Close-in faint companions mimicking interferometric hot exozodiacal dust observations

TL;DR

This study investigates how faint companions can mimic hot exozodiacal dust signatures in interferometric data, revealing limitations of current detection methods and proposing new ways to distinguish between the two sources.

Contribution

The paper demonstrates that faint companions can evade detection in closure phase data yet still affect visibility, challenging previous assumptions and suggesting reevaluation of past studies.

Findings

Faint companions can produce measurable visibility deficits without detectable closure phases.

Current detection criteria may falsely exclude companions, affecting interpretations of exozodiacal dust.

A case study of kappa Tuc A indicates a potential faint companion with 0.7% flux ratio.

Abstract

Context: Interferometric observations of various nearby main-sequence stars show an unexpected infrared excess, raising the question of its origin. The two dominant interpretations favor hot exozodiacal dust or a faint companion, as both can produce similar signatures. Method: We modeled a system consisting of a star and a faint companion within a field of view of 2au x 2au. We calculated the visibility and closure phases for three VLTI instruments (PIONIER, GRAVITY, and MATISSE) and four telescope configurations. Aim: We aim to investigate the interferometric signatures of faint companions and assess their detectability. We explore limitations of current detection methods and evaluate the challenges in distinguishing between hot exozodiacal dust and a faint companion as the source of the observed excess. Results: We derived an upper limit for the companion-induced visibility deficit and closure phase. Contrary to the common interpretation that near-zero closure phases rule out the presence of a companion, we show that companions can remain undetected in closure phase data, as indicated by significant non-detection probabilities, yet, these companions can still produce measurable visibility deficits. We confirmed our results by reevaluating an L-band observation of kappa Tuc A. We found indications for a faint companion with a flux ratio of 0.7% and an estimated non-detection probability of around 21%, which could explain the variability of the previously observed visibility deficit. Conclusions: Previous companion rejection criteria, such as near-zero closure phases and flux estimates based on Gaussian-distributed dust densities, are not universally valid. This highlights the need for a reevaluation of companion rejections in former studies of the hot exozodiacal dust phenomenon. In addition, we propose a method for distinguishing both sources of visibility deficit.