Aerial view of the EGO site, location of the Virgo interferometer
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Quantum effects make Virgo mirrors jitter

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A quantum mechanical effect measured for the first time in the Advanced Virgo and LIGO gravitational-wave detectors.

Quantum mechanics does not only describe how the world works on its smallest scales, but also affects the motion of macroscopic objects, such as the 42 kg mirrors of the Virgo interferometer. To detect gravitational waves, Virgo and LIGO measure tiny changes in the lengths of their laser interferometer arms, changes as small as one thousandth of a proton diameter. The two detectors use laser light to measure, with the highest precision, the relative position of mirrors that are kilometres apart. For this reason, these mirrors are kept as 'still' as possible and are shielded from all possible noises of human or environmental origin. Even in the absence of any gravitational-wave signals or noise sources, these mirror position measurements would show a slight jitter. This is due to the so-called shot noise, i.e. the pattern of the randomly and irregularly arriving light particles. In both Virgo and LIGO, during the third observation period (O3), this noise was reduced by 'squeezing' the light, using a particular quantum optics technique. Unfortunately, it is not possible to do this without paying a price.

Following one of the fundamental laws of quantum mechanics - Heisenberg's uncertainty principle - a reduced shot noise results in increased radiation pressure noise: the force with which the stream of light particles pushes on the mirrors, fluctuates more strongly. As a result, the mirrors, each weighing 42 kg, move back and forth more, simply because of the effects of quantum mechanics. In fact, the shot noise affects the sensitivity of the detector at high frequencies, while the radiation-pressure noise disturbs the detection of signals with lower frequencies. Getting out of this impasse is not easy. If, on the one hand, the detectors increase sensitivity at high frequencies, and therefore to a certain type of gravitational-wave source, on the other, they become less able to identify low-frequency signals.

"Thanks to the collaboration with the Albert Einstein Institute in Hannover", explains Jean Pierre Zendri, senior researcher of the Istituto Nazionale di Fisica Nucleare (INFN) in Padova and member of the Virgo Collaboration, "we succeeded to show for the first time a clear evidence of the radiation-pressure noise on the massive detector mirrors. This was allowed by the extraordinary sensitivity of Advanced Virgo, which allows us to appreciate fluctuations of the mirror positions to less than a thousandth of a proton diameter." The results of this research have now been published in Physical Review Letters.

To further improve the detector's performance, gravitational-wave scientists are developing a new technology, called frequency-dependent squeezing, which will make it possible to reduce the quantum mechanical noise at both high and low frequencies. The implementation of this technology is actually one of the crucial steps of the upgrade of the Advanced Virgo Interferometer, which will be taking place over the coming months at the European Gravitational Observatory near Pisa in Italy.

Image: The Virgo test-mass mirror inside its actuation-cage. The mirror and actuation-cage are both suspended from a Virgo Superattenuator. A layer of protective polymer (visible in pink) still covers the mirror, preventing dust contamination during installation. On the left, two mirrors can be seen. These are part of the sensor that monitors the tiny thermal deformations of the test-mass mirror occurring during operation. Black-coated panels surround the optical elements to absorb residual stray light.

Image credit: EGO/Virgo Collaboration/Perciballi

Posted: 24/09/2020

Virgo and LIGO unveil new and unexpected black hole populations

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Virgo and LIGO have announced the detection of an extraordinarily massive merging binary system: two black holes of 66 and 85 solar masses, which generated a final black hole of 142 solar masses. Both the initial black holes, as well as the remnant, lie in a range of mass that has never before been observed, either via gravitational waves or with electromagnetic observations.

The final black hole is the most massive ever detected with gravitational waves.

The gravitational-wave event was detected by the three interferometers of the global network on the 21st of May, 2019, and is hence named GW190521. Two scientific papers reporting the discovery and its astrophysical implications have been published today (see the scientific papers here and here).

The breaking of the mass record of the Virgo and LIGO observational runs is just one of the many special features that make the detection of this exceptional merger an unprecedented discovery. A crucial aspect, which particularly drew the attention of astrophysicists, is that the remnant belongs to the class of the so-called intermediate-mass black holes (from a hundred up to a hundred thousand times the mass of the Sun).

