Formation | 1993 |
---|---|
Type | International scientific collaboration |
Purpose | Gravitational wave detection |
Headquarters | European Gravitational Observatory |
Location | |
Coordinates | 43°37′53″N10°30′16″E / 43.6313°N 10.5045°E |
Region | Italy |
Fields | Basic research |
Spokesperson | Gianluca Gemme |
Affiliations | LVK (LIGO-Virgo-KAGRA collaboration) |
Budget | About ten million euros per year |
Staff | Around 850 people participate in the Virgo Collaboration |
Website | www |
The Virgo interferometer is a large Michelson interferometer designed to detect the gravitational waves predicted by general relativity. It is in Santo Stefano a Macerata, near the city of Pisa, Italy. The instrument has two arms that are three kilometres long and contain its mirrors and instrumentation inside an ultra-high vacuum.
Virgo is hosted by the European Gravitational Observatory (EGO), a consortium founded by the French Centre National de la Recherche Scientifique (CNRS) and Italian Istituto Nazionale di Fisica Nucleare (INFN). [1] The Virgo Collaboration operates the detector and defines the strategy and policy for its use and upgrades. It is composed of more than 700 members across 16 different countries. [2] The Virgo interferometer operates with similar detectors, including the two LIGO interferometers in the United States (at the Hanford Site and in Livingston, Louisiana) and the Japanese interferometer KAGRA (in the Kamioka mine). Cooperation between several detectors is crucial for detecting gravitational waves and pinpointing their origin, which is why the LIGO and Virgo collaborations have shared their data since 2007, and with KAGRA since 2019, to form the LIGO-Virgo-KAGRA (LVK) collaboration. [3]
The interferometer is named after the Virgo Cluster, a cluster of about 1,500 galaxies in the Virgo constellation, about 50 million light-years from Earth. [4] Founded at a time when gravitational waves were only a prediction by general relativity, it has now participated in detecting multiple gravitational wave events, making its first detection in 2017 (together with the two LIGO detectors), quickly followed by the GW170817 event, the only one to have also been observed with classical methods (optical, gamma-ray, X-ray and radio telescopes) as of 2024. [5] The detector is used for joint observing runs with the other detectors, separated by commissioning periods during which the detector is upgraded to increase its sensitivity and scientific output. [6]
The Virgo experiment is managed by the European Gravitational Observatory (EGO) consortium, created in December 2000 by the CNRS and INFN. [7] The Dutch Institute for Nuclear and High-Energy Physics, Nikhef, later joined as an observer and eventually became a full member. EGO is responsible for the Virgo site and is in charge of the construction, maintenance, and operation of the detector, as well as its upgrades. One of the goals of EGO is also to promote research on and studies of gravitation in Europe. [1]
The Virgo Collaboration consolidates all the researchers working on various aspects of the detector. As of May 2023, around 850 members, representing 142 institutions in 16 different countries, are part of the collaboration. [2] [8] This includes institutions from France, Italy, the Netherlands, Poland, Spain, Belgium, Germany, Hungary, Portugal, Greece, Czechia, Denmark, Ireland, Monaco, China, and Japan. [9]
The Virgo Collaboration is part of the larger LIGO-Virgo-KAGRA (LVK) Collaboration, which gathers scientists from the other major gravitational waves experiment, for the purpose of carrying out joint analysis of the data which is crucial for gravitational wave detections. [10] LVK first started in 2007 [3] as the LIGO-Virgo Collaboration, and was expanded when KAGRA joined in 2019. [11] [12]
The Virgo project was approved in 1992 by the French CNRS and in 1993 by the Italian INFN. The construction of the detector started in 1996 at the Cascina site near Pisa, Italy, and was completed in 2003. After several observation runs in which no gravitational waves were detected, the interferometer was shut down in 2011 to allow for significant upgrades as part of the Advanced Virgo project. It started making observations again in 2017, quickly making its first detections along with the LIGO detectors.[ citation needed ]
Although the concept of gravitational waves is more than 100 years old, having been predicted by Einstein in 1916, [13] it was not before the 1970s that serious projects for detecting them started to appear. The first were the Weber bars, invented by Joseph Weber; [14] while they could in principle detect gravitational waves, none of the experiments succeeded. They did however spark the creation of many research groups dedicated to gravitational waves. [15]
The idea of a large interferometric detector began to gain credibility in the early 1980s, and in 1985, the Virgo project was conceptualized by the Italian researcher Adalberto Giazotto and the French researcher Alain Brillet after they met in Rome. One of the key ideas that set Virgo apart from other projects was targeting low frequencies (around 10 Hz), whereas most projects focused on higher frequencies (around 500 Hz); many believed at the time that this was not doable, and only France and Italy started working on the project, [16] which was first presented in 1987. [17] After being approved by the CNRS and the INFN, the construction of the interferometer began in 1996, with the aim of beginning observations by 2000. [18]
The first goal of Virgo was to directly observe gravitational waves, of which the study of the binary pulsar 1913+16 over three decades had revealed indirect evidence. The observed decrease of this binary pulsar's orbital period was in agreement with the hypothesis that the system was losing energy by emitting gravitational waves. [19]
In the 2000s, the Virgo detector was first built, commissioned, and operated. The instrument successfully reached its expected sensitivity. This initial endeavor was used to validate the Virgo technical design choices; it also demonstrated that giant interferometers were promising devices for detecting gravitational waves in a wide frequency band. [20] [21] This phase is generally named the "initial Virgo" or "original Virgo".
