# First resolved observations of a highly asymmetric debris disc around HD 160305 with VLT/SPHERE

## TL;DR

This paper presents the first resolved near-infrared images of a highly inclined debris disc around HD 160305, revealing asymmetries and disc characteristics that inform our understanding of planetary system structures.

## Contribution

First resolved imaging and detailed analysis of the debris disc around HD 160305 using VLT/SPHERE, including disc morphology, asymmetries, and potential causes.

## Key findings

- Disc is a highly inclined (~82°) ring at ~86 au.
- Brightness asymmetry suggests anisotropic scattering (g>0.5).
- Two point sources are background stars, not companions.

## Abstract

Context. Direct imaging of debris discs gives important information about their nature, their global morphology, and allows us to identify specific structures possibly in connection with the presence of gravitational perturbers. It is the most straightforward technique to observe planetary systems as a whole. Aims. We present the first resolved images of the debris disc around the young F-type star HD 160305, detected in scattered light using the VLT/SPHERE instrument in the near infrared. Methods. We used a post-processing method based on angular differential imaging and synthetic images of debris discs produced with a disc modelling code (GRaTer) to constrain the main characteristics of the disc around HD 160305. All of the point sources in the field of the IRDIS camera were analysed with an astrometric tool to determine whether they are bound objects or background stars. Results. We detect a very inclined (~ 82{\deg}) ring-like debris disc located at a stellocentric distance of about 86au (deprojected width ~27 au). The disc displays a brightness asymmetry between the two sides of the major axis, as can be expected from scattering properties of dust grains. We derive an anisotropic scattering factor g>0.5. A second right-left asymmetry is also observed with respect to the minor axis. We measure a surface brightness ratio of 0.73 $\pm$ 0.18 between the bright and the faint sides. Because of the low signal-to-noise ratio (S/N) of the images we cannot easily discriminate between several possible explanations for this left-right asymmetry, such as perturbations by an unseen planet, the aftermath of the breakup of a massive planetesimal, or the pericenter glow effect due to an eccentric ring. Two epochs of observations allow us to reject the companionship hypothesis for the 15 point sources present in the field.