The interest in this black-hole population is linked to one of the most fascinating and challenging puzzles for astrophysicists and cosmologists: the origin of supermassive black holes. These giant monsters, millions to billions of times heavier than the Sun and often at the centre of galaxies, may arise from the merger of 'smaller' intermediate-mass black holes. Until today, very few intermediate-mass black-hole candidates have been identified through electromagnetic observations alone and the remnant of GW190521 is the first observation of an intermediate-mass black hole via gravitational waves.

Read the full story in the EGO-Virgo press release.

Image: Artistic interpretation of the binary black hole merger responsible for GW190521. Space-time, shown as a fabric on which a view of the cosmos is printed, is distorted by the GW190521 signal. The turquoise and orange mini-grids represent the dragging effects due to the individually rotating black holes. The estimated spin axes, or self-rotations, of the black holes are indicated with the corresponding coloured arrows. The background suggests a star cluster, one of the possible environments in which GW190521 could have occurred.

Image credit: Raúl Rubio / Virgo Valencia Group / The Virgo Collaboration

Posted: 02/09/2020

GW190814 - the merger of a 23-solar-mass black-hole and an enigmatic lighter object

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Another unprecedented discovery has just been unveiled by LIGO-Virgo scientists. Data from the third observation period (O3) of the Advanced LIGO and Advanced Virgo detectors reveal that, at 21:10 (UTC) on the 14th of August, 2019, the three instruments in the network detected a gravitational-wave signal, called GW190814. The signal originated from the merger of an enigmatic couple: a binary system composed of a black hole, 23 times heavier than our sun, and a much lighter object, about 2.6 times the mass of the Sun. The merger resulted in a final black hole about 25 times the mass of the sun.

It is this lighter object that makes GW190814 so special. It may just be either the lightest black hole or the heaviest neutron star ever discovered in a binary system. Another peculiar feature of GW190814 is the mass ratio of the objects in the binary system. The factor 9 ratio is even more extreme than was the case with the first detected merger of a binary with unequal masses, GW190412.

"Once again, gravitational-wave observations are shedding light on the unknown. The lightest object in this system has a mass that has never before been observed", says Giovanni Losurdo, of Istituto Nazionale di Fisica Nucleare (Italy) and the spokesperson of the Virgo Collaboration. "A new discovery, which raises new questions. What is its nature? How did such a binary system form? Virgo, LIGO and, soon, Kagra in Japan, will continue to search for the answers and push forward the frontier of what we know about the cosmos in which we live."

The mass asymmetry causes the presence of higher multipoles in the gravitational radiation, a fact that allows stringent tests of General Relativity. Once again, all our tests confirm the prediction of Einstein’s theory. Moreover, the higher multiples allow us to disentangle the determination of the source distance from the inclination angle of the plane of the orbiting binary. We have found the source of the gravitational wave to be about 800 million light years away!

The signal was clearly detected by the three instruments, with an overall signal-to-noise ratio as high as 25. Thanks mainly to the delay between the signal arrival times at the three, well separated detectors, the network was able to localise the origin of GW190814 to within about 19deg2 in the sky. This is similar to the localisation achieved for the famous GW170817, which gave birth to multi-messenger astronomy with gravitational waves. In the case of GW190814, however, an electromagnetic counterpart has yet to be observed.

"We are very satisfied with the performance of Advanced Virgo during O3," says Maddalena Mantovani, scientist at the European Gravitational Observatory (EGO). "We reached the target sensitivity with a very good duty cycle. This is the result of the hard work of the scientists and technicians that have fine-tuned the machine to provide its best performance. Scientific discoveries such as GW190814 are the best rewards for all those days and nights spent on improving the detector."

Image: Artistic rendering of the GW190814 event, in which a smaller compact object is swallowed by a 9-times-more-massive black-hole. The matter stream between the two objects and the look of the massive black hole are an artistic invention. To the best of our knowledge, the GW190814 fusion is not thought to have emitted any light.

Image/Animation credit: Alex Andrix

Posted: 23/06/2020

GW190412: The merger of two black holes with unequal masses

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The third LIGO-Virgo observing period (O3) is offering new insights into the late inspiral and merger phase of binary black hole (BBH) systems. The first gravitational wave event GW150914, detected back in 2015, originated from a binary black hole merger, and since then this class of events has become the most prominent. This allows us to advance in the characterization of the population of astrophysical BBHs. However, the systems observed so far were formed by black holes of nearly equal masses. This balance was broken by the observation of the merger of a very special BBH on the 12th of April, 2019 at 05:30:44 UTC, just a couple of weeks after the start of O3, on the 1st of April.

