GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run
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October 2020 Deirdre Shoemaker, Ph.D. Center for Gravitational Physics Department of Physics University of Texas at Austin Google Scholar
October 2020 Deirdre Shoemaker, Ph.D. Center for Gravitational Physics Department of Physics University of Texas at Austin Google scholar: http://bit.ly/1FIoCFf I. Earned Degrees B.S. Astronomy & Astrophysics 1990-1994 Pennsylvania State University with Honors and Physics Ph.D. Physics 1995-1999 University of Texas at Austin (advisor: R. Matzner) II. Employment History 1999-2002 Postdoctoral Fellow, Center for Gravitational Wave Physics, Penn State (advisor: S. Finn and J. Pullin) 2002-2004 Research Associate, Center for Radiophysics and Space Research, Cornell (advisor: S. Teukolsky) 2004-2008 Assistant Professor, Physics, Penn State 2008-2011 Assistant Professor, Physics, Georgia Institute of Technology 2009-2011 Adjunct Assistant Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2011-2016 Associate Professor, Physics, Georgia Institute of Technology 2011-2016 Adjunct Associate Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2013-2020 Director, Center for Relativistic Astrophysics 2016-2020 Professor, Physics, Georgia Institute of Technology 2016-2020 Adjunct Professor, School of Computational Science and Engineering, Georgia Institute of Technology 2017-2020 Associate Director of Research and Strategic Initiatives, Institute of Data, Engineering and Science, Georgia Institute of Technology 2020-Present Professor, Physics, University of Texas at Austin 2020-Present Director, Center for Gravitational Physics, University of Texas at Austin III. Honors -
Arxiv:2012.00011V2 [Astro-Ph.HE] 20 Dec 2020 Mergers in Gas-Rich Environments (Mckernan Et Al
Draft version December 22, 2020 Preprint typeset using LATEX style emulateapj v. 12/16/11 MASS-GAP MERGERS IN ACTIVE GALACTIC NUCLEI Hiromichi Tagawa1, Bence Kocsis2, Zoltan´ Haiman3, Imre Bartos4, Kazuyuki Omukai1, Johan Samsing5 1Astronomical Institute, Graduate School of Science, Tohoku University, Aoba, Sendai 980-8578, Japan 2 Rudolf Peierls Centre for Theoretical Physics, Clarendon Laboratory, Parks Road, Oxford OX1 3PU, UK 3Department of Astronomy, Columbia University, 550 W. 120th St., New York, NY, 10027, USA 4Department of Physics, University of Florida, PO Box 118440, Gainesville, FL 32611, USA 5Niels Bohr International Academy, The Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen, Denmark Draft version December 22, 2020 ABSTRACT The recently discovered gravitational wave sources GW190521 and GW190814 have shown evidence of BH mergers with masses and spins outside of the range expected from isolated stellar evolution. These merging objects could have undergone previous mergers. Such hierarchical mergers are predicted to be frequent in active galactic nuclei (AGN) disks, where binaries form and evolve efficiently by dynamical interactions and gaseous dissipation. Here we compare the properties of these observed events to the theoretical models of mergers in AGN disks, which are obtained by performing one-dimensional N- body simulations combined with semi-analytical prescriptions. The high BH masses in GW190521 are consistent with mergers of high-generation (high-g) BHs where the initial progenitor stars had high metallicity, 2g BHs if the original progenitors were metal-poor, or 1g BHs that had gained mass via super-Eddington accretion. Other measured properties related to spin parameters in GW190521 are also consistent with mergers in AGN disks. -
Arxiv:1812.04350V2 [Gr-Qc] 16 Jan 2020 PACS Numbers: 04.70.Bw, 04.80.Nn, 95.10.Fh
