Vertical and radial distribution of atomic carbon in HD 163296^★

¹ University of Chile, Astronomy Deparment, Camino El Observatorio 1515, Santiago, Chile
e-mail: francisco.urbina@ug.uchile.cl
² Departamento de Física, Universidad de Santiago de Chile, Av. Victor Jara 3659, Santiago, Chile
³ Millennium Nucleus on Young Exoplanets and their Moons (YEMS), Santiago, Chile
⁴ Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago, Santiago, Chile
⁵ Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
⁶ Tartu Observatory, University of Tartu, Observatooriumi 1, Tõravere 61602, Estonia

Received: 9 November 2023
Accepted: 1 March 2024

Abstract

Context. In protoplanetary disks, atomic carbon is expected to originate from the photo dissociation region at the disk surface where CO is dissociated by ultraviolet (UV) photons coming from the stellar, or external interstellar, radiation field. Even though atomic carbon has been detected in several protoplanetary disks, there is a lack of spatially resolved observations of it.

Aims. For the HD 163296 protoplanetary disk, we aim to obtain both the radial and vertical structure of [CI] = ³P₁ − ³P₀ line emission and perform the first direct comparison of this tracer with the optically thick line emission ¹²CO J = 2 − 1.

Methods. We used archival ALMA data for [CI] = ³P₁ − ³P₀ and previously published¹² CO J = 2 − 1 data in HD 163296. Through the disksurf software, we extracted the vertical structure; meanwhile, we obtained the radial profiles directly from imaging. Brand new DALI modeling was employed to perform a direct comparison with the data.

Results. We find that these tracers are colocated radially but not vertically, where the ¹²CO J = 2 − 1 emission is, on average, located at higher altitudes, as is also the case for other tracers in the same disk.

Conclusions. Due to this difference in the vertical height of the emission, the optically thick ¹²CO J = 2 − 1 emission line appears to trace the highest altitudes, despite the expected formation mechanism of [CI] in the disk. The latter phenomena may be due to efficient mixing of the upper layers of the disk, or UV photons penetrating deeper than we expected.