http://arxiv.org/abs/2109.08984
We present the first multi-wavelength (near-infrared; $1.1 – 2.4$ $\mu m$) imaging of HD 36546’s debris disk, using the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). As a 3-10 Myr old T Tauri star, HD 36546 presents a rare opportunity to study a debris disk at very early stages. SCExAO/CHARIS imagery resolves the disk over angular separations of $\rho \sim 0.25″ – 1.0″$ (projected separations of $\rm{r_{proj}} \sim 25 – 101$ $\rm{au}$) and enables the first spectrophotometric analysis of the disk. The disk’s brightness appears symmetric between its eastern and western extents and it exhibits slightly blue near-infrared colors on average (e.g. $J-K =-0.4\pm0.1$) $-$ suggesting copious sub-micron sized or highly porous grains. Through detailed modeling adopting a Hong scattering phase function (SPF), instead of the more common Henyey-Greenstein function, and using the differential evolution optimization algorithm, we provide an updated schematic of HD 36546’s disk. The disk has a shallow radial dust density profile ($\alpha_{in} \approx 1.0$ and $\alpha_{out} \approx -1.5$), a fiducial radius of $r_0 \approx 82.7$ au, an inclination of $i \approx 79.1^\circ$, and a position angle of $\rm PA \approx 80.1^\circ$. Through spine tracing, we find a spine that is consistent with our modeling, but also with a “swept-back wing” geometry. Finally, we provide constraints on companions, including limiting a companion responsible for a marginal Hipparcos-Gaia acceleration to a projected separation of $\lesssim 0.2”$ and to a minimum mass of $\lesssim 11$ $\rm M_{Jup}$.
K. Lawson, T. Currie, J. Wisniewski, et. al.
Tue, 21 Sep 21
66/85
Comments: 23 pages, 19 figures
You must be logged in to post a comment.