Orateur
Description
In the context of the orbital modulated waveforms from the white dwarf binary gravitational foreground and the stochastic gravitational wave background (SGWB) in the LISA observation band, the Fisher Information and Markov Chains Monte Carlo methods give an estimation of the LISA noise and the parameters of the three backgrounds (galactic, astrophysical, cosmological). We simulate a complex waveform of the galactic foreground with 35 000 000 binaries. We extract an understanding of the effect of the distribution population across masses and positions in our galaxy, the stellar core type, and the orbital frequency distribution. We also predict the detectable limits for the future LISA measurement of the SGWB in the spectral domain with the three LISA channels A, E and T. We predict detectable limits for the future LISA measurement of the SGWB. Adaptive Markov chain Monte-Carlo methods are used to produce estimates with the simulated data from the LISA Data challenge (LDC). We also calculate the Cramer-Rao lower bound on the variance of the SGWB parameter uncertainties based on the inverse Fisher Information using the Whittle Likelihood. We simultaneously estimate the noise using a LISA noise model. Assuming the expected astrophysical background, a cosmological background and a galactic foreground energy density of around Ω_{GW} ≈ 1×10−12 to 1×10−13 can be detected by LISA.
