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Advanced Virgo: a 2nd generation interferometric gravitational wave detector

F. Acernese, M. Agathos, K. Agatsuma, D. Aisa, N. Allemandou, A. Allocca, J. Amarni, P. Astone, G. Balestri, G. Ballardin, F. Barone, J. -P. Baronick, M. Barsuglia, A. Basti, F. Basti, Th. S. Bauer, V. Bavigadda, M. Bejger, M. G. Beker, C. Belczynski, D. Bersanetti, A. Bertolini, M. Bitossi, M. A. Bizouard, S. Bloemen, M. Blom, M. Boer, G. Bogaert, D. Bondi, F. Bondu, L. Bonelli, R. Bonnand, V. Boschi, L. Bosi, T. Bouedo, C. Bradaschia, M. Branchesi, T. Briant, A. Brillet, V. Brisson, T. Bulik, H. J. Bulten, D. Buskulic, C. Buy, G. Cagnoli, E. Calloni, C. Campeggi, B. Canuel, F. Carbognani, F. Cavalier, R. Cavalieri, G. Cella, E. Cesarini, E. Chassande-Mottin, A. Chincarini, A. Chiummo, S. Chua, F. Cleva, E. Coccia, P. -F. Cohadon, A. Colla, M. Colombini, A. Conte, J. -P. Coulon, E. Cuoco, A. Dalmaz, S. D'Antonio, V. Dattilo, M. Davier, R. Day, G. Debreczeni, J. Degallaix, S. Deléglise, W. Del Pozzo, H. Dereli, R. De Rosa, L. Di Fiore, A. Di Lieto, A. Di Virgilio, M. Doets, V. Dolique, M. Drago, M. Ducrot, G. Endrőczi, V. Fafone, S. Farinon, I. Ferrante, F. Ferrini, F. Fidecaro, I. Fiori, R. Flaminio, J. -D. Fournier, S. Franco, S. Frasca, F. Frasconi, L. Gammaitoni, F. Garufi, M. Gaspard, A. Gatto, G. Gemme, B. Gendre, E. Genin, A. Gennai, S. Ghosh, L. Giacobone, A. Giazotto, R. Gouaty, M. Granata, G. Greco, P. Groot, G. M. Guidi, J. Harms, A. Heidmann, H. Heitmann, P. Hello, G. Hemming, E. Hennes, D. Hofman, P. Jaranowski, R. J. G. Jonker, M. Kasprzack, F. Kéfélian, I. Kowalska, M. Kraan, A. Królak, A. Kutynia, C. Lazzaro, M. Leonardi, N. Leroy, N. Letendre, T. G. F. Li, B. Lieunard, M. Lorenzini, V. Loriette, G. Losurdo, C. Magazzù, E. Majorana, I. Maksimovic, V. Malvezzi, N. Man, V. Mangano, M. Mantovani, F. Marchesoni, F. Marion, J. Marque, F. Martelli, L. Martellini, A. Masserot, D. Meacher, J. Meidam, F. Mezzani, C. Michel, L. Milano, Y. Minenkov, A. Moggi, M. Mohan, M. Montani, N. Morgado, B. Mours, F. Mul, M. F. Nagy, I. Nardecchia, L. Naticchioni, G. Nelemans, I. Neri, M. Neri, F. Nocera, E. Pacaud, C. Palomba, F. Paoletti, A. Paoli, A. Pasqualetti, R. Passaquieti, D. Passuello, M. Perciballi, S. Petit, M. Pichot, F. Piergiovanni, G. Pillant, A Piluso, L. Pinard, R. Poggiani, M. Prijatelj, G. A. Prodi, M. Punturo, P. Puppo, D. S. Rabeling, I. Rácz, P. Rapagnani, M. Razzano, V. Re, T. Regimbau, F. Ricci, F. Robinet, A. Rocchi, L. Rolland, R. Romano, D. Rosińska, P. Ruggi, E. Saracco, B. Sassolas, F. Schimmel, D. Sentenac, V. Sequino, S. Shah, K. Siellez, N. Straniero, B. Swinkels, M. Tacca, M. Tonelli, F. Travasso, M. Turconi, G. Vajente, N. van Bakel, M. van Beuzekom, J. F. J. van den Brand, C. Van Den Broeck, M. V. van der Sluys, J. van Heijningen, M. Vasúth, G. Vedovato, J. Veitch, D. Verkindt, F. Vetrano, A. Viceré, J. -Y. Vinet, G. Visser, H. Vocca, R. Ward, M. Was, L. -W. Wei, M. Yvert, A. Zadrożny, J. -P. Zendri

