Resolving the terrestrial planet forming regions of HD113766 and HD172555 with MIDI

TL;DR

This study uses interferometric and spectroscopic observations to precisely locate dust in young debris disks around HD113766 and HD172555, shedding light on terrestrial planet formation regions.

Contribution

It provides the most accurate direct measurements of dust locations within 1-8AU in young debris disks, enhancing understanding of planet formation environments.

Findings

HD113766's disc is partially resolved with a FWHM of 1.2-1.6AU.

HD172555's disc emission is fully resolved, with dust located >1AU.

Extended emission at 18um suggests a broad or multiple disc components.

Abstract

We present new MIDI interferometric and VISIR spectroscopic observations of HD113766 and HD172555. Additionally we present VISIR 11um and 18um imaging observations of HD113766. These sources represent the youngest (16Myr and 12Myr old respectively) debris disc hosts with emission on <<10AU scales. We find that the disc of HD113766 is partially resolved on baselines of 42-102m, with variations in resolution with baseline length consistent with a Gaussian model for the disc with FWHM of 1.2-1.6AU (9-12mas). This is consistent with the VISIR observations which place an upper limit of 0."14 (17AU) on the emission, with no evidence for extended emission at larger distances. For HD172555 the MIDI observations are consistent with complete resolution of the disc emission on all baselines of lengths 56-93m, putting the dust at a distance of >1AU (>35mas). When combined with limits from TReCS imaging the dust at ~10um is constrained to lie somewhere in the region 1-8AU. Observations at ~18um reveal extended disc emission which could originate from the outer edge of a broad disc, the inner parts of which are also detected but not resolved at 10um, or from a spatially distinct component. These observations provide the most accurate direct measurements of the location of dust at 1-8AU that might originate from the collisions expected during terrestrial planet formation. These observations provide valuable constraints for models of the composition of discs at this epoch and provide a foundation for future studies to examine in more detail the morphology of debris discs.