The signal, named GW190412, was detected by the Advanced Virgo and the two Advanced LIGO detectors, and it was produced by a coalescing BBH system with unequal masses, one component being more than 3 times heavier than the other one. More in detail, the merged black holes had masses respectively about 30 and 8 times the mass of the Sun. The mass difference produces specific signal modulations that were predicted by theory, but have now been observed for the first time. In fact, the mass unbalance produces an unusually high intensity of gravitational radiation in the so-called "Higher Order Modes", which are detectable in GW190412 and provide yet another confirmation of the validity of Einstein’s General Relativity. GW190412 also depends on other parameters of the binary system which cause modulations that enable us to constrain the inclination of the plane of the binary with respect to the line of sight and the distance of the source; two quantities that are otherwise highly correlated.

"The Virgo and LIGO detectors are becoming more and more sensitive, the rate of detections increases and we expect new and unusual events. GW190412 is unusual and interesting, because of the large mass difference between the two coalescing black holes. We are learning that systems of this kind exist and how rare they are. This will allow us to deduce how they formed, which is something that I find exciting", says Giancarlo Cella, researcher at Istituto Nazionale di Fisica Nucleare (INFN) and the Virgo Data Analysis Coordinator.

"The unequal masses of this source caused overtones of the main signal to be visible for the very first time. This provided us with an exciting new opportunity to test an important prediction of Einstein’s theory about what happens when black holes of unequal size collide", says Anuradha Samajdar, postdoc fellow at the Dutch National Institute for Subatomic Physics (Nikhef), and member of the Virgo Collaboration.

Image: The distance inferred for the source of GW191412 versus the inclination angle of the binary’s orbit with respect to the line of sight. In general the two quantities are highly correlated but the different masses of the BH in the binary allow us to partially disentangle them. The distance is most likely about 700 Mpc, that is 2.3 billions of light years.

Image credit: LIGO Scientific Collaboration/Virgo Collaboration

Posted: 20/04/2020

New spokesperson for the Virgo Collaboration

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Giovanni Losurdo, research director at the Institute for Nuclear Physics (INFN) in Italy, has been appointed as the new Spokesperson of the Virgo Collaboration. From 2009 to 2017, he was Project Leader of Advanced Virgo, the programme of upgrades to the detector that made it possible for Virgo to participate alongside the two LIGO detectors, in the US, in the second observation period, called 'O2'.

Giovanni succeeds Jo van den Brand, from Nikhef, Amsterdam, and professor at Maastricht University in The Netherlands, who has served as Virgo Spokesperson from the 1st of May 2017 to the 30th of April 2020. Jo's tenure covered both the second and third joint-observation periods with the LIGO detectors, which have produced a wealth of scientific results.

The Spokesperson represents the 550 scientists, engineers and technicians of the Virgo Collaboration, coming from more than 100 institutions in 10 different European countries. A map of the Virgo Collaboration can be found here.

"Over the next few years we will face very important and exciting challenges," stated the newly-elected Spokesperson. "We will start with a substantial upgrade of the detector, which will allow us to explore a bigger and bigger portion of our universe. In the next data-taking period, for instance, we aim to observe coalescences of neutron stars that are at a distance of up to 300 million light years from us. Subsequently, our collaborations and relations with other astronomers and physicist communities will become even more intense and will have to become even more effective. This will enable us to achieve a deeper understanding of the physics behind the detected events, to further develop multi-messenger astronomy and to fine-tune technologies needed for the next generation of gravitational detectors, such as the Einstein Telescope."

"It has been an honour serving the Virgo Collaboration these last three years," says Jo van den Brand. "Rapid commissioning of Virgo was of paramount importance and in the first three months we managed to increase Virgo's sensitivity from 30 kpc to about 30 Mpc. Then Virgo joined data taking with the LIGO detectors. We immediately made spectacular detections and kicked off the new field of multi-messenger astronomy with gravitational waves. After upgrading and commissioning Virgo to double the sensitivity up to 61 Mpc, we carried out observing run O3. Although COVID-19 forced us to suspend the run early, O3 was a big success. No less than 56 non-retracted alerts were released and the collaboration is now working enthusiastically to extract the science from the O3 data. I thank my colleagues in the Virgo Collaboration and at EGO for their dedication, their inspiring and critical discussions, and their creativity that allowed Virgo to succeed. I am certain that with Giovanni they are in good hands, and I wish him all the best!"

