Studies of Laser Interferometer Design and a Vibration Isolation System for Interferometric Gravitational Wave Detectors.

Details Studies of Laser Interferometer Design and a Vibration Isolation System for Interferometric Gravitational Wave Detectors. Studies of Laser Interferometer Design and a Vibration Isolation System for Interferometric Gravitational Wave Detectors.

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........8g&link_type=abstract

Thesis (PH.D.)--MASSACHUSETTS INSTITUTE OF TECHNOLOGY, 1995.Source: Dissertation Abstracts International, Volume: 56-06, Secti

Computer Science

1

Scientific paper

Two techniques are developed that are needed in the design of an interferometric gravitational wave (GW) detector such as the LIGO, or Long-baseline Interferometric Gravitational-wave Observatory. The detector sensitivity of a long-baseline instrument is studied. A multi-layer mechanical isolation stack to filter seismic noise from test masses is designed, modeled and tested in vacuum. This is a four-stage elastomer (spring) and stainless steel (mass) stack, consisting of a table resting on three separate legs of three layers each. The visco-elastic properties of elastomer springs are exploited to damp the stack's normal modes while providing rapid roll-off of stack transmission above these modal frequencies. The stack's transmission of base motion to top motion is measured in vacuum and compared with 3-D finite-element models. In one tested configuration, at 100 Hz, horizontal transmission is 10^{-7}, vertical transmission is 3 times 10^{-6}, and the cross-coupling terms are between these values. A length detection scheme using RF phase modulated light and synchronous detection is developed for Fabry -Perot arm power-recycled Michelson interferometer GW detectors. This scheme uses an external Mach-Zehnder interferometer to measure the GW signal, and a frequency-shifted subcarrier to measure ancillary interferometer degrees of freedom. Use of the Mach-Zehnder allows rejection of laser source amplitude noise from the output, as well as the ability to exploit well-balanced Fabry-Perot arms to reject frequency noise from the output. A long baseline GW detector using these techniques should meet the LIGO initial goal sensitivity to GW strain of h_{rm RMS} = 10^ {-21} at 100 Hz. (Copies available exclusively from MIT Libraries, Rm. 14-0551, Cambridge, MA 02139-1307. Ph. 617 -253-5668; Fax 617-253-1690.).

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