Einstein Telescope Wiki - User contributions [en]

File:Samuele.jpg

2022-02-02T11:30:01Z

Samuele.ronchini: Samuele.ronchini uploaded a new version of File:Samuele.jpg

Electromagnetic counterparts of GW events

2021-05-03T12:43:23Z

Samuele.ronchini:

[[File:Jet.png|thumb]]
== High energy emission ==
With the joint detection of GW170817/GRB170817 we had for the first time the confirmation that short GRBs are associated to the coalescence of compact binaries. Such epochal discovery opened the door for a revolutionary era for astronomy. 

In our group we work on solving open issues about GRB physics, with both a theoretical and an observational approach. The jet launching mechanism, the jet structure, particle acceleration, emission and dissipation processes are all open points in the GRB field, which need to be addressed. The exploitation of multi-wavelength data from different observatories (from radio to γ-rays) is necessary to fully characterise the spectral and temporal properties of these enigmatic objects. A complete and extensive exploration of the GRB phenomenology is of cardinal importance to establish the optimal observational strategy for current and next-generation astronomical facilities, in synergy with gravitational wave observatories. The optimisation of joint detection strategies relies on the knowledge of GRB population properties, which, for the sub-class of short GRBs, is still incomplete and needs to be refined. 

From the EM observation of GRB170817, it was possible to constrain the jet structure of the GRB, namely its geometry and the angular energy distribution. Such structure likely deviates from the spherical approximation due to the interaction of the jet with the post-merger ejected material. A deeper comprehension of the structure formation and the nature of the emission processes would allow us to correctly predict the EM emission at all angles and in all energy bands. 

As part of our projects, we are developing theoretical tools to predict the EM emission from a structured jet, in order to evaluate the rate of joint detections that ET, in synergy with future astronomical facilities, will be able to achieve. In our treatment we include both the prompt emission component and the following afterglow phase. In this context, the transition from the prompt to the afterglow is strongly dependent on the jet structure, leading to a wide range of possible temporal behaviour of the observed flux, like the steep decay phase or the plateau phase. Such studies can test the intriguing hypothesis of a universal jet structure, which impacts on the overall properties of the short GRB population, e.g. the luminosity function, which is still poorly constrained. 

We are also deeply active in the development of the science case of the mission concept THESEUS, an extremely promising wide field telescope devoted to the high energy observation of GRBs, whose role would be crucial for the future of multi messenger studies. 

== Kilonova emission ==

In coincidence with GW170817, we detected the kilonova AT2017gfo as a thermal electromagnetic transient in the visible and infra-red spectrum. Kilonovae (KN) are powered by the radioactive decay of heavy elements, whose production is due to the rapid neutron capture process in the neutron-rich matter ejected during and/or soon after the merger. In addition to binary neutron stars (BNS), also black hole - neutron (BH-NS) star mergers are expected to be a site for the production of heavy elements and the appearance of KN. To date, the origin of heavy elements in our Universe is still an open problem and the investigation of KN signals will help us in uncovering the mystery. 
The next run of LIGO/VIRGO, and following runs together with Advanced LIGO, Kagra, and LIGO-India, are going to sample more and more BNS and BH-NS mergers. Moreover, next-generation GW interferometers, as the ET and Cosmic Explorer (CE), will enlarge the horizon of detectable binaries and improve the estimate of the source parameters. Moreover, many satellites and telescopes search for the EM counterparts, and next-generation telescopes will allow better measurements at higher luminosity distances.
In our research group, we are involved in the theoretical modeling of the lightcurves and spectra of KN. This allows us to predict the timescales for the appearance and duration of KN in the different portions of the EM spectrum, as well as the energy evolution. These models are pivotal not only to interpret the data but also to coordinate the multi-messenger follow-up after GW events.
The knowledge of kilonova spectra is expected to improve our understanding of the nucleosynthesis processes in compact binary mergers. Moreover, the improvement of kilonova models together with the detections could shed some light on the still unknown equation of state of neutron stars. 

Joint GW+EM detections will also allow to shed light on the nature of the remnant, which in turn is responsible for the jet launching. Indeed, it is currently under debate whether a neutron star, as final product of a compact binary merger, is capable to create the favourable conditions for the jet collimation and ejection. The high sensitivity of future GW detectors, like the Einstein Telescope, will probe the nature of the post-merger object and pose a final answer to this issue.

