Status of the Virgo project
By T. Accadia, F. Acernese, F. Antonucci, P. Astone, G. Ballardin, F. Barone, M. Barsuglia, A. Basti, T. Bauer, M. Bebronne and 173 more. 2011
174 citations recorded by the source corpus.
We describe the present state and future evolution of the Virgo gravitational wave detector, realized by the Virgo Collaboration at the European Gravitational Observatory, in Cascina near Pisa in Italy. We summarize basic principles of the operation and the design features of the Virgo detector. We present the sensitivity evolution due to a series of intermediate upgrades called Virgo+ which is being completed this year and includes new monolithic suspensions. We describe the present scientific potential of the detector. Finally we discuss the plans for the second generation of the detector, called Advanced Virgo, introducing its new features, the expected sensitivity evolution and the scientific potential.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics
View Paper: https://www.semanticscholar.org/paper/1e143bcdce70ccd22c8cd70f2b7ed5772bcef09d
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Citations in the corpus
- Short-Duration Gamma-Ray Bursts (2013, background): “Third, the mergers will be accompanied by strong gravitational wave emission, detectable with the Advanced Short-Duration Gamma-Ray Bursts11 LIGO/Virgo detectors to about 200 Mpc for NS-NS mergers (Abramovici et al. 1992, Harry & LIGO Scientific Collaboration 2010, Accadia et al. 2011).”
- IDENTIFYING ELUSIVE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE MERGERS: AN END-TO-END SIMULATION (2012, background): “…GW interferometers — LIGO in the US and possibly India (Barish & Weiss 1999; Sigg & the LIGO Scientific Collaboration 2008; Sathyaprakash & et al. 2012), Virgo in Italy (Accadia et al. 2011), KAGRA in Japan (Somiya 2012) — will become operational within the frequency range of 10 Hz to a few kHz.”
- The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes (2014, background): “. Gravitational Waves The era of direct gravitational wave detections is expected to commence in a few years, when second-generation ground-based detectors such as Advanced LIGO [360], Advanced Virgo [361], KAGRA [362], and LIGO-India 49 Object (by RA) Disk Reflection Disk Continuum References M33 X-”
- Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, unknown): “The merger of binary neutron stars is one of the most promising gravitational-wave sources for ground-based detectors such as advanced LIGO(Abadie et al. 2010), advanced VIRGO(Accadia et al. 2011), and KAGRA(Kuroda & LCGT Collaboration 2010).”
- RADIATIVE TRANSFER SIMULATIONS OF NEUTRON STAR MERGER EJECTA (2013, methodology): “Next generation GW detectors, such as advanced LIGO, advanced VIRGO, and KAGRA (Abadie et al. 2010b; Kuroda & LCGT Collaboration 2010; Accadia et al. 2011; LIGO Scientific Collaboration et al. 2013), are expected to detect GWs from NS mergers at distances up to within about 200 Mpc. Statistical…”
- Dark matter and fundamental physics with the Cherenkov Telescope Array (2012, background): “ detection of the first gravitationalwave (GW) by ground-basedinterferometers, now in the “advanced sensitivity” design ph ase. The 3km–scale Michelson interferometers Enhanced LIGO and Advanced Virgo [205] are increasing their sensitivity and extending the horizon distance of detectable sources up t”
- The long-term evolution of neutron star merger remnants { II. Radioactively powered transients (2013, background): “…& Georgieva 2013; Rosswog, Piran & Nakar 2013; Piran, Nakar & Rosswog 2013) By the end of this decade the second generation of ground- based GW detectors is expected to be running at their intended design sensitivities (Harry & LIGO Scientific Collaboration 2010; Accadia et al. 2011; Somiya 2012).”