DOCSLIB.ORG

The Future of Ground-Based Gravitational-Wave Detectors

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Future of Ground-Based Gravitational-Wave Detectors Penn State Theory Seminar, March 2, 2018 The Future of Ground-based Gravitational-wave Detectors David Reitze LIGO Laboratory California Institute of Technology LIGO-G1800292-v1 LIGO Hanford Observatory LIGO-G1800292 Outline ● Why Make Bigger and Better Detectors? ● Improving Advanced LIGO: A+ ● Exploiting the Existing LIGO Facility Limits: Voyager ● Future ‘3G’ Facilities: Cosmic Explorer and Einstein Telescope 2 LIGO-G1800292 Some of the Questions That Gravitational Waves Can Answer ● Outstanding Questions in Fundamental Physics Black Hole Merger and Ringdown » Is General Relativity the correct theory of gravity? » How does matter behave under extreme conditions? » No Hair Theorem: Are black holes truly bald? ● Outstanding Questions in Astrophysics, Astronomy, Cosmology Image credit: W. Benger » Do compact binary mergers cause GRBs? » What is the supernova mechanism in core-collapse of massive Neutron Star Formation stars? » How many low mass black holes are there in the universe? » Do intermediate mass black holes exist? » How bumpy are neutron stars? » Can we observe populations of weak gravitational wave Image credit: NASA sources? » Can binary inspirals be used as “standard sirens” to measure GW Upper limit map the local Hubble parameter? » Are LIGO/Virgo’s binary black holes a component of Dark Matter? » Do Cosmic Strings Exist? Credit: LIGO Scientific Collaboration3 LIGO-G1800292 LIGO-G1800292 Observing Plans for the Coming 5 Years NOW Abbott, et al., “Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO, Advanced Virgo and KAGRA”, https://arxiv.org/abs/1304.0670 5 LIGO-G1800292 Gravitational-wave Science is Sensitivity Driven 1) We want more Binary Neutron Stars events 3 running at O2 sensitivity 10 running at O3 sensitivity 825X running at aLIGO O4 sensitivity no A+ upgrade Nevents = <R>VT A+ upgrade 230X Where: 102 120X <R> -- average 45X astrophysical rate 1 10 V -- volume of the universe probed Volume x Time (in units of O1) à (Range)3 100 2016 2018 2020 2022 2024 2026 Calendar year T -- coincident observing time à t linear LIGO-G1800292 6 Gravitational-wave Science is Sensitivity Driven Binary Neutron Stars 2) Many sources 3 running at O2 sensitivity 10 running at O3 sensitivity 825X require higher SNR running at aLIGO O4 sensitivity no A+ upgrade A+ upgrade 230X to uncover new astrophysics: 102 120X - tidal disruption in BNS 45X mergers - tests of alternative 101 theories of gravity - Black hole ringdowns Volume x Time (in units of O1) - Stochastic background - Isolated neutron stars 100 2016 2018 2020 2022 2024 2026 - Galactic supernova Calendar year - .... LIGO-G1800292 7 Example: Probing the Neutron Star Equation of State A+ 8 LIGO-G1800292 Improving LIGO: A+ 9 LIGO-G1800292 A+: a Mid-Life Enhancement for Advanced LIGO Comoving Ranges: NSNS 1.4/1.4 M- and BHBH 30/30 M- ● Near term: ‘A+’, O2 data: NSNS 96 Mpc, BHBH 983 Mpc aLIGO design: NSNS 173 Mpc, BHBH 1606 Mpc a mid-scale Aplus design: NSNS 325 Mpc, BHBH 2563 Mpc upgrade of Advanced LIGO Hz] 10-22 » Improvements across all bands ● Projected time -23 scale for A+ 10 operation: 2023 - Strain noise h [1/ 2025 10-24 101 102 103 Frequency (Hz) 10 LIGO-G1800292 The Rationale