The construction of the initial Virgo detector was completed in June 2003, [22] and several data collection periods ("science runs") followed between 2007 and 2011. [23] [24] Some of these runs were done simultaneously with the two LIGO detectors. There was a shut-down of a few months in 2010 to allow for a major upgrade of the Virgo suspension system: the original steel suspension wires were replaced by glass fibers to reduce the thermal noise. [25] However, the initial Virgo detector was not sensitive enough and after several months of data collection with the upgraded suspension system, the detector was shut down in September 2011 to begin the installation of Advanced Virgo. [26]
The Advanced Virgo detector aimed to increase the sensitivity (and thus the distance at which a signal can be detected) by a factor of 10, allowing it to probe a volume of the Universe 1,000 times larger, making detection of gravitational waves more likely. [16] [27] It benefited from the experience gained with the initial detector and technological advances.
The Advanced Virgo detector kept the same vacuum infrastructure as the initial Virgo, but the remainder of the interferometer was significantly upgraded. Four additional cryotraps were added at both ends of each arm to trap residual particles coming from the mirror towers. The new mirrors were larger (350 mm in diameter, with a weight of 40 kg), and their optical performance was improved. The critical optical elements used to control the interferometer are under vacuum on suspended mountings. A system of adaptive optics was to be installed to correct the mirror aberrations in-situ. In the original plan, the laser power was expected to reach 200 W in its final configuration. [28]
Advanced Virgo started the commissioning process in 2016, joining the two advanced LIGO detectors ("aLIGO") on 1 August 2017, during the "O2" observation period. On 14 August 2017, LIGO and Virgo detected a signal, GW170814, which was reported on 27 September 2017. It was the first binary black hole merger detected by both LIGO and Virgo (and the first one for Virgo). [29] [30]
Just a few days later, GW170817 was detected by LIGO and Virgo on 17 August 2017. The signal was produced by the last minutes of two neutron stars spiralling closer to each other and finally merging, and represents both the first binary neutron star merger observed and the first gravitational wave observation which was confirmed by non-gravitational means. Indeed, the resulting gamma-ray burst was also detected, and optical telescopes later discovered a kilonova corresponding to the merger. [5] [31]
2016 — – 2018 — – 2020 — – 2022 — – 2024 — – 2026 — – 2028 — – 2030 — | O1 O2 O3 O4a O4b O5 (plan) | |||||||
After further upgrades, Virgo started the third observation run ("O3") in April 2019, planned to last one year, [32] but the run ended earlier that expected on 27 March 2020, due to the COVID-19 pandemic. [33]
The upgrades following O3 are part of the "Advanced Virgo +" program, divided in two phases, the first one preceding the O4 run and the second one preceding the O5 run. The first phase focuses on the reduction of quantum noise by introducing a more powerful laser, improving the squeezing introduced in O3, and implementing a new technique called signal recycling; seismic sensors are also installed around the mirrors. The second phase will then try to reduce the mirror thermal noise, by changing the geometry of the laser beam to increase its size on the mirrors (spreading the energy on a larger area and thus reducing the temperature), and by improving the coating of the mirrors; the end mirrors will also be significantly larger, requiring improvements to the suspension. Further improvements for quantum noise reduction are also expected in the second phase, building upon the changes from the first. [34]
The fourth observation run ("O4") was scheduled to start in May 2023, and was planned to last for 20 months, including a commissioning break of up to two months. [6] However, on 11 May 2023, Virgo announced that it would not join at the beginning of O4, as the interferometer was not stable enough to reach the expected sensitivity and needed to undergo the replacement of one of the mirrors, requiring several weeks of work. [35] Virgo has not joined the O4 run during the first part of the run ("O4a"), which ended on 16 January 2024, as it only managed to reach a peak sensitivity of 45 Mpc instead of the 80 to 115 Mpc initially expected; it joined the second part of the run ("O4b") which began on 10 April 2024, with a sensitivity of 50 to 55 Mpc. In June 2024, it was announced that the O4 run would last until 9 June 2025, to get more preparation for the O5 upgrades. [6]
