Bayesian inference in single-line spectroscopic binaries with a visual orbit

TL;DR

This paper introduces a Bayesian inference method using MCMC for estimating orbital parameters of single-line spectroscopic binaries with astrometric data, allowing for improved parameter estimation and uncertainty quantification.

Contribution

The paper presents a novel Bayesian approach that incorporates prior information and handles partial observations to estimate orbital parameters, including component masses, in single-line spectroscopic binaries.

Findings

Mass ratio can be estimated with less than 10% uncertainty.

Method successfully derives full orbital elements for 12 binaries.

Analysis reveals how different data sources influence orbit and velocity uncertainties.

Abstract

We present a Bayesian inference methodology for the estimation of orbital parameters on single-line spectroscopic binaries with astrometric data, based on the No-U-Turn sampler Markov chain Monte Carlo algorithm. Our approach is designed to provide a precise and efficient estimation of the joint posterior distribution of the orbital parameters in the presence of partial and heterogeneous observations. This scheme allows us to directly incorporate prior information about the system - in the form of a trigonometric parallax, and an estimation of the mass of the primary component from its spectral type - to constrain the range of solutions, and to estimate orbital parameters that cannot be usually determined (e.g. the individual component masses), due to the lack of observations or imprecise measurements. Our methodology is tested by analyzing the posterior distributions of well-studied double-line spectroscopic binaries treated as single-line binaries by omitting the radial velocity data of the secondary object. Our results show that the system's mass ratio can be estimated with an uncertainty smaller than 10% using our approach. As a proof of concept, the proposed methodology is applied to twelve single-line spectroscopic binaries with astrometric data that lacked a joint astrometric-spectroscopic solution, for which we provide full orbital elements. Our sample-based methodology allows us also to study the impact of different posterior distributions in the corresponding observations space. This novel analysis provides a better understanding of the effect of the different sources of information on the shape and uncertainty of the orbit and radial velocity curve.