VLT imaging of the {\beta} Pictoris gas disk

TL;DR

This study used high-resolution VLT spectroscopy to map the spatial distribution of Fe I and Ca II gas in the {eta} Pictoris debris disk, revealing asymmetries and vertical structure that inform its origin and dynamics.

Contribution

It provides the first spatially resolved images of Fe I and Ca II gas in the {eta} Pictoris disk, offering new insights into its morphology and gas-dust interactions.

Findings

Fe I dominates along the disk midplane and extends up to 210 AU.

Ca II is more vertically extended and shows opposite asymmetry to Fe I.

The gas disk's scale height increases linearly with radius.

Abstract

Circumstellar debris disks older than a few Myr should be largely devoid of primordial gas remaining from the protoplanetary disk phase. Tracing the origin of observed atomic gas in Keplerian rotation in the edge-on debris disk surrounding the ~12 Myr old star {\beta} Pictoris requires more detailed information about its spatial distribution than has previously been acquired by limited slit spectroscopy. Especially indications of asymmetries and presence of Ca II gas at high disk latitudes call for additional investigation. We set out to recover a complete image of the Fe I and Ca II gas emission around {\beta} Pic by spatially resolved, high-resolution spectroscopic observations to better understand the morphology and origin of the gaseous disk component. The multiple fiber facility FLAMES/GIRAFFE at the VLT, with the large IFU ARGUS, was used to obtain spatially resolved optical spectra in four regions covering the northeast and southwest side of the disk. Emission lines from Fe I and Ca II were mapped and could be used to fit a parametric function for the disk gas distribution, using a gas-ionisation code for gas-poor debris disks. Both Fe I and Ca II emission are clearly detected, with the former dominating along the disk midplane, and the latter revealing vertically more extended gas. The surface intensity of the Fe I emission is lower but more extended in the northeast (reaching the 210 AU limit of our observations) than in the southwest, while Ca II shows the opposite asymmetry. The modelled Fe gas disk profile shows a linear increase in scale height with radius, and a vertical profile that suggests dynamical interaction with the dust. We also qualitatively demonstrate that the Ca II emission profile can be explained by optical thickness in the disk midplane, and does not require Ca to be spatially separated from Fe. [ABRIDGED]