Following the O4 run, the detector will once again be shut down to undergo upgrades, including an improvement in the coating of the mirrors. A fifth observing run (O5) is currently planned for beginning around June 2027; the target sensitivity for Virgo, which was originally set to be 150–260 Mpc, is currently being redefined in light of the performance during O4; plans to enter the O5 run are expected to be known before the end of 2024. [6]
No official plans have been announced for the future of the Virgo installations following the O5 period, although projects for further improving the detectors have been suggested; the current plans of the collaboration are referred to as the Virgo_nEXT project. [36]
Virgo is designed to look for gravitational waves emitted by astrophysical sources across the universe, which can be broadly classified into three types: [37]
The detection of these sources gives a new way to observe them (often carrying different information than more classical ways, e.g. using telescopes), and allows to probe fundamental properties of gravity, such as the polarization of gravitational waves, [38] possible gravitational lensing, [39] or more generally whether the observed signals are correctly described by general relativity. [40] It also provides a way to measure the Hubble constant. [41]
In general relativity, a gravitational wave is a space-time perturbation which propagates at the speed of light. It slightly curves space-time, which locally changes the light path. Concretely, it can be detected using a Michelson interferometer design, where a laser is divided in two beams travelling in orthogonal directions, bouncing on a mirror located at the end of each arm. As the gravitational wave passes, it alters the path of the two beams in a different manner; they are then recombined, and the resulting interferometric pattern is measured using a photodiode. As the induced deformation is extremely small, the design requires an excellent precision in the position of the mirrors, the stability of the laser, the measurements, and a very good isolation from the outside world to reduce the amount of noise. [42]
The laser is the light source of the experiment. It must be powerful, while extremely stable in frequency and amplitude. [43] To meet all these (somewhat opposing) specifications, the beam starts from a very low power, yet very stable, laser. [44] The light from this laser passes through several amplifiers, which enhance its power by a factor of 100. A 50 W output power was achieved for the last configuration of the initial Virgo detector, and later reached 100 W during the O3 run, following the Advanced Virgo upgrades; it is expected to be upgraded to 130 W at the beginning of the O4 run. [34] The original Virgo detector used a master-slave laser system, where a "master" laser is used to stabilize a high-powered "slave" laser; the master laser was a Nd:YAG laser, and the slave laser a Nd:YVO4 laser. [22] The retained solution for Advanced Virgo is to have a fiber laser with an amplification stage made of fibers as well, to improve the robustness of the system; in its final configuration, it is planned to coherently combine the light of two lasers in order to achieve the required power. [28] [45] The wavelength of the laser is 1064 nanometres, in both the original and Advanced Virgo configurations. [34]
This laser is sent into the interferometer after passing through the injection system, which further ensures the stability of the beam, adjusts its shape and power, and positions it correctly for entering the interferometer. Key components of the injection system include the input mode cleaner (a 140-metre-long cavity made for improving the beam quality, by stabilizing the frequency, removing light propagating in an unwanted way and reducing the effect of misalignment of the laser), a Faraday isolator preventing any light from returning to the laser, and a mode-matching telescope, which adapts the size and position of the beam right before it enters the interferometer. [28]
The large mirrors located in each arm are the most critical optics of the interferometer. They include the two end mirrors, located at the ends of the 3-km interferometer arms, and the two input mirrors, located near the beginning of the arms. Together, these mirrors make a resonant optical cavity in each arm, where the light bounces thousands of times before returning to the beam splitter, maximizing the effect of the signal on the laser path. [46] It also allows the power of the light circulating in the arms to be increased. These mirrors have been specifically designed for Virgo and are made from state-of-the-art technologies. They are cylinders 35 cm in diameter and 20 cm thick, [28] made from the purest glass obtainable. [47] The mirrors are polished to the atomic level to avoid diffusing (and hence losing) any light. [48] Finally, a reflective coating (a Bragg reflector made with ion beam sputtering) is added. The mirrors located at the end of the arms reflect almost all incoming light; less than 0.002% of the light is lost at each reflection. [49]
