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Pycbc Inference: a Python-Based Parameter Estimation Toolkit for Compact Binary Coalescence Signals

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Pycbc Inference: a Python-Based Parameter Estimation Toolkit for Compact Binary Coalescence Signals PyCBC Inference: A Python-based parameter estimation toolkit for compact binary coalescence signals C. M. Biwer Los Alamos National Laboratory, Los Alamos, NM 87545, USA Department of Physics, Syracuse University, Syracuse, NY 13244, USA Collin D. Capano Albert-Einstein-Institut, Max-Planck-Institut f¨urGravitationsphysik, D-30167 Hannover, Germany Soumi De Department of Physics, Syracuse University, Syracuse, NY 13244, USA Miriam Cabero Albert-Einstein-Institut, Max-Planck-Institut f¨urGravitationsphysik, D-30167 Hannover, Germany Duncan A. Brown Department of Physics, Syracuse University, Syracuse, NY 13244, USA Alexander H. Nitz Albert-Einstein-Institut, Max-Planck-Institut f¨urGravitationsphysik, D-30167 Hannover, Germany V. Raymond Albert-Einstein-Institut, Max-Planck-Institut f¨urGravitationsphysik, D-14476 Potsdam, Germany School of Physics and Astronomy, Cardiff University, Cardiff, CF243AA, Wales, UK Abstract. We introduce new modules in the open-source PyCBC gravitational- arXiv:1807.10312v1 [astro-ph.IM] 26 Jul 2018 wave astronomy toolkit that implement Bayesian inference for compact-object binary mergers. We review the Bayesian inference methods implemented and describe the structure of the modules. We demonstrate that the PyCBC Inference modules produce unbiased estimates of the parameters of a simulated population of binary black hole mergers. We show that the posterior parameter distributions obtained used our new code agree well with the published estimates for binary black holes in the first LIGO-Virgo observing run. PyCBC Inference: A Python-based parameter estimation toolkit for compact binary coalescence signals 2 1. Introduction of binary black holes and the black-hole mergers detected in the first LIGO-Virgo observing run to The observations of six binary black hole mergers [1, 2, demonstrate the use of PyCBC Inference. We provide 3, 4], and the binary neutron star merger GW170817 [5] the posterior probability densities for the events by Advanced LIGO [6] and Virgo [7] have established GW150914, GW151226, and LVT151012, and the the field of gravitational-wave astronomy. Understand- command lines and configurations to reproduce these ing the origin, evolution, and physics of gravitational- results as supplemental materials [14]. Finally, we wave sources requires accurately measuring the prop- summarize the status of the code and possible future erties of detected events. In practice, this is per- developments in Sec. 5. formed using Bayesian inference [8, 9]. Bayesian in- ference allows us to determine the signal model that 2. Bayesian Inference for Binary Mergers is best supported by observations and to obtain pos- terior probability densities for a model's parameters, In gravitational-wave astronomy, Bayesian methods hence inferring the properties of the source. In this are used to infer the properties of detected astrophys- paper, we present PyCBC Inference; a set of Python ical sources [15, 16, 17, 18]. Given the observed data modules that implement Bayesian inference in the Py- d~(t)|here this is data from a gravitational-wave de- CBC open-source toolkit for gravitational-wave astron- tector network in which a search has identified a sig- omy [10]. PyCBC Inference has been used to perform nal [19, 20, 21]|Bayes' theorem [8, 9] states that for a Bayesian inference for several astrophysical problems, hypothesis H, including: testing the black hole area increase law [11]; p(d~(t)j#;~ H)p(#~jH) combining multi-messenger obervations of GW170817 p(#~jd~(t);H) = : (1) to constrain the viewing angle of the binary [12]; and p(d~(t)jH) determining that the gravitational-wave observations In our case, hypothesis H is the model of the of GW170817 favor a model where both compact ob- gravitational-wave signal and #~ are the parameters of jects have the same equation of state, and measur- this model. Together, these describe the properties of ing the tidal deformabilities and radii of the neutron the astrophysical source of the gravitational waves. In stars [13]. Eq. (1), the prior probability density p(#~jH) describes We provide a comprehensive description of the our knowledge about the parameters before considering methods and code implemented in PyCBC Inference. the observed data d~(t), and the likelihood p(d~(t)j#;~ H) We then demonstrate that PyCBC Inference can is the probability of obtaining the observation d~(t) produce unbiased estimates of the parameters of a given the waveform model H with parameters #~. simulated population of binary black holes. We Often we are only interested in a subset of the show that PyCBC Inference can recover posterior parameters #~. To obtain a probability distribution probability distributions that are in good agreement on one or a few parameters, we marginalize the with the published measurements of the binary black posterior probability by integrating p(d~(t)j#;~ H)p(#~jH) holes detected in the