for A+? ● A+ is an incremental upgrade to aLIGO that can happen in the next 5-7 years ● A+ leverages existing technology and infrastructure, with minimal new investment, and moderate risk ● Target improvement: factor of 1.75* increase in range over aLIGO è A factor of ~ 5 greater CBC event rate ● A+ is a stepping stone to 3G detector technology ● Can be observing within 5 years (possibly late 2022) ● “Scientific breakeven” within 1/2 year of operation ● Incremental cost: a small increment of the aLIGO cost *BBH 30/30 M¤: 1.87x Slide inspiration: Mike Zucker, LIGO Laboratory *BNS 1.4/1.4 M¤: 1.7x LIGO-G1800292 11 Key A+ Upgrades Aplus design curve - NSNS (1.4/1.4 M-) 325 Mpc and BHBH (30/30 M-) 2563 Mpc Quantum Seismic Newtonian Suspension Thermal Reduced Radiation Coating Brownian -22 Pressure via Laser 10 Amplitude ‘Squeezing’ Coating Thermo-optic Substrate Brownian Excess Gas Hz] Total noise Improved Mirror Coatings With Lower Reduced Shot Noise -23 Thermal Noise 10 Via Laser Phase Squeezing Strain [1/ 10-24 101 102 103 Frequency [Hz] 12 LIGO-G1800292 Squeezing: Reducing Quantum Noise • Electromagnetic fields are H. P. Yuen, Phys. Rev. A13, 2226 (1976) C. M. Caves, Phys. Rev. D26, 1817 (1982) quantized: Wu, Kimble, Hall, Wu, PRL (1986) ˆ ˆ ˆ E = X1 cosωt +iX2 sinωt 3.5 dB squeezing Quantum fluctuations exist in the TypicalTypical noisenoise without without squeezing squeezing (1.5X reduced noise) • SqueezingSqueezing-enhanced−enahnced sensitivity sensitivity vacuum state: GEO600 Hz] −21 √ 10 Main Laser Coherent State −22 10 FaradayLIGO H1 Strain Sensitivity [1 / Squeezed Vacuum Isolator Squeezed Vacuum Source x State 2 2.1 dB squeezing (1.27X reduced noise) │E │ −23 Photodiode 10 2 x 3 10 1 10 ϕ Frequency (Hz) Aasi, et al., (LIGO Scientific Collaboration), Nature Physics, 7, 962 (2011); Nature Photonics 7 613 (2013). LIGO-G1800292 13 The Best of Both Worlds: Frequency Dependent Squeezing Squeezed−enhanced aLIGO 18 Quantum−enhanced aLIGO Quantum Noise 16 Coating Brownian −22 14 10 Quantum−enhanced aLIGO Total noise aLIGO quantum noise 12 aLIGO total noise 10 8 Pro.local − 6 Hz] 4 √ MacBook 2 − 0 -2 −23 10 -4 ◦ -6 φ =–2.1 ± 2.3 , ∆γ =39± 43 Hz φ =16.2 ± 1.2◦, ∆γ =–56± 23 Hz -8 ◦ φ =36.4 ± 0.5 , ∆γ =49± 11 Hz -10 φ =67.3 ± 0.2◦, ∆γ =401± 12 Hz Noise relative to coherent vacuum [dB] . ± . ◦ ∆ ± 2012 by lisab on lisabs φ =915 0 2 , γ =–97 17 Hz − -12 Model May -14 − Overall sensitivity improvement -16 2 3 4 10 10 Frequency [Hz] 10 Strain Sensitivity [1/ −24 10 created using gwinc_fig.m on 16 1 2 3 10 10 10 Frequency [Hz] Concept:Oelker, et Kimble, al., “Audio-band Levin, Matsko Frequency-dependent, Thorne, Vyatchanin, Phys.Squeezing”, Rev. D (2001)Phys. Rev. Lett. 116, 041102 (2016). 14 LIGO-G1800292 Thermal Noise in Optical Coatings ω0 Y. Levin Phys. Rev. Δx D 57 659 (1998) 2 > ) ω ( x low Q Δ signal < band ∝ 1/Q high Q ω /ω0 ● Simple picture: kT of energy per mechanical mode, viscous damping ● For coating dominated noise and structural damping: coating thickness coating elastic loss −4 φTiO225 :Ta O =2× 10 2kT d Yʹ Y 5 Slide Credit: B ⎛⎞ 4 10− SfTx (,)≈22φ ⎜⎟+φSiO2 =× Marty Fejer, Stanford π fwY ⎝⎠YYʹ beam radius Compare: Bulk Silica φ ~ 10-6-10-8 LIGO-G1800292 Low-frequency losses in amorphous dielectrics ● Loss mechanism: conventionally associated with low energy excitations (LEEs) » conceptualized as two-level