International Journal of Modern Physics D Testing dispersion of gravitational waves from eccentric extreme-mass-ratio inspirals Shu-Cheng Yang*,y , Wen-Biao Han*,y,x, Shuo Xinz and Chen Zhang*,y *Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, P. R. China ySchool of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, P. R. China zSchool of Physics Sciences and Engineering, Tongji University, Shanghai 200092, P. R. China [email protected] In general relativity, there is no dispersion in gravitational waves, while some modified gravity theories predict dispersion phenomena in the propagation of gravitational waves. In this paper, we demonstrate that this dispersion will induce an observable deviation of waveforms if the orbits have large eccentricities. The mechanism is that the waveform modes with different frequencies will be emitted at the same time due to the existence of eccentricity. During the propagation, because of the dispersion, the arrival time of different modes will be different, then produce the deviation and dephasing of wave- forms compared with general relativity. This kind of dispersion phenomena related with extreme-mass-ratio inspirals could be observed by space-borne detectors, and the con- straint on the graviton mass could be improved . Moreover, we find that the dispersion effect may also be constrained by ground detectors better than the current result if a highly eccentric intermediate-mass-ratio inspirals be observed. Keywords: Gravitational waves; extreme-mass-ratio inspirals; dispersion. arXiv:1812.04350v2 [gr-qc] 16 Jan 2020 PACS numbers: 04.70.Bw, 04.80.Nn, 95.10.Fh 1. -
GW150914: First Results from the Search for Binary Black Hole Coalescence with Advanced LIGO
GW150914: First results from the search for binary black hole coalescence with Advanced LIGO The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Abbott, B.P.; Abbott, R.; Abbott, T.D.; Abernathy, M.R.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R.X.; Adya, V.B. et al. "GW150914: First results from the search for binary black hole coalescence with Advanced LIGO." Physical Review D 93, 122003 (June 2016): 1-21 © 2016 American Physical Society As Published http://dx.doi.org/10.1103/PhysRevD.93.122003 Publisher American Physical Society Version Final published version Citable link http://hdl.handle.net/1721.1/110492 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. PHYSICAL REVIEW D 93, 122003 (2016) GW150914: First results from the search for binary black hole coalescence with Advanced LIGO B. P. Abbott et al.* (LIGO Scientific Collaboration and Virgo Collaboration) (Received 9 March 2016; published 7 June 2016) On September 14, 2015, at 09∶50:45 UTC the two detectors of the Laser Interferometer Gravitational- Wave Observatory (LIGO) simultaneously observed the binary black hole merger GW150914. We report the results of a matched-filter search using relativistic models of compact-object binaries that recovered GW150914 as the most significant event during the coincident observations between the two LIGO detectors from September 12 to October 20, 2015 GW150914 was observed with a matched-filter signal-to- noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203000 years, equivalent to a significance greater than 5.1 σ. -
Stringent Constraints on Neutron-Star Radii from Multimessenger Observations and Nuclear Theory
Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory Collin D. Capano1;2∗, Ingo Tews3, Stephanie M. Brown1;2, Ben Margalit4;5;6, Soumi De6;7, Sumit Kumar1;2, Duncan A. Brown6;7, Badri Krishnan1;2, Sanjay Reddy8;9 1 Albert-Einstein-Institut, Max-Planck-Institut fur¨ Gravitationsphysik, Callinstraße 38, 30167 Hannover, Germany, 2 Leibniz Universitat¨ Hannover, 30167 Hannover, Germany, 3 Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA, 4 Department of Astronomy and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA, 5 NASA Einstein Fellow 6 Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA, 7 Department of Physics, Syracuse University, Syracuse NY 13244, USA, 8 Institute for Nuclear Theory, University of Washington, Seattle, WA 98195-1550, USA, 9 JINA-CEE, Michigan State University, East Lansing, MI, 48823, USA The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints on neutron-star radii by combining multimessenger observations of the binary neutron-star merger GW170817 arXiv:1908.10352v3 [astro-ph.HE] 24 Mar 2020 with nuclear theory that best accounts for density-dependent uncertainties in the equation of state. We construct equations of state constrained by chi- ral effective field theory and marginalize over these using the gravitational- wave observations. Combining this with the electromagnetic observations of the merger remnant that imply the presence of a short-lived hyper-massive 1 neutron star, we find that the radius of a 1:4 M neutron star is R1:4 M = +0:9 11:0−0:6 km (90% credible interval). -
