The Experts below are selected from a list of 33486 Experts worldwide ranked by ideXlab platform
Takashi Nakamura - One of the best experts on this subject based on the ideXlab platform.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with h(rms) approximately 10(-27) at f approximately 0.1 Hz in this century. Using this antenna, (1) typically 10(5) chirp signals of coalescing binary neutron stars per year may be detected with S/N approximately 10(4); (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of Omega(GW) > or similar to 10(-20) predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with ${h}_{\mathrm{rms}}\ensuremath{\sim}{10}^{\ensuremath{-}27}$ at $f\ensuremath{\sim}0.1\mathrm{Hz}$ in this century. Using this antenna, (1) typically ${10}^{5}$ chirp signals of coalescing binary neutron stars per year may be detected with $\mathrm{S}/\mathrm{N}\ensuremath{\sim}{10}^{4}$; (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of ${\ensuremath{\Omega}}_{\mathrm{GW}}\ensuremath{\gtrsim}{10}^{\ensuremath{-}20}$ predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
Naoki Seto - One of the best experts on this subject based on the ideXlab platform.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with h(rms) approximately 10(-27) at f approximately 0.1 Hz in this century. Using this antenna, (1) typically 10(5) chirp signals of coalescing binary neutron stars per year may be detected with S/N approximately 10(4); (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of Omega(GW) > or similar to 10(-20) predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with ${h}_{\mathrm{rms}}\ensuremath{\sim}{10}^{\ensuremath{-}27}$ at $f\ensuremath{\sim}0.1\mathrm{Hz}$ in this century. Using this antenna, (1) typically ${10}^{5}$ chirp signals of coalescing binary neutron stars per year may be detected with $\mathrm{S}/\mathrm{N}\ensuremath{\sim}{10}^{4}$; (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of ${\ensuremath{\Omega}}_{\mathrm{GW}}\ensuremath{\gtrsim}{10}^{\ensuremath{-}20}$ predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
S Kawamura - One of the best experts on this subject based on the ideXlab platform.
-
displacement measuring technique for satellite to satellite Laser Interferometer to determine earth s gravity field
Measurement Science and Technology, 2004Co-Authors: Shigeo Nagano, S Kawamura, T Yoshino, Hiroo Kunimori, Mizuhiko Hosokawa, Takashi Sato, Masashi OhkawaAbstract:We present a new displacement measuring technique with simplicity, robustness, high sensitivity and wide measurement range. A set of a frequency shifter and a voltage–frequency converter is used to lock a homodyne Interferometer on the half-bright fringe by eliminating the Doppler fringe resulting from mirror motion. The mirror displacement is directly retrieved from the feedback signal of a fringe control loop. By developing a table-top Interferometer, we successfully demonstrated signal recovery without significant degradation. The achieved displacement sensitivity and measurement range of the Interferometer were 24 nm Hz−1/2 and 1.3 mm at a Fourier frequency of 0.1 Hz, respectively. This technique was found to have a potential for application to precise displacement measurements. It is, in particular, suitable for a satellite-to-satellite Laser Interferometer to determine Earth's gravity field.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with h(rms) approximately 10(-27) at f approximately 0.1 Hz in this century. Using this antenna, (1) typically 10(5) chirp signals of coalescing binary neutron stars per year may be detected with S/N approximately 10(4); (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of Omega(GW) > or similar to 10(-20) predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
-
possibility of direct measurement of the acceleration of the universe using 0 1 hz band Laser Interferometer gravitational wave antenna in space
Physical Review Letters, 2001Co-Authors: Naoki Seto, S Kawamura, Takashi NakamuraAbstract:It may be possible to construct a Laser Interferometer gravitational wave antenna in space with ${h}_{\mathrm{rms}}\ensuremath{\sim}{10}^{\ensuremath{-}27}$ at $f\ensuremath{\sim}0.1\mathrm{Hz}$ in this century. Using this antenna, (1) typically ${10}^{5}$ chirp signals of coalescing binary neutron stars per year may be detected with $\mathrm{S}/\mathrm{N}\ensuremath{\sim}{10}^{4}$; (2) we can directly measure the acceleration of the universe by a 10 yr observation of binary neutron stars; and (3) the stochastic gravitational waves of ${\ensuremath{\Omega}}_{\mathrm{GW}}\ensuremath{\gtrsim}{10}^{\ensuremath{-}20}$ predicted by the inflation may be detected by correlation analysis. Our formula for phase shift due to accelerating motion might be applied for binary sources of LISA.