Members

2021-04-13T14:31:22Z

Samuele.ronchini:

== Current gravitational-wave group at Gran Sasso Science Institute ==
<gallery caption="" widths=300px heights=300px perrow=4>
File:Eugenio.jpg|'''Eugenio Coccia'''. Full professor and current rector of GSSI.
File:JanHarms.jpg|'''Jan Harms'''. Associate professor working on instrument science of current and future GW detectors, and data analysis of modeled and unmodeled GW signals.
File:Marica.jpg|'''Marica Branchesi'''. Associate professor working on multi-messenger astrophysics and observations with gravitational-waves.
File:AndreaMaselli.jpg|'''Andrea Maselli'''. Assistant professor working on LISA and ET signal modeling and testing GR.
File:Giulia.jpg|'''Giulia Pagliaroli'''. Assistant professor studying supernova neutrino physics and coincidence analyses with gravitational waves.
File:Gor.jpg|'''Gor Oganesyan'''. Postdoc working on the theoretical modeling and analysis of GRB signals and afterglows.
File:MatteoDiGiovanni.jpg|'''Matteo Di Giovanni'''. Postdoc working on the characterization of the Sardinian candidate site of the Einstein Telescope, and GW burst analyses.
File:Simone.jpg|'''Simone Dall'Osso'''. Postdoc studying the physics of magnetars and post-merger GW signal models.
File:SoumenKoley.jpg|'''Soumen Koley'''. Postdoc studying seismic environments of GW detectors and implementing a cancellation system for noise from terrestrial gravity fluctuations.
File:BorisGoncharov.jpg|'''Boris Goncharov'''. Postdoc working on pulsar timing arrays and ET data-analysis problems.
File:Nandita.jpg|'''Nandita Khetan'''. PhD student exploring astrophysical transients for their use as cosmological probes at different scales and developing calibration techniques to standardize them.
File:Tomislav.jpg|'''Tomislav Andric'''. PhD student working on the site characterization of Sardinia candidate site for Einstein Telescope. He also works on estimation, modelling and mitigation of Newtonian Noise in Einstein Telescope.
File:Samuele.jpg|'''Samuele Ronchini'''. PhD student studying prompt and afterglow emissions of GRBs, in the context of joint GW+EM detections with current and future facilities.
File:Nandini.jpg|'''Nandini Hazra'''. PhD student doing cosmology with SFB calibrated signals.
File:EleonoraLoffredo.jpg|'''Eleonora Loffredo'''. PhD student working on theoretical modelling of kilonovae.
File:ElenaCodazzo.jpg|'''Elena Codazzo'''. PhD student modeling the distribution of transient GW signals from star clusters.
</gallery>

== Collaborators at LNGS ==
<gallery caption="" widths=300px heights=300px perrow=4>
File:StefanoPirro.jpg|'''Stefano Pirro''' Staff scientist at INFN LNGS. He dedicates part of his time on cryogenics R&D for the Einstein Telescope.
File:AntonioAddabbo.jpg|'''Antonio D'Addabbo''' Postdoc at GSSI working for Cuore at LNGS. He dedicates part of his time on cryogenics R&D for the Einstein Telescope.
</gallery>

== Former group members ==
<gallery caption="" widths=200px heights=200px perrow=8>
File:Marco.jpg|'''Marco Drago'''. Assistant professor
File:DonatellaFiorucci.jpg|'''Donatella Fiorucci'''. Postdoc
File:MatteoLorenzini.jpg|'''Matteo Lorenzini'''. Postdoc (instrument work at Tor Vergata and Virgo)
File:Ashish Sharma.jpg|'''Ashish Sharma'''. PhD 2021
File:Francesca Badaracco.jpg|'''Francesca Badaracco'''. PhD 2021
File:Stefan.jpg|'''Stefan Grimm'''. PhD 2021
File:Diego.jpg|'''Diego Vescovi'''. PhD 2021
File:Odysse.jpg|'''Odysse Halim'''. PhD 2020
File:AkshatSinghal.jpg|'''Akshat Singal'''. PhD 2019 (thesis work at La Sapienza)
File:LorenzoAiello.jpg|'''Lorenzo Aiello'''. PhD s2019 (thesis work at Tor Vergata)
File:ImranKhan.jpg|'''Imran Khan'''. PhD 2019 (thesis work at Tor Vergata)
File:ShubhanshuTiwari.jpg|'''Shubhanshu Tiwari'''. PhD 2018 (thesis work at Trento)
File:GangWang.jpg|'''Gang Wang'''. PhD 2017 (thesis work at Urbino and Pisa)
</gallery>

Electromagnetic counterparts of GW events

2021-04-08T20:50:45Z

Samuele.ronchini: Created page with "thumb With the joint detection of GW170817/GRB170817 we had for the first time the confirmation that short GRBs are associated to the coalescence of compact b..."

