Caesalpinin B, a Rearranged Cassane Furanoditerpene of Caesalpinia bonduc

Tinto, Winston F.; Lyder, Deon Lucrecia; Bissada, Suzanne; McLean, Stewart; Reynolds, William F.

doi:10.3987/com-98-8159

Cited by 9 publications

(2 citation statements)

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“…The expressions for X, Y and Z remain unchanged apart from allowing for different delays of the counter-propagating beams. These expressions, denoted by X 1 , X 2 , and X 3 for Michelson-type readouts centered on S/C 1, 2, and 3 respectively, have been independently derived by Hellings [11] and Tinto et al [12]. These TDI Michelson readouts have a slightly better gravitational wave sensitivity than the Sagnac outputs particularly around 3 mHz.…”

Section: Sagnac Effect and The Lisa Constellationmentioning

confidence: 99%

“…This was first calculated by Hellings [11]. However, Tinto et al [12] pointed out that ζ can be modified to produce three combinations in which the frequency noise and bench noise are cancelled. In contrast to the symmetric variable ζ, these three combinations, denoted by ζ 1 , ζ 2 , and ζ 3 , combine the data from the three spacecraft asymmetrically.…”

Section: Sagnac Effect and The Lisa Constellationmentioning

confidence: 99%

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Operating LISA as a Sagnac interferometer

Shaddock

2004

Phys. Rev. D

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A phase-locking configuration for LISA is proposed that provides a significantly simpler mode of operation. The scheme provides one Sagnac signal readout inherently insensitive to laser frequency noise and optical bench motion for a non-rotating LISA array. This Sagnac output is also insensitive to clock noise, requires no time shifting of data, nor absolute arm length knowledge. As all measurements are made at one spacecraft, neither clock synchronization nor exchange of phase information between spacecraft is required. The phase-locking configuration provides these advantages for only one Sagnac variable yet retains compatibility with the baseline approach for obtaining the other TDI variables. The orbital motion of the LISA constellation is shown to produce a 14 km path length difference between the counter-propagating beams in the Sagnac interferometer. With this length difference a laser frequency noise spectral density of 1 Hz/ √ Hz would consume the entire optical path noise budget of the Sagnac variables. A significant improvement of laser frequency stability (currently at 30 Hz/ √ Hz) would be needed for full-sensitivity LISA operation in the Sagnac mode. Alternatively, an additional level of time-delay processing could be applied to remove the laser frequency noise. The new time-delayed combinations of the phase measurements are presented.

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Section: Sagnac Effect and The Lisa Constellationmentioning

confidence: 99%

Section: Sagnac Effect and The Lisa Constellationmentioning

confidence: 99%