1,215 results on '"Einstein Telescope"'
Search Results
2. Investigating Earth surface deformation with SAR interferometry and geomodeling in the transborder Meuse-Rhine region.
- Author
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Schlögel, Romy, Owczarz, Karolina, Orban, Anne, and Havenith, Hans-Balder
- Subjects
DEFORMATION of surfaces ,SURFACE of the earth ,GRAVITATIONAL wave detectors ,SYNTHETIC aperture radar ,INTERFEROMETRY ,REGIONAL differences ,CONTENT mining - Abstract
Introduction: This study aims to differentiate local and regional ground uplift, as well as sub-regional subsidence induced by groundwater level drawdown, which are possibly enhanced across fault structures, as monitored by various synthetic aperture radar interferometry (InSAR) processing methods. A buoyant mantle plume under the Eifel may be responsible for the regional ground uplift, including the Weser-Geul (BE) and South Limburg regions (NL), which could negatively affect the area proposed for the future Einstein Telescope. Methods: Different InSAR processing techniques are compared to evaluate their limits in tracking fault structures on a time series of Copernicus Sentinel-1 images while detecting and measuring ground motion based on their phase signature. The results present an overall stable ground for the Euregio Meuse-Rhine region, especially at the Belgian-Dutch border, while tectonic activity is observed along the German side of the Rhine Graben. Results: As the current neotectonic activity in the target area was not well known, we performed a spatiotemporal analysis of ground deformation associated with the presence of NW-SE-trending normal faults where karst also develops, as well as along the Variscan NE-SW-trending thrust faults. This work demonstrates that the identification of deformation hazards using satellite remote sensing (and connected seismological) techniques is challenging mainly due to (very) small regional scale deformation, terrain conditions, and SAR properties. Discussion: Thus, the results mostly indicate ground stability over the area; however, also some agricultural activities were observed, as was deformation along some infrastructure such as railways. Displacements of millimetric order measured along the faults located near the Geul valley (BE) are probably related to old mining activities. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
3. Investigating Earth surface deformation with SAR interferometry and geomodeling in the transborder Meuse–Rhine region
- Author
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Romy Schlögel, Karolina Owczarz, Anne Orban, and Hans-Balder Havenith
- Subjects
Einstein telescope ,neotectonics ,Lower Rhine Embayment ,geomodeling ,time series analysis ,SAR interferometry ,Geophysics. Cosmic physics ,QC801-809 ,Meteorology. Climatology ,QC851-999 - Abstract
Introduction: This study aims to differentiate local and regional ground uplift, as well as sub-regional subsidence induced by groundwater level drawdown, which are possibly enhanced across fault structures, as monitored by various synthetic aperture radar interferometry (InSAR) processing methods. A buoyant mantle plume under the Eifel may be responsible for the regional ground uplift, including the Weser–Geul (BE) and South Limburg regions (NL), which could negatively affect the area proposed for the future Einstein Telescope.Methods: Different InSAR processing techniques are compared to evaluate their limits in tracking fault structures on a time series of Copernicus Sentinel-1 images while detecting and measuring ground motion based on their phase signature. The results present an overall stable ground for the Euregio Meuse–Rhine region, especially at the Belgian–Dutch border, while tectonic activity is observed along the German side of the Rhine Graben.Results: As the current neotectonic activity in the target area was not well known, we performed a spatiotemporal analysis of ground deformation associated with the presence of NW–SE-trending normal faults where karst also develops, as well as along the Variscan NE–SW-trending thrust faults. This work demonstrates that the identification of deformation hazards using satellite remote sensing (and connected seismological) techniques is challenging mainly due to (very) small regional scale deformation, terrain conditions, and SAR properties.Discussion: Thus, the results mostly indicate ground stability over the area; however, also some agricultural activities were observed, as was deformation along some infrastructure such as railways. Displacements of millimetric order measured along the faults located near the Geul valley (BE) are probably related to old mining activities.
- Published
- 2024
- Full Text
- View/download PDF
4. Temporal variations of the ambient seismic field at the Sardinia candidate site of the Einstein Telescope.
- Author
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Di Giovanni, M, Koley, S, Ensing, J X, Andric, T, Harms, J, D'Urso, D, Naticchioni, L, De Rosa, R, Giunchi, C, Allocca, A, Cadoni, M, Calloni, E, Cardini, A, Carpinelli, M, Contu, A, Errico, L, Mangano, V, Olivieri, M, Punturo, M, and Rapagnani, P
- Subjects
- *
GRAVITATIONAL wave detectors , *ECOLOGICAL disturbances , *DETECTORS , *RANDOM fields , *MICROSEISMS , *GRAVITATIONAL waves - Abstract
Einstein Telescope (ET) is a proposed underground infrastructure in Europe to host future generations of gravitational-wave (GW) detectors. One of its design goals is to extend the observation band of terrestrial GW detectors from currently about 20 Hz down to 3 Hz. The coupling of a detector to its environment becomes stronger at lower frequencies, which makes it important to carefully analyse environmental disturbances at ET candidate sites. Seismic disturbances pose the greatest challenge since there are several important mechanisms for seismic vibrations to produce noise in ET, for example, through gravitational coupling, stray light, or through harmful constraints on the design of ET's control system. In this paper, we present an analysis of the time-variant properties of the seismic field at the Sardinia candidate site of ET connected to anthropogenic as well as natural phenomena. We find that temporal variations of source distributions and of the noise spectra generally follow predictable trends in the form of diurnal, weekly, or seasonal cycles. Specific seismic sources were identified such as road bridges, which produce observable disturbances underground. This information can be used to adapt a detector's seismic isolation and control system. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
5. Effects of a Late Gravitational Transition on Gravitational Waves and Anticipated Constraints.
- Author
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Paraskevas, Evangelos Achilleas and Perivolaropoulos, Leandros
- Subjects
- *
GRAVITATIONAL effects , *GRAVITATIONAL wave detectors , *GRAVITATIONAL constant - Abstract
We investigate the evolution of gravitational waves through discontinuous evolution (transition) of the Hubble expansion rate H (z) at a sudden cosmological singularity, which may be due to a transition of the value of the gravitational constant. We find the evolution of the scale factor and the gravitational wave waveform through the singularity by imposing the proper boundary conditions. We also use existing cosmological data and mock data of future gravitational wave experiments (the ET) to impose current and anticipated constraints on the magnitude of such a transition. We show that mock data of the Einstein Telescope can reduce the uncertainties by up to a factor of three depending on the cosmological parameter considered. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
6. Third-Generation Gravitational-Wave Observatories
- Author
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Lück, Harald, Smith, Joshua, Punturo, Michele, Bambi, Cosimo, editor, Katsanevas, Stavros, editor, and Kokkotas, Konstantinos D., editor
- Published
- 2022
- Full Text
- View/download PDF
7. Tunnel Configurations and Seismic Isolation Optimization in Underground Gravitational Wave Detectors.
- Author
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Amann, Florian, Badaracco, Francesca, DeSalvo, Riccardo, Naticchioni, Luca, Paoli, Andrea, Paoli, Luca, Ruggi, Paolo, and Selleri, Stefano
- Subjects
GRAVITATIONAL wave detectors ,SURFACE of the earth ,TUNNELS ,MICROSEISMS ,MICHELSON interferometer ,GRAVITATIONAL waves - Abstract
The Einstein Telescope will be a gravitational wave observatory comprising six nested detectors, three optimized to collect low-frequency signals, and three for high frequency. It will be built a few hundred meters under Earth's surface to reduce direct seismic and Newtonian noise. A critical issue with the Einstein Telescope design are the three corner stations, each hosting at least one sensitive component of all six detectors in the same hall. Maintenance, commissioning, and upgrade activities on a detector will cause interruptions of the operation of the other five, in some cases for years, thus greatly reducing the Einstein Telescope observational duty cycle. This paper proposes a new topology that moves the recombination and input–output optics of the Michelson interferometers, the top stages of the seismic attenuation chains and noise-inducing equipment in separate excavations far from the tunnels where the test masses reside. This separation takes advantage of the shielding properties of the rock mass to allow continuing detection with most detectors even during maintenance and upgrade of others. This configuration drastically improves the observatory's event detection efficiency. In addition, distributing the seismic attenuation chain components over multiple tunnel levels allows the use of effectively arbitrarily long seismic attenuation chains that relegate the seismic noise at frequencies farther from the present low-frequency noise budget, thus keeping the door open for future upgrades. Mechanical crowding around the test masses is eliminated allowing the use of smaller vacuum tanks and reduced cross section of excavations, which require less support measures. [ABSTRACT FROM AUTHOR]
- Published
- 2022
- Full Text
- View/download PDF
8. Research Facilities for Europe's Next Generation Gravitational-Wave Detector Einstein Telescope.
- Author
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Di Pace, Sibilla, Mangano, Valentina, Pierini, Lorenzo, Rezaei, Amirsajjad, Hennig, Jan-Simon, Hennig, Margot, Pascucci, Daniela, Allocca, Annalisa, Tosta e Melo, Iara, Nair, Vishnu G., Orban, Philippe, Sider, Ameer, Shani-Kadmiel, Shahar, and van Heijningen, Joris
- Subjects
GRAVITATIONAL wave detectors ,QUANTUM noise ,SEISMIC arrays ,NOISE control ,DETECTORS ,BORDERLANDS ,TELESCOPES - Abstract
The Einstein Telescope is Europe's next generation gravitational-wave detector. To develop all necessary technology, four research facilities have emerged across Europe: The Amaldi Research Center (ARC) in Rome (Italy), ETpathfinder in Maastricht (The Netherlands), SarGrav in the Sos Enattos mines on Sardinia (Italy) and E-TEST in Liége (Belgium) and its surroundings. The ARC pursues the investigation of a large cryostat, equipped with dedicated low-vibration cooling lines, to test full-scale cryogenic payloads. The installation will be gradual and interlaced with the payload development. ETpathfinder aims to provide a low-noise facility that allows the testing of full interferometer configurations and the interplay of their subsystems in an ET-like environment. ETpathfinder will focus amongst others on cryogenic technologies, silicon mirrors, lasers and optics at 1550 and 2090 nm and advanced quantum noise reduction schemes. The SarGrav laboratory has a surface lab and an underground operation. On the surface, the Archimedes experiment investigates the interaction of vacuum fluctuations with gravity and is developing (tilt) sensor technology for the Einstein Telescope. In an underground laboratory, seismic characterisation campaigns are undertaken for the Sardinian site characterisation. Lastly, the Einstein Telecope Euregio meuse-rhine Site & Technology (E-TEST) is a single cryogenic suspension of an ET-sized silicon mirror. Additionally, E-TEST investigates the Belgian–Dutch–German border region that is the other candidate site for Einstein Telescope using boreholes and seismic arrays and hydrogeological characterisation. In this article, we describe the Einstein Telescope, the low-frequency part of its science case and the four research facilities. [ABSTRACT FROM AUTHOR]
- Published
- 2022
- Full Text
- View/download PDF
9. Improvement of the parameter measurement accuracy by the third-generation gravitational wave detector Einstein Telescope.