Image: Giovanni Losurdo, new Virgo Collaboration Spokesperson.

Image credit: EGO/Virgo Collaboration/D'Andrea

Posted: 18/04/2020

LIGO-Virgo observation period suspended because of COVID-19

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The LIGO Scientific Collaboration and the Virgo Collaboration (the LVC) have agreed to suspend their third observation period, named O3, which has been running since the 1st of April, 2019. The suspension, which will be effective within one week, is motivated by the worldwide COVID-19 pandemic. Public health and worker safety are always the top priority for the LVC.

"It is certainly difficult to be obliged to suspend the run at the moment that Virgo had reached maximum sensitivity and a quasi-faultless operation", says Stavros Katsanevas, director of the European Gravitational Observatory (EGO) that hosts Virgo, "but the first priority of the worldwide collaboration and the EGO-Virgo managements in particular, is to preserve the health of the people; both those working at the site and the public at large. Here I cannot but praise the composure, the calmness and the dedication to the task, of the people on site, with the EGO operators first at the line-front, who have operated the detector these last few weeks, in the difficult conditions we all know. This is certainly a good augur for the restart of the operations, when the conditions permit it."

"Even though we had suspend the run early, O3 has been tremendously successful, thanks to the collective efforts of the LVC", says Jo van den Brand, spokesperson of the Virgo Collaboration, from Nikhef, Amsterdam and professor at Maastricht University in The Netherlands. "The discovery of GW190425, the second observation of a gravitational-wave signal consistent with the merger of a binary-neutron-star system after GW170817, has already been reported."

Much more is expected to be discovered as scientists work on the analysis of the data collected during the run: 56 detection candidates have already been announced as public alerts, as reported in the freely accessible Gravitational Wave Candidate Event Database. The alerts facilitate follow-up observations by other telescopes (e.g. electromagnetic and neutrino) and enhance the extraordinary potential of multi-messenger astronomy, pioneered with the GW170817 event.

O3 had been planned to last for one full year and, taking into account a one-month break, in October 2019, which was dedicated to commissioning activities, had been due to end on the 30th of April, 2020.

Image: The control room of Advanced Virgo at the European Gravitational Observatory, near Pisa (Italy). Shown in the foreground is an EGO operator working on shift to keep the detector running. Usually a lively environment, the control room is now minimally populated because of the COVID-19 pandemic. The image shows only one Virgo scientist working, Julia Casanueva, in the control room along with the EGO operator, Fabio Gherardini.

Image credit: EGO/Virgo Collaboration

Posted: 25/03/2020
A binary neutron star system just before merger: the two stars are deformed by tidal forces and are about to fuse together. The image is produced by a numerical simulation in General Relativity and shows the mass density volume rendering at nuclear densities in blue and lower density material in red. The snapshot refers to the central volume of approximately 45^3 km.

GW190425: the merger of a compact binary with total mass of about 3.4 Msun

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A binary neutron star system just before merger: the two stars are deformed by tidal forces and are about to fuse together. The image is produced by a numerical simulation in General Relativity and shows the mass density volume rendering at nuclear densities in blue and lower density material in red. The snapshot refers to the central volume of approximately 45^3 km. A binary neutron star system just before merger: the two stars are deformed by tidal forces and are about to fuse together. The image is produced by a numerical simulation in General Relativity and shows the mass density volume rendering at nuclear densities in blue and lower density material in red. The snapshot refers to the central volume of approximately 45^3 km.

On April the 25th, 2019, the network of gravitational-wave (GW) detectors formed by the European Advanced Virgo, in Italy, and the two Advanced LIGO, in the US, detected a signal, named GW190425. This is the second observation of a gravitational-wave signal consistent with the merger of a binary-neutron-star system after GW170817. GW190425 was detected at 08:18:05 UTC; about 40 minutes later the LIGO Scientific Collaboration and the Virgo Collaboration sent an alert to trigger follow-up telescope observations.

The source of GW190425 is estimated to be at a distance of 500 million light years from the Earth. It is localized in the sky within an area about 300 times broader than was the case for the BNS observed by LIGO and Virgo in 2017, the famous GW170817, which gave birth to multi-messenger astrophysics. However, unlike GW170817, no counterpart (electromagnetic signals, neutrinos or charged particles) has been found to date.

