Scientific objectives of Einstein Telescope

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

doi:10.1088/0264-9381/29/12/124013

Cited by 501 publications

(422 citation statements)

References 84 publications

Supporting

Mentioning

417

Contrasting

Unclassified

Order By: Relevance

“…Future work will also consider next generation detectors such as the proposed Einstein Telescope [93], which can reach much greater sensitivities and would therefore probe the binary formation and merger history into higher redshifts, enabling tests of more extensive models than considered here. Finally, the more exotic example discussed above, of primordial black holes, provides a proof-of-concept that GW measurements can be used to derive constraints on the primordial spectrum of fluctuations which is imprinted onto the early Universe over cosmological scales by cosmological inflation [94,95].…”

Section: Discussionmentioning

confidence: 99%

Black hole mass function from gravitational wave measurements

et al. 2017

View full text Add to dashboard Cite

We examine how future gravitational-wave measurements from merging black holes (BHs) can be used to infer the shape of the black-hole mass function, with important implications for the study of star formation and evolution and the properties of binary BHs. We model the mass function as a power law, inherited from the stellar initial mass function, and introduce lower and upper mass cutoff parameterizations in order to probe the minimum and maximum BH masses allowed by stellar evolution, respectively. We initially focus on the heavier BH in each binary, to minimize model dependence. Taking into account the experimental noise, the mass measurement errors and the uncertainty in the redshift-dependence of the merger rate, we show that the mass function parameters, as well as the total rate of merger events, can be measured to < 10% accuracy within a few years of advanced LIGO observations at its design sensitivity. This can be used to address important open questions such as the upper limit on the stellar mass which allows for BH formation and to confirm or refute the currently observed mass gap between neutron stars and BHs. In order to glean information on the progenitors of the merging BH binaries, we then advocate the study of the two-dimensional mass distribution to constrain parameters that describe the two-body system, such as the mass ratio between the two BHs, in addition to the merger rate and mass function parameters. We argue that several years of data collection can efficiently probe models of binary formation, and show, as an example, that the hypothesis that some gravitational-wave events may involve primordial black holes can be tested. Finally, we point out that in order to maximize the constraining power of the data, it may be worthwhile to lower the signal-to-noise threshold imposed on each candidate event and amass a larger statistical ensemble of BH mergers.

show abstract

Section: Discussionmentioning

confidence: 99%

Black hole mass function from gravitational wave measurements

et al. 2017

View full text Add to dashboard Cite

show abstract

“…Taking the fact that the expected rise time of ejecta memory is much shorter than the inverse of frequency at which ground-based detectors are most sensitive, (∼ 100 Hz) −1 , it may be possible to detect ejecta memory by the Einstein Telescope [30] if the ejecta is as massive as 0.1M ⊙ .…”

Section: B Gravitational-wave Memorymentioning

confidence: 99%

Anisotropic mass ejection from black hole-neutron star binaries: Diversity of electromagnetic counterparts

Kyutoku

Ioka²,

Shibata³

2013

Phys. Rev. D

149

178

View full text Add to dashboard Cite

The merger of black hole-neutron star binaries can eject substantial material with the mass ∼ 0.01-0.1M⊙ when the neutron star is disrupted prior to the merger. The ejecta shows significant anisotropy, and travels in a particular direction with the bulk velocity ∼ 0.2c. This is drastically different from the binary neutron star merger, for which ejecta is nearly isotropic. Anisotropic ejecta brings electromagnetic-counterpart diversity which is unique to black hole-neutron star binaries, such as viewing-angle dependence, polarization, and proper motion. The kick velocity of the black hole, gravitational-wave memory emission, and cosmic-ray acceleration are also discussed.

show abstract

“…3, right panel), when the source and the observer are in the symmetry axis, d ¼ 0 and we have Á ¼ 0 according to Eq. (35). Then, Eq.…”

Section: B Source and Observer In The Symmetry Axismentioning

confidence: 99%

Rotating black holes in a Randall-Sundrum brane with a cosmological constant

Neves

Molina

2012

Phys. Rev. D

View full text Add to dashboard Cite

In this work we have constructed axially symmetric vacuum solutions of the gravitational field equations in a Randall-Sundrum brane. A non-null effective cosmological constant is considered, and asymptotically de Sitter and anti-de Sitter spacetimes are obtained. The solutions describe rotating black holes in a four-dimensional brane. Optical features of the solutions are treated, emphasizing the rotation of the polarization vector along null congruences.

show abstract

Scientific objectives of Einstein Telescope

Cited by 501 publications

References 84 publications

Black hole mass function from gravitational wave measurements

Black hole mass function from gravitational wave measurements

Anisotropic mass ejection from black hole-neutron star binaries: Diversity of electromagnetic counterparts

Rotating black holes in a Randall-Sundrum brane with a cosmological constant

Contact Info

Product

Resources

About