Scientific objectives of Einstein Telescope

Year: 2012

Authors: Sathyaprakash B.; Abernathy M.; Acernese F.; Ajith P.; Allen B.; Amaro-Seoane P.; Andersson N.; Aoudia S., Arun K.; Astone P., Krishnan B.; Barack L.; Barone F.; Barr B.; Barsuglia M.; Bassan M.; Bssiri R.; Beker M.; Beveridge N.; Bizouard M.; Bond C.; Bose S.; Bosi L.; Braccini S.; Bradaschia C.; Britzger M.; Brueckner F.; Bulik T.; Bulten H.J.; Burmeister O.; Calloni E.; Campsie P.; Carbone L.; Cella G.; Chalkley E.; Chassandre-Mottin E.; Chelkowski S.; Chincarini A.; Di Cintio A.; Clark J.; Coccia E.; Colacino C.; Colas J.; Colla A.; Corsi A.; Cumming A.; Cunningham L.; Cuoco E.; Danilishin S.; Danzmann K.; Daw E.; De Salvo R.; Del Pozzo W.; Dent T.; De Rosa R.; Di Fiore L.; Di Paolo Emilio M.; Di Virgilio A.; Dietz A.; Doets M.; Dueck J.; Edwards M.; Fafone V.; Fairhurst S.; Falferi P.; Favata M.; Ferrari V.; Ferrini F., Fidecaro F.; Flaminio R.; Franc J.; Frasconi F.; Freise A.; Friedrich D.; Fulda P.; Gair J.; Galimberti M.; Gemme G.; Genin E.; Gennai A.; Giazotto A.; Glampedakis K.; Gossan S.; Gouaty R.; Graef C.; Graham W.; Granata M.; Grote H.; Guidi G.; Hallam J.; Hammond G.; Hannam M.; Harms J.; Haughian K.; Hawke I.; Heinert D.; Hendry M.; Heng I.; Hennes E.; Hild S.; Hough J.; Huet D.; Husa S.; Huttner S.; Iyer B.; Jones D.I.; Jones G.; Kamaretsos I.; Kant Mishra C.; Kawazoe F.; Khalili F.; Kley B.; Kokeyama K.; Kokkotas K.; Kroker S.; Kumar R.; Kuroda K.; Lagrange B.; Lastzka N.; Li T.G.F.; Lorenzini M.; Losurdo G.; Luck H.; Majorana E.; Malvezzi V.; Mandel I.; Mandic V.; Marka S.; Marin F.; Marion F.; Marque J.; Martin I.; Mc Leod D.; Mckechan D.; Mehmet M.; Michel C.; Minenkov Y.; Morgado N.; Morgia A.; Mosca S.; Moscatelli L.; Mours B.; Muller-Ebhardt H.; Murray P.; Naticchioni L.; Nawrodt R.; Nelson J.; O’Shaughnessy R.; Ott C. D.; Palomba C.; Paoli A.; Parguez G.; Pasqualetti A.; Passaquieti R.; Passuello D.; Perciballi M.; Piergiovanni F.; Pinard L.; Pitkin M.; Plastino W.; Poggiani R.; Popolizio P.; Porter E.; Prato M.; Prodi G.; Punturo M.; Puppo P.; Rabeling D.; Rapagnani P.; Racz I.; Re V.; Read J.; Regimbau T.; Rehbein H.; Reid S.; Ricci F.; Richard F.; Robinson C.; Rocchi A.; Romano E.; Rowan S.; Ruediger A.; Samblowski A.; Santamaria L.; Sassolas B.; Schmidt P.; Schnabel R.; Schutz B.; Schwarz C.; Scott J.; Seidel P.; Sintes A.; Somiya K.; Sopuerta C. F.; Sorazu B.; Speirits F.; Storchi L.; Strain K.; Strigin S.; Sutton P.; Tarabrin S.; Taylor B.; Thurin A.; Tokmakov K.; Tonelli M.; Tournefier H.; Vaccarone R.; Vahlbruch H.; van den Brand J.; van den Broeck C.; van den Putten S.; van Veggel M.; Vecchio A.; Veitch J.; Vetrano F.; Vicere A.; Vyatchanin S.; Wessels P.; Willke B.; Winkler W.; Woan G.; Woodcraft A.; Yamamoto K.