-
ligo the Laser Interferometer gravitational wave observatory
Science, 1992Co-Authors: Alex Abramovici, F.j. Raab, W E Althouse, R W P Drever, S Kawamura, D H Shoemaker, L Sievers, R Spero, Yekta Gursel, Kip S ThorneAbstract:The goal of the Laser Interferometer Gravitational-Wave Observatory (LIGO) Project is to detect and study astrophysical gravitational waves and use data from them for research in physics and astronomy. LIGO will support studies concerning the nature and nonlinear dynamics of gravity, the structures of black holes, and the equation of state of nuclear matter. It will also measure the masses, birth rates, collisions, and distributions of black holes and neutron stars in the universe and probe the cores of supernovae and the very early universe. The technology for LIGO has been developed during the past 20 years. Construction will begin in 1992, and under the present schedule, LIGO's gravitational-wave searches will begin in 1998.
R Abbott - One of the best experts on this subject based on the ideXlab platform.
-
First Targeted Search for Gravitational-Wave Bursts from Core-Collapse Supernovae in Data of First-Generation Laser Interferometer Detectors
Physical Review D, 2016Co-Authors: B P Abbott, R Abbott, T. D. Abbott, M. R. Abernathy, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R X AdhikariAbstract:We present results from a search for gravitational-wave bursts coincident with a set of two core-collapse supernovae observed between 2007 and 2011. We employ data from the Laser Interferometer Gravitational-wave Observatory (LIGO), the Virgo gravitational-wave observatory, and the GEO 600 gravitational-wave observatory. The targeted core-collapse supernovae were selected on the basis of (1) proximity (within approximately 15 Mpc), (2) tightness of observational constraints on the time of core collapse that defines the gravitational-wave search window, and (3) coincident operation of at least two Interferometers at the time of core collapse. We find no plausible gravitational-wave candidates. We present the probability of detecting signals from both astrophysically well-motivated and more speculative gravitational-wave emission mechanisms as a function of distance from Earth, and discuss the implications for the detection of gravitational waves from core-collapse supernovae by the upgraded Advanced LIGO and Virgo detectors.
-
search for gravitational waves from compact binary coalescence in ligo and virgo data from s5 and vsr1
Physical Review D, 2010Co-Authors: J Abadie, Parameswaran Ajith, B P Abbott, R Abbott, R X Adhikari, M. R. Abernathy, F. Acernese, C. Adams, T Accadia, B AllenAbstract:We report the results of the first search for gravitational waves from compact binary coalescence using data from the Laser Interferometer Gravitational-Wave Observatory and Virgo detectors. Five months of data were collected during the Laser Interferometer Gravitational-Wave Observatory's S5 and Virgo's VSR1 science runs. The search focused on signals from binary mergers with a total mass between 2 and 35M(circle dot). No gravitational waves are identified. The cumulative 90%-confidence upper limits on the rate of compact binary coalescence are calculated for nonspinning binary neutron stars, black hole-neutron star systems, and binary black holes to be 8: 7 X 10(-3) yr(-1) L-10(-1), 2.2 X 10(-3) yr(-1) L-10(-1), and 4.4 X 10(-4) yr(-1) L-10(-1), respectively, where L-10 is 10(10) times the blue solar luminosity. These upper limits are compared with astrophysical expectations.
-
ligo the Laser Interferometer gravitational wave observatory
Reports on Progress in Physics, 2009Co-Authors: B P Abbott, Parameswaran Ajith, R Adhikari, R. S. Amin, G Allen, S. B. Anderson, R Abbott, W.g. AndersonAbstract:The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech?MIT project supported by the National Science Foundation, operates three multi-kilometer Interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources.