In addition, two other mirrors are present in the final design:
To mitigate the seismic noise which could propagate up to the mirrors, shaking them and hence obscuring potential gravitational wave signals, the large mirrors are suspended by a complex system. All of the main mirrors are suspended by four thin fibers made of silica [51] which are attached to a series of attenuators. This chain of suspension, called the "superattenuator", is close to 8 meters high and is also under vacuum. [52] The superattenuators do not only limit the disturbances on the mirrors, they also allow the mirror position and orientation to be precisely steered. The optical table where the injection optics used to shape the laser beam are located, such as the benches used for the light detection, are also suspended and under vacuum, to limit the seismic and acoustic noises. In the Advanced Virgo configuration, the whole instrumentation used to detect gravitational waves signals and to steer the interferometer (photodiodes, cameras, and the associated electronics) is also installed on several suspended benches, and under vacuum. [28]
The design of the superattenuators is mainly based on the passive attenuation of the seismic noise, which is achieved by chaining several pendula, each acting as an harmonic oscillator. They are characterized by a resonance frequency (which diminishes with the length of the pendulum) above which the noise will be dampened; chaining several pendula allows to reduce the noise by twelve orders of magnitude, at the cost of introducing multiple, collective resonance frequencies, which are at a higher frequency than a single long pendulum. [53] In the current design, the highest resonance frequency is around 2 Hz, providing a meaningful noise reduction starting at 4 Hz, [28] and reaching the level needed for detecting gravitational waves around 10 Hz. A limit of the system is that the noise in the resonance frequency band (below 2 Hz) is not filtered and can generate large oscillations; this is mitigated by an active damping system, including sensors measuring the seismic noise and actuators controlling the superattenuator to counteract the noise. [53]
Part of the light circulating in the arm cavities is sent towards the detection system by the beam splitter. In its optimal configuration, the interferometer works close to the "dark fringe", meaning that very little light is sent towards the output (most of it is sent back to the input, to be collected by the power recycling mirror). A fraction of this light is reflected back by the signal recycling mirror, and the rest is collected by the detection system. It first passes through the output mode cleaner, which allows to filter the so-called "high-order modes" (light propagating in an unwanted way, typically introduced by small defects in the mirrors, and susceptible to degrade the measurement [54] ), before reaching the photodiodes, which measure the light intensity. Both the output mode cleaner and the photodiodes are suspended and under vacuum. [27]
Starting with the O3 run, a squeezed vacuum source was introduced to reduce the quantum noise, which is one of the main limitations to sensitivity. When replacing the standard vacuum by a squeezed vacuum, the fluctuations of a quantity are decreased, at the expense of increasing the fluctuations of the other quantity due to Heisenberg's uncertainty principle. In the case of Virgo, the two quantities are the amplitude and the phase of the light. The idea of using squeezed vacuum was first proposed in 1981 by Carlton Caves, during the infancy of gravitational wave detectors. [55] During the O3 run, frequency-independent squeezing was implemented, meaning that the squeezing is identical at all frequencies; it was used to reduce the shot noise (dominant at high frequencies) and increase the radiation pressure noise (dominant at low frequencies), as the latter was not limiting the instrument's sensitivity. [56] Due to the addition of the squeezed vacuum injection, the quantum noise was reduced by 3.2 dB at high frequencies, resulting in an increase of the range of the detector by 5–8%. [57] Currently, more sophisticated squeezed states are produced [58] by combining the technology from O3 with a new 285 m long cavity, known as the filter cavity. This technology is known as frequency-dependent squeezing, and helps reduce the shot noise at high frequencies (where radiation pressure noise is not relevant), and reduce the radiation pressure noise at low frequencies (where shot noise is low). [59] [60]
Seen from the air, the Virgo detector has a characteristic "L" shape with its two 3-km-long perpendicular arms. The arm "tunnels" house pipes in which the laser beams are travelling in a vacuum.