[[File:Jet.png|thumb]]
With the joint detection of GW170817/GRB170817 we had for the first time the confirmation that short GRBs are associated to the coalescence of compact binaries. Such epochal discovery opened the door for a revolutionary era for astronomy. 

In our group we work on solving open issues about GRB physics, with both a theoretical and an observational approach. The jet launching mechanism, the jet structure, particle acceleration, emission and dissipation processes are all open points in the GRB field, which need to be addressed. The exploitation of multi-wavelength data from different observatories (from radio to γ-rays) is necessary to fully characterise the spectral and temporal properties of these enigmatic objects. A complete and extensive exploration of the GRB phenomenology is of cardinal importance to establish the optimal observational strategy for current and next-generation astronomical facilities, in synergy with gravitational wave observatories. The optimisation of joint detection strategies relies on the knowledge of GRB population properties, which, for the sub-class of short GRBs, is still incomplete and needs to be refined. 

From the EM observation of GRB170817, it was possible to constrain the jet structure of the GRB, namely its geometry and the angular energy distribution. Such structure likely deviates from the spherical approximation due to the interaction of the jet with the post-merger ejected material. A deeper comprehension of the structure formation and the nature of the emission processes would allow us to correctly predict the EM emission at all angles and in all energy bands. 

As part of our projects, we are developing theoretical tools to predict the EM emission from a structured jet, in order to evaluate the rate of joint detections that ET, in synergy with future astronomical facilities, will be able to achieve. In our treatment we include both the prompt emission component and the following afterglow phase. In this context, the transition from the prompt to the afterglow is strongly dependent on the jet structure, leading to a wide range of possible temporal behaviour of the observed flux, like the steep decay phase or the plateau phase. Such studies can test the intriguing hypothesis of a universal jet structure, which impacts on the overall properties of the short GRB population, e.g. the luminosity function, which is still poorly constrained. 

We are also deeply active in the development of the science case of the mission concept THESEUS, an extremely promising wide field telescope devoted to the high energy observation of GRBs, whose role would be crucial for the future of multi messenger studies. 

Joint GW+EM detections will also allow to shed light on the nature of the remnant, which in turn is responsible for the jet launching. Indeed, it is currently under debate whether a neutron star, as final product of a compact binary merger, is capable to create the favourable conditions for the jet collimation and ejection. The high sensitivity of future GW detectors, like the Einstein Telescope, will probe the nature of the post-merger object and pose a final answer to this issue.

Main Page

2021-04-08T20:50:26Z

Samuele.ronchini: /* Electromagnetic counterparts of GW events */

= GSSI Gravity Group =
[[File:Group_Logo.jpg|thumb|200px]]
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 =
[[File:Virgo_winning_photo.jpg|Virgo |thumb|600px]]
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 detection led to the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories pointed to the source covering frequencies from radio waves to gamma rays on ground and in space and 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 a 142 solar-mass black hole, which belongs to the class of intermediate-mass black holes, for which we only had vague evidence so far from electromagnetic observations.

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 capabilities 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 [https://gwcenter.icrr.u-tokyo.ac.jp/en/ [KAGRA homepage]], and another detector in India known as LIGO India [https://www.ligo-india.in/[LIGO-India homepage]], 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 =
[[File:ET_infra_nice.jpg|Einstein Telescope (artistic conception)|thumb|600px]]
The Einstein Telescope (ET) is a proposed underground infrastructure to host a third-generation, gravitational-wave observatory [http://www.et-gw.eu/ [ET home page<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/1912.02622 [ET science case<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/2001.11173 [Voyager<nowiki>]</nowiki>]and Cosmic Explorer [https://cosmicexplorer.org/ [Cosmic Explorer<nowiki>]</nowiki>] towards a future global detector network with the Einstein Telescope [https://gwic.ligo.org/3Gsubcomm/documents/3G-observatory-science-case.pdf [3G science case<nowiki>]</nowiki>].

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 [https://arxiv.org/abs/1710.04638 [THESEUS<nowiki>]</nowiki>], E-ELT [https://www.eso.org/sci/facilities/eelt/docs/e-elt_executivesummary.pdf [E-ELT<nowiki>]</nowiki>], or VRO (formerly LSST) [https://en.wikipedia.org/wiki/Vera_C._Rubin_Observatory [VRO<nowiki>]</nowiki>].

