Plans for the Upgrade of the Gravitational Wave Detector Virgo: Advanced Virgo

Accadia, T.; Acernese, F.; Antonucci, F.; Astone, P.; Ballardin, G.; Barone, F.; Barsuglia, M.; Bauer, Th.; Beker, M. G.; Belĺetoile, A.; Birindelli, S.; Bitossi, M.; Bizouard, M. A.; Blom, M.; Bondu, F.; Bonelli, L.; Bonnand, R.; Boschi, V.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.; Budzyński, R.; Bulik, T.; Bulten, H.; Buskulic, D.; Buy, C.; Cagnoli, G.; Calloni, E.; Campagna, E.; Canuel, B.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande–Mottin, E.; Chincarini, A.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Corsi, A.; Coulon, J.‐P.; Cuoco, E.; D’Antonio, S.; Dattilo, V.; Davier, M.; Day, R.; Rosa, R. De; Debreczeni, G.; Prete, M. Del; Fiore, L. Di; Lieto, A. Di; Emilio, M. Di Paolo; Virgilio, A. Di; Dietz, A.; Drago, M.; Fafone, V.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Franc, J.; Frasca, S.; Frasconi, F.; Freise, A.; Galimberti, M.; Gammaitoni, L.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin, É.; Gennai, A.; Giazotto, A.; Gouaty, R.; Granata, M.; Greverie, C.; Guidi, G. M.; Hayau, J.-F.; Heitmann, H.; Hello, P.; Hild, S.; Huet, D.; Jaranowski, P.; Kowalska, I.; Królak, A.; Leroy, N.; Letendre, N.; Li, T. G F; Lorenzini, M.; Loriette, V.; Losurdo, G.; Majorana, E.; Maksimovic, I.; Man, N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Michel, Christoph M.; Milano, L.; Minenkov, Y.; Mohan, M.; Morgado, N.; Morgia, A.; Mosca, S.; Moscatelli, V.; Mours, B.; Neri, I.; Nocera, F.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Paoletti, F.; Pardi, S.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Persichetti, G.; Pichot, M.; Piergiovanni, F.; Piȩtka, M.; Pinard, L.; Poggiani, R.; Prato, Mirko; Prodi, G. A.; Punturo, M.; Puppo, P.; Rabeling, D. S.; Rácz, I.; Rapagnani, P.; Re, V.; Regimbau, T.; Ricci, F.; Robinet, F.; Rocchi, A.; Rolland, L.; Romano, R.; Gondek-Rosińska, D.; Ruggi, P.; Sassolas, B.; Sentenac, D.; Sperandio, L.; Sturani, R.; Swinkels, B. L.; Toncelli, A.; Tonelli, M.; Torre, O.; Tournefier, E.; Travasso, F.; Vajente, G.; Brand, J. F. J. van den; Putten, S. van der; Vasúth, M.; Vavoulidis, M.; Vedovato, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Ward, R. L.; Was, M.; Yvert, M.

doi:10.1142/9789814374552_0313

Cited by 9 publications

(12 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Detectors such as Advanced LIGO, VIRGO, GEO, and KAGRA aim for strain sensitivities approaching 10 −24 [1,2,3,4]. Nevertheless, signal candidates from compact binaries or supernovae will be on the cusp of detectability, with very poor signal to noise ratios requiring matched filtering for detection [5].…”

Section: What Is Characteristic Evolution and Why?mentioning

confidence: 99%

Spectral characteristic evolution: a new algorithm for gravitational wave propagation

Handmer

Szilágyi²

2014

Class. Quantum Grav.

View full text Add to dashboard Cite

Abstract. We present a spectral algorithm for solving the full nonlinear vacuum Einstein field equations in the Bondi framework. Developed within the Spectral Einstein Code (SpEC), we demonstrate spectral characteristic evolution as a technical precursor to Cauchy Characteristic Extraction (CCE), a rigorous method for obtaining gauge-invariant gravitational waveforms from existing and future astrophysical simulations. We demonstrate the new algorithm's stability, convergence, and agreement with existing evolution methods. We explain how an innovative spectral approach enables a two orders of magnitude improvement in computational efficiency. What is Characteristic Evolution, and why?As an international network of gravitational wave observatories come online, the race to the first direct detection of gravitational waves is expected to herald the beginning of gravitational wave astronomy. Detectors such as Advanced LIGO, VIRGO, GEO, and KAGRA aim for strain sensitivities approaching 10 −24 [1,2,3,4]. Nevertheless, signal candidates from compact binaries or supernovae will be on the cusp of detectability, with very poor signal to noise ratios requiring matched filtering for detection [5]. Matched filtering requires a comprehensive template bank, the generation of which has been a primary goal of the field of numerical relativity. These templates cover a range of expected astronomical phenomena, and are generated by a variety of numerical codes, including the Spectral Einstein Code (SpEC) [6]. Filling out the template bank requires a balance of numerical relativity and analytic waveforms and effective-one-body[8]), with waveform models often calibrated using numerical results [9,10,11].One technical challenge facing the construction of a large template bank is extraction of gauge invariant waveforms from simulations. In general, large computationally intensive simulations are needed to describe the physics of events such as supernovae and compact object binary inspirals. While a waveform-like signal can readily be extracted from arXiv:1406.7029v2 [gr-qc] 24 Sep 2014 anywhere in the computational domain, waveforms are only rigorously defined at future null infinity. Finite radii waveform approximations are universally contaminated by coordinate system dynamics, or gauge effects, which are poorly understood and nearly impossible to remove or even quantify. Comparison with Cauchy Characteristic Extraction, or CCE, an alternative which applies Characteristic Evolution to enable waveform computation at future null infinity, suggests that extrapolation gauge errors could dominate the global error [12]. Characteristic Evolution has been previously implemented at up to 4 th order radial accuracy [13], while complete extraction has been achieved with finite difference/volume methods up to 2 nd order [14,15]. Here we implement inner boundary extraction and evolution. This must be combined with an appropriate outer boundary algorithm to generate the gauge-invariant news at future null infinity. In a hypothetical complete ...

