gadre, B U / Gair, J R / Gais, J / Galaudage, S / Gamba, R / Ganapathy, D / Ganguly, A / Gaonkar, S G / Garaventa, B / García-Núñez, C / García-Quirós, C / Garufi, F / Gateley, B / Gaudio, S / Gayathri, V / Gemme, G / Gennai, A / George, J / Gerberding, O / Gergely, L / Gewecke, P / Ghonge, S / Ghosh, Abhirup / Ghosh, Archisman / Ghosh, Shaon / Ghosh, Shrobana / Giacomazzo, B / Giacoppo, L / Giaime, J A / Giardina, K D / Gibson, D R / Gier, C / Giesler, M / Giri, P / Gissi, F / Glanzer, J / Gleckl, A E / Godwin, P / Goetz, E / Goetz, R / Gohlke, N / Goncharov, B / González, G / Gopakumar, A / Gosselin, M / Gouaty, R / Gould, D W / Grace, B / Grado, A / Granata, M / Granata, V / Grant, A / Gras, S / Grassia, P / Gray, C / Gray, R / Greco, G / Green, A C / Green, R / Gretarsson, A M / Gretarsson, E M / Griffith, D / Griffiths, W / Griggs, H L / Grignani, G / Grimaldi, A / Grimm, S J / Grote, H / Grunewald, S / Gruning, P / Guerra, D / Guidi, G M / Guimaraes, A R / Guixé, G / Gulati, H K / Guo, H-K / Guo, Y / Gupta, Anchal / Gupta, Anuradha / Gupta, P / Gustafson, E K / Gustafson, R / Guzman, F / Haegel, L / Halim, O / Hall, E D / Hamilton, E Z / Hammond, G / Haney, M / Hanks, J / Hanna, C / Hannam, M D / Hannuksela, O / Hansen, H / Hansen, T J / Hanson, J / Harder, T / Hardwick, T / Haris, K / Harms, J / Harry, G M / Harry, I W / Hartwig, D / Haskell, B / Hasskew, R K / Haster, C-J / Haughian, K / Hayes, F J / Healy, J / Heidmann, A / Heidt, A / Heintze, M C / Heinze, J / Heinzel, J / Heitmann, H / Hellman, F / Hello, P / Helmling-Cornell, A F / Hemming, G / Hendry, M / Heng, I S / Hennes, E / Hennig, J / Hennig, M H / Hernandez, A G / Vivanco, F Hernandez / Heurs, M / Hild, S / Hill, P / Hines, A S / Hochheim, S / Hofman, D / Hohmann, J N / Holcomb, D G / Holland, N A / Hollows, I J / Holmes, Z J / Holt, K / Holz, D E / Hopkins, P / Hough, J / Hourihane, S / Howell, E J / Hoy, C G / Hoyland, D / Hreibi, A / Hsu, Y / Huang, Y / Hübner, M T / Huddart, A D / Hughey, B / Hui, V / Husa, S / Huttner, S H / Huxford, R / Huynh-Dinh, T / Idzkowski, B / Iess, A / Ingram, C / Isi, M / Isleif, K / Iyer, B R / JaberianHamedan, V / Jacqmin, T / Jadhav, S J / Jadhav, S P / James, A L / Jan, A Z / Jani, K / Janquart, J / Janssens, K / Janthalur, N N / Jaranowski, P / Jariwala, D / Jaume, R / Jenkins, A C / Jenner, K / Jeunon, M / Jia, W / Johns, G R / Jones, A W / Jones, D I / Jones, J D / Jones, P / Jones, R / Jonker, R J G / Ju, L / Junker, J / Juste, V / Kalaghatgi, C V / Kalogera, V / Kamai, B / Kandhasamy, S / Kang, G / Kanner, J B / Kao, Y / Kapadia, S J / Kapasi, D P / Karat, S / Karathanasis, C / Karki, S / Kashyap, R / Kasprzack, M / Kastaun, W / Katsanevas, S / Katsavounidis, E / Katzman, W / Kaur, T / Kawabe, K / Kéfélian, F / Keitel, D / Key, J S / Khadka, S / Khalili, F Y / Khan, S / Khazanov, E A / Khetan, N / Khursheed, M / Kijbunchoo, N / Kim, C / Kim, J C / Kim, K / Kim, W S / Kim, Y-M / Kimball, C / Kinley-Hanlon, M / Kirchhoff, R / Kissel, J S / Kleybolte, L / Klimenko, S / Knee, A M / Knowles, T