systems (TLS); Distribution of TLSs arising from disordered structure » Simple physical mechanism: bond flopping in amorphous materials, e.g. SiO2 E V 2 E1 Δ Single TLS Distribution of TLSs 2 γ2 ωτ Δ −12γ ωτ ⎛⎞Δ Q−12sech⎛⎞ g ( V ) f ( ) dV d QN= 22sech ⎜⎟ =22 ⎜⎟ ΔΔ YkT1+ ωτ ⎝⎠ kT YkT∫∫1+ ωτ ⎝⎠ kT Figures: B.S. Lunin LIGO-G1800292 Routes to Improved Coatings with Low Thermal Noise ● Goal: 2X – 4X reduction in coating thermal noise ● Ultrastable glasses ● Internal friction of films deposited at high » Glasses prepared by physical vapor deposition show temperatures Ts extraordinary stability » very different from film annealed at same – slower cooling liquid reaches lower energy states temperature » simulations suggest surface liquid layer has orders of » φ ~ 2x10-6 vs ~10-4 magnitude higher mobility than caged particles in solids X. Liu, F. Hellman, et al, Phys. Rev. Lett. liquid annealed 350°C 113, 025503 (2014) deposition temperatures, Ts Challenge: extendable to amorphous oxides? Scalable to commercial coating methods? S. Singh, et al. Nature Mater. 12, 139 (2013); Parisi, Nature Mater. 12, 94 (2013) LIGO-G1800292 17 Routes to Improved Coatings with Low Thermal Noise ● Goal: 2X – 4X reduction in coating thermal noise ● Crystalline coatings » molecular beam epitaxy to generate crystalline GaAs/AlGaAs multilayer » mirror disc lithography and etch, substrate removal, and direct bonding on substrate Challenge: i) Scalability Current state-of-the-art: 75 mm aperture. LIGO needs: > 300 mm (Cost!) ii) Coating uniformity: 10-4 (IBS) vs 10-2 (crystalline) G. D. Cole, W. Zhang, M. J. Martin, J. Ye, and M. Aspelmeyer, Nature Photonics (2013) 18 LIGO-G1800292 Preliminary A+ Schedule ● Possible project start date in early 2020 (paced by funding) ● Installation start date early 2022 Start Finish 2017 2018 2019 2020 2021 2022 2023 2024 LIGO Laboratory 19 LIGO-G1800292 Exploiting the LIGO Observatory Facility Limits: LIGO Voyager 20 LIGO-G1800292 LIGO Voyager Concept ● Voyager Key Technologies » Silicon Mirrors: 200 kg, 45 cm dia., mCZ process » Mirror Coatings: �-Si/SiO2 (�-Si: ~lossless thin film) » Cryogenics: 123 K (zero CTE), radiative (non-contact) cooling » Lasers (2000 nm): P~ 180 W, PARM ~ 2800 kW » Wavefront Compensation: thermally adjustable lenses only (no actuation of test mass) » Photodiode Quantum Efficiency: 80 -> 99% for 2 micron (No change to Advanced LIGO seismic isolation system!) LIGO Laboratory 21 LIGO-G1800292 LIGO Voyager Conceptual Design Sensitivity 22 LIGO-G1800292 Voyager Reach for Compact Binary Mergers ObservedBinaries LIGO-G1800292 Technology: 2 Micron Lasers EU Funded 2 micron laser study ● 2 µm Tm:YAG, Ho:YAG commercial lasers exist » low power/low noise, or high power/ high noise ● Challenge is to make high power/low noise ● Development programs underway by several gravitational wave groups » Decade long program envisioned http://isla-project.eu/ Slide inspiration: Rana Adhikari, LIGO Laboratory LIGO Laboratory 24 LIGO-G1800292 Technology: 200 kg Silicon Mirror ● Main challenges are i) mirror 30 cm size, ii) absorption » Goal: absorbed Power < 3 W; » 3 ppm/cm (FZ): max diameter ~ 20 cm » mCZ from SEH can get » samples acquired, absorption measurements done (< 4 ppm) » SEH Japan will make 45 cm diameter mCZ » how to sequence all of the annealing? Different processes for substrates, coatings.
