# A multi-wavelength study of the debris disc around 49 Cet

## TL;DR

This study combines multi-wavelength observations and modeling to analyze the dust properties and structure of the debris disc around 49 Cet, revealing insights into grain size distribution and disc morphology.

## Contribution

It presents new scattered light images and semi-dynamical dust models that unify thermal emission and scattered light data for the 49 Cet debris disc.

## Key findings

- Disc with maximum surface density at 110 au fits observations
- Grains near blow-out limit and large grains originate from same planetesimal population
- Radiation pressure significantly influences dust grain distribution

## Abstract

In a multi-wavelength study of thermal emission and scattered light images we analyse the dust properties and structure of the debris disc around the A1-type main sequence star 49~Cet. As a basis for this study, we present new scattered light images of the debris disc known to possess both a high amount of dust and gas. The outer region of the disc is revealed in former coronagraphic H-band and our new Y-band images from the Very Large Telescope SPHERE instrument. We use the knowledge of the disc's radial extent inferred from ALMA observations and the grain size distribution found by SED fitting to generate semi-dynamical dust models of the disc. We compare the models to scattered light and thermal emission data and find that a disc with a maximum of the surface density at 110~au and shallow edges can describe both thermal emission and scattered light observations. This suggests that grains close to the blow-out limit and large grains stem from the same planetesimal population and are mainly influenced by radiation pressure. The influence of inwards transport processes could not be analysed in this study.