Autors Affiliation: Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales; Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland; Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy; Univ Salerno, I-84084 Salerno, Italy; Caltech CaRT, Pasadena, CA 91125 USA; Leibniz Univ Hannover, D-30167 Hannover, Germany; Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany; Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany; Inst Ciencies Espai, ES-08193 Barcelona, Spain; Univ Southampton, Southampton SO17 1BJ, Hants, England; Chennai Math Inst, Siruseri 603103, India; Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy; Univ Roma La Sapienza, I-00185 Rome, Italy; Univ Paris Diderot, CNRS IN2P3, CEA DSM IRFU, Lab AstroParticule & Cosmol APC,Observ Paris, F-75013 Paris, France; Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy; Univ Roma Tor Vergata, I-00133 Rome, Italy; Nikhef, Amsterdam, Netherlands; Univ Paris 11, LAL, CNRS, IN2P3, F-91898 Orsay, France; Univ Birmingham, Birmingham B15 2TT, W Midlands, England; Washington State Univ, Pullman, WA 99164 USA; Ist Nazl Fis Nucl, Sez Perugia, Milan, Italy; Ist Nazl Fis Nucl, Sez Pisa, Milan, Italy; EGO, I-56021 Cascina, Pi, Italy; Friedrich Schiller Univ Jena PF 07737 Jena, Jena, Germany; Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland; Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands; Univ Naples Federico II, I-80126 Naples, Italy; Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy; Moscow MV Lomonosov State Univ, Moscow 119992, Russia; Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England; Univ Sannio, Benevento, Italy; Univ Savoie, CNRS, IN2P3, LAPP, F-74941 Annecy Le Vieux, France; Fdn Bruno Kessler, CNR, Ist Foton & Nanotecnol, I-38123 Povo, Trento, Italy; Ist Nazl Fis Nucl, Grp Collegato Trento, Milan, Italy; Univ Pisa, Dipartimento Fis, Pisa, Italy; Univ Lyon 1, CNRS, IN2P3, LMA, F-69622 Villeurbanne, Lyon, France; Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England; Univ Tubingen, Theoret Astrophys TAT, D-72076 Tubingen, Germany; Ist Nazl Fis Nucl, Sez Firenze, I-50019 Sesto Fiorentino, Italy; Univ Urbino Carlo Bo, I-61029 Urbino, Italy; Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain; Raman Res Inst, Bangalore 560080, Karnataka, India; Moscow MV Lomonosov State Univ, Moscow 119992, Russia; Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan; MIT Kavli Inst, Cambridge, MA 02139 USA; Univ Minnesota, Minneapolis, MN 55455 USA; Columbia Univ, Dept Phys, New York, NY 10027 USA; Penn State Univ, University Pk, PA 16802 USA; Ist Nazl Fis Nucl, Sez Roma Tre, I-00146 Rome, Italy; Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy; Univ Trento, Trento, Italy; KFKI Res Inst Particle & Nucl Phys, Budapest, Hungary; Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA; Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, F-06304 Nice, France; CALTECH, LIGO, Pasadena, CA 91125 USA; Tokyo Inst Technol, Dept Phys, Tokyo 152, Japan; CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain; Laser Zentrum Hannover eV, D-30419 Hannover, Germany; Royal Observ, Greenwich SE10 8XJ, England; Ist Nazl Fis Nucl, Sez Padova, Milan, Italy

Abstract: The advanced interferometer network will herald a new era in observational astronomy. There is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from 1 Hz to 10 kHz, with sensitivity a factor 10 better in amplitude. Such detectors will be able to probe a range of topics in nuclear physics, astronomy, cosmology and fundamental physics, providing insights into many unsolved problems in these areas.

Journal/Review: CLASSICAL AND QUANTUM GRAVITY

Volume: 29 (12)      Pages from: 124013  to: 124013

More Information: This work was supported by the European Commission under the Framework Programme 7 (FP7) \’Capacities\’, project Einstein Telescope (ET) design study (Grant Agreement 211743), http://www.et-gw.eu/. We thank Drs Asad Ali and Evan Ochsner for comments.
KeyWords: gravitational waves; ET Telescope; gravitational waves observations; gamma-ray bursts; black-hole
DOI: 10.1088/0264-9381/29/12/124013

Citations: 304
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