D / Knyazev, E / Koch, P / Koekoek, G / Koley, S / Kolitsidou, P / Kolstein, M / Komori, K / Kondrashov, V / Kontos, A / Koper, N / Korobko, M / Kovalam, M / Kozak, D B / Kringel, V / Krishnendu, N V / Królak, A / Kuehn, G / Kuei, F / Kuijer, P / Kumar, A / Kumar, P / Kumar, Rahul / Kumar, Rakesh / Kuns, K / Kuwahara, S / Lagabbe, P / Laghi, D / Lalande, E / Lam, T L / Lamberts, A / Landry, M / Lane, B B / Lang, R N / Lange, J / Lantz, B / La Rosa, I / Lartaux-Vollard, A / Lasky, P D / Laxen, M / Lazzarini, A / Lazzaro, C / Leaci, P / Leavey, S / Lecoeuche, Y K / Lee, H M / Lee, H W / Lee, J / Lee, K / Lehmann, J / Lemaître, A / Leroy, N / Letendre, N / Levesque, C / Levin, Y / Leviton, J N / Leyde, K / Li, A K Y / Li, B / Li, J / Li, T G F / Li, X / Linde, F / Linker, S D / Linley, J N / Littenberg, T B / Liu, J / Liu, K / Liu, X / Llamas, F / Llorens-Monteagudo, M / Lo, R K L / Lockwood, A / London, L T / Longo, A / Lopez, D / Portilla, M Lopez / Lorenzini, M / Loriette, V / Lormand, M / Losurdo, G / Lott, T P / Lough, J D / Lousto, C O / Lovelace, G / Lucaccioni, J F / Lück, H / Lumaca, D / Lundgren, A P / Lynam, J E / Macas, R / MacInnis, M / Macleod, D M / MacMillan, I A O / Macquet, A / Hernandez, I Magaña / Magazzù, C / Magee, R M / Maggiore, R / Magnozzi, M / Mahesh, S / Majorana, E / Makarem, C / Maksimovic, I / Maliakal, S / Malik, A / Man, N / Mandic, V / Mangano, V / Mango, J L / Mansell, G L / Manske, M / Mantovani, M / Mapelli, M / Marchesoni, F / Marion, F / Mark, Z / Márka, S / Márka, Z / Markakis, C / Markosyan, A S / Markowitz, A / Maros, E / Marquina, A / Marsat, S / Martelli, F / Martin, I W / Martin, R M / Martinez, M / Martinez, V A / Martinez, V / Martinovic, K / Martynov, D V / Marx, E J / Masalehdan, H / Mason, K / Massera, E / Masserot, A / Massinger, T J / Masso-Reid, M / Mastrogiovanni, S / Matas, A / Mateu-Lucena, M / Matichard, F / Matiushechkina, M / Mavalvala, N / McCann, J J / McCarthy, R / McClelland, D E / McClincy, P K / McCormick, S / McCuller, L / McGhee, G I / McGuire, S C / McIsaac, C / McIver, J / McRae, T / McWilliams, S T / Meacher, D / Mehmet, M / Mehta, A K / Meijer, Q / Melatos, A / Melchor, D A / Mendell, G / Menendez-Vazquez, A / Menoni, C S / Mercer, R A / Mereni, L / Merfeld, K / Merilh, E L / Merritt, J D / Merzougui, M / Meshkov, S / Messenger, C / Messick, C / Meyers, P M / Meylahn, F / Mhaske, A / Miani, A / Miao, H / Michaloliakos, I / Michel, C / Middleton, H / Milano, L / Miller, A / Miller, A L / Miller, B / Millhouse, M / Mills, J C / Milotti, E / Minazzoli, O / Minenkov, Y / Mir, Ll M / Miravet-Tenés, M / Mishra, C / Mishra, T / Mistry, T / Mitra, S / Mitrofanov, V P / Mitselmakher, G / Mittleman, R / Mo, Geoffrey / Moguel, E / Mogushi, K / Mohapatra, S R P / Mohite, S R / Molina, I / Molina-Ruiz, M / Mondin, M / Montani, M / Moore, C J / Moraru, D / Morawski, F / More, A / Moreno, C / Moreno, G / Morisaki, S / Mours, B / Mow-Lowry, C M / Mozzon, S / Muciaccia, F / Mukherjee, Arunava / Mukherjee, D / Mukherjee, Soma / Mukherjee, Subroto / Mukherjee, Suvodip / Mukund, N / Mullavey, A / Munch, J / Muñiz, E A / Murray, P G / Musenich, R / Muusse, S / Nadji, S L / Nagar, A / Napolano, V / Nardecchia, I / Naticchioni, L / Nayak, B / Nayak, R K / Neil, B F / Neilson, J / Nelemans, G / Nelson, T J N / Nery, M / Neubauer, P / Neunzert, A / Ng, K Y / Ng, S W S / Nguyen, C / Nguyen, P / Nguyen, T / Nichols, S A / Nissanke, S / Nitoglia, E / Nocera, F / Norman, M / North, C / Nuttall, L K / Oberling, J / O'Brien, B D / O'Dell, J / Oelker, E / Oganesyan, G / Oh, J J / Oh, S H / Ohme, F / Ohta, H / Okada, M A / Olivetto, C / Oram, R / O'Reilly, B / Ormiston, R G / Ormsby, N D / Ortega, L F / O'Shaughnessy, R / O'Shea, E / Ossokine, S / Osthelder, C / Ottaway, D J / Overmier, H / Pace, A E / Pagano, G / Page, M A / Pagliaroli, G / Pai, A / Pai, S A / Palamos, J R / Palashov, O / Palomba, C / Pan, H / Panda, P K / Pang, P T H / Pankow, C / Pannarale, F / Pant, B C / Panther, F H / Paoletti, F / Paoli, A / Paolone, A / Park, H / Parker, W / Pascucci, D / Pasqualetti, A / Passaquieti, R / Passuello, D / Patel, M / Pathak, M / Patricelli, B / Patron, A S / Paul, S / Payne, E / Pedraza, M / Pegoraro, M / Pele, A / Penn, S / Perego, A / Pereira, A / Pereira, T / Perez, C J / Périgois, C / Perkins, C C / Perreca, A / Perriès, S / Petermann, J / Petterson, D / Pfeiffer, H P / Pham, K A / Phukon, K S / Piccinni, O J / Pichot, M / Piendibene, M / Piergiovanni, F / Pierini, L / Pierro, V / Pillant, G / Pillas, M / Pilo, F / Pinard, L / Pinto, I M / Pinto, M / Piotrzkowski, K / Pirello, M / Pitkin, M D / Placidi, E / Planas, L / Plastino, W / Pluchar, C / Poggiani, R / Polini, E / Pong, D Y T / Ponrathnam, S / Popolizio, P / Porter, E K / Poulton, R / Powell, J / Pracchia, M / Pradier, T / Prajapati, A K / Prasai, K / Prasanna, R / Pratten, G / Principe, M / Prodi, G A / Prokhorov, L / Prosposito, P / Prudenzi, L / Puecher, A / Punturo, M / Puosi, F / Puppo, P / Pürrer, M / Qi, H / Quetschke, V / Quitzow-James, R / Raab, F J / Raaijmakers, G / Radkins, H / Radulesco, N / Raffai, P / Rail, S X / Raja, S / Rajan, C / Ramirez, K E / Ramirez, T D / Ramos-Buades, A / Rana, J / Rapagnani, P / Rapol, U D / Ray, A / Raymond, V / Raza, N / Razzano, M / Read, J / Rees, L A / Regimbau, T / Rei, L / Reid, S / Reid, S W / Reitze, D H / Relton, P / Renzini, A / Rettegno, P / Rezac, M / Ricci, F / Richards, D / Richardson, J W / Richardson, L / Riemenschneider, G / Riles, K / Rinaldi, S / Rink, K / Rizzo, M / Robertson, N A / Robie, R / Robinet, F / Rocchi, A / Rodriguez, S / Rolland, L / Rollins, J G / Romanelli, M / Romano, R / Romel, C L / Romero-Rodríguez, A / Romero-Shaw, I M / Romie, J H / Ronchini, S / Rosa, L / Rose, C A / Rosińska, D / Ross, M P / Rowan, S / Rowlinson, S J / Roy, S / Roy, Santosh / Roy, Soumen / Rozza, D / Ruggi, P / Ryan, K / Sachdev, S / Sadecki, T / Sadiq, J / Sakellariadou, M / Salafia, O S / Salconi, L / Saleem, M / Salemi, F / Samajdar, A / Sanchez, E J / Sanchez, J H / Sanchez, L E / Sanchis-Gual, N / Sanders, J R / Sanuy, A / Saravanan, T R / Sarin, N / Sassolas, B / Satari, H / Sathyaprakash, B S / Sauter, O / Savage, R L / Sawant, D / Sawant, H L / Sayah, S / Schaetzl, D / Scheel, M / Scheuer, J / Schiworski, M / Schmidt, P / Schmidt, S / Schnabel, R / Schneewind, M / Schofield, R M S / Schönbeck, A / Schulte, B W / Schutz, B F / Schwartz, E / Scott, J / Scott, S M / Seglar-Arroyo, M / Sellers, D / Sengupta, A S / Sentenac, D / Seo, E G / Sequino, V / Sergeev, A / Setyawati, Y / Shaffer, T / Shahriar, M S / Shams, B / Sharma, A / Sharma, P / Shawhan, P / Shcheblanov, N S / Shikauchi, M / Shoemaker, D H / Shoemaker, D M / ShyamSundar, S / Sieniawska, M / Sigg, D / Singer, L P / Singh, D / Singh, N / Singha, A / Sintes, A M / Sipala, V / Skliris, V / Slagmolen, B J J / Slaven-Blair, T J / Smetana, J / Smith, J R / Smith, R J E / Soldateschi, J / Somala, S N / Son, E J / Soni, K / Soni, S / Sordini, V / Sorrentino, F / Sorrentino, N / Soulard, R / Souradeep, T / Sowell, E / Spagnuolo, V / Spencer, A P / Spera, M / Srinivasan, R / Srivastava, A K / Srivastava, V / Staats, K / Stachie, C / Steer, D A / Steinlechner, J / Steinlechner, S / Stevenson, S / Stops, D J / Stover, M / Strain, K A / Strang, L C / Stratta, G / Strunk, A / Sturani, R / Stuver, A L / Sudhagar, S / Sudhir, V / Suh, H G / Summerscales, T Z / Sun, H / Sun, L / Sunil, S / Sur, A / Suresh, J / Sutton, P J / Swinkels, B L / Szczepańczyk, M J / Szewczyk, P / Tacca, M / Tait, S C / Talbot, C J / Talbot, C / Tanasijczuk, A J / Tanner, D B / Tao, D / Tao, L / Martín, E N Tapia San / Taranto, C / Tasson, J D / Tenorio, R / Terhune, J E / Terkowski, L / Thirugnanasambandam, M P / Thomas, M / Thomas, P / Thompson, J E / Thondapu, S R / Thorne, K A / Thrane, E / Tiwari, Shubhanshu / Tiwari, Srishti / Tiwari, V / Toivonen, A M / Toland, K / Tolley, A E / Tonelli, M / Torres-Forné, A / Torrie, C I / E Melo, I Tosta / Töyrä, D / Trapananti, A / Travasso, F / Traylor, G / Trevor, M / Tringali, M C / Tripathee, A / Troiano, L / Trovato, A / Trozzo, L / Trudeau, R J / Tsai, D S / Tsai, D / Tsang, K W / Tse, M / Tso, R / Tsukada, L / Tsuna, D / Tsutsui, T / Turbang, K / Turconi, M / Ubhi, A S / Udall, R P / Ueno, K / Unnikrishnan, C S / Urban, A L / Utina, A / Vahlbruch, H / Vajente, G / Vajpeyi, A / Valdes, G / Valentini, M / Valsan, V / van Bakel, N / van Beuzekom, M / van den Brand, J F J / Van Den Broeck, C / Vander-Hyde, D C / van der Schaaf, L / van Heijningen, J V / Vanosky, J / van Remortel, N / Vardaro, M / Vargas, A F / Varma, V / Vasúth, M / Vecchio, A / Vedovato, G / Veitch, J / Veitch, P J / Venneberg, J / Venugopalan, G / Verkindt, D / Verma, P / Verma, Y / Veske, D / Vetrano, F / Viceré, A / Vidyant, S / Viets, A D / Vijaykumar, A / Villa-Ortega, V / Vinet, J-Y / Virtuoso, A / Vitale, S / Vo, T / Vocca, H / von Reis, E R G / von Wrangel, J S A / Vorvick, C / Vyatchanin, S P / Wade, L E / Wade, M / Wagner, K J / Walet, R C / Walker, M / Wallace, G S / Wallace, L / Walsh, S / Wang, J Z / Wang, W H 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    Physical review letters

