Predictions for Ultra Compact X-Ray Binaries from Combined GW and Electromagnetic Wave Observations @LISAcommunity

Uploaded July 2022 | Updated September 2026, 1 hour ago

The purpose of this research was to investigate the sensitivity of characteristic parameters intrinsic of Ultra Compact X-ray Binaries necessary for LISA to determine and distinguish the mass sources in the system. The Gravitational Wave (GW) data was simulated using a Monte-Carlo simulation with different observing times and different system properties, including: masses representing low and high-mass Neutron stars and the threshold for Black Holes, relevant inclination angles with errors on the orbital decay of the systems, and different distance assumptions. The results of this research will suggest a necessary observing time for the LISA mission for these compact systems, and will entertain the degree of importance of the prior knowledge of specific characteristic parameters.

Author and Presenter: Antone Amalbert III

Predictions for Ultra Compact X-Ray Binaries from Combined GW and Electromagnetic Wave Observations

$Testing of a First-Generation Optical Truss Interferometer for the LISA Telescope The LISA telescope is a bidirectional component that is used to expand an outgoing laser beam to the far spacecraft as well as compress a small fraction of a large incoming beam to a diameter of a few mm at the optical bench. Since the telescope lies directly in the path of the long-baseline LISA interferometer, its structure must be dimensionally stable at the pm/âˆšHz level within the 0.1 mHz â€“ 1 Hz frequency band. A way to measure the displacement noise along the optical path of the telescope is with a compact optical truss interferometer (OTI), consisting of three Fabry-Perot cavities mounted along the telescope to monitor structural distortions over time. The premise is that variations in the cavity lengths will be due to dimensional changes in the telescope structure along three different lateral positions. We have developed a fiber-coupled Pound-Drever-Hall (PDH) system that integrates a fiber injector, mode matching optics, and a cavity input mirror into a compact input stage. These input stages will be attached around the primary mirror of the telescope, while the cavity return mirrors will be attached around the secondary mirror of the telescope. Using a PDH-like frequency locking scheme, variations in the cavity lengths will shift the frequency of the locked 1064 nm light which can be monitored through a beat signal between the light from each cavity and a separate laser that is locked to an ultra-stable reference cavity. We have designed and procured three first-generation OTI cavities and are currently testing the prototypes to verify pm/âˆšHz displacement sensitivity. We will present details regarding the design, fabrication, and assembly of the OTI units as well as preliminary results on the prototype testing and plans for future testing and verification. Authors: Kylan Jersey, Ian Harley-Trochimczyk, Yanqi Zhang, Felipe Guzman Presenter: Kylan Jersey$

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