# The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk

## TL;DR

This paper introduces a tomographic method to directly measure the temperature and density structure of an edge-on protoplanetary disk using ALMA observations, revealing detailed thermal and chemical features relevant to planet formation.

## Contribution

It presents a novel direct tomography technique for protoplanetary disks, utilizing velocity and intensity variations to map gas temperature and density without heavy model dependence.

## Key findings

- The disk has a cold mid-plane (<15-12 K) and a warmer atmosphere.
- CO gas extends beyond 200 au along the mid-plane, indicating UV re-heating.
- CO is detected up to 3-4 scale heights, while CS is confined near the mid-plane.

## Abstract

Determining the gas density and temperature structures of protoplanetary disks is a fundamental task to constrain planet formation theories. This is a challenging procedure and most determinations are based on model-dependent assumptions. We attempt a direct determination of the radial and vertical temperature structure of the Flying Saucer disk, thanks to its favorable inclination of 90 degrees. We present a method based on the tomographic study of an edge-on disk. Using ALMA, we observe at 0.5$"$ resolution the Flying Saucer in CO J=2-1 and CS J=5-4. This edge-on disk appears in silhouette against the CO J=2-1 emission from background molecular clouds in $\rho$ Oph. The combination of velocity gradients due to the Keplerian rotation of the disk and intensity variations in the CO background as a function of velocity provide a direct measure of the gas temperature as a function of radius and height above the disk mid-plane. The overall thermal structure is consistent with model predictions, with a cold ($< 15-12 $~K), CO-depleted mid-plane, and a warmer disk atmosphere. However, we find evidence for CO gas along the mid-plane beyond a radius of about 200\,au, coincident with a change of grain properties. Such a behavior is expected in case of efficient rise of UV penetration re-heating the disk and thus allowing CO thermal desorption or favoring direct CO photo-desorption. CO is also detected up to 3-4 scale heights while CS is confined around 1 scale height above the mid-plane. The limits of the method due to finite spatial and spectral resolutions are also discussed. This method appears to be very promising to determine the gas structure of planet-forming disks, provided that the molecular data have an angular resolution which is high enough, of the order of $0.3 - 0.1"$ at the distance of the nearest star forming regions.