- Author
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Cho, Hee-Suk
- Subjects
- *
GRAVITATIONAL wave detectors , *BINARY black holes , *GRAVITATIONAL waves , *TELESCOPES , *STELLAR mass , *ERYTHROCYTE deformability , *NEUTRON stars , *MEASUREMENT errors - Abstract
The Einstein Telescope (ET) has been proposed as one of the third-generation gravitational wave (GW) detectors. The sensitivity of ET would be a factor of 10 better than the second-generation GW detector, advanced LIGO (aLIGO); thus, the GW source parameters could be measured with much better accuracy. In this work, we show how the precision in parameter estimation can be improved between aLIGO and ET by comparing the measurement errors. We apply the TaylorF2 waveform model defined in the frequency domain to the Fisher matrix method which is a semi-analytic approach for estimating GW parameter measurement errors. We adopt as our sources low-mass binary black holes with the total masses of M â©˝ 16 M ⊙ and the effective spins of â'0.9 â©˝ χ eff â©˝ 0.9 and calculate the measurement errors of the mass and the spin parameters using 104 Monte-Carlo samples randomly distributed in our mass and spin parameter space. We find that for the same sources ET can achieve ⼠14 times better signal-to-noise ratio than aLIGO and the error ratios (Ď Î»,ET/ Ď Î»,aLIGO) for the chirp-mass, symmetric mass ratio, and effective spin parameters can be lower than 7% for all binaries. We also consider the equal-mass binary neutron stars with the component masses of 1, 1.4, and 2 M ⊙ and find that the error ratios for the mass and the spin parameters can be lower than 1.5%. In particular, the measurement error of the tidal deformability Λ ~ can also be significantly reduced by ET, with the error ratio of 3.6%â€"6.1%. We investigate the effect of prior information by applying the Gaussian prior on the coalescence phase Ď• c to the Fisher matrix and find that the error of the intrinsic parameters can be reduced to ⼠70 % of the original priorless error ( Ď Î» priorless ) if the standard deviation of the prior is similar to Ď Ď• c priorless . [ABSTRACT FROM AUTHOR]
- Published
- 2022
- Full Text
- View/download PDF
10. Forecasts for ΛCDM and Dark Energy Models through Einstein Telescope Standard Sirens
- Author
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Matteo Califano, Ivan de Martino, Daniele Vernieri, and Salvatore Capozziello
- Subjects
cosmological parameters ,gravitational waves ,neutron star mergers ,Einstein Telescope ,Mechanical drawing. Engineering graphics ,T351-385 ,Physical and theoretical chemistry ,QD450-801 - Abstract
Gravitational wave (GW) astronomy provides an independent way to estimate cosmological parameters. The detection of GWs from a coalescing binary allows a direct measurement of its luminosity distance, so these sources are referred to as “standard sirens” in analogy to standard candles. We investigate the impact of constraining cosmological models on the Einstein Telescope, a third-generation detector which will detect tens of thousands of binary neutron stars. We focus on non-flat ΛCDM cosmology and some dark energy models that may resolve the so-called Hubble tension. To evaluate the accuracy down to which ET will constrain cosmological parameters, we consider two types of mock datasets depending on whether or not a short gamma-ray burst is detected and associated with the gravitational wave event using the THESEUS satellite. Depending on the mock dataset, different statistical estimators are applied: one assumes that the redshift is known, and another marginalizes it, taking a specific prior distribution.
- Published
- 2023
- Full Text
- View/download PDF
11. Tunnel Configurations and Seismic Isolation Optimization in Underground Gravitational Wave Detectors
- Author
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Florian Amann, Francesca Badaracco, Riccardo DeSalvo, Luca Naticchioni, Andrea Paoli, Luca Paoli, Paolo Ruggi, and Stefano Selleri
- Subjects
gravitational waves ,Einstein Telescope ,Newtonian noise ,observatory ,seismic attenuation ,tunnel configuration ,Technology ,Engineering (General). Civil engineering (General) ,TA1-2040 ,Biology (General) ,QH301-705.5 ,Physics ,QC1-999 ,Chemistry ,QD1-999 - Abstract
The Einstein Telescope will be a gravitational wave observatory comprising six nested detectors, three optimized to collect low-frequency signals, and three for high frequency. It will be built a few hundred meters under Earth’s surface to reduce direct seismic and Newtonian noise. A critical issue with the Einstein Telescope design are the three corner stations, each hosting at least one sensitive component of all six detectors in the same hall. Maintenance, commissioning, and upgrade activities on a detector will cause interruptions of the operation of the other five, in some cases for years, thus greatly reducing the Einstein Telescope observational duty cycle. This paper proposes a new topology that moves the recombination and input–output optics of the Michelson interferometers, the top stages of the seismic attenuation chains and noise-inducing equipment in separate excavations far from the tunnels where the test masses reside. This separation takes advantage of the shielding properties of the rock mass to allow continuing detection with most detectors even during maintenance and upgrade of others. This configuration drastically improves the observatory’s event detection efficiency. In addition, distributing the seismic attenuation chain components over multiple tunnel levels allows the use of effectively arbitrarily long seismic attenuation chains that relegate the seismic noise at frequencies farther from the present low-frequency noise budget, thus keeping the door open for future upgrades. Mechanical crowding around the test masses is eliminated allowing the use of smaller vacuum tanks and reduced cross section of excavations, which require less support measures.
- Published
- 2022
- Full Text
- View/download PDF
12. Research Facilities for Europe’s Next Generation Gravitational-Wave Detector Einstein Telescope
- Author
-
Sibilla Di Pace, Valentina Mangano, Lorenzo Pierini, Amirsajjad Rezaei, Jan-Simon Hennig, Margot Hennig, Daniela Pascucci, Annalisa Allocca, Iara Tosta e Melo, Vishnu G. Nair, Philippe Orban, Ameer Sider, Shahar Shani-Kadmiel, and Joris van Heijningen
- Subjects
gravitational waves ,einstein telescope ,seismic noise ,newtonian noise ,thermal noise ,coating noise ,Astronomy ,QB1-991 - Abstract
The Einstein Telescope is Europe’s next generation gravitational-wave detector. To develop all necessary technology, four research facilities have emerged across Europe: The Amaldi Research Center (ARC) in Rome (Italy), ETpathfinder in Maastricht (The Netherlands), SarGrav in the Sos Enattos mines on Sardinia (Italy) and E-TEST in Liége (Belgium) and its surroundings. The ARC pursues the investigation of a large cryostat, equipped with dedicated low-vibration cooling lines, to test full-scale cryogenic payloads. The installation will be gradual and interlaced with the payload development. ETpathfinder aims to provide a low-noise facility that allows the testing of full interferometer configurations and the interplay of their subsystems in an ET-like environment. ETpathfinder will focus amongst others on cryogenic technologies, silicon mirrors, lasers and optics at 1550 and 2090 nm and advanced quantum noise reduction schemes. The SarGrav laboratory has a surface lab and an underground operation. On the surface, the Archimedes experiment investigates the interaction of vacuum fluctuations with gravity and is developing (tilt) sensor technology for the Einstein Telescope. In an underground laboratory, seismic characterisation campaigns are undertaken for the Sardinian site characterisation. Lastly, the Einstein Telecope Euregio meuse-rhine Site & Technology (E-TEST) is a single cryogenic suspension of an ET-sized silicon mirror. Additionally, E-TEST investigates the Belgian–Dutch–German border region that is the other candidate site for Einstein Telescope using boreholes and seismic arrays and hydrogeological characterisation. In this article, we describe the Einstein Telescope, the low-frequency part of its science case and the four research facilities.
- Published
- 2022
- Full Text
- View/download PDF
13. Effects of a Late Gravitational Transition on Gravitational Waves and Anticipated Constraints
- Author
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Perivolaropoulos, Evangelos Achilleas Paraskevas and Leandros
- Subjects
cosmology ,gravitational waves ,gravitational transition ,sudden cosmological singularity ,geodesically complete singularity ,Hubble tension ,Einstein Telescope - Abstract
We investigate the evolution of gravitational waves through discontinuous evolution (transition) of the Hubble expansion rate H(z) at a sudden cosmological singularity, which may be due to a transition of the value of the gravitational constant. We find the evolution of the scale factor and the gravitational wave waveform through the singularity by imposing the proper boundary conditions. We also use existing cosmological data and mock data of future gravitational wave experiments (the ET) to impose current and anticipated constraints on the magnitude of such a transition. We show that mock data of the Einstein Telescope can reduce the uncertainties by up to a factor of three depending on the cosmological parameter considered.
