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| − | Virgo is a laser-interferometric GW detector hosted by the European Gravitational Observatory in Cascina near Pisa [https://www.virgo-gw.eu/ [Virgo homepage<nowiki>]</nowiki>]. It is currently running in its second-generation configuration known as Advanced Virgo. It consists of a developed version of a Michelson interferometer with 3km long detector arms oriented at a right angle. A laser provides a high-power optical beam at a wavelength of 1064nm, which enters the interferometer with several 10W power, then experiencing two stages of resonant amplification to reach several 100kW of light power inside the interferometer arms. The light inside the arms is contained by two pairs of suspended mirrors known as test masses. Changes of the distances between test masses can be measured. Fluctuations of the light in the output of the interferometer are due to instrumental noise (thermal noise, environmental noise, laser noise, quantum noise, ...) or due to GWs. These fluctuations are observed by a photo detector, which is the prime data channel of the Virgo detector. Essential for the operation of the detector is the seismic isolation system, also known as superattentuator in Virgo. It consists of multiple stages of passive mechanical filters (pendula and cantilevers) | + | Virgo is a laser-interferometric GW detector hosted by the European Gravitational Observatory in Cascina near Pisa [https://www.virgo-gw.eu/ [Virgo homepage<nowiki>]</nowiki>]. It is currently running in its second-generation configuration known as Advanced Virgo. It consists of a developed version of a Michelson interferometer with 3km long detector arms oriented at a right angle. A laser provides a high-power optical beam at a wavelength of 1064nm, which enters the interferometer with several 10W power, then experiencing two stages of resonant amplification to reach several 100kW of light power inside the interferometer arms. The light inside the arms is contained by two pairs of suspended mirrors known as test masses. Changes of the distances between test masses can be measured. Fluctuations of the light in the output of the interferometer are due to instrumental noise (thermal noise, environmental noise, laser noise, quantum noise, ...) or due to GWs. These fluctuations are observed by a photo detector, which is the prime data channel of the Virgo detector. Essential for the operation of the detector is the seismic isolation system, also known as superattentuator in Virgo. It consists of multiple stages of passive mechanical filters (pendula and cantilevers), which suppress seismic disturbances of the suspended test masses in Virgo's observation band. |
Together with the two LIGO detectors in the US near Livingston (Louisiana) and Hanford (Washington), Virgo contributed to major discoveries in the past years. Its first breakthrough discovery was the merger of two neutron stars (a signal known as GW170817), where Virgo was important as a component of the detector network with LIGO for the localization of the source. This made possible the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories covering frequencies from radio waves to gamma rays on ground and in space pointed to the source collecting rich information about the physics of the merger. Together with LIGO, Virgo has also provided decisive new insight into the population of black holes in our nearby universe contributing to the detection of a large number of black-hole mergers, which allowed scientists to test population models in galaxies and star clusters. Among these detections of black-hole mergers, a recent one (GW190521) is the merger of two unusually large black holes merging into what is known as intermediate-mass black hole; a new class of black holes, for which we only had vague and indirect evidence so far. | Together with the two LIGO detectors in the US near Livingston (Louisiana) and Hanford (Washington), Virgo contributed to major discoveries in the past years. Its first breakthrough discovery was the merger of two neutron stars (a signal known as GW170817), where Virgo was important as a component of the detector network with LIGO for the localization of the source. This made possible the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories covering frequencies from radio waves to gamma rays on ground and in space pointed to the source collecting rich information about the physics of the merger. Together with LIGO, Virgo has also provided decisive new insight into the population of black holes in our nearby universe contributing to the detection of a large number of black-hole mergers, which allowed scientists to test population models in galaxies and star clusters. Among these detections of black-hole mergers, a recent one (GW190521) is the merger of two unusually large black holes merging into what is known as intermediate-mass black hole; a new class of black holes, for which we only had vague and indirect evidence so far. | ||
Revision as of 22:48, 13 September 2020
Contents
GSSI Gravity Group
This page serves to present the work of the GSSI gravitational-wave group, which means that its content is strongly focused on the group's activities. We do not intend to provide a generic overview of research topics in this field.
Members
Virgo
Virgo is a laser-interferometric GW detector hosted by the European Gravitational Observatory in Cascina near Pisa [Virgo homepage]. It is currently running in its second-generation configuration known as Advanced Virgo. It consists of a developed version of a Michelson interferometer with 3km long detector arms oriented at a right angle. A laser provides a high-power optical beam at a wavelength of 1064nm, which enters the interferometer with several 10W power, then experiencing two stages of resonant amplification to reach several 100kW of light power inside the interferometer arms. The light inside the arms is contained by two pairs of suspended mirrors known as test masses. Changes of the distances between test masses can be measured. Fluctuations of the light in the output of the interferometer are due to instrumental noise (thermal noise, environmental noise, laser noise, quantum noise, ...) or due to GWs. These fluctuations are observed by a photo detector, which is the prime data channel of the Virgo detector. Essential for the operation of the detector is the seismic isolation system, also known as superattentuator in Virgo. It consists of multiple stages of passive mechanical filters (pendula and cantilevers), which suppress seismic disturbances of the suspended test masses in Virgo's observation band.
