Virgo Interferometer

The Virgo interferometer is a large interferometer designed to detect gravitational waves predicted by the general theory of relativity. Virgo 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 in Santo Stefano a Macerata, Italy.

Virgo is hosted by the European Gravitational Observatory (EGO), a consortium founded by the French CNRS and Italian INFN. The ''Virgo Collaboration'' operates the detector and is composed of more than 650 members, representing 119 institutions in 14 different countries. Other interferometers similar to Virgo have the same goal of detecting gravitational waves, including the two LIGO interferometers in the United States (at the Hanford Site and in Livingston, Louisiana). Since 2007, Virgo and LIGO have agreed to share and jointly analyze the data recorded by their detectors and to jointly publish their results. Because the interferometric detectors are not directional (they survey the whole sky) and they are looking for signals which are weak, infrequent, one-time events, simultaneous detection of a gravitational wave in multiple instruments is necessary to confirm the signal validity and to deduce the angular direction of its source.

The interferometer is named for the Virgo Cluster of about 1,500 galaxies in the Virgo constellation, about 50 million light-years from Earth. As no terrestrial source of gravitational wave is powerful enough to produce a detectable signal, Virgo must observe the Universe. The more sensitive the detector, the further it can see gravitational waves, which then increases the number of potential sources. This is relevant as the violent phenomena Virgo is potentially sensitive to (coalescence of a compact binary system, neutron stars or black holes; supernova explosion; etc.) are rare: the more galaxies Virgo is surveying, the larger the probability of a detection.

History

The Virgo project was approved in 1993 by the French CNRS and in 1994 by the Italian INFN, the two institutes at the origin of the experiment. The construction of the detector started in 1996 in the Cascina site near Pisa, Italy. In December 2000, CNRS and INFN created the European Gravitational Observatory (EGO consortium). The Dutch Institute for Nuclear and High-Energy Physics Nikhef later joined as an observer and eventually a full member. EGO is responsible for the Virgo site, in charge of the construction, the maintenance and the operation of the detector, as well as of its upgrades. The goal of EGO is also to promote research and studies about gravitation in Europe.

The ''Virgo Collaboration'' works on the realization and operation of the Virgo interferometer. As of February 2021, more than 650 members, representing 119 institutions in 14 different countries are part of the collaboration. This includes institutions from: France, Italy, the Netherlands, Poland, Spain, Belgium, Germany, Hungary, Portugal, Greece, Czechia, Denmark, Ireland, Monaco, China, and Japan.

The initial Virgo detector

In the 2000s, the Virgo detector was built, commissioned and operated. The instrument reached its design sensitivity to gravitational wave signals. This initial endeavour was used to validate the Virgo technical design choices; and it also demonstrated that giant interferometers are promising devices to detect gravitational waves in a wide frequency band. The construction of the Initial Virgo detector was completed in June 2003 and several data taking periods followed between 2007 and 2011. Some of these runs were done in coincidence with the two LIGO detectors. The initial Virgo detector recorded scientific data from 2007 to 2011 during four science runs. There was a shut-down of a few months in 2010 to allow for a major upgrade of the Virgo suspension system: the original suspension steel wires were replaced by glass fibers in order to reduce the thermal noise. After several months of data taking with this final configuration, the initial Virgo detector was shut down in September 2011 to begin the installation of Advanced Virgo.

The Advanced Virgo detector

However, the initial Virgo detector was not sensitive enough to detect such gravitational waves. Therefore, it was decommissioned in 2011 and replaced by the Advanced Virgo detector which aims at increasing its sensitivity by a factor of 10, allowing it to probe a volume of the Universe 1,000 times larger, making detections of gravitational waves more likely. The original detector is generally referred to as the "initial Virgo" or "original Virgo". The Advanced Virgo detector benefits from the experience gained on the initial detector and from technological advances since it was made.