- Published
- 2023
- Full Text
- View/download PDF
14. Modified propagation of gravitational waves from the early radiation era
- Author
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He, Yutong, Pol, Alberto Roper, Brandenburg, Axel, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and HEP, INSPIRE
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,gravitation: model ,energy spectrum ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,General Relativity and Quantum Cosmology ,Einstein Telescope ,gravitational radiation: propagation ,general relativity ,gravitational radiation: spectrum ,energy: density ,WKB approximation ,LIGO ,numerical calculations ,pulsar ,LISA ,[PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,gravitational radiation: background ,scale: Planck ,VIRGO ,frequency: low ,slope ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,spectral ,[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We study the propagation of cosmological gravitational wave (GW) backgrounds from the early radiation era until the present day in modified theories of gravity. Comparing to general relativity (GR), we study the effects that modified gravity parameters, such as the GW friction $\alpha_{\rm M}$ and the tensor speed excess $\alpha_{\rm T}$, have on the present-day GW spectrum. We use both the WKB estimate, which provides an analytical description but fails at superhorizon scales, and numerical simulations that allow us to go beyond the WKB approximation. We show that a constant $\alpha_{\rm T}$ makes relatively insignificant changes to the GR solution, especially taking into account the constraints on its value from GW observations by the LIGO--Virgo collaboration, while $\alpha_{\rm M}$ can introduce modifications to the spectral slopes of the GW energy spectrum in the low-frequency regime depending on the considered time evolution of $\alpha_{\rm M}$. The latter effect is additional to the damping or growth occurring equally at all scales that can be predicted by the WKB approximation. In light of the recent observations by pulsar timing array (PTA) collaborations, and the potential observations by future detectors such as SKA, LISA, DECIGO, BBO, or ET, we show that, in most of the cases, constraints cannot be placed on the effects of $\alpha_{\rm M}$ and the initial GW energy density $\mathcal{E}_{\rm GW}^*$ separately, but only on the combined effects of the two, unless the signal is observed at different frequency ranges. In particular, we provide some constraints on the combined effects from the reported PTA observations., Comment: 36 pages, 11 figures, 2 tables
- Published
- 2023
15. Development status of the inner thermal shielding for the ET-LF cryogenic payloads
- Author
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Busch, Lennard Niclas and Grohmann, Steffen
- Subjects
Cryogenics ,Einstein Telescope ,Physics ,ddc:530 ,Thermal shield ,Helium - Abstract
Cryogenic operation of ET-LF is imperative for exploiting the full scientific potential of ET, with mirrors operated at temperatures of 10 K to 20 K in order to limit thermal noise. Thermal shielding is essential to support the cool-down process and to reduce both the particle adsorption and the heat load on the optics. Additionally in steady-state operation, mechanical vibrations must be kept to an absolute minimum to limit the noise input by scattered light. We present the development progress of a thermal shield surrounding the cryogenic payloads of ET-LF, which considers rapid cool-down and low vibration in steady-state operation. During cool-down, cooling tubes enable the flow of supercritical helium, driving the shield temperature decrease by forced convection. For steady-state operation, the shield cooling mechanism is converted to heat conduction at 2 K via static He-II in the same tubes. The conceptual design status is explained by means of analytical and numerical modeling results.
- Published
- 2023
16. Seismic noise measures for underground gravitational wave detectors.
- Author
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Somlai, L. Ábel, Gráczer, Zoltán, Lévai, P., Vasúth, M., Wéber, Z., and Ván, P.
- Subjects
- *
GRAVITATIONAL wave detectors , *MICROSEISMS , *SEISMOLOGY , *DISCRETIZATION methods , *TELESCOPES - Abstract
The site characterisation of future underground gravitational wave detectors is based on spectral properties of the low frequency seismic noise. The evaluation of the collected long term seismological data in the Mátra Gravitational and Geophysical Laboratory revealed some aspects that are not apparent in short term spectral noise characterisation. In this paper we survey the methodology. In particular, we argue that the spectral properties are best represented by percentiles of the data instead of the mode, because it is noisy, sensitive to the discretization and intrinsic averaging, therefore it is less suitable for a robust characterisation. The suitable cumulative measures are also scrutinized. [ABSTRACT FROM AUTHOR]
- Published
- 2019
- Full Text
- View/download PDF
17. Filtered asymmetric dark matter during the Peccei-Quinn phase transition
- Author
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M. Ahmadvand
- Subjects
Physics ,Nuclear and High Energy Physics ,Phase transition ,Particle physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Einstein Telescope ,Gravitational wave ,Dark matter ,High Energy Physics::Phenomenology ,FOS: Physical sciences ,QC770-798 ,Cosmology of Theories beyond the SM ,High Energy Physics - Phenomenology ,High Energy Physics - Phenomenology (hep-ph) ,Nuclear and particle physics. Atomic energy. Radioactivity ,Beyond Standard Model ,Strong CP problem ,Symmetry breaking ,Neutrino ,Axion ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
In this paper, we propose a bubble filtering-out mechanism for an asymmetric dark matter scenario during the Peccei-Quinn (PQ) phase transition. Based on a QCD axion model, extended by extra chiral neutrinos, we show that the PQ phase transition can be first order in the parameter space of the model and regarding the PQ symmetry breaking scale, the mechanism can generate PeV-scale heavy neutrinos as a dark matter candidate. Considering a CP-violating source, during the phase transition, discriminating between the neutrino and antineutrino number density, we find the observed dark matter relic abundance, such that the setup can be applied to the first order phase transition with different strengths. We then calculate effective couplings of the QCD axion addressing the strong CP problem within the model. We also study the energy density spectrum of gravitational waves generated from the first order phase transition and show that the signals can be detected by future ground-based detectors such as Einstein Telescope. In particular, for a visible heavy axion case of the model, it is shown that gravitational waves can be probed by DECIGO and BBO interferometers. Furthermore, we discuss the dark matter-standard model neutrino annihilation process as a source for the creation of PeV-scale neutrinos., 20 pages, 6 figures; matches published version
- Published
- 2021
18. ETpathfinder: a cryogenic testbed for interferometric gravitational-wave detectors
- Author
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Utina, A., Amato, A., Arends, J., Arina, C., de Baar, M., Baars, M., Baer, P., van Bakel, N., Beaumont, W., Bertolini, A., van Beuzekom, M., Biersteker, S., Binetti, A., ter Brake, H. J. M., Bruno, G., Bryant, J., Bulten, H. J., Busch, L., Cebeci, P., Collette, C., Cooper, S., Cornelissen, R., Cuijpers, P., van Dael, M., Danilishin, S., Diksha, D., van Doesburg, S., Doets, M., Elsinga, R., Erends, V., van Erps, J., Freise, A., Frenaij, H., Garcia, R., Giesberts, M., Grohmann, S., Van Haevermaet, H., Heijnen, S., van Heijningen, J. V., Hennes, E., Hennig, J.-S., Hennig, M., Hertog, T., Hild, S., Hoffmann, H.-D., Hoft, G., Hopman, M., Hoyland, D., Iandolo, G. A., Ietswaard, C., Jamshidi, R., Jansweijer, P., Jones, A., Jones, P., Knust, N., Koekoek, G., Koroveshi, X., Kortekaas, T., Koushik, A. N., Kraan, M., van de Kraats, M., Kranzhoff, S. L., Kuijer, P., Kukkadapu, K. A., Lam, K., Letendre, N., Li, P., Limburg, R., Linde, F., Locquet, J.-P., Loosen, P., Lueck, H., Martínez, M., Masserot, A., Meylahn, F., Molenaar, M., Mow-Lowry, C., Mundet, J., Munneke, B., van Nieuwland, L., Pacaud, E., Pascucci, D., Petit, S., Van Ranst, Z., Raskin, G., Recaman, P. M., van Remortel, N., Rolland, L., de Roo, L., Roose, E., Rosier, J. C., Ryckbosch, D., Schouteden, K., Sevrin, A., Sider, A., Singha, A., Spagnuolo, V., Stahl, Achim, Steinlechner, J., Steinlechner, S., Swinkels, B., Szilasi, N., Tacca, M., Thienpont, H., Vecchio, A., Verkooijen, H., Vermeer, C. H., Vervaeke, M., Visser, G., Walet, R., Werneke, P., Westhofen, C., Willke, B., Xhahi, A., Zhang, T., (Astro)-Particles Physics, Energy, Materials and Systems, Grav. waves and fundamental physics, RS: FSE Grav. waves and fundamental physics, Theoretical Physics, Physics, Brussels Photonics Team, Mechanics of Materials and Constructions, Applied Physics and Photonics, and Technology Transfer & Interface
- Subjects
Voyager ,Technology ,Physics - Instrumentation and Detectors ,Physics and Astronomy (miscellaneous) ,gr-qc ,third generation of gravitational-wave ,Physics, Multidisciplinary ,FOS: Physical sciences ,gravitational-wave detectors ,General Relativity and Quantum Cosmology (gr-qc) ,third generation of gravitational-wave detectors ,Astronomy & Astrophysics ,General Relativity and Quantum Cosmology ,Physics, Particles & Fields ,Einstein Telescope ,ddc:530 ,SDG 7 - Affordable and Clean Energy ,SILICON ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,physics.ins-det ,detectors ,Science & Technology ,Quantum Science & Technology ,Physics ,Instrumentation and Detectors (physics.ins-det) ,ETpathfinder ,THERMAL NOISE ,Physics and Astronomy ,Physical Sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Cosmic Explorer ,ddc:600 ,astro-ph.IM - Abstract
Classical and quantum gravity 39(21), 215008 (2022). doi:10.1088/1361-6382/ac8fdb, Published by IOP Publ., Bristol
- Published
- 2022
19. Investigation of Infrasound Background Noise at Mátra Gravitational and Geophysical Laboratory (MGGL)
- Author
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Edit Fenyvesi, József Molnár, and Sándor Czellár
- Subjects
gravitational wave detection ,newtonian noise ,infrasound ,site characterization ,einstein telescope ,Elementary particle physics ,QC793-793.5 - Abstract
Infrasound and seismic waves are supposed to be the main contributors to the gravity-gradient noise (Newtonian noise) of the third-generation subterranean gravitational wave detectors. This noise will limit the sensitivity of the instrument at frequencies below 20 Hz. Investigation of its origin and the possible methods of mitigation have top priority during the designing period of the detectors. Therefore, long-term site characterizing measurements are needed at several subterranean sites. However, at some sites, mining activities can occur. These activities can cause sudden changes (transients) in the measured signal, and increase the continuous background noise, too. We have developed an algorithm based on discrete Haar transform to find these transients in the infrasound signal. We found that eliminating the transients decreases the variation of the noise spectra, and therefore results a more accurate characterization of the continuous background noise. We carried out experiments for controlling the continuous noise. Machines operating at the mine were turned on and off systematically in order to see their effect on the noise spectra. These experiments showed that the main contributor of the continuous noise is the ventilation system of the mine. We also estimated the contribution of infrasound Newtonian noise at MGGL to the strain noise of a subterranean GW detector similar to Einstein Telescope.