show abstract

Section: What Is Characteristic Evolution and Why?mentioning

confidence: 99%

Spectral characteristic evolution: a new algorithm for gravitational wave propagation

Handmer

Szilágyi²

2014

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…Gravitational waves (GWs) promise a new and exciting window to the cosmos. Two ground-based interferometer experiments, LIGO and VIRGO, are about to restart operations with greatly increased sensitivity [1,2], and will be joined in a few years by KAGRA [3]. Once working at their design sensitivity, they are expected to quickly detect gravitational wave signals from binary neutron stars [4].…”

Section: Introductionmentioning

confidence: 99%

“…A range of phenomena, such as inflation, topological defects and phase transitions may lead to observable gravitational wave signals across a wide range of frequencies (for a review see [5]). There are a number of proposals to realise a gravitational wave detector in space, in the first place eLISA [6], which is scheduled for launch in 2034. Space-based detectors have much longer arm lengths than ground based ones, and have maximum sensitivity in a frequency range which is relevant for a first order phase transition at the electroweak scale.…”

Section: Introductionmentioning

confidence: 99%

Numerical simulations of acoustically generated gravitational waves at a first order phase transition

et al. 2015

View full text Add to dashboard Cite

We present details of numerical simulations of the gravitational radiation produced by a first order thermal phase transition in the early Universe. We confirm that the dominant source of gravitational waves is sound waves generated by the expanding bubbles of the low-temperature phase. We demonstrate that the sound waves have a power spectrum with a power-law form between the scales set by the average bubble separation (which sets the length scale of the fluid flow L f ) and the bubble wall width. The sound waves generate gravitational waves whose power spectrum also has a power-law form, at a rate proportional to L f and the square of the fluid kinetic energy density. We identify a dimensionless parameterΩ GW characterizing the efficiency of this "acoustic" gravitational wave production whose value is 8πΩ GW ≃ 0.8 AE 0.1 across all our simulations. We compare the acoustic gravitational waves with the standard prediction from the envelope approximation. Not only is the power spectrum steeper (apart from an initial transient) but the gravitational wave energy density is generically larger by the ratio of the Hubble time to the phase transition duration, which can be 2 orders of magnitude or more in a typical first order electroweak phase transition.

show abstract

“…When aLIGO reaches design sensitivity, it will be sensitive to a volume of the universe 1000 times greater than the first-generation LIGO detectors [2]. The French-Italian Advanced Virgo (AdV) detector will begin observations shortly after aLIGO, forming a worldwide network of gravitational-wave observatories [1,3,4]. One of the most interesting sources for aLIGO and AdV is the inspiral and merger of neutron-star-black-hole (NSBH) binaries.…”

Section: Introductionmentioning

confidence: 99%

Investigating the effect of precession on searches for neutron-star–black-hole binaries with Advanced LIGO

et al. 2014

View full text Add to dashboard Cite

The first direct detection of neutron-star-black-hole binaries will likely be made with gravitational-wave observatories. Advanced LIGO and Advanced Virgo will be able to observe neutron-star-black-hole mergers at a maximum distance of 900 Mpc. To achieve this sensitivity, gravitational-wave searches will rely on using a bank of filter waveforms that accurately model the expected gravitational-wave signal. The emitted signal will depend on the masses of the black hole and the neutron star and also the angular momentum of both components. The angular momentum of the black hole is expected to be comparable to the orbital angular momentum when the system is emitting gravitational waves in Advanced LIGO's and Advanced Virgo's sensitive band. This angular momentum will affect the dynamics of the inspiralling system and alter the phase evolution of the emitted gravitational-wave signal. In addition, if the black hole's angular momentum is not aligned with the orbital angular momentum, it will cause the orbital plane of the system to precess. In this work we demonstrate that if the effect of the black hole's angular momentum is neglected in the waveform models used in gravitational-wave searches, the detection rate of ð10 þ 1.4ÞM ⊙ neutronstar-black-hole systems with isotropic spin distributions would be reduced by 33%-37% in comparison to a hypothetical perfect search at a fixed signal-to-noise ratio threshold. The error in this measurement is due to uncertainty in the post-Newtonian approximations that are used to model the gravitational-wave signal of neutron-star-black-hole inspiralling binaries. We describe a new method for creating a bank of filter waveforms where the black hole has nonzero angular momentum that is aligned with the orbital angular momentum. With this bank we find that the detection rate of ð10 þ 1.4ÞM ⊙ neutron-star-black-hole systems would be reduced by 26%-33%. Systems that will not be detected are ones where the precession of the orbital plane causes the gravitational-wave signal to match poorly with nonprecessing filter waveforms. We identify the regions of parameter space where such systems occur and suggest methods for searching for highly precessing neutron-star-black-hole binaries.

show abstract

Plans for the Upgrade of the Gravitational Wave Detector Virgo: Advanced Virgo

Cited by 9 publications

References 0 publications

Spectral characteristic evolution: a new algorithm for gravitational wave propagation

Spectral characteristic evolution: a new algorithm for gravitational wave propagation

Numerical simulations of acoustically generated gravitational waves at a first order phase transition

Investigating the effect of precession on searches for neutron-star–black-hole binaries with Advanced LIGO

Contact Info

Product

Resources

About