== Site Characterization and Evaluation ==

=== [[Site-evaluation parameters]] ===

=== [[Sardinia candidate site]] ===

= Lunar Gravitational-Wave Antenna =
[[File:LGWA_Map.png|Deployment configuration of LGWA seismic array. Red (Apollo landing sites) and yellow (robotic landing sites) markers are indicative of potential scientific interest in these regions, which means that LGWA should avoid proximity to these sites.|thumb|600px]]
With Apollo 17, the Lunar Surface Gravimeter was deployed on the Moon with the main scientific goal to observe gravitational waves (GWs) through the vibrations they cause of the Moon. A technical failure prevented the
experiment to be carried out, and today, we believe that the gravimeter would not have had sufficient sensitivity to observe GWs. The Lunar Gravitational-Wave Antenna (LGWA) is a proposed new detector concept to make GW observations on the Moon possible in the near future [https://ideas.esa.int/servlet/hype/IMT?documentTableId=45087622661984950&userAction=Browse&templateName=&documentId=8e0afc17112fe0a1017f5ba30bce54d3[LGWA ESA lander call]]. The concept is based on the observation of lunar normal modes (vibrational modes) excited by passing gravitational waves. The new key technologies to make this possible are a new generation of ultra-sensitive seismic sensors and noise-cancellation methods to reduce the background of meteoroid impacts and moonquakes. A more detailed description of LGWA and its science case can be found in a recent paper [https://arxiv.org/abs/2010.13726[LGWA paper]].

LGWA would have an observation band that largely overlaps with the LISA observation band with some advantage at frequencies above 0.1Hz and a disadvantage below 10mHz since Moon's response at these frequencies is dominated by a few resonances and therefore cannot deliver the broadband sensitivity below 10mHz like LISA. The observable sources are still mostly the same as of the LISA detector, i.e., black-hole binaries from intermediate mass to supermassive, double white dwarfs (WD/WD), and neutron-star binaries. With its superior sensitivity above 0.1Hz, it might be able to see WD/WD mergers potentially associated with Type 1a supernovae. This is only one example of how GW observations of LGWA can lead to multi-messenger observations together with electromagnetic observatories.

= 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: [https://arxiv.org/abs/1811.12907 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)

A repository of analysis codes for Einstein Telescope is developing here: https://github.com/janosch314/EinsteinTelescope

=== [[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]] ===

=== [[Electromagnetic counterparts of GW events]] ===

= Wiki Software =
Consult the [https://www.mediawiki.org/wiki/Special:MyLanguage/Help:Contents User's Guide] for information on using the wiki software.

== Getting started ==
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:Configuration_settings Configuration settings list]
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* [https://lists.wikimedia.org/mailman/listinfo/mediawiki-announce MediaWiki release mailing list]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Localisation#Translation_resources Localise MediaWiki for your language]
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Main Page

2021-04-08T20:50:02Z

Samuele.ronchini: /* Electromagnetic counterparts of GW events */

= GSSI Gravity Group =
[[File:Group_Logo.jpg|thumb|200px]]
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 =
[[File:Virgo_winning_photo.jpg|Virgo |thumb|600px]]
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 detection led to the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories pointed to the source covering frequencies from radio waves to gamma rays on ground and in space and 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 a 142 solar-mass black hole, which belongs to the class of intermediate-mass black holes, for which we only had vague evidence so far from electromagnetic observations.

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 capabilities 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 [https://gwcenter.icrr.u-tokyo.ac.jp/en/ [KAGRA homepage]], and another detector in India known as LIGO India [https://www.ligo-india.in/[LIGO-India homepage]], 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 =
[[File:ET_infra_nice.jpg|Einstein Telescope (artistic conception)|thumb|600px]]
The Einstein Telescope (ET) is a proposed underground infrastructure to host a third-generation, gravitational-wave observatory [http://www.et-gw.eu/ [ET home page<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/1912.02622 [ET science case<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/2001.11173 [Voyager<nowiki>]</nowiki>]and Cosmic Explorer [https://cosmicexplorer.org/ [Cosmic Explorer<nowiki>]</nowiki>] towards a future global detector network with the Einstein Telescope [https://gwic.ligo.org/3Gsubcomm/documents/3G-observatory-science-case.pdf [3G science case<nowiki>]</nowiki>].

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 [https://arxiv.org/abs/1710.04638 [THESEUS<nowiki>]</nowiki>], E-ELT [https://www.eso.org/sci/facilities/eelt/docs/e-elt_executivesummary.pdf [E-ELT<nowiki>]</nowiki>], or VRO (formerly LSST) [https://en.wikipedia.org/wiki/Vera_C._Rubin_Observatory [VRO<nowiki>]</nowiki>].