- Published
- 2020
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20. Modified gravitational wave propagation and the binary neutron star mass function
- Abstract
Modified gravitational wave (GW) propagation is a generic phenomenon in modified gravity. It affects the reconstruction of the redshift of coalescing binaries from the luminosity distance measured by GW detectors, and therefore the reconstruction of the actual masses of the component compact stars from the observed (‘detector-frame’) masses. We show that, thanks to the narrowness of the mass distribution of binary neutron stars, this effect can provide a clear signature of modified gravity, particularly for the redshifts explored by third generation GW detectors such as Einstein Telescope and Cosmic Explorer.
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- 2022
21. Lensing magnification: gravitational waves from coalescing stellar-mass binary black holes
- Author
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Chengliang Wei, Bin Hu, and Xikai Shan
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Einstein Telescope ,Mass distribution ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,Horizon ,FOS: Physical sciences ,Astronomy and Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,General Relativity and Quantum Cosmology ,Galaxy ,Redshift ,Cover (topology) ,Binary black hole ,Space and Planetary Science ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Gravitational waves (GWs) may be magnified or de-magnified due to lensing. This phenomenon will bias the distance estimation based on the matched filtering technique. Via the multi-sphere ray-tracing technique, we study the GW magnification effect and selection effect with particular attention to the stellar-mass binary black holes (BBHs). We find that, for the observed luminosity distance $\lesssim 3~\mathrm{Gpc}$, which is the aLIGO/Virgo observational horizon limit, the average magnification keeps as unity, namely unbiased estimation, with the relative distance uncertainty $\sigma(\hat{d})/\hat{d}\simeq0.5\%\sim1\%$. Beyond this observational horizon, the estimation bias can not be ignored, and with the scatters $\sigma(\hat{d})/\hat{d} = 1\%\sim 15\%$. Furthermore, we forecast these numbers for Einstein Telescope. We find that the average magnification keeps closely as unity for the observed luminosity distance $\lesssim 90~\mathrm{Gpc}$. The luminosity distance estimation error due to lensing for Einstein Telescope is about $\sigma(\hat{d})/\hat{d} \simeq 10\%$ for the luminosity distance $\gtrsim 25~\mathrm{Gpc}$. Unlike the aLIGO/Virgo case, this sizable error is not due to the selection effect. It purely comes from the unavoidably accumulated lensing magnification. Moreover, we investigated the effects of the orientation angle and the BH mass distribution models. We found that the results are strongly dependent on these two components., Comment: 9 pages, 9 figures, published in MNRAS
- Published
- 2021
22. Status of Gravitational Wave Detection
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Giazotto, Adalberto, Burton, W. B., Series editor, Bertola, F., Series editor, Cassinelli, J. P., Series editor, Cesarsky, C. J., Series editor, Ehrenfreund, P., Series editor, Engvold, O., Series editor, Heck, A., Series editor, Van den Heuvel, E. P. J., Series editor, Kaspi, V. M., Series editor, Kuijpers, J. M. E., Series editor, Van der Laan, H., Series editor, Murdin, P. G., Series editor, Pacini, F., Series editor, Radhakrishnan, V., Series editor, Somov, B. V., Series editor, Sunyaev, R. A., Series editor, Ciufolini, Ignazio, editor, and Matzner, Richard A., editor
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- 2010
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23. The Detection of Gravitational Waves
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Cella, Giancarlo, Carlino, Gianpaolo, editor, D’Ambrosio, Giancarlo, editor, Merola, Leonardo, editor, Paolucci, Pierluigi, editor, and Ricciardi, Giulia, editor
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- 2008
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24. On the population III binary black hole mergers beyond the pair-instability mass gap
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Tomoya Kinugawa, Hideyuki Umeda, Takashi Yoshida, Ataru Tanikawa, and Kotaro Hijikawa
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,education.field_of_study ,Initial mass function ,Einstein Telescope ,Gravitational wave ,Population ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Black hole ,Astrophysics - Solar and Stellar Astrophysics ,Binary black hole ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics - High Energy Astrophysical Phenomena ,education ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Mass gap - Abstract
We perform a binary population synthesis calculation incorporating very massive population (Pop.) III stars up to 1500 $M_\odot$, and investigate the nature of binary black hole (BBH) mergers. Above the pair-instability mass gap, we find that the typical primary black hole (BH) mass is 135-340 $M_\odot$. The maximum primary BH mass is as massive as 686 $M_\odot$. The BBHs with both of their components above the mass gap have low effective inspiral spin $\sim$ 0. So far, no conclusive BBH merger beyond the mass gap has been detected, and the upper limit on the merger rate density is obtained. If the initial mass function (IMF) of Pop. III stars is simply expressed as $\xi_m(m) \propto m^{-\alpha}$ (single power law), we find that $\alpha \gtrsim 2.8$ is needed in order for the merger rate density not to exceed the upper limit. In the future, the gravitational wave detectors such as Einstein telescope and Pre-DECIGO will observe BBH mergers at high redshift. We suggest that we may be able to impose a stringent limit on the Pop. III IMF by comparing the merger rate density obtained from future observations with that derived theoretically., Comment: 6 pages, 9 figures, 1 table. Accepted for publication in MNRAS Letters
- Published
- 2021
25. Testing the general theory of relativity using gravitational wave propagation from dark standard sirens
- Author
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Suvodip Mukherjee, Joseph Silk, Benjamin D. Wandelt, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, and Sorbonne Université (SU)
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,redshift: dependence ,gravitation: model ,General relativity ,FOS: Physical sciences ,detector: network ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,baryon: oscillation: acoustic ,01 natural sciences ,General Relativity and Quantum Cosmology ,electromagnetic field: production ,Einstein Telescope ,statistical analysis ,gravitational radiation: propagation ,numerical methods ,0103 physical sciences ,general relativity ,KAGRA ,LIGO ,numerical calculations ,010303 astronomy & astrophysics ,Luminosity distance ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,LISA ,010308 nuclear & particles physics ,Gravitational wave ,Astronomy and Astrophysics ,Redshift ,Baryon ,VIRGO ,gravitational waves ,Space and Planetary Science ,gravitational radiation: emission ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,large-scale structure of Universe ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Alternative theories of gravity predict modifications in the propagation of gravitational waves (GW) through space-time. One of the smoking-gun predictions of such theories is the change in the GW luminosity distance to GW sources as a function of redshift relative to the electromagnetic (EM) luminosity distance expected from EM probes. We propose a multi-messenger test of the theory of general relativity from the propagation of gravitational waves by combining EM and GW observations to resolve these issues from GW sources without EM counterparts (which are also referred to as dark standard sirens). By using the relation between the geometric distances accessible from baryon acoustic oscillation measurements, and luminosity distance measurements from the GW sources, we can measure any deviation from the general theory of relativity via the GW sources of unknown redshift that will be detectable by networks of GW detectors such as LIGO, Virgo, and KAGRA. Using this technique, the fiducial value of the frictional term can be measured to a precision $\Xi_0=0.98^{+0.04}_{-0.23}$ after marginalizing over redshift dependence, cosmological parameters, and GW bias parameters with $\sim 3500$ dark standard sirens of masses $30\,\rm M_\odot$ each distributed up to redshift $z=0.5$. For a fixed redshift dependence, a value of $\Xi_0=0.99^{+0.02}_{-0.02}$ can be measured with a similar number of dark sirens. Application of our methodology to the far more numerous dark standard sirens detectable with next generation GW detectors, such as LISA, Einstein Telescope and Cosmic Explorer, will allow achievement of higher accuracy than possible from use of bright standard sirens., Comment: 10 pages, 3 figures. Accepted for publication in MNRAS
- Published
- 2021
26. Lensed gravitational waves: Scattering and applications
- Author
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Xilong Fan
- Subjects
Physics ,Black hole ,General Relativity and Quantum Cosmology ,Multidisciplinary ,Gravitational lens ,Gravitational-wave observatory ,Einstein Telescope ,General relativity ,Gravitational wave ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Gravitational-wave astronomy ,LIGO - Abstract
The direct detection of gravitational waves from stellar-mass compact binary merger by ground-based laser interferometer gravitational wave detector LIGO/Virgo has verified the prediction of general relativity and opened a new chapter in gravitational wave astronomy. Up to now, a total of 50 gravitational wave events have been detected and published in GWTC-1 and GWTC-2 catalogue. In the near future, the third-generation ground based gravitational wave detector, such as the Einstein Telescope (ET), will be constructed with sensitivity improved by at least a factor of 10. Tens of thousands of gravitational wave signals are expected to be detected per year in the third-generation detector era. These gravitational wave signals will inevitably overlap with foreground massive celestial bodies (such as black hole, galaxy and galaxy cluster), thus leading to lensed gravitational wave signals which will undoubtedly be another important test of general relativity once detected. Furthermore, strongly lensed gravitational wave signals by galaxy from massive binary black hole could possibly be detected by future space detector, e.g., LISA and DECIGO. Since the wavelengths of gravitational waves are comparable with the size of some lens, the lensed gravitational waves play a unique role in studying the phenomena of wave nature, e.g., interference and diffraction. Lensed gravitational wave-electromagnetic wave system will have a wide range of applications in fundamental physics, cosmology and astrophysics when a series of lensed gravitational wave events and their corresponding electromagnetic counterparts have been detected. The most obvious advantage of lensed gravitational wave-electromagnetic wave system lies in that gravitational wave could provide time delay information with high accuracy, and electromagnetic wave could provide Fermat potential difference with high precision because a relatively complete arc of light could be obtained by electromagnetic wave observations and this is the most important step in measuring the Fermat potential. Thus, by combining the information from both approaches, lensed gravitational wave-electromagnetic wave system could be applied to study the speed of gravitational waves, constrain cosmological parameters, explore the substructure of the dark matter halo and investigate the lens model and so on. In this paper, we will review in detail how to use geodesic equation, lens equation, as well as wave equation to tackle the stationary scattering problem of lensed gravitational waves, and introduce how lensed gravitational wave-electromagnetic wave system could be applied to study the tensor properties, interference and diffraction effects of gravitational wave, as well as its applications in gravitational wave velocity, Hubble constant, cosmic curvature, lens mass, substructure and so on.