Advanced Virgo: Status of the Detector, Latest Results and Future Prospects
universe Review Advanced Virgo: Status of the Detector, Latest Results and Future Prospects Diego Bersanetti 1,* , Barbara Patricelli 2,3 , Ornella Juliana Piccinni 4 , Francesco Piergiovanni 5,6 , Francesco Salemi 7,8 and Valeria Sequino 9,10 1 INFN, Sezione di Genova, I-16146 Genova, Italy 2 European Gravitational Observatory (EGO), Cascina, I-56021 Pisa, Italy; [email protected] 3 INFN, Sezione di Pisa, I-56127 Pisa, Italy 4 INFN, Sezione di Roma, I-00185 Roma, Italy; [email protected] 5 Dipartimento di Scienze Pure e Applicate, Università di Urbino, I-61029 Urbino, Italy; [email protected] 6 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Italy 7 Dipartimento di Fisica, Università di Trento, Povo, I-38123 Trento, Italy; [email protected] 8 INFN, TIFPA, Povo, I-38123 Trento, Italy 9 Dipartimento di Fisica “E. Pancini”, Università di Napoli “Federico II”, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy; [email protected] 10 INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy * Correspondence: [email protected] Abstract: The Virgo detector, based at the EGO (European Gravitational Observatory) and located in Cascina (Pisa), played a significant role in the development of the gravitational-wave astronomy. From its first scientific run in 2007, the Virgo detector has constantly been upgraded over the years; since 2017, with the Advanced Virgo project, the detector reached a high sensitivity that allowed the detection of several classes of sources and to investigate new physics. This work reports the Citation: Bersanetti, D.; Patricelli, B.; main hardware upgrades of the detector and the main astrophysical results from the latest five years; Piccinni, O.J.; Piergiovanni, F.; future prospects for the Virgo detector are also presented. -
Search for Gravitational Waves from High-Mass-Ratio Compact-Binary Mergers of Stellar Mass and Subsolar Mass Black Holes
PHYSICAL REVIEW LETTERS 126, 021103 (2021) Search for Gravitational Waves from High-Mass-Ratio Compact-Binary Mergers of Stellar Mass and Subsolar Mass Black Holes Alexander H. Nitz * and Yi-Fan Wang (王一帆) Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), D-30167 Hannover, Germany and Leibniz Universität Hannover, D-30167 Hannover, Germany (Received 8 July 2020; accepted 11 December 2020; published 12 January 2021) We present the first search for gravitational waves from the coalescence of stellar mass and subsolar mass 3 black holes with masses between 20–100 M⊙ and 0.01–1 M⊙ð10–10 MJÞ, respectively. The observation of a single subsolar mass black hole would establish the existence of primordial black holes and a possible component of dark matter. We search the ∼164 day of public LIGO data from 2015–2017 when LIGO- Hanford and LIGO-Livingston were simultaneously observing. We find no significant candidate gravitational-wave signals. Using this nondetection, we place a 90% upper limit on the rate of 6 4 −3 −1 30–0.01 M⊙ and 30–0.1 M⊙ mergers at < 1.2 × 10 and < 1.6 × 10 Gpc yr , respectively. If we consider binary formation through direct gravitational-wave braking, this kind of merger would be exceedingly rare if only the lighter black hole were primordial in origin (< 10−4 Gpc−3 yr−1). If both black holes are primordial in origin, we constrain the contribution of 1ð0.1ÞM⊙ black holes to dark matter to < 0.3ð3Þ%. DOI: 10.1103/PhysRevLett.126.021103 Introduction.—The first gravitational wave observation known model which can produce subsolar mass black holes from the merger of black holes was detected on September by conventional formation mechanisms; the observation of 14, 2015 [1]. -
Arxiv:1606.03939V2 [Astro-Ph.HE] 20 Sep 2016 P0(X) and P1(X) for Its Detection Statistic X
