Multiband gravitational-wave astronomy: Observing binary inspirals with a decihertz detector, B-DECIGO

被引：141

作者：

Isoyama, Soichiro ^{[1
]}

Nakano, Hiroyuki ^{[2
]}

Nakamura, Takashi ^{[3
,4
]}

机构：

[1] Univ Fed Rio Grande do Norte, Int Inst Phys, Campus Univ, BR-59078970 Natal, RN, Brazil

[2] Ryukoku Univ, Fac Law, Kyoto 6128577, Japan

[3] Kyoto Univ, Ctr Gravitat Phys, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan

[4] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan

来源：

PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS | 2018年 / 2018卷 / 07期

基金：

日本学术振兴会;

关键词：

BLACK-HOLE BINARIES; COMPACT BINARIES; NEUTRON-STARS;

D O I：

10.1093/ptep/pty078

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

An evolving Japanese gravitational-wave (GW) mission in the decihertz 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 intermediatemass binary black holes out to cosmological distances. The B-DECIGO band slots in between the aLIGO-Virgo-KAGRA-IndIGO (hectohertz) and LISA (millihertz) bands for broader bandwidth; the sources described emit GWs for weeks to years across the multiple bands to accumulate high signal-to-noise ratios. This suggests the possibility that joint detection would greatly improve the parameter estimation of the binaries. We examine B-DECIGO's ability to measure binary parameters and assess to what extent multiband analysis could improve such measurement. Using non-precessing post-Newtonian waveforms with the 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 < 5s about a week before alerting aLIGO and electromagnetic facilities. Prior information from B-DECIGO for aLIGO can further reduce the uncertainty in the measurement of, e.g., certain neutron star tidally induced deformations by a factor of similar to 6, and potentially determine the spin-induced neutron star quadrupole moment. Joint LISA and B-DECIGO measurement will also be able to recover the masses and spins of intermediate-mass binary black holes at percent-level precision. However, there will be a large systematic bias in these results due to post-Newtonian approximation of exact GW signals.

引用

页数：23

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