The Advanced Virgo is 10 times more sensitive than the initial Virgo. According to the Advanced Virgo Technical Design Report VIR–0128A–12 of 2012, advanced Virgo keeps the same vacuum infrastructure as Virgo, with four additional cryotraps located at both ends of both three-kilometre-long arms to trap residual particles coming from the mirror towers, but the remainder of the interferometer has been significantly upgraded. The new mirrors are larger (350 mm in diameter, with a weight of 40 kg), and their optical performances have been improved. The critical optical elements used to control the interferometer are under vacuum on suspended benches. A system of adaptive optics was to be installed to correct the mirror aberrations ''in-situ''. In the final Advanced Virgo configuration, the laser power will be 200 W.

Advanced Virgo started the commissioning process in 2016, joining the two advanced LIGO detectors ("aLIGO") for a first "engineering" observing period in May and June 2017. 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).A three-detector observation of gravitational waves from a binary black hole coalescence
, retrieved 27 September 2017

Just few days later, GW170817 was detected by the LIGO and Virgo on 17 August 2017. The GW was produced by the last minutes of two neutron stars spiralling closer to each other and finally merging, and is the first GW observation which has been confirmed by non-gravitational means.

After further upgrades Virgo started the "O3" observation run in April 2019, it was planned to last one year, followed by further upgrades. At 17:00 UTC, 27th of March, 2020, the third observation period (O3) of the Virgo Collaboration and the LIGO Scientific Collaboration was suspended because of the COVID-19 pandemic.

The gravitational wave observatories LIGO, Virgo, and KAGRA are coordinating to continue observations after the COVID-caused stop and as of 9 November 2021, plan to start the O4 Observing run together in mid-December 2022. Virgo projects a sensitivity goal of 80-115 Mpc for binary neutron star mergers (sensitivities: LIGO 160-190 Mpc, KAGRA greater than 1 Mpc).

Science case of Advanced Virgo interferometer

The Advanced Virgo interferometer aims to detect and study gravitational waves from astrophysical sources in the Universe. The main known gravitational-wave emitting systems within the sensibility of ground-base interferometers are: black hole and/or neutron star binary mergers, rotating neutron stars, bursts and supernovae explosions, and even the gravitational-wave background due to the Big Bang. Moreover, gravitational radiation may also lead to the discovery of unexpected and theoretically predicted exotic objects.

Coalescences of black holes and neutron stars

When two massive and compact objects such as black holes and neutron stars start spinning one around the other during the inspiral phase, they emit gravitational radiation and, therefore, lose energy. Hence, they begin to get closer to each other, increasing the frequency and the amplitude of the gravitational waves: it is the coalescence phenomenon and can last for millions of years. The final stage is the merger of the two objects, eventually forming a black hole. The part of the waveform corresponding to the merger has the largest amplitude and highest frequency. It can only be modeled by performing numerical relativity simulations of these systems. The interferometer is designed to be sensitive to the late phase of the coalescence of black hole and neutron star binaries: only between several milliseconds and a seconds of the whole process can be observed. All detections so far have been of black hole or neutron star mergers.

Rotating neutron stars

Neutron stars are the second most compact known object in the Universe, right after black holes. They have approximately one and a half masses as our Sun, but contained within a sphere of approximately 10-km of radius. Pulsars are special cases of neutron stars that emit light pulses periodically: they can spin up to 1000 times per second. Any small deviation from axial symmetry (a tiny "mountain" on the surface) will generate continuous gravitational waves. Advanced Virgo has not detected any signal from known pulsar, which concludes that the deviation from perfect spinning balls is less than 1 mm.

Bursts and supernovae

Any signal lasting from a few milliseconds to a few seconds is considered a gravitational wave burst. Supernovae explosions, the gravitational collapse of massive stars at the end of their lives, emit gravitational radiation that can be seen by the Advanced Virgo interferometer. A multi-messenger detection (electromagnetic and gravitational radiation, and neutrinos) would help to better understand the supernovae process and the formation of black holes.

Gravitational-wave stochastic background

The Cosmic Microwave Background (CMB) is the earliest time of the Universe that can be observed in the electromagnetic spectrum. However, cosmological models predict the emission of gravitational waves generated instants after the Big Bang. Because gravitational waves interact very weakly with matter, detecting such background would give more insight in the cosmological evolution of our Universe.

