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The NANOGrav 12.5-year data set: A computationally efficient eccentric binary search pipeline and constraints on an eccentric supermassive binary candidate in 3C 66B

arXiv

引用

arXiv 2023年

作者： Agazie, Gabriella Arzoumanian, Zaven Baker, Paul T. Bécsy, Bence Blecha, Laura Blumer, Harsha Brazier, Adam Brook, Paul R. Burke-Spolaor, Sarah Casey-Clyde, J. Andrew Charisi, Maria Chatterjee, Shami Cheeseboro, Belinda D. Cohen, Tyler Cordes, James M. Cornish, Neil J. Crawford, Fronefield Cromartie, H. Thankful DeCesar, Megan E. Demorest, Paul B. Dey, Lankeswar Dolch, Timothy Ellis, Justin A. Ferdman, Robert D. Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Garver-Daniels, Nate Gentile, Peter A. Glaser, Joseph Good, Deborah C. Gopakumar, Achamveedu Gültekin, Kayhan Hazboun, Jeffrey S. Jennings, Ross J. Johnson, Aaron D. Jones, Megan L. Kaiser, Andrew R. Kaplan, David L. Kelley, Luke Zoltan Key, Joey S. Laal, Nima Lam, Michael T. Lamb, William G. Lazio, T.W. Joseph Lewandowska, Natalia Liu, Tingting Lorimer, Duncan R. Luo, Jing Lynch, Ryan S. Ma, Chung-Pei Madison, Dustin R. McEwen, Alexander McKee, James W. McLaughlin, Maura A. Meyers, Patrick M. Mingarelli, Chiara M.F. Mitridate, Andrea Ng, Cherry Nice, David J. Ocker, Stella Koch Olum, Ken D. Pennucci, Timothy T. Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Romano, Joseph D. Sardesai, Shashwat C. Schmitz, Kai Siemens, Xavier Simon, Joseph Siwek, Magdalena S. Sosa Fiscella, Sophia V. Spiewak, Renée Stairs, Ingrid H. Stinebring, Daniel R. Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph K. Taylor, Stephen R. Turner, Jacob E. Unal, Caner Vallisneri, Michele Vigeland, Sarah J. Witt, Caitlin A. Young, Olivia Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 GreenbeltMD20771 United States Department of Physics and Astronomy Widener University One University Place ChesterPA19013 United States Department of Physics Oregon State University CorvallisOR97331 United States Physics Department University of Florida GainesvilleFL32611 United States Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV26505 United States Cornell Center for Astrophysics and Planetary Science Department of Astronomy Cornell University IthacaNY14853 United States Cornell Center for Advanced Computing Cornell University IthacaNY14853 United States Institute for Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham Birmingham EdgbastonB15 2TT United Kingdom Department of Physics University of Connecticut 196 Auditorium Road U-3046 StorrsCT06269-3046 United States Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place NashvilleTN37235 United States Department of Physics New Mexico Institute of Mining and Technology 801 Leroy Place SocorroNM87801 United States Department of Physics Montana State University BozemanMT59717 United States Department of Physics and Astronomy Franklin & Marshall College P.O. Box 3003 LancasterPA17604 United States George Mason University The Naval Research Laboratory WashingtonDC20375 United States National Radio Astronomy Observatory 1003 Lopezville Rd. SocorroNM87801 United States Department of Physics Hillsdale College 33 E. College Street HillsdaleMI49242 United States Eureka Scientific 2452 Delmer Street Suite 100 Oakland

The radio galaxy 3C 66B has been hypothesized to host a supermassive black hole binary (SMBHB) at its center based on electromagnetic observations. Its apparent 1.05-year period and low redshift (∼ 0.02) make it an interesting testbed to search for low-frequency gravitational waves (GWs) using Pulsar Timing Array (PTA) experiments. This source has been subjected to multiple searches for continuous GWs from a circular SMBHB, resulting in progressively more stringent constraints on its GW amplitude and chirp mass. In this paper, we develop a pipeline for performing Bayesian targeted searches for eccentric SMBHBs in PTA data sets, and test its efficacy by applying it on simulated data sets with varying injected signal strengths. We also search for a realistic eccentric SMBHB source in 3C 66B using the NANOGrav 12.5-year data set employing PTA signal models containing Earth term-only as well as Earth+Pulsar term contributions using this pipeline. Due to limitations in our PTA signal model, we get meaningful results only when the initial eccentricity e0 0.1. We find no evidence for an eccentric SMBHB signal in our data, and therefore place 95% upper limits on the PTA signal amplitude of 88.1 ± 3.7 ns for the Earth term-only and 81.74 ±0.86 ns for the Earth+Pulsar term searches for e0 0.1. Similar 95% upper limits on the chirp mass are (1.98 ± 0.05) × 109 M☉ and (1.81 ± 0.01) × 109 M☉. These upper limits, while less stringent than those calculated from a circular binary search in the NANOGrav 12.5-year data set, are consistent with the SMBHB model of 3C 66B developed from electromagnetic observations. © 2023, CC BY.