Virgo is the largest ultra-high vacuum installation in Europe, with a total volume of 6,800 cubic meters. [61] The two 3-km arms are made of a long steel pipe 1.2m in diameter in which the target residual pressure is about 1 thousandth of a billionth of an atmosphere (improving by a factor of 100 from the original Virgo level). Thus, the residual gas molecules (mainly hydrogen and water) have a limited impact on the path of the laser beams. [28] Large gate valves are located at both ends of the arms so that work can be done in the mirror vacuum towers without breaking an arm's ultra-high vacuum. The towers containing the mirrors and attenuators are themselves split in two sections with different pressures. [62] The tubes undergo a process called baking, where they are heated at 150°C to remove unwanted particles stuck on the surfaces; while the towers were also baked-out in the initial Virgo design, cryogenic traps are now used to prevent contamination. [28]
Due to the high power in the interferometer, the mirrors are susceptible to thermal effects caused by the heating induced by the laser (despite having an extremely low absorption). These thermal effects can take the shape of a deformation of the surface due to dilation, or a change in the refractive index of the substrate; this results in power escaping from the interferometer and in perturbations of the signal. These two effects are accounted for by the thermal compensation system (TCS), which includes sensors called Hartmann wavefront sensors [63] (HWS), used to measure the optical aberration through an auxiliary light source, and two actuators: CO2 lasers, which selectively heat parts of the mirror to correct the defects, and ring heaters, which precisely adjust the radius of curvature of the mirror. The system also corrects the "cold defects", which are permanent defects introduced during the mirror manufacturing. [64] [28] During the O3 run, the TCS was able to increase the power circulating inside the interferometer by 15%, and decrease the power leaving the interferometer by a factor of 2. [65]
Another important component is the system for controlling stray light, which refers to any light leaving the designated path of the interferometer, either by scattering on a surface or from unwanted reflection. The recombination of this stray light with the main beam of the interferometer can be a significant source of noise, and is often hard to track and to model. Most of the efforts to mitigate stray light are based on absorbing plates called "baffles", placed near the optics as well as within the tubes; additional precautions are needed to prevent the baffles from having an effect on the interferometer operation. [66] [67] [61]
To estimate properly the response of the detector to gravitational waves and thus correctly reconstruct the signal, a calibration step is required, which involves moving the mirrors in a controlled way and measuring the result. During the initial Virgo era, this was primarily achieved by agitating one of the pendulum to which the mirror is suspended using coils to generate a magnetic field interacting with magnets fixed to the pendulum. [68] This technique was employed until O2. For O3, the main calibration method became the photon calibration ("PCal") which had until then been used as a secondary method to validate the results; it uses an auxiliary laser to displace the mirror via radiation pressure. [69] [70] In addition, a new method called Newtonian calibration ("NCal") has been introduced at the end of O2, allowing to validate the Pcal results; it relies on gravity to move the mirror, by placing a rotating mass at a specific distance of the mirror. [71] [70] At the beginning of the second part of O4, the Ncal became the main calibration method after achieving better performance than the Pcal; the Pcal is still used to validate the Ncal results and probe higher frequencies unaccessible to the Ncal. [72]
Finally, the instrument requires an efficient data acquisition system. This system is in charge of managing the data measured at the output of the interferometer and from the many sensors present on the site, writing it in files, and distributing the files for data analysis. To this end, dedicated hardware and software have been developed to accommodate the specific needs of Virgo. [73]
Due to the precision required in the measurement, the Virgo detector is sensitive to several sources of noise which limit its ability to detect gravitational wave signals. Some of these sources correspond to large frequency ranges and limit the overall sensitivity of the detector, [75] [61] such as:
In addition to these broad noise sources, others may affect specific frequencies. These notably include a source at 50 Hz (as well as harmonics at 100, 150, and 200 Hz), corresponding to the frequency of the European power grid; so-called "violin modes" at 300 Hz (and several harmonics), corresponding to the resonance frequency of the suspension fibers (which can vibrate at a specific frequency just as the strings of a violin do); and calibration lines, appearing when mirrors are moved for calibration. [76] [77]
Additional noise sources may also have a short-term impact—bad weather or earthquakes may temporarily increase the noise level. [61]
Finally, several short-lived artifacts may appear in the data due to many possible instrumental issues; these are usually referred to as "glitches". It is estimated that about 20% of the detected events are impacted by glitches, requiring specific data processing methods to mitigate their impact. [78]
As the sensitivity depends on the frequency, it is usually represented as a curve corresponding to the noise power spectrum (or often amplitude spectrum, which is the square root of the power spectrum); the lower the curve, the better the sensitivity. Virgo is a wide band detector whose sensitivity ranges from a few Hz up to 10 kHz; the image attached shows an example of a Virgo sensitivity curve from 2011, plotted using a log-log scale.