== Site Characterization and Evaluation ==

=== [[Site-evaluation parameters]] ===

=== [[Sardinia candidate site]] ===

= Lunar Gravitational-Wave Antenna =
[[File:LGWA_Map.png|Deployment configuration of LGWA seismic array. Red (Apollo landing sites) and yellow (robotic landing sites) markers are indicative of potential scientific interest in these regions, which means that LGWA should avoid proximity to these sites.|thumb|600px]]
With Apollo 17, the Lunar Surface Gravimeter was deployed on the Moon with the main scientific goal to observe gravitational waves (GWs) through the vibrations they cause of the Moon. A technical failure prevented the
experiment to be carried out, and today, we believe that the gravimeter would not have had sufficient sensitivity to observe GWs. The Lunar Gravitational-Wave Antenna (LGWA) is a proposed new detector concept to make GW observations on the Moon possible in the near future [https://ideas.esa.int/servlet/hype/IMT?documentTableId=45087622661984950&userAction=Browse&templateName=&documentId=8e0afc17112fe0a1017f5ba30bce54d3[LGWA ESA lander call]]. The concept is based on the observation of lunar normal modes (vibrational modes) excited by passing gravitational waves. The new key technologies to make this possible are a new generation of ultra-sensitive seismic sensors and noise-cancellation methods to reduce the background of meteoroid impacts and moonquakes. A more detailed description of LGWA and its science case can be found in a recent paper [https://arxiv.org/abs/2010.13726[LGWA paper]].

LGWA would have an observation band that largely overlaps with the LISA observation band with some advantage at frequencies above 0.1Hz and a disadvantage below 10mHz since Moon's response at these frequencies is dominated by a few resonances and therefore cannot deliver the broadband sensitivity below 10mHz like LISA. The observable sources are still mostly the same as of the LISA detector, i.e., black-hole binaries from intermediate mass to supermassive, double white dwarfs (WD/WD), and neutron-star binaries. With its superior sensitivity above 0.1Hz, it might be able to see WD/WD mergers potentially associated with Type 1a supernovae. This is only one example of how GW observations of LGWA can lead to multi-messenger observations together with electromagnetic observatories.

= 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: [https://arxiv.org/abs/1811.12907 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)

A repository of analysis codes for Einstein Telescope is developing here: https://github.com/janosch314/EinsteinTelescope

=== [[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]] ===

=== [[Electromagnetic counterparts of GW events]] ===

With the joint detection of GW170817/GRB170817 we had for the first time the confirmation that short GRBs are associated to the coalescence of compact binaries. Such epochal discovery opened the door for a revolutionary era for astronomy. 

In our group we work on solving open issues about GRB physics, with both a theoretical and an observational approach. The jet launching mechanism, the jet structure, particle acceleration, emission and dissipation processes are all open points in the GRB field, which need to be addressed. The exploitation of multi-wavelength data from different observatories (from radio to γ-rays) is necessary to fully characterise the spectral and temporal properties of these enigmatic objects. A complete and extensive exploration of the GRB phenomenology is of cardinal importance to establish the optimal observational strategy for current and next-generation astronomical facilities, in synergy with gravitational wave observatories. The optimisation of joint detection strategies relies on the knowledge of GRB population properties, which, for the sub-class of short GRBs, is still incomplete and needs to be refined. 

From the EM observation of GRB170817, it was possible to constrain the jet structure of the GRB, namely its geometry and the angular energy distribution. Such structure likely deviates from the spherical approximation due to the interaction of the jet with the post-merger ejected material. A deeper comprehension of the structure formation and the nature of the emission processes would allow us to correctly predict the EM emission at all angles and in all energy bands. 

As part of our projects, we are developing theoretical tools to predict the EM emission from a structured jet, in order to evaluate the rate of joint detections that ET, in synergy with future astronomical facilities, will be able to achieve. In our treatment we include both the prompt emission component and the following afterglow phase. In this context, the transition from the prompt to the afterglow is strongly dependent on the jet structure, leading to a wide range of possible temporal behaviour of the observed flux, like the steep decay phase or the plateau phase. Such studies can test the intriguing hypothesis of a universal jet structure, which impacts on the overall properties of the short GRB population, e.g. the luminosity function, which is still poorly constrained. 

We are also deeply active in the development of the science case of the mission concept THESEUS, an extremely promising wide field telescope devoted to the high energy observation of GRBs, whose role would be crucial for the future of multi messenger studies. 

Joint GW+EM detections will also allow to shed light on the nature of the remnant, which in turn is responsible for the jet launching. Indeed, it is currently under debate whether a neutron star, as final product of a compact binary merger, is capable to create the favourable conditions for the jet collimation and ejection. The high sensitivity of future GW detectors, like the Einstein Telescope, will probe the nature of the post-merger object and pose a final answer to this issue. 