Moreover, an astrophysical background must result from the superposition of all faint and distant sources emitting gravitational waves at all times, that would help to study the evolution of astrophysical sources and star formation.

Exotic sources

Non conventional, alternative models of compact objects have been proposed by physicists. Some examples of these models can be described within General Relativity (quark and strange stars, boson and Proca stars, Kerr black holes with scalar and Proca hair), arise from some approaches to quantum gravity (cosmic strings, fuzzballs, gravastars), and also come from alternative theories of gravity (scalarised neutron stars or black holes, wormholes). Theoretically predicted exotic compact objects could now be detected and would help to elucidate the true nature of gravity or discover new forms of matter. Besides, completely unexpected phenomena may be observed, unveiling new physics.

File:GravitationalWave PlusPolarization.gif, Plus polarization
File:GravitationalWave CrossPolarization.gif, Cross polarization

Gravitational wave polarization

Gravitational waves have two polarization: "plus" and "cross" polarization. The polarization depends on the nature of the source (for instance, precessing spins in a black hole binary merger generate gravitational waves with "cross" polarization). Therefore, detecting the polarization of the gravitational radiation would give more insight in the physical properties of the system.

Goals

The first goal of Virgo is to directly observe gravitational waves, a straightforward prediction of Albert Einstein's general relativity. The study over three decades of the binary pulsar 1913+16, whose discovery was awarded the 1993 Nobel Prize in Physics, led to indirect evidence of the existence of gravitational waves. The observed evolution over time of this binary pulsar's orbital period is in excellent agreement with the hypothesis that the system is losing energy by emitting gravitational waves. The rotation motion is accelerating (its period, reported in 2004 to be 7.75 hours, is decreasing by 76.5 microseconds per year) and the two compact stars get closer by about three meters each year. They should coalesce in about 300 million years. But only the very last moments preceding that particular cosmic collision will generate gravitational waves strong enough to be visible in a detector like Virgo. This theoretical scenario for the evolution of Binary Pulsar B1913+16 would be confirmed by a direct detection of gravitational waves from a similar system, the main goal of giant interferometric detectors like Virgo and LIGO.

The longer term goal, after accomplishing the primary goal of discovering gravitational waves, Virgo aims at being part of the birth of a new branch of astronomy by observing the Universe with a different and complementary perspective than current telescopes and detectors. Information brought by gravitational waves will be added to those provided by the study of the electromagnetic spectrum (microwaves, radio waves, infrared, the visible spectrum, ultraviolet, X-rays and gamma rays), of cosmic rays and of neutrinos. In order to correlate a gravitational wave detection with visible and localized events in the sky, the LIGO and Virgo collaborations have signed bilateral agreements with many teams operating telescopes to quickly inform (on the timescale of a few days or a few hours) these partners that a potential gravitational wave signal has been observed. These alerts must be sent before knowing whether the signal is real or not, because the source (if it is real) may only remain visible during a short amount of time.

Interferometric detection of a gravitational wave

Effect of a gravitational wave in an optical cavity

In general relativity, a gravitational wave is a space-time perturbation which propagates at the speed of light. It then curves slightly the space-time, which changes locally the light path. Mathematically speaking, if $h$ is the amplitude (assumed to be small) of the incoming gravitational wave and $L$ the length of the optical cavity in which the light is in circulation, the change $\delta L$ of the optical path due to the gravitational wave is given by the formula:

$\frac = C \times h$

with $C \le 1$ being a geometrical factor which depends on the relative orientation between the cavity and the direction of propagation of the incoming gravitational wave.

Detection principle

Virgo is a Michelson interferometer whose mirrors are suspended. A laser is divided into two beams by a beam splitter tilted by 45 degrees. The two beams propagate in the two perpendicular arms of the interferometer, are reflected by mirrors located at the end of the arms and recombine on the beam splitter, generating interferences which are detected by a photodiode. An incoming gravitational wave changes the optical path of the laser beams in the arms, which then changes the interference pattern recorded by the photodiode.