- Published
- 2020
27. Post-merger chirps from binary black holes as probes of the final black-hole horizon
- Author
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Deirdre Shoemaker, Pablo Laguna, Christopher Evans, Juan Calderón Bustillo, Grace Kim, and James A. Clark
- Subjects
Physics::General Physics ,Astrophysics::High Energy Astrophysical Phenomena ,General Physics and Astronomy ,FOS: Physical sciences ,lcsh:Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,General Relativity and Quantum Cosmology ,Binary black hole ,0103 physical sciences ,lcsh:QB460-466 ,010306 general physics ,010303 astronomy & astrophysics ,Physics ,Einstein Telescope ,Gravitational wave ,Horizon ,LIGO ,lcsh:QC1-999 ,Black hole ,Numerical relativity ,Apparent horizon ,lcsh:Physics - Abstract
The merger of a binary black hole gives birth to a highly distorted final black hole. The gravitational radiation emitted as this black hole relaxes presents us with the unique opportunity to probe extreme gravity and its connection with the dynamics of the black hole horizon. Using numerical relativity simulations, we demonstrate a connection between a concrete observable feature in the gravitational waves and geometrical features on the dynamical apparent horizon of the final black hole. Specifically, we show how the line-of-sight passage of a "cusp"-like defect on the horizon of the final black hole correlates with "chirp"-like frequency peaks in the post-merger gravitational-waves. These post-merger chirps should be observed and analyzed as the sensitivity of LIGO and Virgo increases and as future generation detectors, such as LISA and the Einstein Telescope, become operational., Comment: Version accepted in Communications Physics. 11 pages, 5 figures in main text, 3 Figures in Supp. Material
- Published
- 2020
28. EUROGRAV 1986–1989: the first attempts for a European Interferometric Gravitational Wave Observatory
- Author
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Adele La Rana
- Subjects
European network ,Einstein Telescope ,Eurograv ,General Physics and Astronomy ,Gravitational waves, Eurograv, Interferometric detectors, European network, Einstein Telescope ,Interferometric detectors ,Gravitational waves - Abstract
At the turn of the 1980s and 1990s, on the eve of the great leap in scale from the resonant bars to the long-baseline interferometers LIGO and Virgo, the four European groups then engaged in the field of interferometric gravitational wave detection in Germany, UK, France and Italy tried to set up a common strategy, with the aim of establishing a network of three long-based antennas in Europe. The paper analyzes the main causes of the failure of those early plans. An attempt is made to outline the parallels and differences with the current times, on the eve of the new leap of scale toward the third generation of gravitational wave interferometers, while the negotiations for the European-born project Einstein Telescope are taking place.
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- 2022
29. Newtonian-noise characterization at Terziet in Limburg-the Euregio Meuse-Rhine candidate site for Einstein Telescope
- Author
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Maria Bader, Soumen Koley, Jo van den Brand, Xander Campman, Henk Jan Bulten, Frank Linde, Bjorn Vink, Grav. waves and fundamental physics, and RS: FSE Grav. waves and fundamental physics
- Subjects
Newtonian-noise ,Einstein Telescope ,Physics and Astronomy (miscellaneous) ,SEISMIC NOISE ,background body-waves ,WAVES ,surface waves ,Physics::Geophysics - Abstract
Limburg, in the border region between Belgium, Germany and the Netherlands, has been identified as the Euregio Meuse–Rhine candidate site for Einstein Telescope. The site hosting this gravitational-wave observatory must minimize the Newtonian coupling of ground vibrations to the core optics of the low-frequency detectors. Newtonian noise depends on the ambient seismic field which is in turn dependent on the site’s geology and the distribution of surface and underground seismic-noise sources. We have characterized the site near Terziet in Limburg in terms of propagation modes, dispersion and angular distribution of seismic noise by employing sensor arrays on the surface. Attenuation of seismic noise with depth was studied with a borehole sensor. Based on the results of these measurements, a realistic seismic-field model has been derived that represents a complete solution of the elastodynamic wave equations for a horizontally-layered soil structure. This seismic-field model allows to estimate the Newtonian-noise contribution to the sensitivity of Einstein Telescope for the characteristic geology and ambient noise conditions in South Limburg. The site’s geology features soft-soil layers on hard-rock and is effective in attenuating Newtonian noise from surface waves below the required sensitivity. A random background of body waves with all possible angles of incidence is expected to constitute the dominant source of Newtonian noise.
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- 2022
30. Surface and underground seismic characterization at Terziet in Limburg-the Euregio Meuse-Rhine candidate site for Einstein Telescope
- Author
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Frank Linde, H. J. Bulten, Maria Bader, S. Koley, Johannes van den Brand, Xander Campman, Bjorn Vink, Grav. waves and fundamental physics, and RS: FSE Grav. waves and fundamental physics
- Subjects
Physics ,Surface (mathematics) ,Physics and Astronomy (miscellaneous) ,Einstein Telescope ,body wave background ,underground seismic noise ,MICROSEISMS ,WAVES ,AREA ,Geophysics ,Newtonian noise ,Physics::Geophysics ,Characterization (materials science) ,AMBIENT NOISE TOMOGRAPHY ,EQUATION ,INVERSION ,ALGORITHM ,FIELD ,Einstein telescope ,ambient seismic noise - Abstract
We present a detailed characterization of surface and underground seismic noise measured at Limburg in the south of the Netherlands. This location is the Euregio Meuse–Rhine candidate for hosting Einstein Telescope, a future observatory for gravitational waves. Seismic noise measurements were performed with an array of seismometers installed on the surface. Passive seismic methods like beamforming were used to extract the propagation wave types of ambient seismic noise and the Rayleigh-wave dispersion in the region. Subsurface shear-wave models sensitive to depths of 300 m were derived by using the Rayleigh-wave dispersion and ellipticity. Subsurface P-wave velocities to depths of 200 m were obtained from an active seismic survey. Wavepath Eikonal tomography was used on the source-receiver refracted-wave travel-times to obtain a subsurface P-wave velocity model. Both the passive and the active seismic data analysis point to the presence of a layered geology with a soft-soil to hard-rock transition occurring at a shallow depth of about 25 to 40 m. The surface arrays are complemented by two permanent tri-axial seismometers installed on the surface and in a borehole at 250 m depth. Their data are used to interpret the surface-wave and body-wave contributions to the observed seismic noise. We use a cross-correlation analysis and compute the theoretical surface-wave eigenfunctions to understand the contributions of the different wave types at different frequencies. We observe that below 4 Hz in the horizontal component and 9 Hz in the vertical component, the seismic noise at depth is dominantly due to surface waves. Above these frequencies a significant contribution can be attributed to both nearby and far-away body-wave sources. At a depth of 250 m we find that the surface noise power has been damped by up to a factor 104 above about 2 Hz. The Limburg geology with soft-soil on top of hard-rock efficiently damps the anthropogenic noise produced at the surface. This implies that Einstein Telescope’s test masses are shielded from anthropogenic seismic noise and construction at greater depth will not bring significant further improvements in this regard. A body-wave background has been identified that contributes about half of the total underground seismic noise at 250 m depth for frequencies above 4 Hz. It remains to be studied if subtraction schemes for Newtonian noise originating from this body-wave background will be necessary. Finally, we estimate an interferometer downtime of about 3% due to regional and teleseismic earthquakes. We believe this is acceptable as it is comparable to current experience at the LIGO and Virgo interferometer sites.