= Wiki Software =
Consult the [https://www.mediawiki.org/wiki/Special:MyLanguage/Help:Contents User's Guide] for information on using the wiki software.

== Getting started ==
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Main Page

2021-04-08T20:46:24Z

Samuele.ronchini:

Electromagnetic counterpart of GW events

2021-04-08T20:45:31Z

Samuele.ronchini:

Electromagnetic counterpart of GW events

2021-04-08T20:18:49Z

Samuele.ronchini:

[[File:Jet.png|thumb]]
With the joint detection of GW170817/GRB170817 we had for the first time the confirmation that short GRBs are associated to the coalescence of compact binaries. Such epochal discovery opened the door for a revolutionary era for astronomy. 

In our group we work on solving open issues about GRB physics, with both a theoretical and an observational approach. The jet launching mechanism, the jet structure, particle acceleration, emission and dissipation processes are all open points in the GRB field, which need to be addressed. The exploitation of multi-wavelength data from different observatories (from radio to γ-rays) is necessary to fully characterise the spectral and temporal properties of these enigmatic objects. A complete and extensive exploration of the GRB phenomenology is of cardinal importance to establish the optimal observational strategy for current and next-generation astronomical facilities, in synergy with gravitational wave observatories. The optimisation of joint detection strategies relies on the knowledge of GRB population properties, which, for the sub-class of short GRBs, is still incomplete and needs to be refined. 

From the EM observation of GRB170817, it was possible to constrain the jet structure of the GRB, namely its geometry and the angular energy distribution. Such structure likely deviates from the spherical approximation due to the interaction of the jet with the post-merger ejected material. A deeper comprehension of the structure formation and the nature of the emission processes would allow us to correctly predict the EM emission at all angles and in all energy bands. 

As part of our projects, we are developing theoretical tools to predict the EM emission from a structured jet, in order to evaluate the rate of joint detections that ET, in synergy with future astronomical facilities, will be able to achieve. Such studies can test the intriguing hypothesis of a universal jet structure, which impact on the overall properties of the short GRB population, e.g. the luminosity function.

Future joint GW+EM detections will also allow to shed light on the nature of the remnant, which in turn is responsible for the jet launching. Indeed, it is currently under debate whether a neutron star, as final product of a compact binary merger, is capable to create the favourable conditions for the jet collimation and ejection. The high sensitivity of future GW detectors, like the Einstein Telescope, will probe the nature of the post-merger object and pose a final answer to this issue.

Electromagnetic counterpart of GW events

2021-04-08T16:11:03Z

Samuele.ronchini:

Electromagnetic counterpart of GW events

2021-04-08T08:56:49Z

Samuele.ronchini: Created page with "thumb"

[[File:Jet.png|thumb]]

File:Jet.png

2021-04-08T08:56:41Z

Samuele.ronchini:

jet illustration

Main Page

2021-04-08T08:45:02Z

Samuele.ronchini: /* Multi-messenger astronomy */

= GSSI Gravity Group =
[[File:Group_Logo.jpg|thumb|200px]]
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 =
[[File:Virgo_winning_photo.jpg|Virgo |thumb|600px]]
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 detection led to the largest multi-messenger observational campaign in astronomy with virtually all major electromagnetic observatories pointed to the source covering frequencies from radio waves to gamma rays on ground and in space and 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 a 142 solar-mass black hole, which belongs to the class of intermediate-mass black holes, for which we only had vague evidence so far from electromagnetic observations.

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 capabilities 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 [https://gwcenter.icrr.u-tokyo.ac.jp/en/ [KAGRA homepage]], and another detector in India known as LIGO India [https://www.ligo-india.in/[LIGO-India homepage]], 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 =
[[File:ET_infra_nice.jpg|Einstein Telescope (artistic conception)|thumb|600px]]
The Einstein Telescope (ET) is a proposed underground infrastructure to host a third-generation, gravitational-wave observatory [http://www.et-gw.eu/ [ET home page<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/1912.02622 [ET science case<nowiki>]</nowiki>]. 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 [https://arxiv.org/abs/2001.11173 [Voyager<nowiki>]</nowiki>]and Cosmic Explorer [https://cosmicexplorer.org/ [Cosmic Explorer<nowiki>]</nowiki>] towards a future global detector network with the Einstein Telescope [https://gwic.ligo.org/3Gsubcomm/documents/3G-observatory-science-case.pdf [3G science case<nowiki>]</nowiki>].