关键词： Gravity waves

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The NANOGrav 15 yr Data Set: Harmonic Analysis of the Pulsar Angular Correlations

arXiv

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arXiv 2024年

作者： Agazie, Gabriella Baier, Jeremy G. Baker, Paul T. Bécsy, Bence Blecha, Laura Boddy, Kimberly K. Brazier, Adam Brook, Paul R. Burke-Spolaor, Sarah Burnette, Rand Casey-Clyde, J. Andrew Charisi, Maria Chatterjee, Shami Cohen, Tyler Cordes, James M. Cornish, Neil J. Crawford, Fronefield Cromartie, H. Thankful DeCesar, Megan E. Demorest, Paul B. Deng, Heling Dey, Lankeswar Dolch, Timothy Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Gardiner, Emiko C. Gersbach, Kyle A. Glaser, Joseph Good, Deborah C. Gültekin, Kayhan Hazboun, Jeffrey S. Jennings, Ross J. Johnson, Aaron D. Kaplan, David L. Kelley, Luke Zoltan Key, Joey S. Laal, Nima Lam, Michael T. Lamb, William G. Larsen, Bjorn Lazio, Joseph W.T. Lewandowska, Natalia Liu, Tingting Luo, Jing Lynch, Ryan S. Ma, Chung-Pei Madison, Dustin R. McEwen, Alexander McKee, James W. McLaughlin, Maura A. Meyers, Patrick M. Mingarelli, Chiara M.F. Mitridate, Andrea Nay, Jonathan Nice, David J. Ocker, Stella Koch Olum, Ken D. Pennucci, Timothy T. Petrov, Polina Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Runnoe, Jessie C. Saffer, Alexander Sardesai, Shashwat C. Schmitz, Kai Siemens, Xavier Simon, Joseph Siwek, Magdalena S. Smith, Tristan L. Fiscella, Sophia Sosa V. Stairs, Ingrid H. Stinebring, Daniel R. Susobhanan, Abhimanyu Swiggum, Joseph K. Taylor, Jacob Taylor, Stephen R. Turner, Jacob E. Unal, Caner Vallisneri, Michele van Haasteren, Rutger Verbiest, Joris Vigeland, Sarah J. Witt, Caitlin A. Wright, David Young, Olivia Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States Department of Physics Oregon State University CorvallisOR97331 United States Department of Physics and Astronomy Widener University One University Place ChesterPA19013 United States Physics Department University of Florida GainesvilleFL32611 United States Department of Physics The University of Texas at Austin AustinTX78712 United States Cornell Center for Astrophysics and Planetary Science Department of Astronomy Cornell University IthacaNY14853 United States Cornell Center for Advanced Computing Cornell University IthacaNY14853 United States Institute for Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham Edgbaston BirminghamB15 2TT United Kingdom Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV26505 United States Department of Physics University of Connecticut 196 Auditorium Road U-3046 StorrsCT06269-3046 United States Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place NashvilleTN37235 United States Department of Physics New Mexico Institute of Mining and Technology 801 Leroy Place SocorroNM87801 United States Department of Physics Montana State University BozemanMT59717 United States Department of Physics and Astronomy Franklin & Marshall College P.O. Box 3003 LancasterPA17604 United States National Research Council Research Associate National Academy of Sciences WashingtonDC20001 United States Naval Research Laboratory WashingtonDC20375 United States George Mason University FairfaxVA22030 United States U.S. Naval Research Laboratory WashingtonDC20375 United States National Radio Astronomy Observatory 1003 Lopezville Rd. So

Pulsar timing array observations have found evidence for an isotropic gravitational wave background with the Hellings-Downs angular correlations, expected from general relativity. This interpretation hinges on the measured shape of the angular correlations, which is predominately quadrupolar under general relativity. Here we explore a more flexible parameterization: we expand the angular correlations into a sum of Legendre polynomials and use a Bayesian analysis to constrain their coefficients with the 15-year pulsar timing data set collected by the North American Nanohertz Observatory for Gravitational Waves (NANOGrav). When including Legendre polynomials with multipoles ≥ 2, we only find a significant signal in the quadrupole with an amplitude consistent with general relativity and non-zero at the ∼ 95% confidence level and a Bayes factor of 200. When we include multipoles ≤ 1, the Bayes factor evidence for quadrupole correlations decreases by more than an order of magnitude due to evidence for a monopolar signal at approximately 4 nHz which has also been noted in previous analyses of the NANOGrav 15-year data. Further work needs to be done in order to better characterize the properties of this monopolar signal and its effect on the evidence for quadrupolar angular correlations. © 2024, CC BY.

关键词： Polynomials

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The NANOGrav 15 year Data Set: Removing pulsars one by one from the pulsar timing array