There are a few explanations for the origin of GW190425. The most likely is the merger of a BNS system. Alternatively, it might have been produced by the merger of a system with a black hole (BH) as one or both components, even if light BHs in the mass-range consistent with GW190425 have not been observed. Yet, on the basis solely of GW data, these exotic scenarios cannot be ruled out. The estimated total mass of the compact binary is 3.4 times the mass of the Sun. Under the hypothesis that GW190425 originated from the merger of a BNS system, the latter would have been considerably different to all known BNS in our galaxy, the total mass range of which is between 2.5 and 2.9 times the mass of the Sun. This indicates that the NS system that originated GW190425 may have formed differently than known galactic BNSs.

"After the surprise of the initial results", says Alessandro Nagar of the Istituto Nazionale di Fisica Nucleare (INFN) of Turin, Italy, "we have finally reached a reliable understanding of this event. Although predicted theoretically, heavy binary systems like those that might have originated GW190425 may be invisible through electromagnetic observations."

"While we did not observe the object formed by the coalescence, our computer simulations based on general relativity predict that the probability that a BH is formed promptly after the merger is high, about 96%", says Sebastiano Bernuzzi of the University of Jena, Germany.

Image: A binary neutron star system just before merger: the two stars are deformed by tidal forces and are about to fuse together. The image is produced by a numerical simulation in General Relativity (animation) and shows the mass density volume rendering at nuclear densities in blue and lower density material in red. The snapshot refers to the central volume of approximately 45 km in diameter.

Image credit: CoRe / Jena FSU

Press release - Communiqué de presse - Notas de prensa - Materiały dla prasy

Posted: 06/01/2020

O3 restarts

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Advanced Virgo and the two Advanced LIGO detectors resume the taking of science data on the 1st of November, 2019, following a one-month-long stop. This event marks the restart of the third observation period, named O3, which started on the 1st of April, 2019. All three of the interferometers in the global gravitational-wave observatory paused O3 on the 1st October, 2019, in order to work on improvements to enhance the performance of the detectors.

On the Virgo side, the focus was on increasing the laser power injected into the interferometer, from 19 W to 26 W. This increase has been effective in improving the detector sensitivity at high frequencies, but has required a complete re-tuning of the interferometer.

Effort was also devoted to the study of selected noise sources. The lessons learned will be useful for the future operation of the instrument.

"The month of commissioning has been quite intense. We performed many activities, both to better understand the noise that limits the sensitivity and to handle a 30% increase in the laser input power", says Matteo Tacca, researcher at Nikhef in The Netherlands, and the Virgo Commissioning Coordinator.

"We were able to find the sources of some of the noise limiting Virgo’s sensitivity. A few of them have been removed, while others require further measurements. Also mitigation strategies are under investigation. After a lot of work fine-tuning the interferometer, we were able to recover stable operation with higher input power".

Many activities were also performed at the two LIGO detectors in the US, such as the installation of special fences at the Hanford site in order to reduce wind noise. For more information see ligo.org.

O3 will now run with no further interruptions until the 30th of April, 2020.

Image: Scientist at work in the Advanced Virgo detection area, investigating noise caused by scattered light. The pipes in the picture have been temporarily equipped with monitoring accelerometers and actuators in order to perform diagnostic measurements Virgo laser source.

Image credit: EGO/Virgo Collaboration/Francescon

Posted: 04/11/2019
O3 start

Virgo and LIGO join forces for a new year-long signal hunt

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O3 start O3 start

The Virgo and LIGO detectors are ready to start the new Observing run called O3, lasting a whole year. The hunt for gravitational waves is set to start on April 1st when the European Virgo detector, based in Italy at the European Gravitational Observatory (EGO), and the LIGO twin detectors, located in the state of Washington and Louisiana (USA), will start to take data becoming together the most sensitive gravitational wave observatory to date. During a one-year period the LIGO and Virgo Collaborations will register science data continuously, and the three detectors will operate as a global observatory.

"With respect to the second observation period O2, the Virgo sensitivity has improved by about a factor of 2, which means that the volume of the observable Universe has increased by a factor of 8", says Alessio Rocchi, researcher at INFN and Virgo’s commissioning coordinator.

