Straight to the Source: Detecting Aggregate Objects in Astronomical Images with Proper Error Control

TL;DR

This paper introduces a statistical method for detecting aggregate objects in astronomical images that controls error rates rigorously, improving source detection accuracy for large telescope data and applicable to other fields like neuroimaging.

Contribution

It presents a novel technique combining source detection with rigorous error control, addressing limitations of existing algorithms and enabling reliable identification of sources in large astronomical datasets.

Findings

Effectively controls false source detection rate

Detects nearly all sources identified by traditional methods

Identifies a new source missed by previous studies

Abstract

The next generation of telescopes will acquire terabytes of image data on a nightly basis. Collectively, these large images will contain billions of interesting objects, which astronomers call sources. The astronomers' task is to construct a catalog detailing the coordinates and other properties of the sources. The source catalog is the primary data product for most telescopes and is an important input for testing new astrophysical theories, but to construct the catalog one must first detect the sources. Existing algorithms for catalog creation are effective at detecting sources, but do not have rigorous statistical error control. At the same time, there are several multiple testing procedures that provide rigorous error control, but they are not designed to detect sources that are aggregated over several pixels. In this paper, we propose a technique that does both, by providing rigorous statistical error control on the aggregate objects themselves rather than the pixels. We demonstrate the effectiveness of this approach on data from the Chandra X-ray Observatory Satellite. Our technique effectively controls the rate of false sources, yet still detects almost all of the sources detected by procedures that do not have such rigorous error control and have the advantage of additional data in the form of follow up observations, which will not be available for upcoming large telescopes. In fact, we even detect a new source that was missed by previous studies. The statistical methods developed in this paper can be extended to problems beyond Astronomy, as we will illustrate with an example from Neuroimaging.