arXiv

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arXiv 2024年

作者： Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne M. Arzoumanian, Zaven Baier, Jeremy G. Baker, Paul T. Bécsy, Bence Blecha, Laura Brazier, Adam Brook, Paul R. Burke-Spolaor, Sarah Casey-Clyde, J. Andrew Charisi, Maria Chatterjee, Shami Cohen, Tyler Cordes, James M. Cornish, Neil J. Crawford, Fronefield Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan E. Demorest, Paul B. Deng, Heling Dey, Lankeswar Dolch, Timothy Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Gardiner, Emiko C. Garver-Daniels, Nate Gentile, Peter A. Gersbach, Kyle A. Glaser, Joseph Good, Deborah C. Guertin, Lydia Gültekin, Kayhan Hazboun, Jeffrey S. Jennings, Ross J. Johnson, Aaron D. Jones, Megan L. Kaiser, Andrew R. Kaplan, David L. Kelley, Luke Zoltan Kerr, Matthew Key, Joey S. Laal, Nima Lam, Michael T. Lamb, William G. Larsen, Bjorn Lazio, T.W. Joseph Lewandowska, Natalia Liu, Tingting Lorimer, Duncan R. Luo, Jing Lynch, Ryan S. Ma, Chung-Pei Madison, Dustin R. McEwen, Alexander McKee, James W. McLaughlin, Maura A. McMann, Natasha Meyers, Bradley W. Meyers, Patrick M. Middleton, Hannah Mingarelli, Chiara M.F. Mitridate, Andrea Moore, Christopher J. Ng, Cherry Nice, David J. Ocker, Stella Koch Olum, Ken D. Pennucci, Timothy T. Perera, Benetge B.P. Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Romano, Joseph D. Runnoe, Jessie C. Saffer, Alexander Sardesai, Shashwat C. Schmiedekamp, Ann Schmiedekamp, Carl Schmitz, Kai Shapiro-Albert, Brent J. Siemens, Xavier Simon, Joseph Siwek, Magdalena S. Sosa Fiscella, Sophia V. Stairs, Ingrid H. Stinebring, Daniel R. Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph K. Taylor, Stephen R. Turner, Jacob E. Unal, Caner Vallisneri, Michele Vecchio, Alberto Vigeland, Sarah J. Wahl, Haley M. Witt, Caitlin A. Wright, David Young, Olivia Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States Newcastle University NE1 7RU United Kingdom X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 GreenbeltMD20771 United States Department of Physics Oregon State University CorvallisOR97331 United States Department of Physics and Astronomy Widener University One University Place ChesterPA19013 United States Physics Department University of Florida GainesvilleFL32611 United States Cornell Center for Astrophysics and Planetary Science Department of Astronomy Cornell University IthacaNY14853 United States Cornell Center for Advanced Computing Cornell University IthacaNY14853 United States Institute for Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham Edgbaston BirminghamB15 2TT United Kingdom Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV26505 United States Department of Physics University of Connecticut 196 Auditorium Road U-3046 StorrsCT06269-3046 United States Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place NashvilleTN37235 United States Department of Physics New Mexico Institute of Mining and Technology 801 Leroy Place SocorroNM87801 United States Department of Physics Montana State University BozemanMT59717 United States Department of Physics and Astronomy Franklin & Marshall College P.O. Box 3003 LancasterPA17604 United States National Research Council Research Associate National Academy of Sciences WashingtonDC20001 United States Naval Research Laboratory WashingtonDC20375 United States Department of Physics and Astronomy University of British Columbia 6224 Agricultural Road VancouverBCV6T 1Z1 Cana

Evidence has emerged for a stochastic signal correlated among 67 pulsars within the 15-year pulsar-timing data set compiled by the NANOGrav collaboration. Similar signals have been found in data from the European, Indian, Parkes, and Chinese PTAs. This signal has been interpreted as indicative of the presence of a nanohertz stochastic gravitational wave background. To explore the internal consistency of this result we investigate how the recovered signal strength changes as we remove the pulsars one by one from the data set. We calculate the signal strength using the (noise-marginalized) optimal statistic, a frequentist metric designed to measure correlated excess power in the residuals of the arrival times of the radio pulses. We identify several features emerging from this analysis that were initially unexpected. The significance of these features, however, can only be assessed by comparing the real data to synthetic data sets. After conducting identical analyses on simulated data sets, we do not find anything inconsistent with the presence of a stochastic gravitational wave background in the NANOGrav 15-year data. The methodologies developed here can offer additional tools for application to future, more sensitive data sets. While this analysis provides an internal consistency check of the NANOGrav results, it does not eliminate the necessity for additional investigations that could identify potential systematics or uncover unmodeled physical phenomena in the data. © 2024, CC BY.

关键词： Gravitational effects

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FAIR Principles:Interpretations and Implementation Considerations

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Data Intelligence 2020年第1期2卷 10-29,293-302,322页

