The Einstein Telescope: a third-generation gravitational wave observatory

Punturo, M.; Abernathy, M. R.; Acernese, F.; Allen, B.; Andersson, Nils; Arun, K. G.; Barone, F.; Barr, B.; Barsuglia, M.; Beker, M. G.; Beveridge, N.; Birindelli, S.; Bose, S.; Bosi, L.; Braccini, S.; Bradaschia, C.; Bulik, T.; Calloni, E.; Cella, G.; Mottin, Eric; Chelkowski, S.; Chincarini, A.; Clark, J. A.; Coccia, E.; Colacino, C. N.; Colas, J.; Cumming, A.; Cunningham, L.; Cuoco, E.; Danilishin, S. L.; Danzmann, K.; Luca, Gaetano De; Salvo, R. De; Dent, T.; Rosa, R. De; Fiore, L. Di; Virgilio, A. Di; Doets, M.; Fafone, V.; Falferi, P.; Flaminio, R.; Franc, J.; Frasconi, F.; Freise, A.; Fulda, P.; Gair, J. R.; Gemme, G.; Gennai, A.; Giazotto, A.; Glampedakis, Kostas; Granata, M.; Grote, H.; Guidi, G. M.; Hammond, G.; Hannam, M. D.; Harms, J.; Heinert, D.; Hendry, M.; Heng, I. S.; Hennes, E.; Hild, S.; Hough, J.; Husa, S.; Huttner, S. H.; Jones, Gareth; Khalili, F. Y.; Kokeyama, K.; Kokkotas, Kostas D.; Krishnan, B.; Lorenzini, M.; Lück, H.; Majorana, E.; Mandel, Ilya; Mandic, V.; Martin, I. W.; Michel, C.; Minenkov, Y.; Morgado, N.; Mosca, S.; Mours, B.; Müller‐Ebhardt, H.; Murray, P. G.; Nawrodt, R.; Nelson, J.; O’Shaughnessy, R.; Ott, Christian D.; Palomba, C.; Paoli, A.; Parguez, G.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Pinard, L.; Poggiani, R.; Popolizio, P.; Prato, Mirko; Puppo, P.; Rabeling, D. S.; Rapagnani, P.; Read, J.; Regimbau, T.; Rehbein, H.; Reid, S.; Rezzolla, Luciano; Ricci, F.; Richard, Frédéric; Rocchi, A.; Rowan, S.; Rüdiger, A.; Sassolas, B.; Sathyaprakash, B. S.; Schnabel, R.; Schwarz, Christian; Seidel, P.; Sintes, A. M.; Somiya, K.; Speirits, Fiona C.; Strain, K. A.; Strigin, S.; Sutton, P. J.; Tarabrin, S. P.; Thüring, A.; Brand, J. van den; Leewen, C. van; Veggel, Mariëlle van; Broeck, C. Van Den; Vecchio, A.; Veitch, J.; Vetrano, F.; Viceré, A.; Vyatchanin, S. P.; Willke, B.; Woan, G.; Wolfango, P.; Yamamoto, K.

doi:10.1088/0264-9381/27/19/194002

Cited by 1,603 publications

(1,297 citation statements)

References 38 publications

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“…In particular, if the radius of these stars as well as their masses can be inferred with precision and reliability, this will serve as a valuable input to nuclear physics theories (see [164,165,166] for a discussion of the current systematics-dominated estimates of radii, as well as of the good prospects for measuring radii using X-ray observations with the NASA mission NICER [167] and the planned European Space Agency (ESA) mission LOFT [168]). Plans are also being made for third-generation detectors such as the proposed Einstein Telescope [169], which would have 10-km underground arms and many other advances; this could reach ten times the sensitivity of Advanced LIGO and would thus greatly increase both the rates and precision of observations.…”

Section: Summary and Future Prospectsmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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Section: Summary and Future Prospectsmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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“…Regardless of which approach, either GBDs or PTAs, achieves a GW detection first, the two independent detections are necessary, because they target orthogonal classes of sources, therefore provid-ing complementary information about the Universe. The invaluable scientific promises of GW astronomy are potentially so revolutionary that the design of a third generation of GBDs -the Einstein telescope (ET)-is now being investigated (Punturo et al 2010), and the European Space Agency (ESA) has selected The Gravitational Universe science theme (eLISA Consortium 2013) for the L3 launch slot, with eLISA -the evolved laser interferometer space antenna-put forward as strawman mission design, now scheduled for 2034.…”

Section: Introductionmentioning

confidence: 99%

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Rosado

Sesana

Gair

2015

Monthly Notices of the Royal Astronomical Society

182

230

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In this paper we attempt to investigate the nature of the first gravitational wave (GW) signal to be detected by pulsar timing arrays (PTAs): will it be an individual, resolved supermassive black hole binary (SBHB), or a stochastic background made by the superposition of GWs produced by an ensemble of SBHBs? To address this issue, we analyse a broad set of simulations of the cosmological population of SBHBs, that cover the entire parameter space allowed by current electromagnetic observations in an unbiased way. For each simulation, we construct the expected GW signal and identify the loudest individual sources. We then employ appropriate detection statistics to evaluate the relative probability of detecting each type of source as a function of time for a variety of PTAs; we consider the current International PTA, and speculate into the era of the Square Kilometre Array. The main properties of the first detectable individual SBHBs are also investigated. Contrary to previous work, we cast our results in terms of the detection probability (DP), since the commonly adopted criterion based on a signal-to-noise ratio threshold is statistic-dependent and may result in misleading conclusions for the statistics adopted here. Our results confirm quantitatively that a stochastic signal is more likely to be detected first (with between 75 to 93 per cent probability, depending on the array), but the DP of single-sources is not negligible. Our framework is very flexible and can be easily extended to more realistic arrays and to signal models including environmental coupling and SBHB eccentricity.

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“…The Einstein Telescope (ET) is a European project aimed at directly detecting gravitational waves from astrophysical sources on a daily basis [1]. This detector is the planned successor of the Advanced LIGO and Advanced Virgo interferometers currently in their installation phase and early commissioning [2].…”

Section: Introductionmentioning

confidence: 99%

“…To greatly increase the detection rate in the following decade, the ET has been designed to be ten times more sensitive than the advanced detectors [1], probing a volume of space a thousand times larger. To achieve this goal, this observatory will be composed of two complementary interferometers sharing a common underground infrastructure.…”

Section: Introductionmentioning

confidence: 99%

Measurement of the optical absorption of bulk silicon at cryogenic temperature and the implication for the Einstein Telescope

Degallaix

Komma

Forest

et al. 2014

Class. Quantum Grav.

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We report in this article on the measurement of the optical absorption of moderately doped crystalline silicon samples at 1550 nm, which is a candidate material for the main optics of the low temperature interferometer of the Einstein Telescope (ET). We observe a nearly constant absorption from room temperature down to cryogenic temperatures for two silicon samples presenting an optical absorption of 0.029 cm −1 and 780 ppm cm −1 , both crystals doped with boron. This is in contradiction to what was assumed previously-a negligible optical absorption at low temperature due to the carrier freezeout. As the main consequence, if the silicon intrinsic absorption can not be lowered, the cross section of the mirror suspension of the ET must be increased to be able to carry away the excess heat generated by the partially absorbed laser beam during the operation of the interferometer.

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The Einstein Telescope: a third-generation gravitational wave observatory

Cited by 1,603 publications

References 38 publications

Implications of the gravitational wave event GW150914

Implications of the gravitational wave event GW150914

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Measurement of the optical absorption of bulk silicon at cryogenic temperature and the implication for the Einstein Telescope

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