For more information about how to access your purchased licenses visit the vGPU Software Downloads page. Need Help? Technical Support. Today, the Virgo Collaboration assigned the first ever Virgo Award, a prize that will be given annually to one Early Career Virgo Member who has made a significant and sustained contribution to the experiment.
The prize was awarded to Dr. Nardecchia "in recognition of her many relevant and continued contributions to the Virgo experiment, in particular of her deep involvement in the modeling and experimental activities which led to a successful implementation of the Virgo Thermal Compensation System. Congratulations to Ilaria Nardecchia, awardee, for this well deserved success! The award ceremony took place today at the European Gravitational Observatory, during the Virgo Week, the first in-person collaboration-wide meeting since the beginning of the pandemic.
The LIGO, Virgo, and KAGRA scientific collaborations are closely coordinating in order to begin the fourth observation period O4 together and have today announced that, despite local and global adversities, they plan to start the run in mid-December, LIGO has a sensitivity goal of Mpc for binary neutron stars. Virgo aims for a target sensitivity of Mpc. KAGRA should be running with greater than 1 Mpc sensitivity by the beginning of O4 and will work to improve the sensitivity toward the end of the run.
We believe this is the best strategy to maximise the science outcome of the run and the chances for multimessenger observations. Since then, we have begun the commissioning of the detector and we plan to be ready to restart data taking in one year from now. Image: The Control Room of the Virgo detector, from which the interferometer is operated. Most of the new signals originate from the whirling spiral of two merging black holes: cosmic quakes that shake the fabric of spacetime, generating a powerful burst of gravitational waves.
Two other events, one already reported last June , were instead identified as mergers between a neutron star and a black hole, a source observed for the first time in this last LIGO-Virgo run.
A further event, detected in February, , could come from either a pair of black holes or from a mixed pair of a black hole with a neutron star. The dataset, published today in the so-called third Catalog Paper, outlines the features of new populations of black holes, the masses of which, together with those of the observed neutron stars, may provide clues about how stars live and die, further broadening the horizons of gravitational astronomy.
No confident GW counterparts have been observed; in parallel, no signals of a different kind e. This allows the whole research community to perform independent analyses and checks, maximising the wealth of scientific results. The progress achieved in a few years by gravitational-wave scientists has been amazing, passing from the first detection to the observation of a number of events per month.
This has been possible thanks to the programme of continuous technological upgrades, which have transformed the first pioneering instruments into increasingly sensitive detectors.
The progress in detector sensitivity due to the technological upgrades and commissioning is evident, considering that, of the 90 gravitational-wave events published today, as many as 79 refer exclusively to the most recent observation period, which ran from April, , to March, The LIGO and Virgo observatories are currently undergoing a further upgrade and will start the upcoming fourth observing period, in the second half of , with an even greater sensitivity, corresponding to a volume of the Universe almost 5 times larger than before and, therefore, a much greater probability of picking up gravitational signals.
The expansion of the network of detectors able to jointly take data will further increase the accuracy of source localisation, a key feature for future developments in multi-messenger astronomy. Each box represents one event, with its name reported at the bottom of the box.
The masses of the merging objects either black holes or neutron stars as well as the final merged object are indicated in solar masses.
The colour of each box highlights in which of the three observing runs the event was detected: O1, in ; O2, in ; and O3, in The increase in the number of events in O3 was made possible by the improved performance of all three of the detectors in the network. Note that GW is also shown, even though it is considered a marginal event meaning its astrophysical origin is uncertain , which explains why 91 boxes are displayed.
This was made possible by the detection, in January , of gravitational signals nicknamed GW and GW from the dates of their detection emitted by two systems, in which a black hole and a neutron star, rotating around each other, merged into a single compact object. The existence of these systems was predicted by astronomers several decades ago, but they had never been observed with confidence, either through electromagnetic or gravitational signals, until now.
The result and its astrophysical implications have today been published in The Astrophysical Journal Letters. The gravitational signals detected in January encode valuable information about the physical features of the systems, such as the mass and distance of the two NSBH pairs, as well as about the physical mechanisms that have generated them and bring them to collapse.
The signal analysis has shown that the black hole and neutron star that created GW are, respectively, about 8. The result announced today, alongside the dozens of detections made by Virgo and LIGO to date, allow us, for the first time, a close observation of some of the most violent and rare phenomena in the Universe and to draw an unprecedented picture of the crowded and chaotic regions that are one of the possible nursery environments of these events.
Furthermore, the detailed information we have started to collect about the physics of the black hole and star mergers, gives us the chance to test the fundamental laws of physics at extreme conditions, which obviously we will never be able to reproduce on Earth. We are now upgrading the detectors with the aim of looking much farther into the depth of the cosmos, searching for new gems, seeking a deeper understanding of the universe we live in. To learn more, please click here.
How does a black hole and neutron star pair form and merge? The current astrophysical models roughly consider two main theoretical scenarios for the formation of NSBH pairs. The other possibility is that the neutron star NS and black hole BH form from separate stars in unrelated supernova explosions, and only afterwards find one another.
Based on these different theoretical scenarios it is possible to make predictions, for example, about the orientations of the black hole and neutron star rotations with respect to the orbital motions i.
Thanks to the detections announced today, for the first time, these predictions can be compared with the data of the two observed NSBH pairs, and we can start discriminating between the different astrophysical models. For instance, considering that only these two NSBH events have been detected during all of the LIGO and VIRGO observing runs, it turns out that between 5 and 15 such systems merge per year within the distance of one billion light years.
This rate appears to be especially consistent with both the isolated binary evolution and the dynamical interaction in young star clusters or in active galactic nuclei; however this estimated rate, as well as the measured spin values of GW and GW, do not allow to single out just one specific formation scenario. The last upgrade works, that marked the end of Phase I in the past few weeks, have been the installation of the new payload for the Input Mode Cleaner and the depolyment of the sensors for fighting Newtonian noise.
The new IMC payload brings in improvements on both the mechanics and surface quality of the mirror; it is also equipped with brand new baffle to absorb diffused light, instrumented to sensors that allows to monitor such diffused light, a significant source of noise for the interferometer.
Newtonian noise at Virgo is mainly due to small changes of the gravitational field around the interferometer mirrors, caused by density fluctuations of seismic origin. The newly installed sensors will allow to monitor such noise, which can later be subtracted. Other major works in this upgrades phase concerned a more powerful laser source, the installation of a suspended Signal Recycling Mirror, that allows to increase the effect of the gravitational wave measured by the interferometer, and the upgrade of the squeezing technique, already used in the past Observing run O3.
Squeezing is a technique that uses quantum mechanics to improve the sensitivity of the detector. For the next run O4, thanks to the upgrade Virgo will be able to use a frequency-dependent squeezing so to gain in sensitivity at high frequencies by reducing the photon counting noise while avoid being limited at low frequencies.
To make this possible a new, m long, ultra-low-loss optical cavity had to be installed, parallel to the 3km long North arm of Advanced Virgo, in a separated vacuum pipeline. The goal of these and other upgrades that have been carried out is to bring Virgo, after commissioning, to a sensitivity that is about double that of the last observing period. This means that during its fourth observation run O4 which will start next year, Advanced Virgo could be able to explore a portion of the universe about ten times bigger, with chances of detecting gravitational wave signals every day!
In the latest issue of the scientific journal Nature, a roadmap dedicated to the future of gravitational wave research has been published.
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