Together with the two LIGO detectors in the US near Livingston (Louisiana) and Hanford (Washington), Virgo contributed to major discoveries in the past years. Its first breakthrough discovery was the merger of two neutron stars (a signal known as GW170817), where Virgo was important as a component of the detector network with LIGO for the localization of the source. This made possible the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories covering frequencies from radio waves to gamma rays on ground and in space pointed to the source collecting rich information about the physics of the merger. Together with LIGO, Virgo has also provided decisive new insight into the population of black holes in our nearby universe contributing to the detection of a large number of black-hole mergers, which allowed scientists to test population models in galaxies and star clusters. Among these detections of black-hole mergers, a recent one (GW190521) is the merger of two unusually large black holes merging into what is known as intermediate-mass black hole; a new class of black holes, for which we only had vague and indirect evidence so far.
The Advanced Virgo and LIGO detectors and their upgrades are expected to operate until at least 2027 with the end of their fifth observing run (known as O5). Whether the infrastructures will be maintained beyond this date has not been decided yet. Preliminary studies have shown that these detectors could play an important role for GW science even in the era of third-generation detectors. In any case, new detectors with infrastructure similar to LIGO and Virgo are on the horizon already with the Japanese underground detector KAGRA (whose commissioning has already begun) as part of the Kamioka Observatory, and another detector in India known as LIGO India, which is the product of a collaboration between the LIGO project and the consortium IndIGO of Indian research institutions. The LIGO India detector is currently being constructed near Aundha Nagnath in the Hingoli district.
Einstein Telescope
The Einstein Telescope (ET) is a proposed underground infrastructure to host a third-generation, gravitational-wave observatory [ET home page]. It builds on the success of current, second-generation laser-interferometric detectors Advanced Virgo and Advanced LIGO, whose breakthrough discoveries of merging black holes (BHs) and neutron stars over the past 5 years have ushered scientists into the new era of gravitational-wave astronomy. The Einstein Telescope will achieve a greatly improved sensitivity by increasing the size of the interferometer from the 3km arm length of the Virgo detector to 10km, and by implementing a series of new technologies. These include a cryogenic system to cool some of the main optics to 10 – 20K, new quantum technologies to reduce the fluctuations of the light, and a set of infrastructural and active noise-mitigation measures to reduce environmental perturbations.
The Einstein Telescope will make it possible, for the first time, to explore the Universe through gravitational waves along its cosmic history up to the cosmological dark ages, shedding light on open questions of fundamental physics and cosmology [ET science case]. It will probe the physics near black-hole horizons (from tests of general relativity to quantum gravity), help understanding the nature of dark matter (such as primordial BHs, axion clouds, dark matter accreting on compact objects), and the nature of dark energy and possible modifications of general relativity at cosmological scales. Exploiting the ET sensitivity and frequency band, the entire population of stellar and intermediate mass black holes will be accessible over the entire history of the Universe, enabling to understand their origin (stellar versus primordial), evolution, and demography. ET will observe the neutron-star inspiral phase and the onset of tidal effects with high signal-to-noise ratio providing an unprecedented insight into the interior structure of neutron stars and probing fundamental properties of matter in a completely unexplored regime (QCD at ultra-high densities and possible exotic states of matter). The excellent sensitivity extending to kilohertz frequencies will also allow us to probe details of the merger and post-merger phase. ET will operate together with a new innovative generation of electromagnetic observatories covering the band from radio to gamma rays (such as the Square Kilometer Array, the Vera Rubin Observatory, E-ELT, Athena, CTA).
The beginning of construction is foreseen in 2026 with the goal to start observations in 2035. Two candidate sites are under investigation: one in Sardinia and one in the Euregio Meuse-Rhine. Site-characterization studies are under way towards a site selection, which is expected for 2024. The evaluation of the sites must consider the feasibility of the construction and predict the impact of the local environment on the detector sensitivity and operation. The gravitational-wave community in the US is currently working on its own third-generation detector concepts Voyager [Voyager]and Cosmic Explorer [Cosmic Explorer] towards a future global detector network with the Einstein Telescope [3G science case].
At the Gran Sasso Science Institute, the GW group is involved in experimental and design studies of the instrument, in the development of data-analysis techniques as well as the evaluation of the science capacity of the ET detector configuration, and the group also develops the science case in combination with (potential or certain) future EM facilities like THESEUS [THESEUS], E-ELT [E-ELT], or VRO (formerly LSST) [VRO].
Site Characterization and Evaluation
Site-evaluation parameters
Sardinia candidate site
Lunar Gravitational-Wave Antenna
GW Data Analysis
Advanced LIGO and Virgo detectors started the first scientific run on September 2015, and just completed the O3 run. On the first two runs, a total of 11 GW signals have been detected: O1-O2 Catalog paper. They were all coming from the coalescence and merging of compact objects, 10 from Black Hole Binaries (BBH) and 1 from a Binary Neutron Star (BNS)
The BNS arrived on is the first case of Multi-Messenger Astronomy between GW and EM.
Parameter estimation of compact binaries
Cosmology: Probing the Early Universe
Searches for generic GW transients
Instrument Science
Cryogenics
Environmental Noise
Detector Control
Earthquake early warning with gravitational sensors
Quantum noise modeling and detector configurations
Thermal noise in GW detectors
Multi-messenger astronomy
Cosmology with multi-messenger transients
Multimessenger Search of Core-Collapse Supernovae
Wiki Software
Consult the User's Guide for information on using the wiki software.