Load more

Recommended publications
  • Abstracts and Speaker Profiles
    Project: Laser Interferometer Gravitational-Wave Observatory (LIGO) Dr. David Reitze, Executive Director, LIGO Laboratory The Gravitational Wave Astronomical Revolution: India's Emerging Role Abstract: • The past four years have witnessed a revolution in astronomy, enabled by the first detections of gravitational waves from colliding black holes and neutron stars through the direct observation of their gravitational wave emissions by the LIGO and Virgo observatories. These discoveries have profound implications for our understanding of the Universe. Gravitational waves provide unique information about nature's most energetic astrophysical events, revealing insights into the nature of gravity, matter, space, and time that are unobtainable by any other means. In this talk, I will briefly discuss how we detect gravitational waves, how gravitational-wave observatories will revolutionize astronomy in the coming years and decades, and how India is poised to play a key role in the future gravitational wave astronomy. About the Speaker: • David Reitze holds joint positions as the Executive Director of the LIGO Laboratory at the California Institute of Technology and as a Professor of Physics at the University of Florida. His research focuses on the development of gravitational-wave detectors. He received a B.A. in Physics with Honors from Northwestern Univ. and a Ph. D. in Physics from the University of Texas of Austin. He is a Fellow of the American Association for the Advancement of Science, the American Physical Society, and the Optical Society. and was jointly awarded the 2017 US National Academy of Sciences Award for Scientific Discovery for his leadership role in LIGO. He is a member of the international LIGO Scientific Collaboration that received numerous awards for the first direct detection of gravitational waves in 2015, including the Special Breakthrough Prize in Fundamental Physics, the Gruber Prize for Cosmology, the Princess Asturias Award for Scientific and Technical Achievement, and the American Astronomical Society Bruno Rossi Prize.
    [Show full text]
  • Acceptance Speech Kip S. Thorne
    Ceremony of the Doctorate Honoris Causa Award to Prof. Kip S. Thorne Universitat Politècnica de Catalunya•BarcelonaTech (UPC). 25th May 2017. Acceptance Speech Kip S. Thorne Thank you, Enrique, for your much too generous description of me and my contributions to science. This honorary doctorate from the Universitat Politècnica de Catalunya is of great significance to me. It honors, especially, my contributions to LIGO’s discovery of gravitational waves. For this reason, I regard myself as sharing it with the large team of scientists and engineers, whose contributions were essential to our discovery. There are only two types of waves that bring us information about the universe: electromagnetic waves and gravitational waves. They travel at the same speed, but aside from this, they could not be more different. Electromagnetic waves—which include light, infrared waves, microwaves, radio waves, ultraviolet waves, X-rays and gamma rays— these are all oscillations of electric and magnetic fields that travel through space and time. Gravitational waves are oscillations in the fabric of space and time. Galileo Galilei opened up electromagnetic astronomy 400 years ago, when he built a small optical telescope, turned it on the sky, and discovered the four largest moons of Jupiter. We LIGO scientists opened up gravitational astronomy in 2015 when our complex detectors discovered gravitational waves from two colliding black holes, a billion light years from Earth. The efforts that produced these two discoveries could not have been more different. Galileo made his discovery alone, though he built on ideas and technology of others. We LIGO scientists made our discovery through a tight collaboration of more than 1000 scientists and engineers.
    [Show full text]
  • LIGO SCIENTIFIC COLLABORATION LIGO Scientific Collaboration
    LIGO SCIENTIFIC COLLABORATION Document Type LIGO-M-1900084 LIGO Scientific Collaboration Program 2019-2020 The LSC Program Committee: Gabriela Gonzalez,´ Stephen Fairhurst, P. Ajith, Patrick Brady, Alessandra Buonanno, Alessandra Corsi, Peter Fritschel, Bala Iyer, Joey Key, Sergey Klimenko, Brian Lantz, Albert Lazzarini, David McClelland, David Reitze, Keith Riles, Sheila Rowan, Alicia Sintes, Josh Smith WWW: http://www.ligo.org/ Processed with LATEX on 2019/05/30 LIGO Scientific Collaboration Program 2019-2020 Contents 1 Overview 3 1.1 The LIGO Scientific Collaboration’s Scientific Mission . .3 1.2 LSC Science Goals: Gravitational Wave Targets . .4 1.3 LSC Science Goals: Gravitational Wave Astronomy . .5 2 LIGO Scientific Operations and Scientific Results 7 2.1 LIGO Observatory Operations . .7 2.2 LSC Detector Commissioning and Detector Improvement activities . .8 2.3 Detector Calibration and Data Timing . .8 2.4 Operating computing systems and services for modeling, analysis, and interpretation . .9 2.5 Detector Characterization . 10 2.6 The operations of data analysis search, simulation and interpretation pipelines . 10 2.7 LSC Fellows Program . 11 2.8 Development of data analysis tools to search and interpret the gravitational wave data . 12 2.9 Dissemination of LIGO data and scientific results . 13 2.10 Outreach to the public and the scientific community . 14 2.11 A+ Upgrade Project . 15 2.12 LIGO-India . 15 2.13 Roles in LSC organization . 15 3 Advancing frontiers of Gravitational-Wave Astrophysics, Astronomy and Fundamental Physics: Improved Gravitational Wave Detectors 17 3.1 Substrates . 17 3.2 Suspensions and seismic isolation . 18 3.3 Optical Coatings . 18 3.4 Cryogenics .