- Published
- 2022
31. Sensitivity of third-generation interferometers to extra polarizations in the stochastic gravitational wave background
- Author
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Loris Amalberti, Nicola Bartolo, and Angelo Ricciardone
- Subjects
gravitational radiation: polarization ,noise ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,gravitational radiation: stochastic ,gravitation: model ,interferometer ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,General Relativity and Quantum Cosmology ,High Energy Physics - Phenomenology (hep-ph) ,Einstein Telescope ,stochastic [gravitational radiation] ,general relativity ,ddc:530 ,energy: density ,background [gravitational radiation] ,gravitational radiation: frequency ,gravitational radiation: background ,model [gravitation] ,family: 3 ,polarization [gravitational radiation] ,sensitivity ,background: stochastic ,observatory ,High Energy Physics - Phenomenology ,stochastic [background] ,frequency [gravitational radiation] ,network ,3 [family] ,density [energy] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Physical review / D 105(6), 064033 (2022). doi:10.1103/PhysRevD.105.064033, When modified theories of gravity are considered, at most six gravitational wave polarization modes are allowed and classified in tensor modes, the only ones predicted by general relativity (GR), along with additional vector and scalar modes. Therefore, gravitational waves represent a powerful tool to test alternative theories of gravitation. In this paper, we forecast the sensitivity of third-generation ground-based interferometers, Einstein Telescope and Cosmic Explorer, to non-GR polarization modes focusing on the stochastic gravitational wave background. We consider the latest technical specifications of the two independent detectors and the full network in order to estimate both the optimal signal-to-noise ratio and the detectable energy density limits relative to all polarization modes in the stochastic background for several locations on Earth and orientations of the two observatories. By considering optimal detector configurations, we find that in 5 years of observation the detection limit for tensor and extra polarization modes could reach $h^2_0Ω_{GW}^{T,V,S}≈10^{-12}-10^{-11}$, depending on the network configuration and the stochastic background (i.e., if only one among vector and scalar modes exists or both are present). This means that the network sensitivity to different polarization modes can be approximately improved by a factor 103 with respect to second-generation interferometers. We finally discuss the possibility of breaking the scalar modes degeneracy by considering both detectors angular responses to sufficiently high gravitational wave frequencies., Published by Inst., Melville, NY
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- 2022
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32. Dancing in the dark: detecting a population of distant primordial black holes
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Matteo Martinelli, Francesca Scarcella, Natalie B. Hogg, Bradley J. Kavanagh, Daniele Gaggero, Pierre Fleury, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Agenzia Spaziale Italiana, Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Fundación 'la Caixa', Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), Ministero dell'Istruzione, dell'Università e della Ricerca, Ministerio de Ciencia, Innovación y Universidades (España), Istituto Nazionale di Fisica Nucleare, and Generalitat Valenciana
- Subjects
High Energy Physics - Theory ,data analysis method ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,black hole: binary: coalescence ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,luminosity: redshift ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,General Relativity and Quantum Cosmology ,gravitational waves / experiments ,Einstein Telescope ,Astrophysics::Galaxy Astrophysics ,density ,dark matter theory ,[PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th] ,primordial black holes ,family: 3 ,gravitational radiation ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,gravitational radiation detector ,observatory ,confidence limit ,collapse ,High Energy Physics - Theory (hep-th) ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,gravitational waves / sources ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,black hole: primordial ,statistical ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Primordial black holes (PBHs) are compact objects proposed to have formed in the early Universe from the collapse of small-scale over-densities. Their existence may be detected from the observation of gravitational waves (GWs) emitted by PBH mergers, if the signals can be distinguished from those produced by the merging of astrophysical black holes. In this work, we forecast the capability of the Einstein Telescope, a proposed third-generation GW observatory, to identify and measure the abundance of a subdominant population of distant PBHs, using the difference in the redshift evolution of the merger rate of the two populations as our discriminant. We carefully model the merger rates and generate realistic mock catalogues of the luminosity distances and errors that would be obtained from GW signals observed by the Einstein Telescope. We use two independent statistical methods to analyse the mock data, finding that, with our more powerful, likelihood-based method, PBH abundances as small as fPBH ≈ 7 × 10-6 (fPBH ≈ 2×10-6) would be distinguishable from fPBH = 0 at the level of 3σ with a one year (ten year) observing run of the Einstein Telescope. Our mock data generation code, darksirens, is fast, easily extendable and publicly available on GitLab., MM acknowledges funding by the Agenzia Spaziale Italiana (ASI) under agreement n. 2018-23-HH.0. FS was supported by the Spanish Agencia Estatal de Investigacion through the grants IFT Centro de Excelencia Severo Ochoa CEX2020-001007-S and PGC2018-095161-BI00, and, during the early stages of this work, through the grants Severo Ochoa SEV-2016-0597 and Red Consolider MultiDark FPA2017-90566-REDC. FS has received financial support through la Caixa Banking Foundation (grant n. LCF/BQ/LI18/11630014) during the early stages of the project. NBH is supported by a postdoctoral position previously funded through two “la Caixa” Foundation fellowships (ID00010434), with codes LCF/BQ/PI19/11690015 and LCF/BQ/PI19/11690018 respectively, and currently funded by the French Commissariat a l’energie atomique et aux energies alternatives (CEA). BJK thanks the Spanish Agencia Estatal de Investigacion (AEI, MICIU) for the support to the Unidad de Excelencia Maria de Maeztu Instituto de Fisica de Cantabria, ref. MDM-2017-0765. DG has received financial support through the Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation (grant n. LCF/BQ/LI18/11630014) during the early stage of the project. DG was also supported by the Spanish Agencia Estatal de Investigacion through the grants PGC2018-095161-B-I00, IFT Centro de Excelencia Severo Ochoa SEV-2016-0597, and Red Consolider MultiDark FPA2017-90566-REDC during the early stages of the project. DG acknowledges funding from the “Department of Excellence” grant awarded by the Italian Ministry of Education, University and Research (MIUR) in October-December 2021. DG also acknowledges support from the INFN grant “LINDARK,” and the project “Theoretical Astroparticle Physics (TAsP)” funded by the INFN in October-December 2021. DG acknowledges support from Generalitat Valenciana through the plan GenT program (CIDEGENT/2021/017) starting from 01/01/2022. In the early stages of this work, MM and PF received the support of a fellowship from “la Caixa” Foundation (ID 100010434). The fellowship codes are LCF/BQ/PI19/11690015 and LCF/BQ/PI19/11690018 for MM and PF respectively.
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- 2022
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33. A lower limit for Newtonian-noise models of the Einstein Telescope
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Jan Harms, Luca Naticchioni, Enrico Calloni, Rosario De Rosa, Fulvio Ricci, Domenico D’Urso, Harms, J., Naticchioni, L., Calloni, E., De Rosa, R., Ricci, F., and D'Urso, D.
- Subjects
Fluid Flow and Transfer Processes ,Einstein Telescope ,FOS: Physical sciences ,General Physics and Astronomy ,Newtonian noise ,ET ,General Relativity and Quantum Cosmology (gr-qc) ,General Relativity and Quantum Cosmology - Abstract
The Einstein Telescope (ET) is a proposed third-generation gravitational-wave (GW) underground observatory. It will have greatly increased sensitivity compared to current GW detectors, and it is designed to extend the observation band down to a few Hz. At these frequencies, a major limitation of the ET sensitivity is predicted to be due to gravitational fluctuations produced by the environment, most importantly by the seismic field, which give rise to the so-called Newtonian noise (NN). Accurate models of ET NN are crucial to assess the compatibility of an ET candidate site with the ET sensitivity target also considering a possible reduction of NN by noise cancellation. With NN models becoming increasingly complex as they include details of geology and topography, it is crucial to have tools to make robust assessments of their accuracy. For this purpose, we derive a lower bound on seismic NN spectra, which is weakly dependent on geology and properties of the seismic field. As a first application, we use the lower limit to compare it with NN estimates recently calculated for the Sardinia and Euregio Meuse-Rhine (EMR) candidate sites. We find the utility of the method, which shows an inconsistency with the predictions for the EMR site, which indicates that ET NN models require further improvement., 16 pages, 4 figures, 2 tables
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- 2022
34. Gravitational radiation from inspiralling compact objects: Spin effects to the fourth post-Newtonian order
- Author
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Porto Pereira, Rafael Alejandro, Yang, Zixin, and Cho, Gihyuk
- Subjects
High Energy Physics - Theory ,higher-order: 4 ,LISA ,spin: effect ,gravitational radiation: flux ,binary ,orbit: circle ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,expansion: higher-order ,4 [higher-order] ,General Relativity and Quantum Cosmology ,effect [spin] ,Einstein Telescope ,effective field theory ,higher-order [expansion] ,High Energy Physics - Theory (hep-th) ,finite size ,general relativity ,overlap ,ddc:530 ,flux [gravitational radiation] ,circle [orbit] - Abstract
Physical review / D 106(10), L101501 (2022). doi:10.1103/PhysRevD.106.L101501, The linear- and quadratic-in-spin contributions to the binding potential and gravitational-wave flux from binary systems are derived to next-to-next-to-leading order in the post-Newtonian (PN) expansion of general relativity, including finite-size and tail effects. The calculation is carried out through the worldline effective field theory framework. We find agreement in the overlap with the available PN and self-force literature. As a direct application, we complete the knowledge of spin effects in the evolution of the orbital phase for aligned-spin circular orbits to fourth PN order. We estimate the impact in the number of accumulated gravitational-wave cycles and find they make a significant contribution for next-generation observatories. The results presented here will therefore play an important role in providing reliable physical interpretation of gravitational-wave signals from spinning binaries with future gravitational-wave detectors such as LISA and the Einstein Telescope., Published by Inst., Melville, NY
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- 2022
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35. Gravitational radiation from inspiralling compact objects: Spin effects to fourth Post-Newtonian order
- Author
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Porto Pereira, Rafael Alejandro, Yang, Zixin, and Cho, Gihyuk
- Subjects
higher-order: 4 ,General Relativity and Quantum Cosmology ,LISA ,Einstein Telescope ,effective field theory ,finite size ,spin: effect ,gravitational radiation: flux ,binary ,general relativity ,orbit: circle ,overlap ,expansion: higher-order - Abstract
The linear- and quadratic-in-spin contributions to the binding potential and gravitational-wave flux from binary systems are derived to next-to-next-to-leading order in the Post-Newtonian (PN) expansion of general relativity, including finite-size and tail effects. The calculation is carried out through the worldline effective field theory framework. We find agreement in the overlap with the available PN literature and test-body limit. As a direct application, we complete the knowledge of spin effects in the evolution of the orbital phase for aligned-spin circular orbits to fourth PN order. We estimate the impact of the new results in the number of accumulated gravitational-wave cycles. We find they will play an important role in providing reliable physical interpretation of gravitational-wave signals from spinning binaries with future detectors such as LISA and the Einstein Telescope.
