SCExAO/CHARIS Multi-Wavelength, High-Contrast Imaging of the BD+45$^\circ$598 Debris Disk

TL;DR

This study uses multi-wavelength high-contrast imaging to analyze the debris disk around BD+45°598, constraining its structure, dust properties, and planet detection limits, providing insights into early debris disk evolution.

Contribution

First multi-wavelength high-contrast imaging study of BD+45°598's debris disk, revealing its geometry, dust grain size, and planet detection sensitivities.

Findings

Disk peak density radius of 109.6 au

Sensitivity to planets as small as 10 M_Jup at 12 au

Minimum dust grain size constrained between 0.13 and 1.01 μm

Abstract

We present a multi-wavelength (1.16$\mu$m-2.37$\mu$m) view of the debris disk around BD+45$^\circ$598, using the Subaru Coronagraphic Extreme Adaptive Optics system paired with the Coronagraphic High Angular Resolution Imaging Spectrograph. With an assumed age of 23 Myr, this source allows us to study the early evolution of debris disks and search for forming planets. We fit a scattered light model to our disk using a differential evolution algorithm, and constrain its geometry. We find the disk to have a peak density radius of $R_0 = 109.6$ au, an inclination of $i = 88.1^\circ$, and position angle $PA = 111.0^\circ$. While we do not detect a substellar companion in the disk, our calculated contrast limits indicate sensitivity to planets as small as $\sim 10 M_{\rm Jup}$ at a projected separation of 12 au of the star, and as small as $\sim 4 M_{\rm Jup}$ beyond 38 au. When measuring intensity as a function of wavelength, the disk color constrains the minimum dust grain size within a range of $\sim0.13$ to 1.01$\mu$m.