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Jan.harms at 11:06, 6 May 2025

2025-05-06T11:06:34Z

Jan.harms at 11:03, 6 May 2025

2025-05-06T11:03:13Z

Jan.harms at 09:48, 11 April 2025

2025-04-11T09:48:03Z

Jan.harms: /* Einstein Telescope */

2023-07-12T17:10:45Z

‎Einstein Telescope

Jan.harms: /* Lunar Gravitational-Wave Antenna */

2023-07-11T18:37:10Z

‎Lunar Gravitational-Wave Antenna

Jan.harms: /* Lunar Gravitational-Wave Antenna */

2023-07-11T18:29:38Z

‎Lunar Gravitational-Wave Antenna

Jan.harms: /* Lunar Gravitational-Wave Antenna */

2023-07-11T18:28:52Z

‎Lunar Gravitational-Wave Antenna

Jan.harms: /* Einstein Telescope */

2023-07-11T18:27:57Z

‎Einstein Telescope

Jan.harms: /* Einstein Telescope */

2023-07-11T18:27:18Z

‎Einstein Telescope

Jan.harms: /* Einstein Telescope */

2023-07-11T17:49:05Z

‎Einstein Telescope

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 === [[Cryogenics]] ===
 === [[Detector Control]] ===
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 === [[Earthquake early warning with gravitational sensors]] ===
 = Multi-messenger astronomy =

← Older revision		Revision as of 11:03, 6 May 2025
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	= Instrument Science =		= Instrument Science =
		+
		+	=== [[Noise modeling]] ===

	=== [[Cryogenics]] ===		=== [[Cryogenics]] ===

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-= GSSI Gravity Group =
+= GSSI Gravitational-wave 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.

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 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>].
+The beginning of construction is foreseen in 2027 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 2025. 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>].

@@ Line 30: / Line 30: @@
 [[File:LGWA_crater_mod_small.png|Deployment configuration of LGWA seismic array. The array resides in a permanent shadow, which requires new technologies to power the experiment. Here shown is a possible laser power beaming system.|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 [http://lgwa.unicam.it[LGWA home page]]. 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://iopscience.iop.org/article/10.3847/1538-4357/abe5a7[LGWA paper]].
+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 [http://lgwa.unicam.it[LGWA home page]]. 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 first description of LGWA and its science case was published in [https://iopscience.iop.org/article/10.3847/1538-4357/abe5a7[LGWA paper]], and the payload concept was described in greater detail in [https://doi.org/10.1063/5.0144687[LGWA payload 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.

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 = 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>] [https://www.einstein-telescope.it/ [ET Italia 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 (ET) is a proposed underground infrastructure to host a third-generation, gravitational-wave observatory [http://www.et-gw.eu/ [ET home page<nowiki>]</nowiki>] [https://www.einstein-telescope.it/ [ET Italy 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).

@@ Line 23: / Line 23: @@
 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-evaluation parameters]] ===
+=== [[Sardinia candidate site]] ===
-=== [[Sardinia candidate site]] ===
+=== [[GEMINI]] ===
 = Lunar Gravitational-Wave Antenna =