http://arxiv.org/abs/1802.06977
An evolving Japanese gravitational-wave (GW) mission at deci-Hz band: B-DECIGO (DECihertz laser Interferometer Gravitational wave Observatory) will enable us to detect GW150914-like binary black-holes, GW170817-like binary neutron-stars, and the intermediate mass binary black-holes out to cosmological distances. The B-DECIGO band slots in between the aLIGO-Virgo-KAGRA-IndIGO (hecto-Hz) and LISA (milli-Hz) bands to broader bandwidth, and these sources emit GWs for weeks to years across the multiband to accumulate high signal-to-noise ratios. This suggests the possibility that the joint detection would greatly improve the parameter estimation of the binaries. We examine the B-DECIGO’s ability to measure binary parameters and assess what extent multiband analysis could improve such measurement, thanks to the broader bandwidth. Using non-precessing post-Newtonian waveforms with Fisher matrix approach, we find for systems like GW150914 and GW170817 that B-DECIGO can measure the mass ratio to within $< 0.1\%$, the individual black-hole spins to within $< 10\%$, and the coalescence time to within $< 2\,$s about a week before to alert aLIGO and electromagnetic facilities. aLIGO having prior information from B-DECIGO can further reduce the uncertainty in the measurement of, e.g., certain neutron-star tidal deformability by factor of $\sim 4$. Joint LISA and B-DECIGO measurement will also be able to recover masses and spins of intermediate mass binary black-holes at percent-level precision. However, there will be large systematic bias in these results due to post-Newtonian approximation to exact GW signals.
S. Isoyama, H. Nakano and T. Nakamura
Wed, 21 Feb 18
26/58
Comments: 16 pages, 2 figures