A Surface Density Perturbation in the TW Hydrae Disk at 95 au Traced by Molecular Emission

Abstract

We present ALMA Cycle~2 observations at $0.5^{\prime \prime }$ resolution of TW Hya of CS $J=5-4$ emission. The radial profile of the integrated line emission displays oscillatory features outwards of $1.5^{\prime \prime }$ ($\approx 90$ au). A dip-like feature at $1.6^{\prime \prime }$ is coincident in location, depth and width with features observed in dust scattered light at near-infrared wavelengths. Using a thermochemical model indicative of TW Hya, gas-grain chemical modelling and non-LTE radiative transfer, we demonstrate that such a feature can be reproduced with a surface density depression, consistent with the modelling performed for scattered light observations of TW Hya. We further demonstrate that a gap in the dust distribution and dust opacity only cannot reproduce the observed CS feature. The outer enhancement at $3.1^{\prime \prime }$ is identified as a region of intensified desorption due to enhanced penetration of the interstellar FUV radiation at the exponential edge of the disk surface density, which intensifies the photochemical processing of gas and ices.

arXiv comment12 pages, 16 figures, published in ApJ

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