"The quality of the data collected by the instruments is a determining factor to detect gravitational-wave signals buried into noise and to measure their properties", said Nicolas Arnaud, CNRS researcher currently seconded to EGO and Virgo detector characterization coordinator. "A lot of progress has been made in that direction since O2, thanks to the combined effort of the collaboration as a whole, from the instrumentalists to the data analysts".

For more information, please click here.

The scientific output of O3 is expected to be tremendous and it will potentially reveal new exciting signals coming form new sources such as the merger of mixed binaries made by a black hole and a neutron star. The O3 run will also target long lasting gravitational waves produced for instance by spinning neutron stars which are not symmetric with respect to their axis; however, the detection of such signals is still an enormous challenge and the LIGO and Virgo Collaborations are raising up to it. Furthermore, signals for the merger of binary black holes are expected to become quite common, perhaps up to one per week. Scientists also expect to observe several binary neutron star mergers.

"The new software we have built is able to send Open Public Alerts within five minutes", says Sarah Antier, postdoc at the Université Paris Diderot and responsible of the low latency program for the Virgo Collaboration. "This will allow to follow-up the gravitational wave signal with neutrino and/or electromagnetic searches, that may lead to multimessenger discoveries. Observations of many signals as we expect during O3 will give us a census of the population of stellar mass remnants and a better understanding of the violent Universe."

Since August 2017 both LIGO and Virgo have been updated and tested. In particular Virgo has fully replaced the steel wires which were used in O2 to suspend the four main mirrors of the 3 km long interferometer: the mirrors are now suspended with thin fused-silica (‘glass’) fibres, a procedure which has allowed to increase the sensitivity in the low-medium frequency region, and has a dramatic impact in the capabilities to detect mergers of compact binary systems. A second major upgrade was the installation of a more powerful laser source, which improves the sensitivity at high frequencies. Last but not least squeezed vacuum states are now injected into Advanced Virgo, thanks to a collaboration with the Albert Einstein Institute in Hannover, Germany. This technique takes advantage of the quantum nature of light and improves the sensitivity at high frequencies.

Image: The image shows the rear-side view of a suspended mirror. The coating reflects the Virgo near-infrared laser beam, but is transparent in the visible range. A scientist is finally releasing the safety stops used during installation. The 42kg-mass mirror is suspended from four thin fused-silica fibres, which are bonded to the sides of the mirror.

Image credit: EGO/Virgo Collaboration/Perciballi

Posted: 26/03/2019
O2 dataset

O2 data set now available

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O2 dataset O2 dataset

LIGO and Virgo have made publicly available the strain data from the O2 observing run. These data are now available through the Gravitational Wave Open Science Center.

The O2 observing run began on the 30th of November, 2016 and ended on the 25th of August, 2017. This was the second observing run of Advanced LIGO, and the first observing run of Advanced Virgo, which joined O2 on the 1st of August, 2017.

The release includes over 150 days of recorded data from each of the two LIGO observatories, as well as 20 days of recorded data from Virgo, making this the largest data set of 'advanced' gravitational-wave detectors to date. Observations in O2 include seven binary black hole mergers, as well as the first binary neutron star merger observed in gravitational waves, all recently published in the GWTC-1 catalogue. Along with the strain data, the release contains detailed documentation and links to open-source software tools. As with previous data releases, the O2 data set should be useful for both scientific investigations and educational activities.

The figure on the left shows the sensitivity achieved during O2 of the three detectors in the network.

Posted: 28/02/2019

About

Working in the tower

What is Virgo?

Virgo is an interferometric gravitational-wave antenna. It consists of two 3-kilometre-long arms, which house the various machinery required to form a laser interferometer.

A beam-splitter divides a laser beam into two equal components, which are subsequently sent into the two interferometer arms. In each arm, a two-mirror Fabry-Perot resonant cavity extends the optical length from 3 kilometres to approximately 100. This is because of multiple reflections that occur within each cavity and which consequently amplify the tiny distance variation caused by a gravitational wave.

The two beams of laser light that return from the two arms are recombined out of phase so that, in principle, no light reaches the so-called 'dark fringe' of the detector. Any variation caused by an alteration in the distance between the mirrors, produces a very small shift in phase between the beams and, thus, a variation of the intensity of the light, which is proportional to the wave's amplitude.

Click here for more information on the Virgo experiment and its science.