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 [https://arxiv.org/abs/1710.04638 [THESEUS<nowiki>]</nowiki>], E-ELT [https://www.eso.org/sci/facilities/eelt/docs/e-elt_executivesummary.pdf [E-ELT<nowiki>]</nowiki>], or VRO (formerly LSST) [https://en.wikipedia.org/wiki/Vera_C._Rubin_Observatory [VRO<nowiki>]</nowiki>].

== Site Characterization and Evaluation ==

=== [[Site-evaluation parameters]] ===

=== [[Sardinia candidate site]] ===

= Lunar Gravitational-Wave Antenna =
[[File:LGWA_Map.png|Deployment configuration of LGWA seismic array. Red (Apollo landing sites) and yellow (robotic landing sites) markers are indicative of potential scientific interest in these regions, which means that LGWA should avoid proximity to these sites.|thumb|600px]]
With Apollo 17, the Lunar Surface Gravimeter was deployed on the Moon with the main scientific goal to observe gravitational waves (GWs) through the vibrations they cause of the Moon. A technical failure prevented the
experiment to be carried out, and today, we believe that the gravimeter would not have had sufficient sensitivity to observe GWs. The Lunar Gravitational-Wave Antenna (LGWA) is a proposed new detector concept to make GW observations on the Moon possible in the near future [https://ideas.esa.int/servlet/hype/IMT?documentTableId=45087622661984950&userAction=Browse&templateName=&documentId=8e0afc17112fe0a1017f5ba30bce54d3[LGWA ESA lander call]]. The concept is based on the observation of lunar normal modes (vibrational modes) excited by passing gravitational waves. The new key technologies to make this possible are a new generation of ultra-sensitive seismic sensors and noise-cancellation methods to reduce the background of meteoroid impacts and moonquakes. A more detailed description of LGWA and its science case can be found in a recent paper [https://arxiv.org/abs/2010.13726[LGWA paper]].

LGWA would have an observation band that largely overlaps with the LISA observation band with some advantage at frequencies above 0.1Hz and a disadvantage below 10mHz since Moon's response at these frequencies is dominated by a few resonances and therefore cannot deliver the broadband sensitivity below 10mHz like LISA. The observable sources are still mostly the same as of the LISA detector, i.e., black-hole binaries from intermediate mass to supermassive, double white dwarfs (WD/WD), and neutron-star binaries. With its superior sensitivity above 0.1Hz, it might be able to see WD/WD mergers potentially associated with Type 1a supernovae. This is only one example of how GW observations of LGWA can lead to multi-messenger observations together with electromagnetic observatories.

= 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: [https://arxiv.org/abs/1811.12907 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)

A repository of analysis codes for Einstein Telescope is developing here: https://github.com/janosch314/EinsteinTelescope

=== [[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]] ===

=== [[Electromagnetic counterpart of GW events]] ===

= Wiki Software =
Consult the [https://www.mediawiki.org/wiki/Special:MyLanguage/Help:Contents User's Guide] for information on using the wiki software.

== Getting started ==
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:Configuration_settings Configuration settings list]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:FAQ MediaWiki FAQ]
* [https://lists.wikimedia.org/mailman/listinfo/mediawiki-announce MediaWiki release mailing list]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Localisation#Translation_resources Localise MediaWiki for your language]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:Combating_spam Learn how to combat spam on your wiki]

Members

2021-04-08T08:42:53Z

Samuele.ronchini: /* Current gravitational-wave group at Gran Sasso Science Institute */