The most common measure for the sensitivity of a gravitational wave detector is the "horizon distance", defined as the distance at which a binary neutron star with masses 1.4 M☉–1.4 M☉ (where M☉ is the solar mass) produces a signal-to-noise ratio of 8 in the detector. It is generally expressed in megaparsecs. [80] For instance, the range for Virgo during the O3 run was between 40 and 50 Mpc. [6] This range is only an indicator and does not represent a maximal range for the detector; signals from more massive sources will have a larger amplitude, and can thus be detected from further away.
Calculations show that the detector sensitivity roughly scales as , where is the arm cavity length and the laser power on the beam splitter. To improve it, these two quantities must be increased. This is achieved by having long arms, using optical cavities inside the arm to maximize the exposition to the signal, and implementing power recycling to increase the power in the arms. [75] [81]
An important part of the Virgo collaboration resources is dedicated to the development and deployment of data analysis software designed to process the output of the detector. Apart from the data acquisition software and the tools for distributing the data, this effort is mostly shared with members of the LIGO and KAGRA collaborations, as part of the LIGO-Virgo-KAGRA (LVK) collaboration. [82]
The data from the detector is initially only available to LVK members; segments of data around detected events are released at the time of publication of the related paper, and the full data is released after a proprietary period, currently lasting 18 months. During the third observing run (O3), this resulted in two separated data releases (O3a and O3b), corresponding to the first six months and last six months of the run respectively. [83] The data is then available for anyone on the Gravitational Wave Open Science Center (GWOSC) platform. [84] [85]
The analysis of the data requires a variety of different techniques, targeting the different type of sources. The major part of the effort is dedicated to the detection and analysis of mergers of compact objects, the only type of source detected up until now. Several different analysis software are running on the data searching for this type of event, and a dedicated infrastructure is used to emit alerts to the online community. [86] Other efforts are carried out after the data taking period ("offline"), including searches for continuous sources [87] or for a stochastic background, [88] as well as deeper analysis of the detected events. [86]
The first detection of a gravitational signal by Virgo took place at during the second observing run (O2) of the "Advanced" era, as only the LIGO detectors were operating during the first observing run. The event, named GW170814, was a coalescence between two black holes, and also the first event to be detected by three different detectors, allowing for its localization to be greatly improved compared to the events from the first observing run. It also allowed for the first conclusive measure of gravitational wave polarizations, providing evidence against the existence of polarizations other than the ones predicted by general relativity. [29]
It was soon followed by the more famous GW170817, first merger of two neutron stars detected by the gravitational wave network, and as of January 2023 the only event with a confirmed detection of an electromagnetic counterpart, both in gamma rays and in optical telescopes, and later in the radio and x-ray domains. While no signal was observed in Virgo, this absence was crucial to put tighter constraints on the localization of the event. [5] This event had tremendous repercussions in the astronomical community, involving more than 4000 astronomers, [89] improving the understanding of neutron star mergers, [90] and putting very tight constraints on the speed of gravity. [91]
Several searches for continuous gravitational waves have been performed on data from the past runs. On the O3 run, these include an all-sky search, [92] targeted searches toward Scorpius X-1 [93] and several known pulsars (including the Crab and Vela pulsars), [94] [95] and directed search towards the supernova remnants Cassiopeia A and Vela Jr. [96] and the Galactic Center. [97] While none of the searches managed to identify a signal, this allowed upper limits to be set on some parameters; in particular, it was found that the deviation from perfect spinning balls for close known pulsars is at most of the order of 1 mm. [92]
Virgo was included in the latest search for a gravitational wave background along with LIGO, combining the results of O3 with the ones from the O1 and O2 runs (which only used LIGO data). No stochastic background was observed, improving previous constraints on the energy of the background by an order of magnitude. [98]
Broad estimates of the Hubble constant have also been obtained and the current best estimate is 68+12
-8 km s−1 Mpc−1, combining results from binary black holes and from the GW170817 event. This result is coherent with other estimates of the constant, but not precise enough to solve the current debates on its exact value. [41]