    [Show full text]
  • Making Waves in Spacetime 22 July 2016, by Barbara K
    Making waves in spacetime 22 July 2016, by Barbara K. Kennedy This gravity-driven merger warped space and sent waves speeding outward, making ripples in the fabric of spacetime. Before the first indication by LIGO, these waves had not ever been detected on Earth. "We now have far more confidence that mergers of two black holes are common in the nearby universe," Hanna said. "Now that we are able to detect gravitational waves, they are going to be a phenomenal source of new information about our galaxy and an entirely new channel for discoveries about the universe." Credit: Michelle Bixby Physicists have concluded that the newly detected gravitational-wave event was produced during the final moments of the merger of two black holes Waves on Earth's oceans move in endless rhythm whose masses were notably smaller than the along sandy beaches. Another kind of wave ripples masses of the black holes whose merger produced to our planet from distant black holes in the LIGO's first detection. This new merger united black universe. holes with masses 14 and 8 times the mass of the sun, producing a spinning black hole that is 21 Less than four months after the historic first-ever times the mass of the sun. detection of gravitational waves, scientists on a team that includes Penn State physicists and "It is very significant that these black holes were astronomers detected another gravitational wave much less massive than those in the first washing over the Earth. detection," said Gabriela Gonzalez, professor of physics and astronomy at Louisiana State "I would never have guessed that we would be so University, spokesperson of the international LIGO fortunate to have not only one, but two definitive Scientific Collaboration (LSC), and a former binary black-hole detections within the first few assistant professor of physics at Penn State.
    [Show full text]
  • Program 2020 – 21
    LIGO-M2000130 PROGRAM 2020 – 21 Image credit: LIGO/Sonoma State University/A. Simonnet LIGO SCIENTIFIC COLLABORATION Document Type LIGO-M2000130-v3 LIGO Scientific Collaboration Program 2020–2021 The LSC Program Committee: Stephen Fairhurst, Stefan Ballmer, P. Ajith, Christopher Berry, Sukanta Bose, Patrick Brady, Alessandra Buonanno, Joey Shapiro Key, Sergey Klimenko, Brian Lantz, Albert Lazzarini, David Ottaway, David Reitze, Sheila Rowan, Jax Sanders, Alicia M. Sintes, Josh Smith WWW: http://www.ligo.org/ Processed with LATEX on 2020/07/08 LIGO Scientific Collaboration Program 2020–2021 Contents 1 Overview 3 1.1 The LIGO Scientific Collaboration’s Scientific Mission . .3 1.2 LSC Science Goals: Gravitational Wave Targets . .4 1.3 LSC Science Goals: Gravitational Wave Astronomy . .5 2 LIGO Scientific Operations and Scientific Results 7 2.1 Observatory Operations . .7 2.2 Detector Commissioning and Detector Improvement activities . .8 2.3 LSC Fellows Program . .9 2.4 Detector Calibration and Data Timing . .9 2.5 Operating computing systems and services for modeling, analysis, and interpretation . 10 2.6 Detector Characterization . 11 2.7 The operations of data analysis search, simulation and interpretation pipelines . 12 2.8 Deliver data analysis tools to search and interpret the gravitational wave data . 13 2.9 Dissemination of LIGO data and scientific results . 14 2.10 Outreach to the public and the scientific community . 16 2.11 A+ Upgrade Project . 17 2.12 LIGO-India . 17 2.13 Post-A+ planning . 18 2.14 Roles in LSC organization . 18 3 Advancing frontiers of Gravitational-Wave Astrophysics, Astronomy and Fundamental Physics: Improved Gravitational Wave Detectors 19 3.1 Substrates .