The signal induced by a potential gravitational wave is thus "embedded" in the light intensity variations detected at the interferometer output. Yet, several external causes—globally denoted as noise—change the interference pattern perpetually and significantly. Should nothing be done to remove or mitigate them, the expected physical signals would be buried in noise and would then remain undetectable. The design of detectors like Virgo and LIGO thus requires a detailed inventory of all noise sources which could impact the measurement, allowing a strong and continuing effort to reduce them as much as possible. During the data taking periods, dedicated software monitors in real time the noise levels in the interferometer, and deep studies are carried out to identify the loudest noises and mitigate them. Each period during which a detector is found to be "too noisy" is excluded from the data analysis: these dead times need to be reduced as much as possible.

Detector sensitivity

A detector like Virgo is characterized by its sensitivity, a figure of merit providing information about the tiniest signal the instrument could detect—the smaller the value of the sensitivity, the better the detector. The sensitivity varies with frequency as each noise has its own frequency range. For instance, it is foreseen that the sensitivity of the advanced Virgo detector be ultimately limited by:
* seismic noise (any ground motion whose sources are numerous: waves in the Mediterranean sea, wind, human activity for instance the traffic during daytime, etc.) in the low frequencies up to about 10 Hertz (Hz);
* the thermal noise of the mirrors and their suspension wires, from a few tens of Hz up to a few hundreds;
* the laser shot noise above a few hundreds of Hz.

Virgo is a wide band detector whose sensitivity ranges from a few Hz up to 10 kHz. Mathematically speaking, its sensitivity is characterized by its power spectrum which is computed in real time using the data recorded by the detector. The curve opposite shows an example of a Virgo amplitude spectrum density (the square root of the power spectrum) from 2011, plotted using log-log scale.

Improving the sensitivity

Using an interferometer rather than a single optical cavity allows one to enhance significantly the sensitivity of the detector to gravitational waves. Indeed, in this configuration based on an interference measurement, the contributions from some experimental noises are strongly reduced: instead of being proportional to the length of the single cavity, they depend in that case on the length difference between the arms (so equal arm length cancels the noise). In addition, the interferometer configuration benefits from the differential effect induced by a gravitational wave in the plane transverse to its direction of propagation: when the length of an optical path $L$ changes by a quantity $\delta L$, the perpendicular optical path of same length changes by $-\delta L$ (same magnitude but opposite sign). And the interference at the output port of a Michelson interferometer depends on the difference of length between the two arms: the measured effect is hence amplified by a factor 2 with respect to a simple cavity.

Then, one has to "freeze" the various mirrors of the interferometer: when they move, the optical cavity length changes and so does the interference signal read at the instrument output port. The mirror positions relative to a reference and their alignment are monitored accurately in real time with a precision better than the tenth of a nanometre for the lengths; at the level of a few nanoradians for the angles. The more sensitive the detector, the narrower its optimal working point.

Reaching that working point from an initial configuration in which the various mirrors are moving freely is a control system challenge. In a first step, each mirror is controlled locally to damp its residual motion; then, an automated sequence of steps, usually long and complex, allows one to make the transition between a series of independent local controls to a unique global control steering the interferometer as a whole. Once this working point is reached, it is simpler to keep it as error signals read in real time provide a measurement of the deviation between the actual state of the interferometer and its optimal condition. From the measured differences, mechanical corrections are applied on the various mirrors to bring the system closer to its best working point.

The optimal working point of an interferometric detector of gravitational waves is slightly detuned from the "dark fringe", a configuration in which the two laser beams recombined on the beam splitter interfere in a destructive way: almost no light is detected at the output port. Calculations show that the detector sensitivity scales as $\frac$, where $L$ is the arm cavity length and $P$ the laser power on the beam splitter. To improve it, these two quantities must be increased.
* The arms of the Virgo detector are thus 3-km long.
* To increase even more (by a factor 50) the length of the laser optical paths, highly reflecting mirrors are installed at the entry of the kilometric arms to create Fabry-Perot cavities.
* Finally, as the interferometer is tuned on the dark fringe and that the mirrors located at the end of the arms are highly reflecting as well, almost all the laser power is sent back to the laser source from the beam splitter. Therefore, an additional highly reflecting mirror is located in this area to recycle the light and store it inside the instrument.