TL;DR

Advanced Virgo describes a second-generation upgrade to the Virgo interferometer aimed at roughly 1000× larger surveyed volume and a three-orders-of-magnitude increase in GW detection rate. The design integrates dual recycling with signal recycling, larger beam sizes, higher finesse, and a high-power laser, complemented by advanced thermal compensation, monolithic suspensions, and enhanced seismic isolation. Key contributions include detailed optical design choices (arms, recycling cavities, and RoC), substrate/coating innovations, and a comprehensive infrastructure overhaul (vacuum, data acquisition, and control) to support SR operation and stable high-power performance. The work demonstrates a path toward a sensitive, robust detector within a global network, enabling early detections and opening a new era of GW astronomy.

Abstract

Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this paper we describe the main features of the Advanced Virgo detector and outline the status of the construction.

Advanced Virgo: a 2nd generation interferometric gravitational wave detector

TL;DR

Advanced Virgo describes a second-generation upgrade to the Virgo interferometer aimed at roughly 1000× larger surveyed volume and a three-orders-of-magnitude increase in GW detection rate. The design integrates dual recycling with signal recycling, larger beam sizes, higher finesse, and a high-power laser, complemented by advanced thermal compensation, monolithic suspensions, and enhanced seismic isolation. Key contributions include detailed optical design choices (arms, recycling cavities, and RoC), substrate/coating innovations, and a comprehensive infrastructure overhaul (vacuum, data acquisition, and control) to support SR operation and stable high-power performance. The work demonstrates a path toward a sensitive, robust detector within a global network, enabling early detections and opening a new era of GW astronomy.

Abstract

Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this paper we describe the main features of the Advanced Virgo detector and outline the status of the construction.

Paper Structure

This paper contains 82 sections, 29 figures.

Table of Contents

  1. Introduction: scope of the Advanced Virgo upgrade
  2. Interferometer optical configuration
  3. Increased laser power
  4. Mirrors
  5. Stray light control
  6. Payloads and vibration isolation
  7. General detector infrastructure
  8. Sensitivity goals
  9. Target sensitivity for AdV
  10. Further progress
  11. Timeline
  12. Optical design
  13. Design of the arm cavities
  14. Choice of the recycling cavities
  15. Mirror technology
  16. ...and 67 more sections

Figures (29)

  • Figure 1: AdV sensitivity for the three benchmark configurations as defined in the TDR: early operation (dash-dotted line), 25 W input power, no SR; mid-term operation, wideband tuning (dashed line), 125 W input power, tuned SR; late operation, optimized for BNS (black solid line), 125 W input power, detuned SR (0.35 rad). In the legend, the inspiral ranges for BNS and BBH (each BH of 30 $M_\odot$) in Mpc are reported. The best sensitivity obtained with Virgo+ is shown for comparison.
  • Figure 2: The AdV reference sensitivity (solid black) compared to an AdV noise budget (dashed black) using the new models for suspension thermal noise, gravity gradient noise and some modeled technical noises, computed in the configuration optimized for BNS detection with 125W of input laser power. See Section \ref{['sec:agencies']} for further details
  • Figure 3: Simplified optical layout of the Advanced Virgo interferometer. Each 3 km-long arm-cavity is formed by an Input Mirror (IM) and an End Mirror (EM). The recycling cavities at the center of the interferometer are 12 meters long and are formed by the Power Recycling Mirror (PRM), the Signal Recycling Mirror (SRM) and the two IM.
  • Figure 4: LEFT: Power Recycling substrate (35 cm in diameter, left) beside the large Beam Splitter of 55 cm. RIGHT: a test mass.
  • Figure 5: Planetary motion of the large substrates inside the coating chamber.
  • ...and 24 more figures