    [Show full text]
  • Future Ground-Based Gravitational-Wave Observatories: Synergies with Other Scientific Communities
    Future Ground-Based Gravitational-Wave Observatories: Synergies with Other Scientific Communities GWIC April 2021 COMMUNITY NETWORKING SUBCOMMTTEE Michele Punturo, INFN - Perugia, Italy (Co-chair) David Reitze, Caltech, USA (Co-chair) David Shoemaker, MIT, USA STEERING COMMITTEE Michele Punturo, INFN - Perugia, Italy (Co-chair) David Reitze, Caltech, USA (Co-chair) Peter Couvares, Caltech, USA Stavros Katsanevas, European Gravitational Observatory, Italy Takaaki Kajita, University of Tokyo, Japan Vicky Kalogera, Northwestern University, USA Harald Lueck, Albert Einstein Institute, Germany David McClelland, Australian National University, Australia Sheila Rowan, University of Glasgow, UK Gary Sanders, Caltech, USA B.S. Sathyaprakash, Penn State University, USA and Cardiff University, UK David Shoemaker, MIT, USA (Secretary) Jo van den Brand, Nikhef, Netherlands GRAVITATIONAL WAVE INTERNATIONAL COMMITTEE This document was produced by the GWIC 3G Subcommittee and the GWIC 3G Synergies with Scientific Communities Subcommittee Final release, April 2021 Cover: LIGO/Caltech/MIT/Sonoma State (Aurore Simonnet) Contents 1 Introduction ........................................................1 2 Constituencies & Affiliated Communities .......................2 3 Engaging with Constituencies & Communities .................7 4 Summary of Recommendations ................................ 11 1. Introduction Planning for the development of a 3rd generation global gravitational-wave detector array is a multifaceted and complex effort that will necessarily need a high level of community input. Interfacing to extant and new stakeholders in the broader scientific constituencies is absolutely necessary to, first, keep them aware of the activities taking place in the ground-based gravitational-wave community and, second, receive input to inform and evolve the planning. The Community Networking Subcommittee within the GWIC 3G Planning Committee is charged with organizing and facilitating communications between 3rd generation projects and the relevant scientific communities.
    [Show full text]
  • Visiting Associate, California Institute of Technology Maître De Recherche
    November 2014 DAVID HOWARD REITZE Address LIGO Laboratory California Institute of Technology MS 100-36 1200 E. California Avenue Pasadena, CA 91125 Telephone (626) 395-6274 (office); (626) 395-2763 (fax) E-mail [email protected] PROFESSIONAL APPOINTMENTS August 2011-Present Executive Director, LIGO Laboratory California Institute of Technology, Pasadena, CA August 2003-Present Professor of Physics (on long term leave) The University of Florida, Gainesville, FL August 1998-August 2003 Associate Professor of Physics The University of Florida, Gainesville, FL August 1993-July 1998 Assistant Professor of Physics The University of Florida, Gainesville, FL November 1992- August 1993 Physicist, Ultrashort Pulse Laser Group, L Division Lawrence Livermore National Laboratory, Livermore, CA October 1990- October 1992 Postdoctoral Member of Technical Staff Bell Communications Research (Bellcore), Red Bank, NJ AFFILIATE APPOINTMENTS 1996, 2000, 2007-2011 Visiting Associate, California Institute of Technology 2001, 2008 Maître de Recherche, Laboratoire d’Optique Appliquée, Palaiseau, France EDUCATION September 1983 Ph. D. in Physics - December 1990 The University of Texas at Austin, Austin, TX Thesis Advisor: Michael Downer, Professor of Physics Thesis Title: Femtosecond Melting Dynamics in Silicon and Carbon September 1979 B. A. in Physics - June 1983 Northwestern University, Evanston, IL HONORS, AWARDS, SERVICE 2015 Fellow, Optical Society of America (OSA) 2014-present Member, National Research Council Committee on Atomic, Molecular, and Optical
    [Show full text]
  • National Science Foundation LIGO BIOS
    BIOS France Córdova is 14th director of the National Science Foundation. Córdova leads the only government agency charged with advancing all fields of scientific discovery, technological innovation, and STEM education. Córdova has a distinguished resume, including: chair of the Smithsonian Institution’s Board of Regents; president emerita of Purdue University; chancellor of the University of California, Riverside; vice chancellor for research at the University of California, Santa Barbara; NASA’s chief scientist; head of the astronomy and astrophysics department at Penn State; and deputy group leader at Los Alamos National Laboratory. She received her B.A. from Stanford University and her Ph.D. in physics from the California Institute of Technology. Gabriela González is spokesperson for