The goal with LISA (Laser Interferometer Space Antenna) is to detect and study low-frequency astrophysical gravitational radiation. LISA will complement the next-generation ground-based detectors (VIRGO, LIGO) by accessing the important low-frequency regime (10-4 to 10https://www.u-gov.unisalento.it/unile/#-1 Hz), which will never be observable from the Earth because of terrestrial disturbances. This low-frequency window affords access to the most exciting signals, those generated by massive black-hole information and coalescenes, as well as the most certain signals, such as those from galactic binaries. LISA will detect strains down to a level of order 10-23 in one year of observation time, by measuring the fluctuations in separation between shielded proof masses located 5 x 106 km apart. The measurement is performed by optical interferometry, which determines the phase shift of laser light transmitted between the proof masses. Each proof mass is shielded from extraneous distrubances by the 'drag-free' spacecraft in which it is accommodated. In the baseline for the study summarized in this paper, there are four spacecraft - two at a central vertex and two remote, forming a double-arm interferometer - located at 1 AU from the Sun, 20 deg behind the Earth.
LISA, Laser Interferometer Space Antenna for Gravitational Wave Measurements
CIUFOLINI, Ignazio
1994-01-01
Abstract
The goal with LISA (Laser Interferometer Space Antenna) is to detect and study low-frequency astrophysical gravitational radiation. LISA will complement the next-generation ground-based detectors (VIRGO, LIGO) by accessing the important low-frequency regime (10-4 to 10https://www.u-gov.unisalento.it/unile/#-1 Hz), which will never be observable from the Earth because of terrestrial disturbances. This low-frequency window affords access to the most exciting signals, those generated by massive black-hole information and coalescenes, as well as the most certain signals, such as those from galactic binaries. LISA will detect strains down to a level of order 10-23 in one year of observation time, by measuring the fluctuations in separation between shielded proof masses located 5 x 106 km apart. The measurement is performed by optical interferometry, which determines the phase shift of laser light transmitted between the proof masses. Each proof mass is shielded from extraneous distrubances by the 'drag-free' spacecraft in which it is accommodated. In the baseline for the study summarized in this paper, there are four spacecraft - two at a central vertex and two remote, forming a double-arm interferometer - located at 1 AU from the Sun, 20 deg behind the Earth.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