作者： Annika Jacobsen Ricardo de Miranda Azevedo Nick Juty Dominique Batista Simon Coles Ronald Cornet Melanie Courtot Merce Crosas Michel Dumontier Chris T.Evelo Carole Goble Giancarlo Guizzardi Karsten Kryger Hansen Ali Hasnain Kristina Hettne Jaap Heringa Rob W.W.Hooft Melanie Imming Keith G.Jeffery Rajaram Kaliyaperumal Martijn GKersloot Christine R.Kirkpatrick Tobias Kuhn Ignasi Labastida Barbara Magagna PeterMcQuilton Natalie Meyers Annalisa Montesanti Mirjam van Reisen Philippe Rocca-Serra Robert Pergl Susanna-Assunta Sansone Luiz Olavo Bonino da Silva Santos Juliane Schneider George Strawn Mark Thompson Andra Waagmeester Tobias Weigel Mark D.Wilkinson Egon L.Willighagen Peter Wittenburg Marco Roos Barend Mons Erik Schultes Leiden University Medical Center Leiden2333 ZAThe Netherlands Institute of Data Science Maastricht UniversityUniversiteitssingel 60Maastricht 6229 ERThe Netherlands Department of Computer Science The University of ManchesterOxford RoadManchester M139PLUK Oxford e-Research Centre Department of Engineering SciencesUniversity of OxfordOxford OX13PJUK School of Chemistry Faculty of Engineering and Physical SciencesUniversity of SouthamptonSO171BJUK Amsterdam UMC University of AmsterdamAmsterdam 1000 GGThe Netherlands European Bioinformatics Institute(EMBL-EBI) HinxtonCambridgeCB101SDUK Harvard University CambridgeMassachusetts 02138USA Department of Bioinformatics–BiGCaT NUTRIMMaastricht UniversityMaastricht 6229 ERThe Netherlands Conceptual and Cognitive Modeling Research Group(CORE) Free University of Bozen-BolzanoBolzano 39100Italy Aalborg University Aalborg DK-9220Denmark Insight Centre for Data Analytics National University of Ireland GalwayH91 TK33Ireland Centre for Digital Scholarship Leiden University LibrariesLeiden2333 ZAThe Netherlands Department of Computer Science Vrije Universiteit AmsterdamDe Boelelaan 11051081 HV AmsterdamThe Netherlands Dutch Techcentre for Life Sciences(DTL) UtrechtThe Netherlands SURF Utrecht 3511 EPThe Netherlands Keith G Jeffery Consultants FaringdonUK Castor EDC Paasheuvelweg 25Wing 5D1105 BPAmsterdamThe Netherlands San Diego Supercomputer Center University of California San DiegoLa JollaCalifornia 92093USA Learning and Research Resources Centre(CRAI) Universitat de Barcelona08007 BarcelonaSpain Environment Agency Austria A-1090 ViennaAustria University of Notre Dame 75004 ParisFrance Health Research Board(HRB) Dublin 2DO2 H638Ireland Liacs Institute of Advanced Computer Science Leiden University2311 GJ LeidenThe Netherlands Czech Technical University in Prague Faculty of Information Technology(FIT CTU)16000 Prague 6Czech Republic GO FAIR International Support&Coordination Office(GFISCO) LeidenThe Netherlands Harvard Catalys

The FAIR principles have been widely cited,endorsed and adopted by a broad range of stakeholders since their publication in *** intention,the 15 FAIR guiding principles do not dictate specific technological implementations,but provide guidance for improving Findability,Accessibility,Interoperability and Reusability of digital *** has likely contributed to the broad adoption of the FAIR principles,because individual stakeholder communities can implement their own FAIR ***,it has also resulted in inconsistent interpretations that carry the risk of leading to incompatible ***,while the FAIR principles are formulated on a high level and may be interpreted and implemented in different ways,for true interoperability we need to support convergence in implementation choices that are widely accessible and(re)-*** introduce the concept of FAIR implementation considerations to assist accelerated global participation and convergence towards accessible,robust,widespread and consistent FAIR *** self-identified stakeholder community may either choose to reuse solutions from existing implementations,or when they spot a gap,accept the challenge to create the needed solution,which,ideally,can be used again by other communities in the ***,we provide interpretations and implementation considerations(choices and challenges)for each FAIR principle.

关键词： FAIR guiding principles FAIR implementation FAIR convergence FAIR communities choices and challenges

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Searching for Gravitational Waves from Cosmological Phase Transitions with the NANOGrav 12.5-Year Dataset

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Physical Review Letters 2021年第25期127卷 251302-251302页

作者： Zaven Arzoumanian Paul T. Baker Harsha Blumer Bence Bécsy Adam Brazier Paul R. Brook Sarah Burke-Spolaor Maria Charisi Shami Chatterjee Siyuan Chen James M. Cordes Neil J. Cornish Fronefield Crawford H. Thankful Cromartie Megan E. DeCesar Paul B. Demorest Timothy Dolch Justin A. Ellis Elizabeth C. Ferrara William Fiore Emmanuel Fonseca Nathan Garver-Daniels Peter A. Gentile Deborah C. Good Jeffrey S. Hazboun A. Miguel Holgado Kristina Islo Ross J. Jennings Megan L. Jones Andrew R. Kaiser David L. Kaplan Luke Zoltan Kelley Joey Shapiro Key Nima Laal Michael T. Lam T. Joseph W. Lazio Vincent S. H. Lee Duncan R. Lorimer Jing Luo Ryan S. Lynch Dustin R. Madison Maura A. McLaughlin Chiara M. F. Mingarelli Andrea Mitridate Cherry Ng David J. Nice Timothy T. Pennucci Nihan S. Pol Scott M. Ransom Paul S. Ray Brent J. Shapiro-Albert Xavier Siemens Joseph Simon Renée Spiewak Ingrid H. Stairs Daniel R. Stinebring Kevin Stovall Jerry P. Sun Joseph K. Swiggum Stephen R. Taylor Jacob E. Turner Michele Vallisneri Sarah J. Vigeland Caitlin A. Witt Kathryn M. Zurek X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 Greenbelt Maryland 20771 USA Department of Physics and Astronomy Widener University One University Place Chester Pennsylvania 19013 USA Department of Physics and Astronomy West Virginia University P.O. Box 6315 Morgantown West Virginia 26506 USA Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building Morgantown West Virginia 26505 USA Department of Physics Montana State University Bozeman Montana 59717 USA Cornell Center for Astrophysics and Planetary Science and Department of Astronomy Cornell University Ithaca New York 14853 USA Cornell Center for Advanced Computing Cornell University Ithaca New York 14853 USA CIFAR Azrieli Global Scholars program CIFAR Toronto Canada Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place Nashville Tennessee 37235 USA Station de Radioastronomie de Nancay Observatoire de Paris Universite PSL CNRS Universite d’Orleans 18330 Nancay France FEMTO-ST Institut de recherche Department of Time and Frequency UBFC and CNRS ENSMM 25030 Besancon France Laboratoire de Physique et Chimie de l’Environment et de l’Espace LPC2E UMR7328 Universite d’Orleans CNRS 45071 Orleans France Department of Physics and Astronomy Franklin & Marshall College P.O. Box 3003 Lancaster Pennsylvania 17604 USA Department of Physics Lafayette College Easton Pennsylvania 18042 USA George Mason University Fairfax Virginia 22030 USA National Radio Astronomy Observatory 1003 Lopezville Road Socorro New Mexico 87801 USA Department of Physics Hillsdale College 33 E. College Street Hillsdale Michigan 49242 USA Eureka Scientific Inc. 2452 Delmer Street Suite 100 Oakland California 94602-3017 Infinia ML 202 Rigsbee Avenue Durham North Carolina 27701 USA Department of Astronomy University of Maryland College Park Maryland 20742 USA Center for Research and Exploration in Space Science and Technolog