first LIGO-Virgo observing over the unwanted parameters. Marginalizing over all run [1]. This paper is organized as follows: Sec. 2 parameters yields the evidence, p(d~(t)jH), which is gives an overview of the Bayesian inference methods the denominator in Eq. (1). The evidence serves as a used in gravitational-wave astronomy for compact- normalization constant of the posterior probability for object binary mergers. We provide an overview of the given model H. If we have two competing models the waveform models used; the likelihood function H and H , the evidence can be used to determine for a known signal in stationary, Gaussian noise; A B which model is favored by the data via the Bayes the sampling methods used to estimate the posterior factor [22, 23, 24], probability densities and the evidence; the selection of ~ independent samples; and the estimation of parameter p(d(t)jHA) B = : (2) ~ values from posterior probabilities. Sec. 3 describes p(d(t)jHB) the design of the PyCBC Inference software and how If B is greater than 1 then model HA is favored over the methods described in Sec. 2 are implemented HB, with the magnitude of B indicating the degree of in the code. Sec. 4 uses a simulated population belief. PyCBC Inference: A Python-based parameter estimation toolkit for compact binary coalescence signals 3 PyCBC Inference can compute Bayes factors and angular momentum), reducing the dimensionality of produce marginalized posterior probability densities the waveform parameters space. given the data from a network of gravitational-wave Given a set of parameters #~, one can obtain ~ observatories with N detectors d(t) = fdi(t); 1 < i < a model of the gravitational-wave signal from a Ng, and a model H that describes the astrophysical binary merger using a variety of different methods, source. In the remainder of this section, we review the including: post-Newtonian theory (see e.g. Ref. [33] methods used to compute these quantities. and references therein), analytic models calibrated against numerical simulations [34, 35, 36, 37, 38, 39, 2.1. Waveform Models 40], perturbation theory [41, 42], and full numerical solution of the Einstein equations (see e.g. Ref. [43] and The gravitational waves radiated in a binary merger's references therein). Obtaining posterior probabilities source frame are described by the component masses and evidences can require calculating O 109 template m1;2, the three-dimensional spin vectors ~s1;2 of the waveforms, which restricts us to models that are compact objects [25], and the binary's eccentricity computationally efficient to calculate. The cost of e [26]. A parameter φ describes the phase of the binary full numerical simulations makes them prohibitively at a fiducial reference time, although this is not usually expensive at present. Even some analytic models are of physical interest. For binaries containing neutron too costly to be used, and surrogate models have been stars, additional parameters Λ1;2 describe the star's developed that capture the features of these waveforms tidal deformabilities [27, 28], which depend on the at reduced computational cost [44, 45]. equation of state of the neutron stars. The waveform The specific choice of the waveform model H observed by the Earth-based detector network depends for an analysis depends on the physics that we wish on seven additional parameters: the signal's time of to explore, computational cost limitations, and the arrival tc, the binary's luminosity distance dL, and level of accuracy desired in the model. A variety four Euler angles that describe the transformation from of waveform models are available for use in PyCBC the binary's frame to the detector network frame [29]. Inference, either directly implemented in PyCBC or These angles are typically written as the binary's right via calls to the LIGO Algorithm Library (LAL) [46]. ascension α, declination δ, a polarization angle Ψ, and We refer to the PyCBC and LAL documentation, and the inclination angle ι (the angle between the binary's references therein, for detailed descriptions of these angular momentum axis and the line of sight). models. In this paper, we demonstrate the use of Binary mergers present a challenging problem PyCBC Inference using the IMRPhenomPv2 [47, 48] for Bayesian inference, as the dimensionality of the waveform model for binary black hole mergers. This signal parameter space is large. This is further model captures the inspiral-merger-ringdown physics complicated by correlations between the signal's of spinning, precessing binaries and parameterizing parameters. For example, at leading order the spin effects using a spin magnitude aj, an azimuthal gravitational waveform depends on the chirp mass a p angle θj , and a polar angle θj for each of the two M [30]. The mass ratio enters the waveform compact objects. Examples of using PyCBC Inference at higher orders and is more difficult to measure. with different waveform models include the analysis This results in an amplitude-dependent degeneracy of Ref. [13] that used the TaylorF2 post-Newtonian between the component masses [18]. Similarly, waveform model with tidal corrections, and Ref.
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