== Current gravitational-wave group at Gran Sasso Science Institute ==
<gallery caption="" widths=300px heights=300px perrow=4>
File:Eugenio.jpg|'''Eugenio Coccia'''. Full professor and current rector of GSSI.
File:JanHarms.jpg|'''Jan Harms'''. Associate professor working on instrument science of current and future GW detectors, and data analysis of modeled and unmodeled GW signals.
File:Marica.jpg|'''Marica Branchesi'''. Associate professor working on multi-messenger astrophysics and observations with gravitational-waves.
File:AndreaMaselli.jpg|'''Andrea Maselli'''. Assistant professor working on LISA and ET signal modeling and testing GR.
File:Giulia.jpg|'''Giulia Pagliaroli'''. Assistant professor studying supernova neutrino physics and coincidence analyses with gravitational waves.
File:Gor.jpg|'''Gor Oganesyan'''. Postdoc working on the theoretical modeling and analysis of GRB signals and afterglows.
File:MatteoDiGiovanni.jpg|'''Matteo Di Giovanni'''. Postdoc working on the characterization of the Sardinian candidate site of the Einstein Telescope, and GW burst analyses.
File:Simone.jpg|'''Simone Dall'Osso'''. Postdoc studying the physics of magnetars and post-merger GW signal models.
File:SoumenKoley.jpg|'''Soumen Koley'''. Postdoc studying seismic environments of GW detectors and implementing a cancellation system for noise from terrestrial gravity fluctuations.
File:BorisGoncharov.jpg|'''Boris Goncharov'''. Postdoc working on pulsar timing arrays and ET data-analysis problems.
File:Nandita.jpg|'''Nandita Khetan'''. PhD student exploring astrophysical transients for their use as cosmological probes at different scales and developing calibration techniques to standardize them.
File:Tomislav.jpg|'''Tomislav Andric'''. PhD student working on the site characterization of Sardinia candidate site for Einstein Telescope. He also works on estimation, modelling and mitigation of Newtonian Noise in Einstein Telescope.
File:Samuele.jpg|'''Samuele Ronchini'''. PhD student studying prompt and afterglow emissions of GRBs, in the context of joint GW+EM detections with current and future facilities.
File:Nandini.jpg|'''Nandini Hazra'''. PhD student doing cosmology with SFB calibrated signals.
File:EleonoraLoffredo.jpg|'''Eleonora Loffredo'''. PhD student.
File:ElenaCodazzo.jpg|'''Elena Codazzo'''. PhD student modeling the distribution of transient GW signals from star clusters.
</gallery>

== Collaborators at LNGS ==
<gallery caption="" widths=300px heights=300px perrow=4>
File:StefanoPirro.jpg|'''Stefano Pirro''' Staff scientist at INFN LNGS. He dedicates part of his time on cryogenics R&D for the Einstein Telescope.
File:AntonioAddabbo.jpg|'''Antonio D'Addabbo''' Postdoc at GSSI working for Cuore at LNGS. He dedicates part of his time on cryogenics R&D for the Einstein Telescope.
</gallery>

== Former group members ==
<gallery caption="" widths=200px heights=200px perrow=8>
File:Marco.jpg|'''Marco Drago'''. Assistant professor
File:DonatellaFiorucci.jpg|'''Donatella Fiorucci'''. Postdoc
File:MatteoLorenzini.jpg|'''Matteo Lorenzini'''. Postdoc (instrument work at Tor Vergata and Virgo)
File:Ashish Sharma.jpg|'''Ashish Sharma'''. PhD 2021
File:Francesca Badaracco.jpg|'''Francesca Badaracco'''. PhD 2021
File:Stefan.jpg|'''Stefan Grimm'''. PhD 2021
File:Diego.jpg|'''Diego Vescovi'''. PhD 2021
File:Odysse.jpg|'''Odysse Halim'''. PhD 2020
File:AkshatSinghal.jpg|'''Akshat Singal'''. PhD 2019 (thesis work at La Sapienza)
File:LorenzoAiello.jpg|'''Lorenzo Aiello'''. PhD s2019 (thesis work at Tor Vergata)
File:ImranKhan.jpg|'''Imran Khan'''. PhD 2019 (thesis work at Tor Vergata)
File:ShubhanshuTiwari.jpg|'''Shubhanshu Tiwari'''. PhD 2018 (thesis work at Trento)
File:GangWang.jpg|'''Gang Wang'''. PhD 2017 (thesis work at Urbino and Pisa)
</gallery>

Main Page

2020-02-20T09:59:11Z

Samuele.ronchini:

= GSSI gravity group =
=== [[Members]] ===

= Einstein Telescope =
[[File:ETArtist.jpg|Einstein Telescope (artistic conception)|thumb]]

== Site Characterization and Evaluation ==

=== [[Site-evaluation parameters]] ===

=== [[Results from Sardinia]] ===

== R&D ==

=== [[Newtonian Noise]] ===

== Physics with Einstein Telescope ==

=== [[Cosmology: Probing the Early Universe]] ===

= Electromagnetic counterpart of gravitational waves =

= Wiki Software =
Consult the [https://www.mediawiki.org/wiki/Special:MyLanguage/Help:Contents User's Guide] for information on using the wiki software.

== Getting started ==
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:Configuration_settings Configuration settings list]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:FAQ MediaWiki FAQ]
* [https://lists.wikimedia.org/mailman/listinfo/mediawiki-announce MediaWiki release mailing list]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Localisation#Translation_resources Localise MediaWiki for your language]
* [https://www.mediawiki.org/wiki/Special:MyLanguage/Manual:Combating_spam Learn how to combat spam on your wiki]