An interferometric study of the Fomalhaut inner debris disk II. Keck Nuller mid-infrared observations

TL;DR

This study uses high-contrast mid-infrared interferometric observations to investigate the inner debris disk of Fomalhaut, revealing a complex two-component dust structure within 2AU, with implications for dust dynamics and replenishment mechanisms.

Contribution

It presents the first detailed modeling of Fomalhaut's inner debris disk combining mid-infrared interferometry with Bayesian analysis to propose a two-component dust structure.

Findings

Detected a 0.35% null excess indicating hot dust within 2AU.

Proposed a two-component dust model with small carbon-rich grains close to 0.1AU and larger silicate grains around 1AU.

Suggested mechanisms for the presence of small grains despite radiation pressure expulsion.

Abstract

We report on high contrast mid-infrared observations of Fomalhaut obtained with the Keck Interferometer Nuller (KIN) showing a small resolved excess over the level expected from the stellar photosphere. The measured null excess has a mean value of 0.35% +/- 0.10% between 8 and 11 microns and increases from 8 to 13 microns. Given the small field of view of the instrument, the source of this marginal excess must be contained within 2AU of Fomalhaut. This result is reminiscent of previous VLTI K-band observations, which implied the presence of a ~ 0.88% excess, and argued that thermal emission from hot dusty grains located within 6 AU from Fomalhaut was the most plausible explanation. Using a parametric 2D radiative transfer code and a Bayesian analysis, we examine different dust disk structures to reproduce both the near and mid-infrared data simultaneously. While not a definitive explanation of the hot excess of Fomalhaut, our model suggests that the most likely inner few AU disk geometry consists of a two-component structure, with two different and spatially distinct grain populations. The 2 to 11 microns data are consistent with an inner hot ring of very small (~ 10 to 300 nm) carbon-rich grains concentrating around 0.1AU. The second dust population consists of larger grains (size of a few microns to a few tens of microns) located further out in a colder region where regular astronomical silicates could survive, with an inner edge around 1AU. From a dynamical point of view, the presence of the inner concentration of sub-micron sized grains is surprising, as such grains should be expelled from the inner planetary system by radiation pressure within only a few years. This could either point to some inordinate replenishment rates (e.g. many grazing comets coming from an outer reservoir) or to the existence of some braking mechanism preventing the grains from moving out.