Realistic Detection and Early Warning of Binary NS with Decihertz Gravitational-wave Observatories @LISAcommunity

Uploaded July 2022 | Updated September 2026, 2 hours ago

The joint detection of the binary neutron star (BNS) inspiral GW170817 by gravitational-wave (GW) detectors and electromagnetic (EM) facilities has opened an era of multi-messenger astronomy. A successful multi-messenger detection requires prompt communication of source location and merger time from GW data to EM facilities, which drives the research on the real-time detections and early warnings from GW detectors.

We extend early studies on decihertz BNS detections by simulating detections in real observing scenarios and exploring the distributions of the accuracy in localization and timing. Using the Fisher information matrix method, we investigate the realistic detections and early warnings of 4 BNS population models with 4 representative decihertz GW observatories. We demonstrate that the detected BNSs can be divided into three categories based on their observational properties: (a) sources that merge within 1 year, which have less accurate localization and timing precision; (b) sources that merge in 1 to 4 years, which have stable and the best parameter estimation results, and (c) sources that do not merge within the mission time, which could still offer early warning alerts. Moreover, we also compare their detection performances with the ET, and discuss the influence of the confusion noise.

Authors: Chang Liu, Yacheng Kang, Lijing Shao
Presenters: Chang Liu

Realistic Detection and Early Warning of Binary NS with Decihertz Gravitational-wave Observatories

$Thermo-elastic and thermo-optical effects on-board LISA Pathfinder Thermal gradients on board the LISA Pathfinder mission induced effects with a potential impact to perturb the main differential acceleration measurement between both free-falling test masses. Temperature gradients across the housing produced forces through three different effects, namely asymmetric outgassing, radiation pressure and radiometer effect. The latter is related to the residual gas pressure around the test mass and, therefore, allows the estimation of the Brownian noise contribution, one of the limiting noise contributions for a future observatory like LISA. In addition to thermal forces arising due to gradients around the proof mass, thermo-optical and thermo-elastic effects can also contribute to instrument noise. There were two places where such distortion could be critical. First, the optical window, i.e. the interface between the optical bench and the test mass. This optical element the only not bonded on the Zerodur optical bench was clamped in a Titanium ring and therefore was susceptible to mechanical stress or changes in the refractive index due to thermal gradients across the glass. The second location were the struts holding the optical bench inside the thermal shield acting as the main thermal link to the outside (thermally noisier) environment. Temperature changes in these structures induced net displacements or tilts of the bench with direct impact on the interferometer read-out. During the LISA Pathfinder mission we have carried out several experiments by which we characterized and quantified the previous effects. The aim of this presentation is to update the results about the impact of thermo-elastic and thermo-optical effects, that we have obtained by analyzing the experiments, on the main differential acceleration measurement. In the same way we want to give an estimate of the impact of these thermal effects for the LISA mission. Authors: PhD Francisco Rivas (Presenting) Universidad Loyola Andalucía, Sevilla, Spain$

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