Concepts and research for future detectors

Acernese, F.; Barone, F.; Bell, A. S.; Bergmann, G.; Blair, D. G.; Born, M.; Brown, D. D.; Chen, X.; Danilishin, S. L.; Degallaix, J.; Denker, T.; Virgilio, A. Di; Frajuca, Carlos; Friedrich, Daniel; Fulda, P.; Grote, H.; Huttner, S. H.; Kato, J.; Köhlenbeck, S.; Leavey, S.; Lück, H.; Nakano, Masayuki; Palmer, Rebecca; Punturo, M.; Raffai, P.; Schutte, Dirk; Simakov, D.; Slagmolen, B. J. J.; Somiya, K.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Wade, A. R.; Wang, M.; Westphal, T.; Zhao, C.; Adhikari, R. X.; Adier, M.; Agatsuma, K.; Barr, B.; Bassiri, R.; Bauchrowitz, J.; Blair, C. D.; Bond, C.; Bongs, Kai; Bortoli, F. S.; Cagnoli, G.; Calia, P.; Canonico, Rosangela; Carbone, L.; Chua, S.; Coccia, E.; Cripe, J.; Cunningham, L.; Danzmann, K.; Rosa, R. De; Fafone, V.; Fejer, M. M.; Flaminio, R.; Fontaine, J. P.; Forest, Danièle; Freise, A.; Furusawa, Akira; Garufi, F.; Giordano, G.; Gondán, L.; Gordon, Neil; Goßler, S.; Gräf, Christian; Granata, M.; Hammerer, Klemens; Heng, I. S.; Heurs, M.; Hild, S.; Hirobayashi, Shigeki; Hough, J.; Li, Ju; Kaufer, H.; Kawamura, Hiroshi; Kawamura, Seiji; Kelecsényi, Nándor; Khalaidovski, A.; Khalili, F. Y.; Kuroda, K.; Loddo, Gianraffaele; Logue, J.; Ma, Y.; Macarthur, J.; Magalhães, Nadja S.; Majorana, E.; Malvezzi, V.; Márka, S.; Márka, Z.; Martin, I. W.; McClelland, D. E.; Meinders, M.; Michel, C.; Miller, John M.; Morgado, N.; Müller‐Ebhardt, H.; Naticchioni, L.; Nguyen, T. T.; Perciballi, M.; Pinard, L.; Puppo, P.; Rapagnani, P.; Ricci, F.; Risson, P.; Rocchi, A.; Rocco, Emanuele; Romano, R.; Route, R.; Rowan, S.; Sakata, S.; Schnabel, R.; Shaddock, D. A.; Sorazu, B.; Stefszky, Michael; Steinmeyer, D.; Strain, K. A.; Voronchev, N. V.; Ward, R. L.; Wimmer, M. H.

doi:10.1007/s10714-014-1700-8

Cited by 2 publications

(3 citation statements)

References 40 publications

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“…Recent work [10] has shown that the room temperature bulk optical absorption at 1550 nm of some commercially available material is at a level suitable for its use as a mirror substrate in a GW detector, and further investigations [11] indicate that the cryogenic absorption is similar. Operating at cryogenic temperatures requires control of heat input to the test mass, to keep the mass at the operating temperature.…”

Section: Introductionmentioning

confidence: 99%

“…Intrinsically, the optical absorption in pure silicon above 1450 nm is negligible (<10 −8 cm −1 ) [9], but impurities can cause absorption directly, or by providing additional free carriers within the material. Recent work [10] has shown that the room temperature bulk optical absorption at 1550 nm of some commercially available material is at a level suitable for its use as a mirror substrate in a GW detector, and further investigations [11] indicate that the cryogenic absorption is similar. Operating at cryogenic temperatures requires control of heat input to the test mass, to keep the mass at the operating temperature.…”

Section: Introductionmentioning

confidence: 99%

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Anomalous optical surface absorption in nominally pure silicon samples at 1550 nm

Bell

Steinlechner

Martin

et al. 2017

Class. Quantum Grav.

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The announcement of the direct detection of gravitational waves (GW) by the LIGO and Virgo collaboration in February 2016 has removed any uncertainty around the possibility of GW astronomy. It has demonstrated that future detectors with sensitivities ten times greater than the Advanced LIGO detectors would see thousands of events per year. Many proposals for such future interferometric GW detectors assume the use of silicon test masses. Silicon has low mechanical loss at low temperatures, which leads to low displacement noise for a suspended interferometer mirror. In addition to the low mechanical loss, it is a requirement that the test masses have a low optical loss. Measurements at 1550 nm have indicated that material with a low enough bulk absorption is available; however there have been suggestions that this low absorption material has a surface absorption of >100 ppm which could preclude its use in future cryogenic detectors. We show in this paper that this surface loss is not intrinsic but is likely to be a result of particular polishing techniques and can be removed or avoided by the correct polishing procedure. This is an important step towards high gravitational wave detection rates in silicon based instruments.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Anomalous optical surface absorption in nominally pure silicon samples at 1550 nm

Bell

Steinlechner

Martin

et al. 2017

Class. Quantum Grav.

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“…In this article, we investigate a novel approach for the earthbound detection of GWs at frequencies around 0.1-10 Hz by utilizing repeatedly free falling test masses [22,23]. By overcoming limits that are related with seismic attenuation and suspension thermal noise, we aim to complement advanced detectors at their lower frequency range.…”

Section: Introductionmentioning

confidence: 99%

Juggled interferometer for the detection of gravitational waves around 0.1–10 Hz

Friedrich

Nakano

Kawamura

et al. 2014

Class. Quantum Grav.

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We propose a novel type of earthbound gravitational wave detector targeting a frequency band of 0.1–10 Hz. By using repeatedly free falling test masses—juggling—one can in principle decouple test masses from the seismically noisy environment and avoid suspension thermal noise in a straightforward manner. As a consequence, the measurement process will not be continuous anymore. We show that to a given extent, continuous signals can be extracted from the discontinuous data by removing a linear trend for the data as well as for the filter templates in each measurement cycle. Moreover, using a laser interferometer topology in principle allows for scaling to a long-baseline detector to achieve scientifically significant strain sensitivities and to be complementary to advanced detectors that are optimized for a frequency band of 10–104 Hz. The presented Michelson type juggled interferometer offers a variety of interesting technical as well as theoretical challenges during the development to an instrument for new astronomy.

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Concepts and research for future detectors

Abstract: Technologies, design aspects and recent progresses for future gravitational wave (GW) detectors are mentioned in this summary of the C4 session of the Amaldi 10 conferenc

Cited by 2 publications

References 40 publications

Anomalous optical surface absorption in nominally pure silicon samples at 1550 nm

Anomalous optical surface absorption in nominally pure silicon samples at 1550 nm

Juggled interferometer for the detection of gravitational waves around 0.1–10 Hz

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