Estimating spinning binary parameters and testing alternative theories of gravity with LISA
By Emanuele Berti, A. Buonanno, C. Will. 2004
264 citations recorded by the source corpus.
We investigate the effect of spin-orbit and spin-spin couplings on the estimation of parameters for inspiralling compact binaries of massive black holes, and for neutron stars inspiralling into intermediate-mass black holes, using hypothetical data from the proposed Laser Interferometer Space Antenna (LISA). We work both in Einstein’s theory and in alternative theories of gravity of the scalar-tensor and massive-graviton types. We restrict the analysis to non-precessing spinning binaries, i.e. to cases where the spins are aligned normal to the orbital plane. We find that the accuracy with which intrinsic binary parameters such as chirp mass and reduced mass can be estimated within general relativity is degraded by between one and two orders of magnitude. We find that the bound on the coupling parameter ωBD of scalar-tensor gravity is significantly reduced by the presence of spin couplings, while the reduction in the graviton-mass bound is milder. Using fast Monte-Carlo simulations of 10 4 binaries, we show that inclusion of spin terms in massive blackhole binaries has little effect on the angular resolution or on distance determination accuracy. For stellar mass inspirals into intermediate-mass black holes, the angular resolution and the distance are determined only poorly, in all cases considered. We also show that, if LISA’s low-frequency noise sensitivity can be extrapolated from 10 −4 Hz to as low as 10 −5 Hz, the accuracy of determining both extrinsic parameters (distance, sky location) and intrinsic parameters (chirp mass, reduced mass) of massive binaries may be greatly improved.
Subfields: Astronomy and Astrophysics, Oceanography
View Paper: https://www.semanticscholar.org/paper/6134dcadb290184dcc39434115edcdb13f79c275
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Citations in the corpus
- Unveiling the gravitational universe at μ-Hz frequencies (2019, background): “much better sky localization, mass measurements, and so on [43].”
- The Confrontation between General Relativity and Experiment (2005, methodology): “For example, for the inspiral of two 10(6)M black holes with aligned spins at a distance of 3 Gpc observed by LISA, a bound of 2× 10(16) km could be placed [27].”
- Primordial black holes confront LIGO/Virgo data: current situation (2020, background): “J C A P 0 6 ( 2 0 2 0 ) 0 4 4 The final SNR can be then obtained by performing an average over the isotropic sky locations and orientations, finding that [78, 79]”
- Approximate Universal Relations for Neutron Stars and Quark Stars (2016, methodology): “We will here use the same waveform model as that used in Yagi and Yunes [48, 49], with the same Gaussian priors [392, 403, 404] that physically enforce δm ≤ 1/3, χs ≤ 0.”
- Massive Gravity (2014, unknown): “The detection of GWs in Advanced LIGO could then bound the graviton mass potentially all the way down to m < 10−29 eV [487, 486, 71].”
- Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy (2018, background): “For LISA, the GW bound could improve significantly, due to the lower frequencies and higher distances, possibly reaching mg < 10−26eV/c2 (Berti et al., 2005).”
- Cosmological Black Hole Spin Evolution by Mergers and Accretion (2008, background): “These plots are useful to isolate the contribution of mergers to the spin evolution of the whole BH population, and they are of direct interest for LISA observations of massive BH inspiral, merger and ringdown (Berti et al. 2005, 2006; Lang & Hughes 2006; Kocsis et al. 2007).”