The current worldwide interferometer network comprises detectors in the US (LIGO) and Europe (GEO600 and VIRGO) as well as advanced facilities in Japan (TAMA, CLIO) and Australia (ACIGA). Detectors currently have the sensitivity to detect neutron star binary coalescences out to approximately 15Mpc (the Virgo supercluster). Furthermore the long baseline instruments (LIGO and VIRGO) will shortly be undergoing upgrades which will see their sensitivity increase by an order of magnitude by 2014. These detectors, together with an upgraded GEO detector, should make routine detections and open up the gravitational window on the universe. In the longer term, 3rd generation detectors operating post 2018 will further increase the sensitivity by an additional order of magnitude and will likely feature underground operation at cryogenic temperatures or operation in space.
Hammond G., d.f.t.L.S.C.a.V.C., Cuoco, E. (2011). GRAVITATIONAL WAVE ASTRONOMY: AN EXPERIMENTAL OVERVIEW.
GRAVITATIONAL WAVE ASTRONOMY: AN EXPERIMENTAL OVERVIEW
Cuoco E.
2011
Abstract
The current worldwide interferometer network comprises detectors in the US (LIGO) and Europe (GEO600 and VIRGO) as well as advanced facilities in Japan (TAMA, CLIO) and Australia (ACIGA). Detectors currently have the sensitivity to detect neutron star binary coalescences out to approximately 15Mpc (the Virgo supercluster). Furthermore the long baseline instruments (LIGO and VIRGO) will shortly be undergoing upgrades which will see their sensitivity increase by an order of magnitude by 2014. These detectors, together with an upgraded GEO detector, should make routine detections and open up the gravitational window on the universe. In the longer term, 3rd generation detectors operating post 2018 will further increase the sensitivity by an additional order of magnitude and will likely feature underground operation at cryogenic temperatures or operation in space.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