- Published
- 2022
- Full Text
- View/download PDF
36. Thermal design of the He-II suspension tube for ET-LF: Status and outlook
- Author
-
Busch, Lennard Niclas and Grohmann, Steffen
- Subjects
Technology ,Einstein Telescope ,Cryogenics ,Suspension ,ddc:600 ,ET ,Helium - Published
- 2022
37. Transient gravitational waves from pulsar post-glitch recoveries
- Author
-
Garvin Yim and David Jones
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Einstein Telescope ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics ,01 natural sciences ,General Relativity and Quantum Cosmology ,LIGO ,Neutron star ,Amplitude ,Pulsar ,Space and Planetary Science ,0103 physical sciences ,Transient (oscillation) ,Glitch (astronomy) ,Astrophysics - High Energy Astrophysical Phenomena ,010306 general physics ,010303 astronomy & astrophysics - Abstract
This work explores whether gravitational waves (GWs) from neutron star (NS) mountains can be detected with current 2nd-generation and future 3rd-generation GW detectors. In particular, we focus on a scenario where transient mountains are formed immediately after a NS glitch. In a glitch, a NS's spin frequency abruptly increases and then often exponentially recovers back to, but never quite reaches, the spin frequency prior to the glitch. If the recovery is ascribed to an additional torque due to a transient mountain, we find that GWs from that mountain are marginally-detectable with Advanced LIGO at design sensitivity and is very likely to be detectable for 3rd-generation detectors such as the Einstein Telescope. Using this model, we are able to find analytical expressions for the GW amplitude and its duration in terms of observables., 16 pages, 3 figures. Small changes made in response to referee comments. Accepted for publication in MNRAS
- Published
- 2020
38. Probing compact dark matter with gravitational wave fringes detected by the Einstein Telescope
- Author
-
Xuheng Ding, Shuxun Tian, and Kai Liao
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Einstein Telescope ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Primordial black hole ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Electromagnetic radiation ,General Relativity and Quantum Cosmology ,LIGO ,Space and Planetary Science ,Binary star ,Astrophysics::Earth and Planetary Astrophysics ,Schwarzschild radius ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Unlike the electromagnetic radiation from astrophysical objects, gravitational waves (GWs) from binary star mergers have much longer wavelengths and are coherent. For ground-based GW detectors, when the lens object between the source and the earth has mass $\sim 1-10^5M_\odot$, the diffraction effect should be considered since the chirping wavelengths are comparable to the scale of the barrier (its Schwarzschild radius). The waveform will thus be distorted as the fringes. In this work, we show that signals from the third-generation GW detectors like the Einstein Telescope (ET) would be a smoking gun for probing the nature of compact dark matter (CDM) or primordial black holes. Detection of the lensing effects becomes harder when the lens mass is smaller. ET is more sensitive than LIGO, the constraint is available for CDM mass $>5M_\odot$ while LIGO can only detect the mass $>100M_\odot$. For a null search of the fringes, one-year observation of ET can constrain the CDM density fraction to $\sim10^{-2}-10^{-5}$ in the mass range $M_{\rm{CDM}}=10M_\odot-100M_\odot$., 6 pages, 3 figures, accepted by MNRAS
- Published
- 2020
39. Three-dimensional core-collapse supernova simulations of massive and rotating progenitors
- Author
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Bernhard Müller and Jade Powell
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Accretion (meteorology) ,Einstein Telescope ,010308 nuclear & particles physics ,Astrophysics::High Energy Astrophysical Phenomena ,Star (game theory) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Type II supernova ,7. Clean energy ,01 natural sciences ,Stars ,Neutron star ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Red supergiant ,Neutrino ,Astrophysics - High Energy Astrophysical Phenomena ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We present three-dimensional simulations of the core-collapse of massive rotating and non-rotating progenitors performed with the general relativistic neutrino hydrodynamics code CoCoNuT-FMT and analyse their explosion properties and gravitational-wave signals. The progenitor models include Wolf-Rayet stars with initial helium star masses of $39\,M_{\odot}$ and $20\,M_{\odot}$, and an $18\,M_{\odot}$ red supergiant. The $39\,M_{\odot}$ model is a rapid rotator, whereas the two other progenitors are non-rotating. Both Wolf-Rayet models produce healthy neutrino-driven explosions, whereas the red supergiant model fails to explode. By the end of the simulations, the explosion energies have already reached $1.1\times 10^{51}\,\mathrm{erg}$ and $0.6\times 10^{51}\,\mathrm{erg}$ for the $39\,M_{\odot}$ and $20\,M_{\odot}$ model, respectively. The explosions produce neutron stars of relatively high mass, but with modest kicks. Due to the alignment of the bipolar explosion geometry with the rotation axis, there is a relatively small misalignment of $30^\circ$ between the spin and the kick in the $39\,M_{\odot}$ model. In terms of gravitational-wave signals, the massive and rapidly rotating $39\,M_{\odot}$ progenitor stands out by large gravitational-wave amplitudes that would make it detectable out to almost 2 Mpc by the Einstein Telescope. For this model, we find that rotation significantly changes the dependence of the characteristic gravitational-wave frequency of the f-mode on the proto-neutron star parameters compared to the non-rotating case. The other two progenitors have considerably smaller detection distances, despite significant low-frequency emission in the most sensitive frequency band of current gravitational-wave detectors due to the standing accretion shock instability in the $18\,M_{\odot}$ model.
- Published
- 2020
40. Exploring the CPT violation and birefringence of gravitational waves with ground- and space-based gravitational-wave interferometers
- Author
-
Sai Wang
- Subjects
Physics::General Physics ,Physics and Astronomy (miscellaneous) ,Dephasing ,Physics::Optics ,FOS: Physical sciences ,lcsh:Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,General Relativity and Quantum Cosmology ,Gravitation ,lcsh:QB460-466 ,Astronomical interferometer ,lcsh:Nuclear and particle physics. Atomic energy. Radioactivity ,Engineering (miscellaneous) ,Circular polarization ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Birefringence ,Einstein Telescope ,Gravitational wave ,High Energy Physics::Phenomenology ,Astrophysics::Instrumentation and Methods for Astrophysics ,Interferometry ,Quantum electrodynamics ,lcsh:QC770-798 ,High Energy Physics::Experiment ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
In the gravitational sector, we study the CPT violation and birefringence of gravitational waves. In presence of the CPT violation, a relative dephasing is generated between two circular polarization states of gravitational waves. This effect induces the birefringence of gravitational waves. We predict the gravitational waveform corrected by it and estimate the expected constraints on it from Advanced Laser Interferometer Gravitational-Wave Observatory, Einstein Telescope and Laser Interferometer Space Antenna., Comment: Preprint, 16 pages, 1 figure, 1 table, 2 appendices. All comments are welcome
- Published
- 2020
41. Peccei-Quinn phase transition at LIGO
- Author
-
Oriol Pujolàs, Benedict von Harling, Fabrizio Rompineve, and Alex Pomarol
- Subjects
Nuclear and High Energy Physics ,Phase transition ,Particle physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,FOS: Physical sciences ,01 natural sciences ,General Relativity and Quantum Cosmology ,High Energy Physics - Phenomenology (hep-ph) ,0103 physical sciences ,lcsh:Nuclear and particle physics. Atomic energy. Radioactivity ,Symmetry breaking ,010306 general physics ,Axion ,media_common ,Physics ,Einstein Telescope ,010308 nuclear & particles physics ,Gravitational wave ,Electroweak interaction ,High Energy Physics::Phenomenology ,Cosmology of Theories beyond the SM ,LIGO ,Universe ,High Energy Physics - Phenomenology ,Beyond Standard Model ,lcsh:QC770-798 ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The LIGO observatories can potentially detect stochastic gravitational waves arising from phase transitions which happened in the early universe at temperatures around $T\sim 10^{8}$ GeV. This provides an extraordinary opportunity for discovering the phase transition associated with the breaking of the Peccei-Quinn symmetry, required in QCD axion models. Here we consider the simplest Peccei-Quinn models and study under which conditions a strong first-order phase transition can occur, analyzing its associated gravitational wave signal. To be detectable at LIGO, we show that some supercooling is needed, which can arise either in Coleman-Weinberg-type symmetry breaking or in strongly-coupled models. We also investigate phase transitions that interestingly proceed by first breaking the electroweak symmetry at large scales before tunneling to the Peccei-Quinn breaking vacuum. In this case, the associated gravitational wave signal is more likely to be probed at the proposed Einstein Telescope., Comment: 27 pages, 7 figure. v2: references added
- Published
- 2020
42. Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys
- Author
-
Joseph Silk, Benjamin D. Wandelt, Suvodip Mukherjee, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), and Sorbonne Universités
- Subjects
cosmological model ,Physics::General Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Virgo interferometer ,General Relativity and Quantum Cosmology (gr-qc) ,detector: network ,Astrophysics::Cosmology and Extragalactic Astrophysics ,redshift: low ,01 natural sciences ,General Relativity and Quantum Cosmology ,dark matter ,Gravitation ,Einstein Telescope ,gravitational lensing: weak ,gravitation: lens ,gravitational radiation: propagation ,0103 physical sciences ,structure ,Weak lensing ,dark energy ,gravitational wave ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Physics ,LISA ,010308 nuclear & particles physics ,Gravitational wave ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,LIGO ,Redshift ,Automatic Keywords ,VIRGO ,Gravitational lens ,space-time ,gravitational waves ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,galaxy ,large-scale structure of Universe ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The cross-correlation of gravitational wave strain with upcoming galaxy surveys probe theories of gravity in a new way. This method enables testing the theory of gravity by combining the effects from both gravitational lensing of gravitational waves and the propagation of gravitational waves in spacetime. We find that within 10 years, the combination of the Advanced-LIGO and VIRGO detector networks with planned galaxy surveys should detect weak gravitational lensing of gravitational waves in the low redshift Universe ($z, 16 pages, 7 figures. Minor changes in the text and added new references. Matches the version accepted for publication in MNRAS