We search for a first-order phase transition gravitational wave signal in 45 pulsars from the NANOGrav 12.5-year dataset. We find that the data can be modeled in terms of a strong first order phase transition taking place at temperatures below the electroweak scale. However, we do not observe any strong preference for a phase-transition interpretation of the signal over the standard astrophysical interpretation in terms of supermassive black hole mergers; but we expect to gain additional discriminating power with future datasets, improving the signal to noise ratio and extending the sensitivity window to lower frequencies. An interesting open question is how well gravitational wave observatories could separate such signals.

关键词： First order phase transitions Gravitational wave detection Gravitational wave sources Gravitational waves

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Neutron Imaging for Intermetallic Alloy using a Delay Line Current-Biased Kinetic-Inductance Detector

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Journal of Physics: Conference Series 2021年第1期1975卷

作者： Hiroaki Shishido The Dang Vu Kazuya Aizawa Kenji M. Kojima Tomio Koyama Kenichi Oikawa Masahide Harada Takayuki Oku Kazuhiko Soyama Shigeyuki Miyajima Mutsuo Hidaka Soh Y. Suzuki Manobu M. Tanaka Shuichi Kawamata Takekazu Ishida Department of Physics and Electronics Graduate School of Engineering Osaka Prefecture University Sakai Osaka 599-8531 Japan NanoSquare Research Institute Osaka Prefecture University Sakai Osaka 599-8570 Japan Materials and Life Science Division J-PARC Center Japan Atomic Energy Agency Tokai Ibaraki 319-1195 Japan Centre for Molecular and Materials Science TRIUMF and Stewart Blusson Quantum Matter Institute University of British Columbia Vancouver BC V6T 2A3 and V6T 1Z4 Canada Division of Quantum and Radiation Engineering Osaka Prefecture University Sakai Osaka 599-8570 Japan Advanced ICT Research Institute National Institute of Information and Communications Technology 588-2 Iwaoka Nishi-ku Kobe Hyogo 651-2492 Japan National Institute of Advanced Industrial Science and Technology Tsukuba Ibaraki 305-8568 Japan Computing Research Center Applied Research Laboratory High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan Institute of Particle and Nuclear Studies High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan

The current-biased kinetic-inductance detector (CB-KID) is a solid-state superconducting neutron detector with high spatial and temporal resolutions, and multi-hit tolerance. We demonstrate high temperature operation of CB-KID at 7.9 K with the delay-line method. High temperature operation reduces imaging pixel size by suppressing signal propagation velocity. High spatial neutron transmission image for a mixed metal alloy consisting of heavy elements Sm and Sn is successfully constructed. We also examine the capability of element discrimination imaging based on the resonance dip analysis.

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Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