The Virgo Collaboration

Virgo is a gravitational-wave interformeter designed, built and operated by a collaboration made up of 20 laboratories in 6 countries and involves the following institutions:

CNRS INFN NIKHEF EGO WIGNER IMPAS VALENCIA

Virgo Outreach

Interesting events are always being prepared at EGO-Virgo. Please view our Outreach website for details on up and coming, as well as recent, events.

Virgo and LIGO

Virgo and the LIGO Scientific Community work together in many areas and have a specific agreement on the exchange of data. More information on the work of our LIGO colleagues is available here.

More information on the identification and follow up of electromagnetic counterparts of gravitational wave candidate events is available here.

The Virgo-EGO Scientific Forum

Virgo and EGO have also established a scientific forum - the VESF - for astrophysicists and theorists, dedicated specifically to the furthering of scientific knowledge related to Virgo. More information is available here.

A payload

ET - Einstein Telescope

The Einstein Telescope (ET) project is dedicated to the development of a critical research infrastructure for a third-generation gravitational-wave interferometer. More information about the project, which is supported by the European Commission as part of the Framework Programme 7, is available here.

Other gravitational-wave experiments

Have a look at some of the other gravitational wave experiments:

Interferometric experiments

Pulsar-timing-array experiments

Other gravitational-wave-related websites

Jobs & Fellowships

The following roles are currently being advertised within the Virgo Collaboration:

Roles at the European Gravitational Observatory (EGO) are advertised on the EGO website.

Visits

Virgo viewed from the south

Events

If you are looking for information on an up-coming or recent event, please visit our Outreach website.

Opening hours

The Reception at the EGO site is open at the following times:

  • Monday to Friday, from 08:30 to 13:00 and 14:00 to 17:30
  • Closed on Saturdays and Sundays (except when site visits are scheduled)

How to get to Virgo

Virgo is at the site of the European Gravitational Observatory (EGO), the organisation responsible for the site, and is located in:

Via Amaldi
56021 Santo Stefano a Macerata – Cascina (Pisa), Italy.

As Virgo is located in the countryside, it is not particularly easy to access without a car, as there are no public transport links directly to it.

Arriving by car

The EGO-Virgo site GPS coordinates (in DD) are:

  • Latitude: 43.6305 N
  • Longitude: 10.5021

Arriving by plane/train and taxi

The nearest airport to Virgo is Pisa Galileo Galilei International Airport.

If you are travelling by aeroplane and arrive at the Pisa Galileo Galilei International Airport, or by train and arrive at Pisa Central train station, we recommend that you call a taxi (Co.Ta.Pi Radiotaxi Pisa, +39 050 54 16 00) complete your journey to EGO-Virgo.

It takes about 20-30 minutes to reach the site coming from Pisa when coming by car. The taxi fare from Pisa to the EGO-Virgo site costs about €35-40.

What do on arrival at the EGO-Virgo site

All visitors must present themselves at the site-entrance gate, where they will be met by their EGO contact person.

Visitors' vehicles may be parked at the site, in the appropriate parking areas.

New Virgo collaborators

New Virgo collaborators must complete the association and safety procedures before starting any activity on site. To this end, they should contact the EGO Administration (Building 4, first floor, +39 050 752 522/325) and the Safety and Security Office (Building 1, +39 050 752 416/544).

Badges to access the site and an account to access the Virgo documentation will only be granted by the IT department on completion of this process.

Contact

The Virgo experiment at the European Gravitational Observatory

Address: Via Amaldi, 56021 Santo Stefano a Macerata, Cascina (Pisa), Italy.

Phone: +39 050 752 511

Fax: +39 050 752 550

Email: info@ego-gw.it

Web: http://www.virgo-gw.eu

Twitter: https://twitter.com/ego_virgo

Facebook: https://it-it.facebook.com/EGOVirgoCollaboration/

Youtube: EGO & the Virgo Collaboration - LIGO-Virgo

Instagram: LIGO-Virgo

Giovanni Losurdo, Virgo Spokesperson

Phone: +39(0) 75 2317

Email: losurdo@pi.infn.it

Web: https://www.pi.infn.it/~losurdo/

Address: INFN - Pisa Division - Largo Pontecorvo 3, Ed. C - 56127 - Pisa - Italy

The Virgo Collaboration

A full list of members of the Virgo Collaboration and their contact details is available here.

Please get in contact if you would like more information.