the LIGO Scientific Collaboration. She completed her PhD at Syracuse University in 1995, then worked as a staff scientist in the LIGO group at MIT until 1997, when she joined the faculty at Penn State. In 2001, she joined the faculty at Louisiana State University, where she is a professor of physics and astronomy. The González group’s current research focuses on characterization of the LIGO detector noise, detector calibration, and searching for gravitational waves in the data. In 2007, she was elected a fellow of the American Physical Society for her experimental contributions to the field of gravitational wave detection, her leadership in the analysis of LIGO data for gravitational wave signals, and for her skill in communicating the excitement of physics to students and the public. David Reitze is executive director of the LIGO Laboratory at Caltech. In 1990, he completed his PhD at the University of Texas, Austin, where his research focused on ultrafast laser-matter interactions.
    [Show full text]
  • Stefan W. Ballmer
    Stefan W. Ballmer Curriculum Vitae Department of Physics Phone: +1-315-443-3882 Syracuse University Cell: +1-315-278-1154 Syracuse, NY 13244 Fax: +1-315-443-9103 USA E-mail: [email protected] Citizenship: USA, Switzerland Web: thecollege.syr.edu/people/faculty/ballmer-stefan RECENT AND CURRENT POSITIONS Jun 2016 - Associate Professor of Physics present Syracuse University, Syracuse, NY May 2019 - Visiting Associate Professor of Physics Jun 2019 Institute for Cosmic Ray Research, University of Tokyo, Japan May 2018 - Visiting Associate Professor of Physics Jun 2018 Institute for Cosmic Ray Research, University of Tokyo, Japan May 2017 - Visiting Associate Professor of Physics Jun 2017 University of Tokyo, Japan Jun 2013 - Research leave at the LIGO Hanford Observatory Aug 2014 Commissioning the Advanced LIGO interferometer Aug 2010 - Assistant Professor of Physics May 2016 Syracuse University, Syracuse, NY Dec 2009 - NAOJ Visiting Researcher Aug 2010 National Astronomical Observatory of Japan. Sep 2009 - JSPS Postdoctoral Fellow (Gaikokujin Tokubetsu Kenkyuin) Nov 2009 National Astronomical Observatory of Japan. Jul 2006 - Robert A. Millikan Postdoctoral Fellow Aug 2009 California Institute of Technology, Pasadena, CA EDUCATION Jun 2006 Ph.D. Physics, Massachusetts Institute of Technology (MIT), Cambridge, MA Experimental Astrophysics, Laser Interferometer Gravitational Wave Observatory (LIGO). Apr 2000 Diploma (equivalent to Master of Science), Physics, Swiss Federal Institute of Technology (ETH) Zurich, Switzerland With honor, in Theoretical
    [Show full text]
  • A Brief History of LIGO
    A Brief History of LIGO One hundred years ago, using his recently formulated general relativity theory, Albert Einstein predicted the existence of gravitational waves and described their properties. To Einstein these waves seemed too weak ever to be detected, even for the strongest sources that he could conceive. Over the subsequent decades, our improving knowledge of the universe (black holes, neutron stars, supernovae …) and the march of technology (lasers, computers, solid state electronics, low loss optics….) have changed that. In the 1960s, Joseph Weber at the University of Maryland pioneered the effort to build detectors for gravitational waves, using large cylinders of aluminum that vibrate in response to a passing wave, an approach which broke the ground for the field of gravitational-wave searches. LIGO’s approach, using laser interferometry to monitor the relative motion of freely hanging mirrors, was proposed as a theoretical concept form in 1962 by Michael Gertsenshtein and Vladislav Pustovoit in Moscow Russia, and independently several years later by Weber and by Rainer Weiss in America. In 1967, Weiss investigated a laser interferometer limited at some frequencies by quantum shot noise, and in 1972 he completed the invention of the interferometric gravitational wave detector by identifying all the fundamental noise sources that such a detector must face, and conceiving ways to deal with each of them, and by showing that — at least in principle — these ways could lead to detector sensitivities good enough to detect waves from astrophysical sources. Prototype interferometric gravitational wave detectors (“interferometers”) were built in the late 1960s by Robert Forward and colleagues at Hughes Research Laboratories (with mirrors mounted on a vibration isolated plate rather than free swinging), and in the 1970s (with free swinging mirrors between which light bounced many times) by Weiss at MIT, and then by Hans Billing and colleagues in Garching Germany, and then by Ronald Drever, James Hough and colleagues in Glasgow Scotland.
