Peter Fritschel
A5101485028- Pulsars and Gravitational Waves Research
- Geophysics and Sensor Technology
- Advanced Frequency and Time Standards
- Cold Atom Physics and Bose-Einstein Condensates
- Mechanical and Optical Resonators
- Geophysics and Gravity Measurements
- Seismic Waves and Analysis
- Advanced Fiber Laser Technologies
- Cosmology and Gravitation Theories
- Atomic and Subatomic Physics Research
- Astrophysical Phenomena and Observations
- Magnetic confinement fusion research
- Adaptive optics and wavefront sensing
- Advanced Measurement and Metrology Techniques
- Gamma-ray bursts and supernovae
- Astronomical Observations and Instrumentation
- Photorefractive and Nonlinear Optics
- Photonic and Optical Devices
- Optical Coatings and Gratings
- Solid State Laser Technologies
- Ultrasonics and Acoustic Wave Propagation
- Spectroscopy and Laser Applications
- High-pressure geophysics and materials
- Acoustic Wave Resonator Technologies
- Nonlinear Dynamics and Pattern Formation
Massachusetts Institute of Technology
2015-2025
LIGO Scientific Collaboration
2021-2024
IIT@MIT
2018
Jet Propulsion Laboratory
2007
California Institute of Technology
2001
Pennsylvania State University
2001
Université Paris Cité
1994
Université Paris-Sud
1994
The Laser Interferometer Gravitational Wave Observatory (LIGO) has been directly detecting gravitational waves from compact binary mergers since 2015. We report on the first use of squeezed vacuum states in direct measurement with Advanced LIGO H1 and L1 detectors. This achievement is culmination decades research to implement gravitational-wave During ongoing O3 observation run, are improving sensitivity interferometers signals above 50 Hz by up 3 dB, thereby increasing expected detection...
The Big Bang Observer is a proposed space-based gravitational-wave detector intended as follow on mission to the Laser Interferometer Space Antenna (LISA). It designed detect stochastic background of gravitational waves from early universe. We discuss how interferometry can be arranged between three spacecraft for this and what research development key technologies are necessary realize scheme.
On April 1st, 2019, the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), joined by Virgo detector, began third observing run, a year-long dedicated search for gravitational radiation. The LIGO detectors have achieved higher duty cycle and greater sensitivity to waves than ever before, with Hanford achieving angle-averaged binary neutron star coalescences distance of 111 Mpc, Livingston 134 Mpc factors 74.6% 77.0% respectively. improvement in stability is result several...
Quantum noise imposes a fundamental limitation on the sensitivity of interferometric gravitational-wave detectors like LIGO, manifesting as shot and quantum radiation pressure noise. Here, we present first realization frequency-dependent squeezing in full-scale detectors, resulting reduction both noise, with broadband detector enhancement from tens hertz to several kilohertz. In LIGO Hanford detector, reduced amplitude by factor 1.6 (4.0 dB) near 1 kHz; Livingston was 1.9 (5.8 dB). These...
The first detection of gravitational waves by the Laser Interferometer Gravitational-Wave Observatory (LIGO) in 2015 launched era gravitational-wave astronomy. quest for signals from objects that are fainter or farther away impels technological advances to realize ever more sensitive detectors. Since 2019, one advanced technique, injection squeezed states light, is being used improve shot-noise limit sensitivity Advanced LIGO detectors, at frequencies above ∼50 Hz. Below this frequency,...
The motion of a mechanical object, even human-sized should be governed by the rules quantum mechanics. Coaxing them into state is, however, difficult because thermal environment masks any signature object's motion. also effects proposed modifications mechanics at large mass scales. We prepared center-of-mass 10-kilogram oscillator in with an average phonon occupation 10.8. reduction temperature, from room temperature to 77 nanokelvin, is commensurate 11 orders-of-magnitude suppression...
Cosmic Explorer is a next-generation ground-based gravitational-wave observatory concept, envisioned to begin operation in the 2030s and expected be capable of observing binary neutron star black hole mergers back time first stars. Explorer's sensitive band will extend below 10 Hz, where design predominantly limited by geophysical, thermal, quantum noises. In this work, seismic, gravity-gradient, quantum, residual gas, scattered-light, servo-control noises are analyzed order motivate...
Abstract Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore Universe on all scales from nuclear physics cosmos massive potential further impact fundamental physics, astrophysics, cosmology for decades come. In this paper we studied science capabilities of network LIGO detectors when they reach their best possible sensitivity, called A <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"...
Thermal fluctuations in the coatings used to make high reflectors are becoming significant noise sources precision optical measurements and particularly relevant advanced gravitational-wave detectors. There two recognized of coating thermal noise; mechanical loss dissipation. dissipation causes which produce via thermoelastic thermorefractive mechanisms. We treat these mechanisms coherently, give a correction for finite thickness, evaluate implications Advanced LIGO.
The Heisenberg uncertainty principle dictates that the position and momentum of an object cannot be simultaneously measured with arbitrary precision, giving rise to apparent limitation known as standard quantum limit (SQL). Gravitational-wave detectors use photons continuously measure positions freely falling mirrors so are affected by SQL. We investigated performance Laser Interferometer Gravitational-Wave Observatory (LIGO) after experimental realization frequency-dependent squeezing...
