Tomographic approach to resolving the distribution of LISA Galactic binaries

Abstract

The space based gravitational wave detector LISA is expected to observe a large population of Galactic white dwarf binaries whose collective signal is likely to dominate instrumental noise at observational frequencies in the range 10^{-4} to 10^{-3} Hz. The motion of LISA modulates the signal of each binary in both frequency and amplitude, the exact modulation depending on the source direction and frequency. Starting with the observed response of one LISA interferometer and assuming only doppler modulation due to the orbital motion of LISA, we show how the distribution of the entire binary population in frequency and sky position can be reconstructed using a tomographic approach. The method is linear and the reconstruction of a delta function distribution, corresponding to an isolated binary, yields a point spread function (psf). An arbitrary distribution and its reconstruction are related via smoothing with this psf. Exploratory results are reported demonstrating the recovery of binary sources, in the presence of white Gaussian noise.

arXiv comment13 Pages and 9 figures high resolution figures can be obtains from http://www.phys.utb.edu/~rajesh/lisa_tomography.pdf

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• An investigation of uniform expansions of large order Bessel functions in Gravitational Wave Signals from Pulsars
• The Carter Constant for Inclined Orbits About a Massive Kerr Black Hole: I. circular orbits
• Extracting overlapping gravitational-wave signals of galactic compact binaries: a mini review
• Addressing LISA Science Analysis Challenges
• Facing the LISA Data Analysis Challenge