    [Show full text]
  • Curriculum Vitae – UMD Format
    Peter S. Shawhan Curriculum Vitae – UMD format I. Personal Information Full name: Peter Sven Shawhan UMD UID: 109265683 Address: Physical Sciences Complex (Building 415), room 2120 The University of Maryland College Park, MD 20742-2440 Phone: 301-405-1580 Email: [email protected] Web: http://umdphysics.umd.edu/people/faculty/current/item/472-pshawhan.html Academic Appointments at UMD Professor, July 2017 – present Associate Professor, July 2012 – June 2017 Assistant Professor, May 2006 – June 2012 Administrative Appointments at UMD Associate Chair for Graduate Education, Department of Physics, July 2014 – June 2019 Other Employment Senior Scientist, California Institute of Technology, 2002 – 2006 Millikan Prize Postdoctoral Fellow, California Institute of Technology, 1999 – 2002 Educational Background The University of Chicago, September 1990 – August 1999 . M.S. in Physics, December 1992 . Ph.D. in Physics, December 1999 Dissertation: “Observation of Direct CP Violation in KS,L Decays” Faculty advisor: Prof. Bruce D. Winstein Washington University in St. Louis, August 1986 – May 1990 . A.B. (Physics major, Chemistry and Math minor), summa cum laude, May 1990 Professional Certifications, Licenses, and Memberships Fellow of the American Physical Society Member of the American Astronomical Society Life Member of the International Society on General Relativity and Gravitation Member of the American Association of Physics Teachers 1 II. Research, Scholarly, Creative and/or Professional Activities Notes about authorship conventions: Most of my research has been conducted within large collaborations, and I am a co-author on many papers as a result. The standard practice in these collaborations is to list all active members as authors, strictly alphabetically in most cases, to represent the contributions that all of us have made to the assembly, testing, infrastructure, operation, data analysis and internal review for the experiments and results.
    [Show full text]
  • Unlocking the Secrets of the Universe: Gravitational Waves”
    Gabriela González Written Testimony “Unlocking the Secrets of the Universe: Gravitational Waves” February 24, 2016 Mr. Chairman Smith, Ranking Member Johnson, and Members of the Committee: it is an honor to testify here on behalf of my collaborators. We thank you for your interest in gravitational wave science, and your support of the National Science Foundation funding our research in the US. INTRODUCTION I am Gabriela González, a professor of Physics anD Astronomy at Louisiana State University, and the current spokesperson of the LIGO Scientific Collaboration. My colleague Dr. Reitze has described the exciting science of this discovery. I will describe the role of the international LIGO Scientific Collaboration in current and future research for LIGO, and the contributions of that research to the eDucation and training of the future scientific workforce. THE LIGO SCIENTIFIC COLLABORATION Our charter Defines our mission: “The LIGO Scientific Collaboration (LSC) is a self- governing collaboration seeking to Detect gravitational waves, use them to explore the funDamental physics of gravity, anD Develop gravitational wave observations as a tool of astronomical Discovery. The LSC works towarD this goal through research on, anD Development of techniques for, gravitational wave detection; and the Development, commissioning anD exploitation of gravitational wave Detectors. No inDiviDual or group will be DenieD membership on any basis except scientific merit and the willingness to participate and contribute as described in this Charter.” The LSC was formeD in 1997 to exploit fully the scientific potential of the LIGO instruments then under construction, and to engage in the research and Development necessary to go significantly beyond the first generation of interferometers.
    [Show full text]