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Abstract: The Laser Interferometer Space Antenna LISA is designed to detectgravitational wave signals from astrophysical sources, including those fromcoalescing binary systems of compact objects such as black holes. Collidinggalaxies have central black holes that sink to the center of the merged galaxyand begin to orbit one another and emit gravitational waves. Some galaxyevolution models predict that the binary black hole system will enter the LISAband with significant orbital eccentricity, while other models suggest that theorbits will already have circularized. Using a full seventeen parameterwaveform model that includes the effects of orbital eccentricity, spinprecession and higher harmonics, we investigate how well the source parameterscan be inferred from simulated LISA data. Defining the reference eccentricityas the value one year before merger, we find that for typical LISA sources, itwill be possible to measure the eccentricity to an accuracy of parts in athousand. The accuracy with which the eccentricity can be measured depends onlyvery weakly on the eccentricity, making it possible to distinguish circularorbits from those with very small eccentricities. LISA measurements of theorbital eccentricity can help constraints theories of galaxy mergers in theearly universe. Failing to account for the eccentricity in the waveformmodeling can lead to a loss of signal power and bias the estimation ofparameters such as the black hole masses and spins.



Author: Joey Shapiro Key, Neil J. Cornish

Source: https://arxiv.org/







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