The Virgo collaboration participates in several activities promoting communication and education on gravitational waves for the general public. [99] One of the more forefront activities is the organization of guided tours of the Virgo facilities for schools, universities, and the general public; [100] however, many of the outreach activities take place outside the Virgo site. This includes educational activities such as public lectures and courses about Virgo activities, including to school classes, [99] but also participating in several science festivals, [101] [102] [103] which involves the development of methods and devices for the public understanding of gravitational waves (and related topics). The collaboration is also involved in several artistic projects, ranging from visual projects such as "The Rhythm of Space" at the Museo della Grafica in Pisa, [104] or "On Air" at the Palais de Tokyo, [105] to musical ones with different concerts. [106] It also includes activities promoting gender equality in science, for instance highlighting the women working in Virgo in communications to the general public. [107]
The Laser Interferometer Gravitational-Wave Observatory (LIGO) is a large-scale physics experiment and observatory designed to detect cosmic gravitational waves and to develop gravitational-wave observations as an astronomical tool. Two large observatories were built in the United States with the aim of detecting gravitational waves by laser interferometry. These observatories use mirrors spaced four kilometers apart to measure changes in length—over an effective span of 1120 km—of less than one ten-thousandth the charge diameter of a proton.
The Laser Interferometer Space Antenna (LISA) is a planned space probe to detect and accurately measure gravitational waves—tiny ripples in the fabric of spacetime—from astronomical sources. LISA will be the first dedicated space-based gravitational-wave observatory. It aims to measure gravitational waves directly by using laser interferometry. The LISA concept features three spacecraft arranged in an equilateral triangle with each side 2.5 million kilometers long, flying in an Earth-like heliocentric orbit. The distance between the satellites is precisely monitored to detect a passing gravitational wave.
The Max Planck Institute for Gravitational Physics is a Max Planck Institute whose research is aimed at investigating Einstein's theory of relativity and beyond: Mathematics, quantum gravity, astrophysical relativity, and gravitational-wave astronomy. The institute was founded in 1995 and is located in the Potsdam Science Park in Golm, Potsdam and in Hannover where it closely collaborates with the Leibniz University Hannover. Both the Potsdam and the Hannover parts of the institute are organized in three research departments and host a number of independent research groups.
GEO600 is a gravitational wave detector located near Sarstedt, a town 20 kilometres (12 mi) to the south of Hanover, Germany. It is designed and operated by scientists from the Max Planck Institute for Gravitational Physics, Max Planck Institute of Quantum Optics and the Leibniz Universität Hannover, along with University of Glasgow, University of Birmingham and Cardiff University in the United Kingdom, and is funded by the Max Planck Society and the Science and Technology Facilities Council (STFC).
The gravitational wave background is a random background of gravitational waves permeating the Universe, which is detectable by gravitational-wave experiments, like pulsar timing arrays. The signal may be intrinsically random, like from stochastic processes in the early Universe, or may be produced by an incoherent superposition of a large number of weak independent unresolved gravitational-wave sources, like supermassive black-hole binaries. Detecting the gravitational wave background can provide information that is inaccessible by any other means about astrophysical source population, like hypothetical ancient supermassive black-hole binaries, and early Universe processes, like hypothetical primordial inflation and cosmic strings.
The Kamioka Gravitational Wave Detector (KAGRA) is a large interferometer designed to detect gravitational waves predicted by the general theory of relativity. KAGRA is a Michelson interferometer that is isolated from external disturbances: its mirrors and instrumentation are suspended and its laser beam operates in a vacuum. The instrument's two arms are three kilometres long and located underground at the Kamioka Observatory which is near the Kamioka section of the city of Hida in Gifu Prefecture, Japan.
Gravitational waves are transient displacements in a gravitational field – generated by the motion or acceleration of gravitating masses – that radiate outward from their source at the speed of light. They were first proposed by Oliver Heaviside in 1893 and then later by Henri Poincaré in 1905 as the gravitational equivalent of electromagnetic waves. In 1916, Albert Einstein demonstrated that gravitational waves result from his general theory of relativity as ripples in spacetime.
