K. D. Giardina
A5102844874- Pulsars and Gravitational Waves Research
- Geophysics and Gravity Measurements
- Geophysics and Sensor Technology
- Mechanical and Optical Resonators
- Seismic Waves and Analysis
- Astrophysical Phenomena and Observations
- High-pressure geophysics and materials
- Statistical and numerical algorithms
- Cosmology and Gravitation Theories
- Gamma-ray bursts and supernovae
- Astronomical Observations and Instrumentation
- Magnetic confinement fusion research
- Radio Astronomy Observations and Technology
- Atomic and Subatomic Physics Research
- Advanced Frequency and Time Standards
- Radiation Dose and Imaging
- Planetary Science and Exploration
- Black Holes and Theoretical Physics
- Adaptive optics and wavefront sensing
- Solar and Space Plasma Dynamics
- Astrophysics and Cosmic Phenomena
- GNSS positioning and interference
- Mechanics and Biomechanics Studies
LIGO Scientific Collaboration
2014-2025
California Institute of Technology
2009
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 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...
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...
Gravitational Wave interferometers achieve their profound sensitivity by combining a Michelson interferometer with optical cavities, suspended masses, and now, squeezed quantum states of light. These modify the measurement process LIGO, VIRGO GEO600 to reduce noise that masks astrophysical signals; thus, improvements squeezing are essential further expand our gravitational view universe. Further reducing will require both lowering decoherence from losses as well more sophisticated...
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...
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...
The sensitivity of the Advanced LIGO detectors to gravitational waves can be affected by environmental disturbances external themselves. Since transition from former initial phase, many improvements have been made equipment and techniques used investigate these effects. These methods aided in tracking down mitigating noise sources throughout first three observing runs advanced detector era, keeping ambient contribution below background levels detectors. In this paper we describe how they led...
This paper presents an analysis of the transient behavior Advanced LIGO suspensions used to seismically isolate optics. We have characterized transients in longitudinal motion quadruple during LIGO's first observing run. Propagation between stages is consistent with modelled transfer functions, such that originating at top suspension chain significantly reduced amplitude test mass. find there are seen by monitors suspensions, but they not correlated above noise floor gravitational wave...
On May 24th, 2023, the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO), joined by Virgo and KAGRA detectors, began fourth observing run for a two-year-long dedicated search gravitational waves. The LIGO Hanford Livingston detectors have achieved an unprecedented sensitivity to waves, with angle-averaged median range binary neutron star mergers of 152 Mpc 160 Mpc, duty cycles 65.0% 71.2%, respectively, coincident cycle 52.6%. maximum detector is 165 177 both during second...
Advanced LIGO and Virgo have detected gravitational waves from astronomical sources to open a new window on the Universe. To explore this realm requires an exquisite level of detector sensitivity, meaning that much stronger signal instrumental environmental noise must be rejected. Selected examples unwanted in are presented. The initial focus is how existence (characterized by particular frequencies or time intervals) was discovered. Then, variety methods used track down source noise, e.g.,...
High-quality optical resonant cavities require low loss, typically on the scale of parts per million. However, unintended micron-scale contaminants resonator mirrors that absorb light circulating in cavity can deform surface thermoelastically and thus increase losses by scattering out mode. The point absorber effect is a limiting factor some high-power experiments, for example, Advanced LIGO gravitational-wave detector. In this Letter, we present general approach to from first principles...