    2022  Volume 129, Issue 6, Page(s) 61104

    Abstract: We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2  M_{⊙} and 1.0  M_{⊙} in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend ...

    Abstract We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2  M_{⊙} and 1.0  M_{⊙} in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend our previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio q≥0.1. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14  yr^{-1}. This implies an upper limit on the merger rate of subsolar binaries in the range [220-24200]  Gpc^{-3} yr^{-1}, depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes in the mass range 0.2  M_{⊙}<m_{PBH}<1.0  M_{⊙} is f_{PBH}≡Ω_{PBH}/Ω_{DM}≲6%. This improves existing constraints on primordial black hole abundance by a factor of ∼3. The other is a dissipative dark matter model, in which fermionic dark matter can collapse and form black holes. The upper limit on the fraction of dark matter black holes depends on the minimum mass of the black holes that can be formed: the most constraining result is obtained at M_{min}=1  M_{⊙}, where f_{DBH}≡Ω_{DBH}/Ω_{DM}≲0.003%. These are the first constraints placed on dissipative dark models by subsolar-mass analyses.<br />
    Language English
    Publishing date 2022-08-28
    Publishing country United States
    Document type Journal Article
    ZDB-ID 208853-8
    ISSN 1079-7114 ; 0031-9007
    ISSN (online) 1079-7114
    ISSN 0031-9007
    DOI 10.1103/PhysRevLett.129.061104
    Database MEDical Literature Analysis and Retrieval System OnLINE

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  9. Article ; Online: GW190521: A Binary Black Hole Merger with a Total Mass of 150  M_{⊙}.

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    Physical review letters

    2021  Volume 125, Issue 10, Page(s) 101102

    Abstract: On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search ... ...

    Abstract On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85_{-14}^{+21}  M_{⊙} and 66_{-18}^{+17}  M_{⊙} (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65  M_{⊙}. We calculate the mass of the remnant to be 142_{-16}^{+28}  M_{⊙}, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3_{-2.6}^{+2.4}  Gpc, corresponding to a redshift of 0.82_{-0.34}^{+0.28}. The inferred rate of mergers similar to GW190521 is 0.13_{-0.11}^{+0.30}  Gpc^{-3} yr^{-1}.
    Language English
    Publishing date 2021-02-08
    Publishing country United States
    Document type Journal Article
    ZDB-ID 208853-8
    ISSN 1079-7114 ; 0031-9007
    ISSN (online) 1079-7114
    ISSN 0031-9007
    DOI 10.1103/PhysRevLett.125.101102
    Database MEDical Literature Analysis and Retrieval System OnLINE

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  10. Article ; Online: Constraints on Cosmic Strings Using Data from the Third Advanced LIGO-Virgo Observing Run.

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    Physical review letters

    2021  Volume 126, Issue 24, Page(s) 241102

    Abstract: We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks, and, for the first time, ...

    Abstract We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks, and, for the first time, kink-kink collisions. A template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension Gμ as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models. Additionally, we develop and test a third model that interpolates between these two models. Our results improve upon the previous LIGO-Virgo constraints on Gμ by 1 to 2 orders of magnitude depending on the model that is tested. In particular, for the one-loop distribution model, we set the most competitive constraints to date: Gμ≲4×10^{-15}. In the case of cosmic strings formed at the end of inflation in the context of grand unified theories, these results challenge simple inflationary models.
    Language English
    Publishing date 2021-07-02
    Publishing country United States
    Document type Journal Article
    ZDB-ID 208853-8
    ISSN 1079-7114 ; 0031-9007
    ISSN (online) 1079-7114
    ISSN 0031-9007
    DOI 10.1103/PhysRevLett.126.241102
    Database MEDical Literature Analysis and Retrieval System OnLINE

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