- Published
- 2020
43. Continuous gravitational wave from magnetized white dwarfs and neutron stars: possible missions for LISA, DECIGO, BBO, ET detectors
- Author
-
Surajit Kalita and Banibrata Mukhopadhyay
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Einstein Telescope ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,White dwarf ,Astronomy ,Astronomy and Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology ,LIGO ,Luminosity ,Black hole ,Neutron star ,Supernova ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics - Abstract
Recent detection of gravitational wave from nine black hole merger events and one neutron star merger event by LIGO and VIRGO shed a new light in the field of astrophysics. On the other hand, in the past decade, a few super-Chandrasekhar white dwarf candidates have been inferred through the peak luminosity of the light-curves of a few peculiar type Ia supernovae, though there is no direct detection of these objects so far. Similarly, a number of neutron stars with mass $>2M_\odot$ have also been observed. Continuous gravitational wave can be one of the alternate ways to detect these compact objects directly. It was already argued that magnetic field is one of the prominent physics to form super-Chandrasekhar white dwarfs and massive neutron stars. If such compact objects are rotating with certain angular frequency, then they can efficiently emit gravitational radiation, provided their magnetic field and rotation axes are not aligned, and these gravitational waves can be detected by some of the upcoming detectors, e.g. LISA, BBO, DECIGO, Einstein Telescope etc. This will certainly be a direct detection of rotating magnetized white dwarfs as well as massive neutron stars., Updated version combining original paper (MNRAS 490, 2692-2705 (2019)) and corrections in erratum (MNRAS 491, 4396-4397 (2020))
- Published
- 2019
44. Impact of Schumann resonances on the Einstein Telescope and projections for the magnetic coupling function
- Author
-
Katarina Martinovic, Mairi Sakellariadou, Kamiel Janssens, Nelson Christensen, Patrick Meyers, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)
- Subjects
010308 nuclear & particles physics ,interferometer ,effect: magnetic ,Physics ,gravitational radiation: background ,family: 3 ,FOS: Physical sciences ,magnetic field ,General Relativity and Quantum Cosmology (gr-qc) ,noise: magnetic ,01 natural sciences ,gravitational radiation detector ,General Relativity and Quantum Cosmology ,detector: sensitivity ,VIRGO ,Einstein Telescope ,13. Climate action ,correlation ,0103 physical sciences ,site ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,LIGO ,coupling: magnetic ,010306 general physics - Abstract
Correlated magnetic noise in the form of Schumann resonances could introduce limitations to the gravitational-wave background searches of future Earth-based gravitational-wave detectors. We consider recorded magnetic activity at a candidate site for the Einstein Telescope, and forecast the necessary measures to ensure that magnetic contamination will not pose a threat to the science goals of this third-generation detector. In addition to global magnetic effects, we study local magnetic noise and the impact it might have on co-located interferometers. We express our results as upper limits on the coupling function of magnetic fields to the interferometer arms, implying that any larger values of magnetic coupling into the strain channel would lead to a reduction in the detectors' sensitivity. For gravitational-wave background searches below $\sim 30$ Hz it will be necessary for the Einstein Telescope magnetic isolation coupling to be two to four orders of magnitude better than that measured in the current Advanced LIGO and Virgo detectors., Comment: May 30th 2022 - New version contains updated figures in agreement with erratum: https://doi.org/10.1103/PhysRevD.105.109904
- Published
- 2021
45. Gravitational shine of dark domain walls
- Author
-
Babichev, E., Gorbunov, D., Ramazanov, S., Vikman, A., Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
- Subjects
defect ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,domain wall ,General Relativity and Quantum Cosmology (gr-qc) ,dark matter ,General Relativity and Quantum Cosmology ,topological ,spectrum ,Einstein Telescope ,High Energy Physics - Phenomenology (hep-ph) ,emission ,freeze-out ,plasma ,LISA ,formation ,gravitational radiation ,spontaneous symmetry breaking ,Astronomy and Astrophysics ,critical phenomena ,tension ,High Energy Physics - Phenomenology ,frequency ,[PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph] ,production ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Cosmic domain walls are harmless, provided that their tension decreases with expansion of the Universe. This setup can be realized, if the scale of spontaneous symmetry breaking is induced dynamically through the interaction with hot primordial plasma. In that case, the domain wall tension can attain large values in the early Universe without any conflict with observations. Owing to the large initial tension, these topological defects may serve as a powerful source of gravitational waves. We make a preliminary estimate of the gravitational wave spectrum and argue that it is distinct from the spectrum produced by other sources, in particular by domain walls of a constant tension. The resulting gravitational wave signal is in the range accessible by Einstein Telescope, DECIGO, TianQin, LISA, IPTA, or SKA, if the field constituting the domain walls is very feebly coupled with hot primordial plasma and has tiny self-interactions. In particular, one can consider this field for the role of Dark Matter. We discuss various Dark Matter production mechanisms and properties of the emitted gravitational waves associated with them. We find that the conventional freeze-out and freeze-in mechanisms lead to large and perhaps unobservable frequency of gravitational waves. However, the Dark Matter production is also possible at the second order phase transition leading to the domain wall formation or at the inverse phase transition, when the domain walls get dissolved eventually. In both cases, there is essentially no lower bound on the frequency of emitted gravitational waves., 38 pages, 5 figures; matches journal version
- Published
- 2021
46. Detectability of gravitational higher order modes in the third-generation era
- Author
-
Divyajyoti, Chandra Kant Mishra, K. G. Arun, and Preet Baxi
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,education.field_of_study ,Gravitational-wave observatory ,Einstein Telescope ,Gravitational wave ,Population ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics ,Mass ratio ,General Relativity and Quantum Cosmology ,Redshift ,LIGO ,Binary black hole ,Astrophysics - High Energy Astrophysical Phenomena ,education - Abstract
Detection of higher order modes of gravitational waves in third-generation (3G) ground-based detectors such as Cosmic Explorer and Einstein Telescope is explored. Using the astrophysical population of binary black holes based on events reported in the second gravitational wave catalog by Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo (GWTC-2), in conjunction with the Madau-Dickinson model for redshift evolution of the binary black hole mergers, we assess the detectability of these higher order modes using a network consisting of three third-generation detectors. We find that the two subleading modes [(3,3) and (4,4)] can be detected in approximately 30% of the population with a network signal-to-noise ratio of 3 or more, and for nearly 10% of the sources, the five leading modes will be detectable. Besides, a study concerning the effect of binary's mass ratio and its orbital inclination with the observer's line-of-sight in detecting various modes is presented. For a few selected events of the LIGO-Virgo catalog, we identify the modes that would have been detected if a third-generation detector was operational when these events were recorded. We also compute the detectability of higher modes by Voyager and find that only $\sim$ 6 and 2% of the detectable population will have an associated detection of (3,3) and (4,4) modes, respectively. Observing these higher order modes in the 3G era would have a huge impact on the science possible with these detectors ranging from astrophysics and cosmology to testing strong-field gravity.
- Published
- 2021
47. Probing modified gravitational wave propagation with strongly lensed coalescing binaries
- Author
-
Stefano Foffa, Francesco Iacovelli, Andreas Finke, Michele Mancarella, Michele Maggiore, Finke, A, Foffa, S, Iacovelli, F, Maggiore, M, and Mancarella, M
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Einstein Telescope ,Gravitational wave ,Detector ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,General Relativity and Quantum Cosmology ,Galaxy ,LIGO ,Third generation ,strong lensing ,Sensitivity (control systems) ,KAGRA ,dark energy ,gravitational wave ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
It has been recently shown that quadruply lensed gravitational-wave (GW) events due to coalescing binaries can be localized to one or just a few galaxies, even in the absence of an electromagnetic counterpart. We discuss how this can be used to extract information on modified GW propagation, which is a crucial signature of modifications of gravity at cosmological scales. We show that, using quadruply lensed systems, it is possible to constrain the parameter $\Xi_0$ that characterizes modified GW propagation, without the need of imposing a prior on $H_0$. A LIGO/Virgo/Kagra network at target sensitivity might already get a significant measurement of $\Xi_0$, while a third generation GW detector such as the Einstein Telescope could reach a very interesting accuracy., Comment: 11 pages, 5 figures
- Published
- 2021
48. UNDERGROUND GRAVITATIONAL WAVE OBSERVATORIES: KAGRA AND ET.
- Author
-
PUNTURO, MICHELE and KENTARO SOMIYA
- Subjects
- *
GRAVITATIONAL wave astronomy , *ASTRONOMICAL observatories , *BOSE-Einstein condensation , *TELESCOPES , *RELATIVISTIC electrons , *DARK matter - Published
- 2015
49. Seismic and Newtonian noise modeling for Advanced Virgo and Einstein Telescope
- Published
- 2021
50. Seismic and Newtonian noise modeling for Advanced Virgo and Einstein Telescope
- Published
- 2021
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