The Laser Interferometer Space Antenna (LISA) telescopes must be able to send to and receive light from the other two distant spacecraft. The angle between the distant spacecraft will vary by about one degree in the course of a year. In addition the send and receive directions, for any one telescope, will also vary because of changes in distance, relative velocities of the spacecraft and the flight time of the light. All of these (angular) motions place requirements on the telescope pointing mechanism and the compensating proof mass motions. In this paper we will present the magnitudes of these angular motions, within the context of Keplerian orbits, and the resulting image motions on the detectors.
LISA Optics and Orbital Motions
Almaldi-5 Conference ; 2003 ; Piza, Italy
2003-01-01
Conference paper
No indication
English
NTRS | 2002
|LISA Optics Model: Early Results
NTRS | 2003
|Preliminary Orbital Control Strategy for LISA
British Library Conference Proceedings | 1999
|Wiley | 2015
|Computing Long-Term Orbital Motions
NTRS | 1987
|