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Inference on Gravitational Waves from Coalescences of Stellar-Mass Compact Objects and Intermediate-Mass Black Holes

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Globular Cluster Binaries and Gravitational Wave Parameter Estimation

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Abstract

This chapter is adapted from a paper by Carl-Johan Haster, Zhilu Wang, Christopher P. L. Berry, Simon Stevenson, John Veitch and Ilya Mandel. My contribution to this work was to (i) design the initial parameters of this study, (ii) aid Zhilu Wang (a summer student in the group) to run the simulations, (iii) lead the post-processing and collating of the results, (iv) write the paper. This paper is published in MNRAS [23] and has arXiv number 1511.01431.

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Notes

  1. 1.

    The inspiral of an IMBH into a supermassive BH is also referred to as an IMRI. GWs from such IMRIs are potential sources for a space-borne detector [8], as are the most massive (redshifted total masses of \(\gtrsim 10^3~\mathrm {M}_\odot \)) IMBHBs [17, 34].

  2. 2.

    For comparison, \(\sim \)30 coalescences of stellar-mass BH binaries originating in globular clusters could be detected per year ([46], and erratum).

  3. 3.

    The median SNR of detected signals, assuming that sources are uniformly distributed in (Euclidean) volume is \(\rho _\mathrm {med} = 2^{1/3} \rho _\mathrm {det}\), where \(\rho _\mathrm {det}\) is the detection threshold [48]. Taking a detection threshold of \(\rho _\mathrm {det} = 12\) [5], \(\rho _\mathrm {med} \simeq 15\).

  4. 4.

    The presence of non-stationary noise features (glitches) could impact PE leading to systematic errors. Realistic non-stationary, non-Gaussian noise has been shown not to affect PE performance for binary neutron stars [10]; however, these noise features could be more significant in analysing short-duration, low-frequency IMRAC signals.

  5. 5.

    A component of the LIGO Scientific Collaboration Algorithm Library (LAL) suite http://www.lsc-group.phys.uwm.edu/lal.

  6. 6.

    Veitch et al. [56] found that \(m_1 \gtrsim 130~\mathrm {M}_\odot \) was required to infer the presence of an IMBH in an IMBHB at \(95\%\) confidence.

  7. 7.

    In IMRPhenomD, IMR refers to inspiral–merger–ringdown, not intermediate mass ratio.

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  1. Canadian Institute for Theoretical Astrophysics, Toronto, ON, Canada

    Carl-Johan Haster

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Haster, CJ. (2017). Inference on Gravitational Waves from Coalescences of Stellar-Mass Compact Objects and Intermediate-Mass Black Holes. In: Globular Cluster Binaries and Gravitational Wave Parameter Estimation. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-63441-8_3

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