Publications
The first results from ARKS are published in a series of 10 papers:
ARKS I: Motivation, sample, data reduction, and results overview, by Marino et al., this paper describes the motivation, sample, and data reduction procedures, and gives an overview of the results.
ARKS II: The radial structure of debris discs, by Han et al. While the radial structure of debris disks is broadly consistent with inheritance from the earlier, protoplanetary disk stage, some debris disks are substantially broader than their younger counterparts. Many of the smaller systems have sharp edges consistent with sculpting by low-mass planets, and several systems exhibit narrow rings surrounded by broad haloes of large dust grains.
ARKS III: The vertical structure of debris disks, by Zawadzki et al. When we model the vertical structure of systems viewed close to edge-on, we find that a majority prefer a two-scale vertical structure with both a broad and a narrow component. This structure is reminiscent of the solar system’s Kuiper belt, which has a narrow cold classical component and a scattered component largely due to Neptune’s outward migration.
ARKS IV: CO gas imaging and overview, by Mac Manamon et al. The radial profile of CO gas emission tends to be both broader than, and shifted radially inward from, the dust. The optical depth is not well constrained with just one transition.
ARKS V: Comparison between scattered light and thermal emission, by Milli et al. 15 of the 24 ARKS targets are also detected in scattered light. For gas-rich systems, the small dust grains are shifted outward by about 10%, indicating the interplay between radiation pressure and gas drag on small dust grains.
ARKS VI: Asymmetries and offsets, by Lovell et al. 10 of the 24 systems show significant dust asymmetries, mostly in the form of stellocentric offsets, arcs, and clumps. Asymmetries seem skewed towards gas-rich systems.
ARKS VII: Optically thick gas with broad CO gaussian local line profiles in the HD 121617 disc, by Brennan et al. HD 121617 exhibits optically thick gas emission and linewidths consistent with low excitation temperature.
ARKS VIII: A dust arc and non-Keplerian gas kinematics in HD 121617, by Marino et al. HD 121617 also has a dust arc seen only in the distribution of large mm-sized grains, and non-Keplerian gas kinematics due to strong pressure gradients.
ARKS IX: Gas-driven origin for the continuum arc in the debris disc of HD121617, by Weber et al., explores the origin of the dust arc as caused by dust trapping in a vortex using hydrodynamic simulations.
ARKS X: Interpreting the peculiar dust rings around HD 131835, by Jankovic et al. HD 131835 exhibits at least two distinct dust rings that flip their relative brightness in millimetre emission vs. scattered light, suggesting substantial grain size segregation due to gas dynamics.