arXiv

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arXiv 2023年

作者： Falxa, M. Babak, S. Baker, P.T. Bécsy, B. Chalumeau, A. Chen, S. Chen, Z. Cornish, N.J. Guillemot, L. Hazboun, J.S. Mingarelli, C.M.F. Parthasarathy, A. Petiteau, A. Pol, N.S. Sesana, A. Spolaor, S.B. Taylor, S.R. Theureau, G. Vallisneri, M. Vigeland, S.J. Witt, C.A. Zhu, X. Antoniadis, J. Arzoumanian, Z. Bailes, M. Bhat, N.D.R. Blecha, L. Brazier, A. Brook, P.R. Caballero, N. Cameron, A.D. Casey-Clyde, J.A. Champion, D. Charisi, M. Chatterjee, S. Cognard, I. Cordes, J.M. Crawford, F. Cromartie, H.T. Crowter, K. Dai, S. DeCesar, M.E. Demorest, P.B. Desvignes, G. Dolch, T. Drachler, B. Feng, Y. Ferrara, E.C. Fiore, W. Fonseca, E. Garver-Daniels, N. Glaser, J. Goncharov, B. Good, D.C. Griessmeier, J. Guo, Y.J. Gültekin, K. Hobbs, G. Hu, H. Islo, K. Jang, J. Jennings, R.J. Johnson, A.D. Jones, M.L. Kaczmarek, J. Kaiser, A.R. Kaplan, D.L. Keith, M. Kelley, L.Z. Kerr, M. Key, J.S. Laal, N. Lam, M.T. Lamb, W.G. Lazio, T.J.W. Liu, K. Liu, T. Luo, J. Lynch, R.S. Madison, D.R. Main, R. Manchester, R. McEwen, A. McKee, J. McLaughlin, M.A. Ng, C. Nice, D.J. Ocker, S. Olum, K.D. Oslowski, S. Pennucci, T.T. Perera, B.B.P. Perrodin, D. Porayko, N. Possenti, A. Quelquejay-Leclere, H. Ransom, S.M. Ray, P.S. Reardon, D.J. Russell, C.J. Samajdar, A. Sarkissian, J. Schult, L. Shaifullah, G. Shannon, R.M. Shapiro-Albert, B.J. Siemens, X. Simon, J.J. Siwek, M. Smith, T.L. Speri, L. Spiewak, R. Stairs, I.H. Stappers, B. Stinebring, D.R. Swiggum, J.K. Tiburzi, C. Turner, J. Vecchio, A. Verbiest, J.P.W. Wahl, H. Wang, S.Q. Wang, J. Wang, J. Wu, Z. Zhang, L. Zhang, S. Université de Paris CNRS Astroparticule et Cosmologie Paris75013 France Department of Physics and Astronomy Widener University One University Place ChesterPA19013 United States Department of Physics Montana State University BozemanMT59717 United States Dipartimento di Fisica "G. Occhialini" Universitá degli Studi di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy Beijing Normal University Beijing100875 China Station de Radioastronomie de Nançay Observatoire de Paris PSL University CNRS Université d’Orléans Nançay18330 France Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E UMR7328 Université d’Orléans CNRS Orléans45071 France Department of Physics Oregon State University CorvallisOR97331 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Physics University of Connecticut 196 Auditorium Road U-3046 StorrsCT06269-3046 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place NashvilleTN37235 United States INFN Sezione di Milano-Bicocca Piazza della Scienza 3 Milano20126 Italy Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Laboratoire Univers et Théories LUTh Observatoire de Paris Université PSL CNRS Université de Paris Meudon92190 France Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 MilwaukeeWI53201 United States Northwestern University EvanstonIL60208 United States Adler Planet

The International Pulsar Timing Array 2nd data release is the combination of datasets from worldwide collaborations. In this study, we search for continuous waves: gravitational wave signals produced by individual supermassive black hole binaries in the local universe. We consider binaries on circular orbits and neglect the evolution of orbital frequency over the observational span. We find no evidence for such signals and set sky averaged 95% upper limits on their amplitude h95. The most sensitive frequency is 10nHz with ℎ95 = 9.1 × 10−15. We achieved the best upper limit to date at low and high frequencies of the PTA band thanks to improved effective cadence of observations. In our analysis, we have taken into account the recently discovered common red noise process, which has an impact at low frequencies. We also find that the peculiar noise features present in some pulsars data must be taken into account to reduce the false alarm. We show that using custom noise models is essential in searching for continuous gravitational wave signals and setting the upper limit. Copyright © 2023, The Authors. All rights reserved.

关键词： Pulsars

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MITIGATING THE NOISE OF DESI MOCKS USING ANALYTIC CONTROL VARIATES

arXiv

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arXiv 2023年

作者： Hadzhiyska, Boryana White, Martin Chen, Xinyi Garrison, Lehman DeRose, Joseph Padmanabhan, Nikhil Garcia-Quintero, Cristhian Mena-Fernández, Juan Chen, Shi-Fan Seo, Hee-Jong McDonald, Patrick Aguilar, Jessica Ahlen, Steven Brooks, David Claybaugh, Todd de la Macorra, Axel Doel, Peter Font-Ribera, Andreu Forero-Romero, Jaime E. Gontcho, Satya Gontcho A. Honscheid, Klaus Kremin, Anthony Landriau, Martin Manera, Marc Miquel, Ramon Nie, Jundan Palanque-Delabrouille, Nathalie Rezaie, Mehdi Rossi, Graziano Sanchez, Eusebio Schubnell, Michael Tarlé, Gregory Zhou, Zhimin Vargas-Magana, M. Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States University of California Berkeley 110 Sproul Hall #5800 BerkeleyCA94720 United States Department of Physics University of California Berkeley 366 LeConte Hall MC 7300 BerkeleyCA94720-7300 United States Physics Department Yale University P.O. Box 208120 New HavenCT06511 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Scientific Computing Core Flatiron Institute 162 5th United States Department of Physics The University of Texas at Dallas RichardsonTX75080 United States CIEMAT Avenida Complutense 40 MadridE-28040 Spain Institute for Advanced Study 1 Einstein Drive PrincetonNJ08540 United States Department of Physics & Astronomy Ohio University AthensOH45701 United States Physics Dept. Boston University 590 Commonwealth Avenue BostonMA02215 United States Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Instituto de Física Universidad Nacional Autónoma de México Cd. de MéxicoC.P. 04510 Mexico The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Departamento de Física Universidad de los Andes Cra. 1 No. 18A-10 Edificio Ip BogotáCP 111711 Colombia Observatorio Astronómico Universidad de los Andes Cra. 1 No. 18A-10 Edificio H BogotáCP 111711 Colombia Center for Cosmology and AstroParticle Physics The Ohio State University 191 West Woodruff Avenue ColumbusOH43210 United States Department of Physics The Ohio State University 191 West Woodruff Avenue ColumbusOH43210 United States The Ohio State University Columbus43210 OH United States Departament de Física Serra Húnter Universitat Autònoma de Barcelona Bellaterra Barcelona08193 Spain Institució Catalana de Recerca i Estudis Avançats Passeig de Lluís Companys 23 Barcelona08010 Spain National Astronomical Observatories C