Draft version September 21, 2016 Preprint typeset using LATEX style AASTeX6 v. 1.0 SUPPLEMENT: THE RATE OF BINARY BLACK HOLE MERGERS INFERRED FROM ADVANCED LIGO OBSERVATIONS SURROUNDING GW150914 B. P. Abbott,1 yDeceased, May 2015. zDeceased, March 2015. (LIGO Scientific Collaboration and Virgo Collaboration) (and The LIGO Scientific Collaboration and Virgo Collaboration) 1LIGO, California Institute of Technology, Pasadena, CA 91125, USA ABSTRACT Supplemental information for a Letter reporting the rate of binary black hole (BBH) coalescences in- ferred from 16 days of coincident Advanced LIGO observations surrounding the transient gravitational wave (GW) signal GW150914. In that work we reported various rate estimates whose 90% credible 3 1 intervals (CIs) fell in the range 2{600 Gpc− yr− . Here we give details of our method and com- putations, including information about our search pipelines, a derivation of our likelihood function for the analysis, a description of the astrophysical search trigger distribution expected from merging BBHs, details on our computational methods, a description of the effects and our model for calibration uncertainty, and an analytic method of estimating our detector sensitivity that is calibrated to our measurements. The first detection of a gravitational wave (GW) sig- a coincident counterpart in the other detector to form a nal from a merging binary black hole (BBH) system is multiple-detector likelihood ratio. described in Abbott et al.(2016d). Abbott et al.(2016g) Both pipelines rely on an empirical estimate of the reports on inference of the local BBH merger rate from search background, making the assumption that trig- surrounding Advanced LIGO observations. This Sup- gers of terrestrial origin occur independently in the two plement provides supporting material and methodolog- detectors. -
Recent Observations of Gravitational Waves by LIGO and Virgo Detectors
universe Review Recent Observations of Gravitational Waves by LIGO and Virgo Detectors Andrzej Królak 1,2,* and Paritosh Verma 2 1 Institute of Mathematics, Polish Academy of Sciences, 00-656 Warsaw, Poland 2 National Centre for Nuclear Research, 05-400 Otwock, Poland; [email protected] * Correspondence: [email protected] Abstract: In this paper we present the most recent observations of gravitational waves (GWs) by LIGO and Virgo detectors. We also discuss contributions of the recent Nobel prize winner, Sir Roger Penrose to understanding gravitational radiation and black holes (BHs). We make a short introduction to GW phenomenon in general relativity (GR) and we present main sources of detectable GW signals. We describe the laser interferometric detectors that made the first observations of GWs. We briefly discuss the first direct detection of GW signal that originated from a merger of two BHs and the first detection of GW signal form merger of two neutron stars (NSs). Finally we present in more detail the observations of GW signals made during the first half of the most recent observing run of the LIGO and Virgo projects. Finally we present prospects for future GW observations. Keywords: gravitational waves; black holes; neutron stars; laser interferometers 1. Introduction The first terrestrial direct detection of GWs on 14 September 2015, was a milestone Citation: Kro´lak, A.; Verma, P. discovery, and it opened up an entirely new window to explore the universe. The combined Recent Observations of Gravitational effort of various scientists and engineers worldwide working on the theoretical, experi- Waves by LIGO and Virgo Detectors. -
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: Gw170817 and Grb 170817A
GRAVITATIONAL WAVES AND GAMMA-RAYS FROM A BINARY NEUTRON STAR MERGER: GW170817 AND GRB 170817A The gravitational-wave signal GW170817 was detected on August 17, 2017 by the Advanced LIGO and Virgo observatories. This is the first signal thought to be due to the merger of two neutron stars. Only 1.7 seconds after the gravitational-wave signal was detected, the Fermi Gamma-ray Burst Monitor (GBM) and the Anticoincidence Shield for the SPectrometer for the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL SPI-ACS) detected a short gamma-ray burst GRB 170817A. For decades astronomers suspected that short gamma-ray bursts were produced by the merger of two neutron stars or a neutron star and a black hole. The combination of GW170817 and GRB 170817A provides the first direct evidence that colliding neutron stars can indeed produce short gamma-ray bursts. INTRODUCTION FIGURES FROM THE PUBLICATION Gamma-Ray Bursts (GRBs) are some of the most energetic events