ph 103c: the physics of ligo 27 may 1994 lecture 18...ph 103c: the physics of ligo 27 may 1994...
TRANSCRIPT
Ph 103c: The Physics of LIGO 27 May 1994
LECTURE 18
The 40 Meter prototype Interferometer as an Example of Many of the Issues Studied in this Course
Lecture by Robert Spero
Assigned Reading:
XX. R. Weiss, Quart. Prog. Rep. Res. Lab. Electron. M.l. T. 105, 54 (1972). [The seminal paper presenting in detail how laser interferometers can be used for gravitational wave detection, including a comprehensive analysis of noise sources.]
YY. Robert L. Forward, "Wideband laser-interferometer gravitational-radiation experiment ," Phys. Rev. D 17(2) , 379-390 (1977). [A description of the first interferometric gravitational-wave detector to be built (a 2 m Michelson interferometer) and the first search for gravitational waves using such a detector (a coincidence run conducted in 1972 between the interferometer and several bar detectors).]
A Few Suggested Problems: Note: Your homework for Lectures 17 and 18 is to be turned in to Shirley Hampton in room 151 Bridge Annex before 1:00PM Friday June 3
1. In this course you have encountered all the significant noise sources for interferometric detectors that the LIGO team is now aware of. Which of these were unanticipated by Weiss in Ref. 1 above; and are they "fundamental" or are they "technical"?
2. The interferometer described in Weiss's paper has a different optical configuration from the 40 m interferometer, but the shot noise calculated by Weiss is similar to that achieved in the 40 m. Why? Compare the shot noise limited sensitivity calculated by Weiss with the sensitivity achieved by Forward, and account for the difference.
3. The thermal noise calculated by Weiss is based on viscous damping [4>(w) <X w] . How does the thermal noise prediction change when if the damping is structural [4>(w) independent of w]? cf. Lectures 13 and 14.
4. Weiss calculated noise from laser intensity fluctuations acting on the test masses via radiation pressure. Intensity fluctuations also result in noise (in a manner discussed in Spero's lecture) if the interferometer's operating point is offset from a "dark fringe" at the photodiode. Under what circumstances will this noise be larger than that due to radiation-pressure fluctuations.
1
Lecture 18 The 40 Meter Prototype Interferometer as an Example
of Many of the Issues Studied in this Course
by Robert Spero, 27 May 1994
Spero lectured from the following transparencies. Kip has annotated them a hit.
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