In order to address fundamental questions related to the expansion history of the Universe and its primordial nature with the next generation of galaxy experiments, we need to model reliably large-scale structure observables such as the correlation function and the power spectrum. Cosmological N-body simulations provide a reference through which we can test our models, but their output suffers from sample variance on large scales. Fortunately, this is the regime where accurate analytic approximations exist. To reduce the variance, which is key to making optimal use of these simulations, we can leverage the accuracy and precision of such analytic descriptions using Control Variates (CV). The power of control variates stems from utilizing inexpensive but highly correlated surrogates of the statistics one wishes to measure. The stronger the correlation between the surrogate and the statistic of interest, the larger the variance reduction delivered by the method. We apply two control variate formulations to mock catalogs generated in anticipation of upcoming data from the Dark Energy Spectroscopic Instrument (DESI) to test the robustness of its analysis pipeline. Our CV-reduced measurements, of the power spectrum and correlation function, both pre- and post-reconstruction, offer a factor of 5-10 improvement in the measurement error compared with the raw measurements from the DESI mock catalogs. We explore the relevant properties of the galaxy samples that dictate this reduction and comment on the improvements we find on some of the derived quantities relevant to Baryon Acoustic Oscillation (BAO) analysis. We also provide an optimized package for computing the power spectra and other two-point statistics of an arbitrary galaxy catalog as well as a pipeline for obtaining CV-reduced measurements on any of the AbacusSummit cubic box outputs. We make our scripts, notebooks, and benchmark tests against existing software publicly available and report a speed improvement of a f

关键词： Galaxies

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Ctapipe - Prototype Open Event Reconstruction Pipeline for the Cherenkov Telescope Array 38

Ctapipe - Prototype Open Event Reconstruction Pipeline for t...

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Linhoff, Maximilian Beiske, Lukas Biederbeck, Noah Fröse, Stefan Kosack, Karl Nickel, Lukas Abe, K. Abe, S. Acharyya, A. Adam, R. Aguasca-Cabot, A. Agudo, I. Alfaro, J. Alvarez-Crespo, N. Alves Batista, R. Amans, J.-P. Amato, E. Ambrosino, F. Angüner, E.O. Antonelli, L.A. Aramo, C. Arcaro, C. Arrabito, L. Asano, K. Aschersleben, J. Ashkar, H. Augusto Stuani, L. Baack, D. Backes, M. Balazs, C. Balbo, M. Baquero Larriva, A. Barbosa Martins, V. de Almeida, U. Barres Barrio, J.A. Bastieri, D. Batista, P.I. Batkovic, I. Batzofin, R. Baxter, J. Beck, G. Becker Tjus, J. Beiske, L. Belardinelli, D. Benbow, W. Bernardini, E. Bernete Medrano, J. Bernlöhr, K. Berti, A. Beshley, V. Bhattacharjee, P. Bhattacharyya, S. Bi, B. Biederbeck, N. Biland, A. Bissaldi, E. Blanch, O. Blazek, J. Boisson, C. Bolmont, J. Bonnoli, G. Bordas, P. Bosnjak, Z. Bradascio, F. Braiding, C. Bronzini, E. Brose, R. Brown, A.M. Brun, F. Brunelli, G. Bulgarelli, A. Burelli, I. Burmistrov, L. Burton, M. Bylund, T. Calisse, P.G. Campoy-Ordaz, A. Cantlay, B.K. Capalbi, M. Caproni, A. Capuzzo-Dolcetta, R. Carlile, C. Caroff, S. Carosi, A. Carosi, R. Carrasco, M.-S. Cascone, E. Cassol, F. Castrejon, N. Catalani, F. Cerasole, D. Cerruti, M. Chaty, S. Chen, A.W. Chernyakova, M. Chiavassa, A. Chudoba, J. Coimbra Araujo, C.H. Conforti, V. Conte, F. Contreras, J.L. Cossou, C. Costa, A. Costantini, H. Cristofari, P. Cuevas, O. Curtis-Ginsberg, Z. D'Amico, G. D'Ammando, F. Dadina, M. Dalchenko, M. David, L. Davids, I.D. Dazzi, F. De Angelis, A. de Bony de Lavergne, M. De Caprio, V. De Cesare, G. de Gouveia Dal Pino, E.M. De Lotto, B. De Lucia, M. de Menezes, R. de Naurois, M. de Ona Wilhelmi, E. De Simone, N. de Souza, V. del Peral, L. del Valle, M.V. Delagnes, E. Delgado Giler, A.G. Delgado, C. Dell'aiera, M. Della Ceca, R. Della Valle, M. della Volpe, D. Depaoli, D. Dettlaff, A. Di Girolamo, T. Di Piano, A. Di Pierro, F. Di Tria, R. Di Venere, L. Díaz-Bahamondes, C. Dib, C. Diebold, S. Dima, R. Dinesh, A. Djannati-Ataï, A. Djuvsland, J. Department of Physics Tokai University 4-1-1 Kita-Kaname Kanagawa Hiratsuka259-1292 Japan Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa Chiba277-8582 Japan University of Alabama Tuscaloosa Department of Physics and Astronomy Gallalee Hall Box 870324 TuscaloosaAL35487-0324 United States Université Côte d'Azur Observatoire de la Côte d'Azur CNRS Laboratoire Lagrange France Laboratoire Leprince-Ringuet CNRS IN2P3 École polytechnique Institut Polytechnique de Paris Palaiseau91120 France Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Martí i Franquès 1 Barcelona08028 Spain Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía s/n Granada18008 Spain Pontificia Universidad Católica de Chile Av. Libertador Bernardo O'Higgins 340 Santiago Chile IPARCOS-UCM Instituto de Física de Partículas y del Cosmos EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain Instituto de Física Teórica UAM CSIC Departamento de Física Teórica Universidad Autónoma de Madrid c/ Nicolás Cabrera 13-15 Campus de Cantoblanco UAM Madrid28049 Spain LUTH GEPI LERMA Observatoire de Paris Université PSL Université Paris Cité CNRS 5 place Jules Janssen Meudon92190 France INAF Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze50125 Italy INAF Osservatorio Astronomico di Roma Via di Frascati 33 Monteporzio Catone 00040 Italy TÜBITAK Research Institute for Fundamental Sciences Gebze Kocaeli41470 Turkey INFN Sezione di Napoli Via Cintia ed. G Napoli80126 Italy INFN Sezione di Padova Via Marzolo 8 Padova35131 Italy Laboratoire Univers et Particules de Montpellier Université de Montpellier CNRS IN2P3 CC 72 Place Eugène Bataillon 5 MontpellierF-34095 Cedex France Kapteyn Astronomical Institute University of Groningen Landleven 12 Groningen9747 AD Netherlands Instituto de Física de São Carlos Universidade de