Interferometric gravitational-wave antennas are based on Michelson interferometers whose sensitivity to small differential length changes has been enhanced by the addition of multiple coupled optical resonators. The use cavities is essential for reaching required but sets challenges control system, which must maintain near resonance. goal strain Laser Interferometer Gravitational-Wave Observatory (LIGO) 10(-21) rms, integrated over a 100-Hz bandwidth centered at 150 Hz. We present major...
Balanced homodyne detection is typically used to measure quantum-noise-limited optical beams, including squeezed states of light, at audio-band frequencies. Current designs advanced gravitational wave interferometers use some type readout for signal detection, in part because its compatibility with the light. The scheme Advanced LIGO, called DC readout, however not a balanced scheme. Instead, local oscillator field, generated from dark fringe offset, co-propagates field anti-symmetric output...
Interferometric gravitational-wave detectors like LIGO need to be able measure changes in their arm lengths of order ${10}^{\ensuremath{-}18}\text{ }\text{ }\mathrm{m}$ or smaller. This requires very high laser power raise the signal above shot noise. One significant limitation increased is an optomechanical interaction between field and detector's test masses that can form unstable feedback loop. Such parametric instabilities have long been studied as a limiting effect at power, were first...
We present a pair of seismometers capable measurement in all six axes rigid motion. The vacuum-compatible devices implement compact interferometric displacement sensors to surpass the sensitivity typical electrical-readout schemes. Together with capability subtract sensitivity-limiting coupling ground tilt into horizontal motion, our can widen sensing band toward megahertz frequencies. This has notable applications across range fields requiring access low-frequency signals, such as...
We present an analysis of Brownian force noise from residual gas damping reference test masses as a fundamental sensitivity limit in small experiments. The resulting acceleration increases significantly when the distance mass to surrounding experimental apparatus is smaller than dimension itself. For Advanced LIGO interferometric gravitational wave observatory, where relevant suspended 340 mm diameter cylindrical end mirror, power increased by roughly factor 40 presence similarly shaped...
Noise due to scattered light has been a frequent disturbance in the Advanced LIGO gravitational wave detectors, hindering detection of waves. The non stationary scatter noise caused by low frequency motion can be recognized as arches time-frequency plane channel. In this paper, we characterize scattering for LIGO's third observing run O3 from April, 2019 March, 2020. We find at least two different populations and investigate multiple origins one them well its mitigation. that relative...
Precision measurements of space and time, like those made by the detectors Laser Interferometer Gravitational-wave Observatory (LIGO), are often confronted with fundamental limitations imposed quantum mechanics. The Heisenberg uncertainty principle dictates that position momentum an object cannot both be precisely measured, giving rise to apparent limitation called Standard Quantum Limit (SQL). Reducing noise below SQL in gravitational-wave detectors, where photons used continuously measure...
Interferometric gravitational-wave detectors, such as the Laser Interferometer Gravitational Wave Observatory (LIGO) detectors currently under construction, are based on kilometer-scale Michelson interferometers, with sensitivity that is enhanced by addition of multiple coupled optical resonators. Reducing relative optic motions to bring system resonant operating point a significant challenge. We present new approach lock acquisition, used LIGO interferometer, whereby sensor transformation...
Teleseismic, or distant, earthquakes regularly disrupt the operation of ground--based gravitational wave detectors such as Advanced LIGO. Here, we present \emph{EQ mode}, a new global control scheme, consisting an automated sequence optimized filters that reduces and coordinates motion seismic isolation platforms during earthquakes. This, in turn, suppresses differential interferometer arms with respect to one another, resulting reduction DARM signal at frequencies below 100\,mHz. Our method...
We describe the first experimental demonstration of light recycling a Michelson interferometer with Fabry–Perot cavities in arms interferometer. Light is technique for efficiently using long-baseline interferometers, such as those being proposed detection gravitational radiation. An increase circulating power by factor 18 observed, which good agreement expected gain given losses system. Several phenomena associated this configuration coupled optical are discussed.
We describe a rigid, internally modulated Michelson interferometer with Fabry–Perot cavities in the arms. The high contrast (0.986) and small cavity losses (2.7%) permit efficient use of light power available. measured shot-noise-limited displacement sensitivity for 35mW is 2.5×10-17m/Hz, good agreement calculated signal-to-noise ratio.
Small, highly absorbing points are randomly present on the surfaces of main interferometer optics in Advanced LIGO. The resulting nano-meter scale thermo-elastic deformations and substrate lenses from these micron-scale absorbers significantly reduces sensitivity directly though a reduction power-recycling gain indirect interactions with feedback control system. We review expected surface deformation point provide pedagogical description impact power build-up second generation gravitational...
Gravitational-wave observations by the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo have provided us a new tool to explore Universe on all scales from nuclear physics cosmos massive potential further impact fundamental physics, astrophysics, cosmology for decades come. In this paper we studied science capabilities of network LIGO detectors when they reach their best possible sensitivity, called A#, given infrastructure in which exist generation observatories that are...