Great News for Impatient Scientists!

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Title: Orbits for the Impatient: A Bayesian Rejection Sampling Method for Quickly Fitting the Orbits of Long-Period Exoplanets
Authors: Sarah Blunt, Eric L. Nielsen, Robert J. De Rosa, et al.
First Author’s Institution: Brown University
Status: Published in ApJ, open access

Discoveries of exoplanets happen quite often these days — so much so that the discovery alone is not enough to satisfy collective scientific curiosity. Discovery with direct imaging, in particular, does not usually reveal much about the planet, other than its existence. However, unlike the transit method and radial velocity measurements, direct imaging allows us to observe exoplanets with very long periods, which is an under-sampled population among currently known exoplanets. Still, this double-edged method of measurement cannot give us full orbital parameters of the planetary system. Long-period exoplanets cannot be easily observed by any other method but direct imaging, so the question arises — how can we find the orbital properties of this planetary population with the measurements we have?

orbits

A visualization of the OFTI method sampling, scaling and rotating a randomly selected orbit of the fitted exoplanet. In the lowest image, the red lines are the accepted orbits while the gray lines show the rejected orbits. [Blunt et al. 2017]

The authors of today’s paper use a new rejection sampling method to quickly find the orbits of these exoplanets, called Orbits for the Impatient (OFTI). This method generates random orbital fits from astrometric measurements, then scales and rotates the orbits, and then rejects orbits too unlikely. A visualization of this process is shown in the figure to the left.

This method uses astrometric observations and their uncertainties with prior probability density functions to produce posterior probability density functions of generated orbits. The main process of a rejection sampling method goes like this: the code generates random sets of orbital parameters, calculates a probability for each value, then rejects values with lower probabilities. The rejection process in OFTI is determined by comparing the generated probability to a selected number in (0,1). If the generated probability is greater than the random variable, then the orbit is accepted. This process repeats until any desired numbers of orbits have been selected.

Usually, algorithms such as Metropolis-Hastings MCMC are used for orbital fitting problems. However, this method takes far less time than an MCMC approach. The OFTI trials are independent, so the fitting and rejection-sampling can be done several times without incurring a bias in fitting. Running OFTI for several successive trials gives an unbiased estimate of the orbit up to 100 times faster than traditional Metropolis-Hasting MCMC fitting.

You may wonder how this method manages to run quickly without compromising the accuracy of its results. The answer to this musing is, of course, clever computational and statistical tricks. OFTI uses vectorized arrays rather than iterative loops when possible, and it is specifically designed to run multiple trials in parallel. Since there is an associated error with the astrometric measurements that OFTI uses to generate orbits, it first calculates the minimum χ2 value of all orbits tested during an initial run. Then it subtracts the minimum χ2 value from all other generated χ2 values. This way, orbits with an artificially high χ2 are not unfairly flat-out rejected. OFTI also confines the inclination and mass based on prior measurements, then uses the maximum, minimum and standard deviation of the array to change the range of values for these parameters, which prevents the generation of obviously unlikely orbits.

In this paper, the authors use this fitting method to find orbital parameters for 10 directly imaged exoplanets and other objects, including brown dwarfs and low-mass stars. The objects have at least two measured epochs of astrometry each; however in these cases, the orbits have not yet been measured because the measurements only cover a short range of the objects’ orbits. Using OFTI, the authors were able to successfully solve for the orbits of each of these substellar objects. The fitting for one of these objects, GJ 504 b, the current coldest imaged exoplanet, is shown in the figure below.

GJ 504 b

The orbit sampling of the planet GJ 504 b around star GJ 504 A. The 100 most probable orbits are colored accordingly. The right section of the image shows the measurements made of the object in black, and the red line shows the minimum orbit. [Blunt et al. 2017]

The most obvious application of this new process is long-period exoplanets, but the authors also solve for the orbits of a variety of other systems, including trinary stars and brown-dwarf systems. OFTI is also very useful in planning follow-up observations of targets. This method is incredibly useful, not only to planetary scientists but also to all kinds of stellar specialists. Impatient scientists can now use this method to achieve quick and accurate results — which are, quite frankly, the best kind of results.

About the author, Mara Zimmerman:

Mara is working on her PhD in Astronomy at the University of Wyoming. She has done research with binary stars, including “heartbeat” stars, and currently works on modeling debris disks.

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