The instrument

Seen from the air, the Virgo detector has a characteristic "L" shape with its two 3-km long perpendicular arms. The arm "tunnels" house vacuum pipes with a 120 cm diameter in which the laser beams are travelling under ultra-high vacuum. To increase the interaction between the light and an incoming gravitational wave, a Fabry-Perot optical cavity is installed in each arm as well as a mirror called "recycling mirror" at the instrument entrance, between the laser source and the beam splitter.

Virgo is sensitive to gravitational waves in a wide frequency range, from 10 Hz to 10,000 Hz. The main components of the detector are the following:

* The laser is the light source of the experiment. It must be powerful, while extremely stable in frequency as well as in amplitude. To meet all these specifications which are somewhat opposing, the beam starts from a very low power, yet very stable, laser. The light from this laser passes through several amplifiers which enhance its power by a factor 100. A 50 W output power was achieved for the last configuration of the initial Virgo detector—called "Virgo+"—while in the final configuration of Advanced Virgo, the laser will deliver 200 W. The retained solution is to have a fully fibered laser with an amplification stage made of fibers as well, to improve the robustness of the system. That laser is actively stabilised in amplitude, frequency and position, in order to not inject additional noise in the interferometer, and hence to improve the sensitivity to the gravitational wave signal.
* The large mirrors of the arm cavities are the most critical optics of the interferometer. Those mirrors make a resonant optical cavity in each arm and allow to increase the power of the light stored in the 3-km arms. Thanks to this setup, the interaction time between the light and the gravitational wave signal is significantly increased. Those mirrors are non-standard pieces, made from state-of-the-art technologies. They are cylinders 35 cm in diameter and 20 cm thick, made from the purest glass in the world. The mirrors are polished to the atomic level in order to not diffuse (and hence lose) any light. Finally, a reflective coating (a Bragg reflector made with ion beam sputtering, or IBS) is added. The mirrors located at the end of the arms reflect all incoming light; less than 0.002% of the light is lost at each reflection.
* In order 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 (hence in glass) which are attached to a series of attenuators. This chain of suspension, called the 'superattenuator', is close to 10 meters high and is also under vacuum. 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, in order to limit the seismic and acoustic noises. For advanced Virgo, the whole instrumentation used to detect gravitational waves signals and to steer the interferometer (photodiodes, cameras and the associated electronics) are also installed on several suspended benches, and under vacuum. This choice and the use of light traps (called baffles) inside the vacuum pipes, prevent the residual seismic noise from being reintroduced into the dark port signals because of spurious reflections from diffused light.
* Virgo is the largest ultra-high vacuum installation in Europe, with a total volume of 6,800 cubic meters. The two 3-km arms are made of a long pipe 1.2m in diameter in which the residual pressure is about 1 thousandth of a billionth of an atmosphere. Thus, the residual air molecules are not disturbing the path of the laser beams. Large gate valves are located at both ends of the arms so that work can be done in the mirror vacuum towers without breaking the arm ultra-high vacuum. Indeed, both Virgo arms have been kept under vacuum since 2008.Private communication from Carlo Bradaschia, Virgo vacuum group leader (2015).

Gallery

File:Virgo Cascina panorama.jpg, Overview of the Virgo site.
File:VirgoDetectorAerialView.jpg, Aerial view of the Virgo detector.
File:IGP9215.JPG, View of the 3 km-long Virgo north arm.
File:IGP9210.JPG, The Virgo site with, in the foreground, the building which hosts the detector control room and the local computer center.
File:Virgo Cascina Central building.jpg, The Virgo central building which hosts the laser and the beamsplitter mirror.
File:IGP9212.JPG, View of the 3 km-long Virgo west arm (right pipe). The tube on the left, which is 150 m-long, hosts the mode-cleaner cavity which is used to spatially filter the laser beam.

See also

* BlackGEM

References

External links

Description on EGO's website


Virgo's homepage

Advanced Virgo Technical Design Report

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Interferometric gravitational-wave instruments
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