A gravitational-wave detector is any device designed to measure tiny distortions of spacetime called gravitational waves. Since the 1960s, various kinds of gravitational-wave detectors have been built and constantly improved. The present-day generation of laser interferometers has reached the necessary sensitivity to detect gravitational waves from astronomical sources, thus forming the primary tool of gravitational-wave astronomy.
Gravitational-wave astronomy is a subfield of astronomy concerned with the detection and study of gravitational waves emitted by astrophysical sources.
Carlton Morris Caves is an American theoretical physicist. He is currently professor emeritus and research professor of physics and astronomy at the University of New Mexico. Caves works in the areas of physics of information; information, entropy, and complexity; quantum information theory; quantum chaos, quantum optics; the theory of non-classical light; the theory of quantum noise; and the quantum theory of measurement. He is a Fellow of the American Physical Society and of the American Association for the Advancement of Science and is a member of the US National Academy of Sciences.
INDIGO or IndIGO is a consortium of Indian gravitational wave physicists. It is an initiative to set up advanced experimental facilities for a multi-institutional observatory project in gravitational-wave astronomy to be located near Aundha Nagnath, Hingoli District, Maharashtra, India. Predicted date of commission is in 2030.
The International Pulsar Timing Array (IPTA) is a multi-institutional, multi-telescope collaboration comprising the European Pulsar Timing Array (EPTA), the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), the Parkes Pulsar Timing Array (PPTA) in Australia, and the Indian Pulsar Timing Array Project (InPTA). The goal of the IPTA is to detect ultra-low-frequency gravitational waves, such as from mergers of supermassive black holes, using an array of approximately 30 pulsars. This goal is shared by each of the participating institutions, but they have all recognized that their goal will be achieved more quickly by combining their respective efforts and resources.
The first direct observation of gravitational waves was made on 14 September 2015 and was announced by the LIGO and Virgo collaborations on 11 February 2016. Previously, gravitational waves had been inferred only indirectly, via their effect on the timing of pulsars in binary star systems. The waveform, detected by both LIGO observatories, matched the predictions of general relativity for a gravitational wave emanating from the inward spiral and merger of a pair of black holes of around 36 and 29 solar masses and the subsequent "ringdown" of the single resulting black hole. The signal was named GW150914. It was also the first observation of a binary black hole merger, demonstrating both the existence of binary stellar-mass black hole systems and the fact that such mergers could occur within the current age of the universe.
In quantum physics, light is in a squeezed state if its electric field strength Ԑ for some phases has a quantum uncertainty smaller than that of a coherent state. The term squeezing thus refers to a reduced quantum uncertainty. To obey Heisenberg's uncertainty relation, a squeezed state must also have phases at which the electric field uncertainty is anti-squeezed, i.e. larger than that of a coherent state. Since 2019, the gravitational-wave observatories LIGO and Virgo employ squeezed laser light, which has significantly increased the rate of observed gravitational-wave events.
GW 190412 was a gravitational wave (GW) signal observed by the LIGO and Virgo detectors on 12 April 2019. In April 2020, it was announced as the first time a collision of a pair of very differently sized black holes has been detected. As a result of this asymmetry, the signal included two measurable harmonics with frequencies approximately a factor 1.5 apart.
Rana X. Adhikari is an American experimental physicist. He is a professor of physics at the California Institute of Technology (Caltech) and an associate faculty member of the International Centre for Theoretical Sciences of Tata Institute of Fundamental Research (ICTS-TIFR).
Lisa Barsotti is a research scientist at the Massachusetts Institute of Technology Kavli Institute.
C. S. Unnikrishnan is an Indian physicist and professor known for his contributions in multiple areas of experimental and theoretical physics. He has been a professor at the Tata Institute of Fundamental Research Mumbai and is currently a professor in the School of Quantum Technology at the Defence Institute of Advanced Technology in Pune. He has made significant contributions in foundational issues in gravity and quantum physics and has published over 250 research papers and articles. Unnikrishnan is also a key member of the LIGO-India project and a member of the global LIGO Scientific Collaboration
Ground-based interferometric gravitational-wave search refers to the use of extremely large interferometers built on the ground to passively detect gravitational wave events from throughout the cosmos. Most recorded gravitational wave observations have been made using this technique; the first detection, revealing the merger of two black holes, was made in 2015 by the LIGO sites.
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