-
searching for a stochastic background of gravitational waves with the Laser Interferometer gravitational wave observatory
The Astrophysical Journal, 2007Co-Authors: B Abbott, Parameswaran Ajith, R. S. Amin, W.g. Anderson, R Abbott, R X Adhikari, J Agresti, B Allen, S Anderson, M C ArayaAbstract:The Laser Interferometer Gravitational-Wave Observatory (LIGO) has performed the fourth science run, S4, with significantly improved Interferometer sensitivities with respect to previous runs. Using data acquired during this science run, we place a limit on the amplitude of a stochastic background of gravitational waves. For a frequency independent spectrum, the new Bayesian 90% upper limit is ΩGW × [H0/(72 km s−1 Mpc−1)]2 < 6.5 × 10-5. This is currently the most sensitive result in the frequency range 51-150 Hz, with a factor of 13 improvement over the previous LIGO result. We discuss the complementarity of the new result with other constraints on a stochastic background of gravitational waves, and we investigate implications of the new result for different models of this background.
B P Abbott - One of the best experts on this subject based on the ideXlab platform.
-
First Targeted Search for Gravitational-Wave Bursts from Core-Collapse Supernovae in Data of First-Generation Laser Interferometer Detectors
Physical Review D, 2016Co-Authors: B P Abbott, R Abbott, T. D. Abbott, M. R. Abernathy, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R X AdhikariAbstract:We present results from a search for gravitational-wave bursts coincident with a set of two core-collapse supernovae observed between 2007 and 2011. We employ data from the Laser Interferometer Gravitational-wave Observatory (LIGO), the Virgo gravitational-wave observatory, and the GEO 600 gravitational-wave observatory. The targeted core-collapse supernovae were selected on the basis of (1) proximity (within approximately 15 Mpc), (2) tightness of observational constraints on the time of core collapse that defines the gravitational-wave search window, and (3) coincident operation of at least two Interferometers at the time of core collapse. We find no plausible gravitational-wave candidates. We present the probability of detecting signals from both astrophysically well-motivated and more speculative gravitational-wave emission mechanisms as a function of distance from Earth, and discuss the implications for the detection of gravitational waves from core-collapse supernovae by the upgraded Advanced LIGO and Virgo detectors.
-
search for gravitational waves from compact binary coalescence in ligo and virgo data from s5 and vsr1
Physical Review D, 2010Co-Authors: J Abadie, Parameswaran Ajith, B P Abbott, R Abbott, R X Adhikari, M. R. Abernathy, F. Acernese, C. Adams, T Accadia, B AllenAbstract:We report the results of the first search for gravitational waves from compact binary coalescence using data from the Laser Interferometer Gravitational-Wave Observatory and Virgo detectors. Five months of data were collected during the Laser Interferometer Gravitational-Wave Observatory's S5 and Virgo's VSR1 science runs. The search focused on signals from binary mergers with a total mass between 2 and 35M(circle dot). No gravitational waves are identified. The cumulative 90%-confidence upper limits on the rate of compact binary coalescence are calculated for nonspinning binary neutron stars, black hole-neutron star systems, and binary black holes to be 8: 7 X 10(-3) yr(-1) L-10(-1), 2.2 X 10(-3) yr(-1) L-10(-1), and 4.4 X 10(-4) yr(-1) L-10(-1), respectively, where L-10 is 10(10) times the blue solar luminosity. These upper limits are compared with astrophysical expectations.
-
ligo the Laser Interferometer gravitational wave observatory
Reports on Progress in Physics, 2009Co-Authors: B P Abbott, Parameswaran Ajith, R Adhikari, R. S. Amin, G Allen, S. B. Anderson, R Abbott, W.g. AndersonAbstract:The goal of the Laser Interferometric Gravitational-Wave Observatory (LIGO) is to detect and study gravitational waves (GWs) of astrophysical origin. Direct detection of GWs holds the promise of testing general relativity in the strong-field regime, of providing a new probe of exotic objects such as black holes and neutron stars and of uncovering unanticipated new astrophysics. LIGO, a joint Caltech?MIT project supported by the National Science Foundation, operates three multi-kilometer Interferometers at two widely separated sites in the United States. These detectors are the result of decades of worldwide technology development, design, construction and commissioning. They are now operating at their design sensitivity, and are sensitive to gravitational wave strains smaller than one part in 1021. With this unprecedented sensitivity, the data are being analyzed to detect or place limits on GWs from a variety of potential astrophysical sources.