The Cherenkov Telescope Array Observatory (CTAO) is the next-generation ground-based gamma-ray observatory currently under construction. It will improve over the current generation of imaging atmospheric Cherenkov telescopes (IACTs) by a factor of five to ten in sensitivity and it will be able to observe the whole sky from a combination of two sites: a northern site in La Palma, Spain, and a southern one in Paranal, Chile. CTAO will also be the first open ground-based gamma-ray observatory. Accordingly, the CTAO data processing pipeline is developed as open-source software and ctapipe will be a core package therein. The event reconstruction pipeline accepts raw data of the telescopes and processes it to produce suitable input for the higher-level science tools. Its primary tasks include reconstructing the physical properties of each recorded air shower and providing the corresponding instrument response functions. ctapipe is a python framework providing algorithms and command-line tools to facilitate raw data calibration, image extraction, image parametrization and event reconstruction. Its current main focus is the analysis of simulated data but it has also been successfully applied for the analysis of data obtained with the CTA prototype telescopes, and first science results have now been obtained by the LST-1 collaboration using ctapipe. A plugin system also allows the processing of nonCTA data. Recent updates, including event reconstruction using machine learning and a new plugin system as well as the roadmap towards a 1.0 release will be presented. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Open source software

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Energy-Resolved Neutron Imaging using a Delay Line Current-Biased Kinetic-Inductance Detector

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Journal of Physics: Conference Series 2020年第1期1590卷

作者： Hiroaki Shishido Kazuma Nishimura The Dang Vu Kenji M. Kojima Tomio Koyama Kenichi Oikawa Masahide Harada Shigeyuki Miyajima Mutsuo Hidaka Takayuki Oku Kazuhiko Soyama Kazuya Aizawa Soh Y. Suzuki Takekazu Ishida Department of Physics and Electronics Graduate School of EngineeringOsaka Prefecture University Sakai Osaka 599-8531 Japan NanoSquare Research Institute Osaka Prefecture University Sakai Osaka 599-8570 Japan Materials and Life Science Division J-PARC Center Japan Atomic Energy Agency Tokai Ibaraki 319-1195 Japan Center for Molecular and Materials Science TRIUMF and Stewart Blusson Quantum Matter Institute University of British Columbia Vancouver BC V6T 2A3 and V6T 1Z4 Canada Division of Quantum and Radiation Engineering Osaka Prefecture University Sakai Osaka 599-8570 Japan Advanced ICT Research Institute National Institute of Information and Communications Technology 588-2 Iwaoka Nishi-ku Kobe Hyogo 651-2492 Japan Advanced Industrial Science and Technology Tsukuba Ibaraki 305-8568 Japan Computing Research Center Applied Research Laboratory High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan

We demonstrate the development of an energy resolved neutron transmission imaging system via a solid-state superconducting detector, called current-biased kinetic-inductance detector (CB-KID). CB-KIDs comprise X and Y superconducting Nb meanderlines with Nb ground plane and a 10B conversion layer, which converts a neutron to two charged particles. High-energy charged particles are able to create quasi-particle hot spots simultaneously in the X and Y meander lines, and thus, the local Cooper pair density in meander lines is reduced temporary. When DC-bias currents are fed into the meander lines, double pairs of voltage pulses are generated at the hot spots and propagate toward both ends of the meander lines as electromagnetic waves. The position of the original hot spot is determined by a difference in arrival times of the two pulses at the two ends for X and Y meander lines, independently. This is so-called the delay-line method, and allows us to reconstruct the two-dimensional neutron transmission image of a test sample with four signal readout lines. We examined the capability of high spatial and energy (wavelength) resolved neutron transmission imaging over the sensor active area of 15 ×15 mm2 for various samples, including biological and metal ones. We also demonstrated the capability for the Bragg edge transmission and an energy-resolved neutron image in which stainless-steel specimens were discriminating from other specimens.

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