L'étude présentée porte sur le contrôle actif des supensions pour Advanced LIGO. LIGO est un projet américain ayant pour but la détection d'ondes gravitationnelles, prédites par Einstein. Afin de mesurer ces ondes, le bruit sismique dot être atténué par un facteur de plusieurs milliards. Le dernier étage du système d'isolation sismique est un pendule filtrant le bruit sismique à hautes fréquences. Ce pendule présente d'importantes résonances à basses fréquences qui sont amorties par contrôle actif. Toutefois, ce contrôle re-injecte le bruit de mesure et détériore les performances d'isolation du pendule. La problématique est donc de concevoir une boucle de contrôle qui amortie les résonances tout en minimisant la réinjection du bruit de mesu...
To meet the overall isolation and alignment requirements for the optics in Advanced LIGO, the planne...
The suspended test masses of gravitational-wave (GW) detectors require precise alignment to be able ...
Seismic noise is the major source of noise at frequencies below 100 Hz in current LIGO detectors. Th...
Ground-based interferometric gravitational wave observatories such as Advanced LIGO must isolate the...
Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Mechanical Engineering, 2007.Includes...
The second generation of LIGO detectors has finished construction and the commissioning effort is pu...
We have developed, produced and characterized integrated sensors, actuators and the related read-out...
Multiple-stage seismic vibration isolation stacks, which consist of alternating layers of stiff mass...
Le projet LIGO a pour but la détection et l'étude d'ondes gravitationnelles via un réseau de détecte...
We demonstrate feed-forward vibration isolation on a suspended Fabry-Perot interferometer using Wien...
Teleseismic, or distant, earthquakes regularly disrupt the operation of ground-based gravitational w...
The suspension noise in interferometric gravitational wave detectors is caused by losses at the top ...
A new passive seismic attenuation system is being developed to replace the current passive attenuati...
We describe the design of the suspension systems for the major optics for Advanced LIGO, the upgrade...
To meet the overall isolation and alignment requirements for the optics in Advanced LIGO, the planne...
To meet the overall isolation and alignment requirements for the optics in Advanced LIGO, the planne...
The suspended test masses of gravitational-wave (GW) detectors require precise alignment to be able ...
Seismic noise is the major source of noise at frequencies below 100 Hz in current LIGO detectors. Th...
Ground-based interferometric gravitational wave observatories such as Advanced LIGO must isolate the...
Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Mechanical Engineering, 2007.Includes...
The second generation of LIGO detectors has finished construction and the commissioning effort is pu...
We have developed, produced and characterized integrated sensors, actuators and the related read-out...
Multiple-stage seismic vibration isolation stacks, which consist of alternating layers of stiff mass...
Le projet LIGO a pour but la détection et l'étude d'ondes gravitationnelles via un réseau de détecte...
We demonstrate feed-forward vibration isolation on a suspended Fabry-Perot interferometer using Wien...
Teleseismic, or distant, earthquakes regularly disrupt the operation of ground-based gravitational w...
The suspension noise in interferometric gravitational wave detectors is caused by losses at the top ...
A new passive seismic attenuation system is being developed to replace the current passive attenuati...
We describe the design of the suspension systems for the major optics for Advanced LIGO, the upgrade...
To meet the overall isolation and alignment requirements for the optics in Advanced LIGO, the planne...
To meet the overall isolation and alignment requirements for the optics in Advanced LIGO, the planne...
The suspended test masses of gravitational-wave (GW) detectors require precise alignment to be able ...
Seismic noise is the major source of noise at frequencies below 100 Hz in current LIGO detectors. Th...