For more information on the meaning of these figures, see the full publication here. observed in Nature. They typically release as much energy in just a few seconds as our Sun will throughout its 10 billion-year life. They occur approximately once a day and come from random points on the sky. These GRBs can last anywhere from fractions of seconds to thousands of seconds. However, we usually divide them in two groups based roughly on their duration, with the division being at the 2 second mark (although more sophisticated features are also taken into account in the classification). Long GRBs (>2 seconds) are caused by the core-collapse of rapidly rotating massive stars. -
2020-21 LSU Research Magazine, Frontiers
Office of Research & Economic Development ···························· The Constant Pursuit of Discovery | 2020-21 TABLE OF CONTENTS 8 CORONAVIRUS 26 BLACK HOLE 18 EXPEDITION 32 CARBON 22 FOUNTAIN OF YOUTH News Scholarship Recognition 3 Briefs 36 Black and Essential 48 Rainmakers 6 Q&A 40 Feltus Taylor 51 Accolades 45 Microbes 57 Distinguished Research Masters 59 Media Shelf NEWS BRIEFS ABOUT THIS ISSUE LSU Research is published annually by the Office of NEWS Research & Economic Development, Louisiana State University, with editorial offices in 134 David F. Boyd Hall, LSU, Baton Rouge, LA 70803. Any written portion of this Newly Discovered Mineral Named Tracking the Dangers of Vaping publication may be reprinted without permission as long as credit for LSU Research is given. Opinions expressed for LSU Geologist By Sandra Sarr herein do not necessarily reflect those of LSU faculty or administration. By Jonathan Snow When electronic cigarettes made their debut on the market Send correspondence to the Office of Research & Like stars and ships, it is rare about 10 years ago, the general public believed they offered Economic Development at the address above or email a harmless alternative to cigarette smoking. However, that [email protected], call 225-578-5833, and visit us at: for a new mineral to be named lsu.edu/research. For more great research stories, visit: after a living person. However, notion has gone up in smoke as evidence of harmful health lsu.edu/research/news. that honor was accorded effects builds. As of December 2019, more than 2,561 people throughout the U.S. have been hospitalized or died due to lung Louisiana State University and Office of Research to LSU mineralogist Barb & Economic Development Administration Dutrow by the International injuries linked to vaping or e-cigarette use, according to the FROM THE Thomas Galligan, Interim President Mineralogical Association. -
R-Process Nucleosynthesis in Neutron Star Mergers and GW170817
r-Process nucleosynthesis in neutron star mergers and GW170817 Jonas Lippuner July 18, 2018 FRIB and the GW170817 Kilonova FRIB/NSCL/MSU, East Lansing MI Operated by Los Alamos National Security, LLC for the U.S. Department of Energy’s NNSA Los Alamos National Laboratory UNCLASSIFIED LA-UR-18-21867 Outline 1. r-Process nucleosynthesis overview 2. r-Process in neutron star mergers 3. Observational signature and first detection Los Alamos National Laboratory UNCLASSIFIED 3/19/2018 | 2 Solar system abundances Los Alamos National Laboratory UNCLASSIFIED 3/19/2018 | 3 Solar system abundances Los Alamos National Laboratory UNCLASSIFIED 3/19/2018 | 3 The s-process slow neutron capture 90Zr 91Zr 92Zr τ ≪ τ ∼ 2 − 5 89 β− n 10 10 yr Y 84Sr 86Sr 87Sr 88Sr 85Rb 87Rb 78Kr 80Kr 82Kr 83Kr 84Kr 86Kr 79Br 81Br 74Se 76Se 77Se 78Se 80Se 82Se 75As 70Ge 72Ge 73Ge 74Ge 76Ge 69Ga 71Ga 66Zn 67Zn 68Zn 70Zn 65Cu closed neutron shell Los Alamos National Laboratory UNCLASSIFIED 3/19/2018 | 4 The s-process slow neutron capture 90Zr 91Zr 92Zr τ ≪ τ ∼ 2 − 5 89 β− n 10 10 yr Y 84Sr 86Sr 87Sr 88Sr 85Rb 87Rb 78Kr 80Kr 82Kr 83Kr 84Kr 86Kr 79Br 81Br 74Se 76Se 77Se 78Se 80Se 82Se 75As 70Ge 72Ge 73Ge 74Ge 76Ge 69Ga 71Ga 66Zn 67Zn 68Zn 70Zn 65Cu closed neutron shell Los Alamos National Laboratory UNCLASSIFIED 3/19/2018 | 4 The r-process rapid neutron capture 90Zr 91Zr 92Zr τ ≪ τ ∼ n β− 10 ms – 10 s 89Y 84Sr 86Sr 87Sr 88Sr 85Rb 87Rb 78Kr 80Kr 82Kr 83Kr 84Kr 86Kr 79Br 81Br 74Se 76Se 77Se 78Se 80Se 82Se 75As 70Ge 72Ge 73Ge 74Ge 76Ge 69Ga 71Ga 66Zn 67Zn 68Zn 70Zn 65Cu neutron drip