Search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS). I. Indication for a centrifugal barrier in the environment of a single high-mass envelope

The conditions leading to the formation of the most massive O-type stars are still an enigma in modern astrophysics. To assess the physical conditions of high-mass protostars in their main accretion phase, here we present a case study of a young massive clump selected from the ATLASGAL survey, G328.2551-0.5321. The source exhibits a bolometric luminosity of 1.3 × 104 L☉, which allows us to estimate that its current protostellar mass lies between 11 and 16 M☉. We show high angular resolution observations with ALMA that reach a physical scale of 400 au. To reveal the structure of this high-mass protostellar envelope in detail at a 0.17'' resolution, we used the thermal dust continuum emission and spectroscopic information, amongst others from the CO (J = 3-2) line, which is sensitive to the high-velocity molecular outflow of the source. We also used the SiO (J = 8-7) and SO2 (J = 82,6 - 71,7) lines, which trace shocks along the outflow, as well as several CH3OH and HC3N lines that probe the gas of the inner envelope in the closest vicinity of the protostar. Our observations of the dust continuum emission reveal a single high-mass protostellar envelope, down to our resolution limit. We find evidence for a compact, marginally resolved continuum source that is surrounded by azimuthal elongations that could be consistent with a spiral pattern. We also report on the detection of a rotational line of CH3OH within its vt = 1 torsionally excited state. This shows two bright emission peaks that are spatially offset from the dust continuum peak and exhibit a distinct velocity component ±4.5 km s-1 offset from the systemic velocity of the source. Rotational diagram analysis and models based on local thermodynamic equilibrium assumption require high CH3OH column densities that reach N(CH3OH) = 1.2-2 × 1019 cm-2, and kinetic temperatures of the order of 160-200 K at the position of these peaks. A comparison of their morphology and kinematics with those of the outflow component of the CO line and the SO2 line suggests that the high-excitation CH3OH spots are associated with the innermost regions of the envelope. While the HC3N v7 = 0 (J = 37-36) line is also detected in the outflow, the HC3N v7 = 1e (J = 38-37) rotational transition within the first vibrationally excited state of the molecule shows a compact morphology. We find that the velocity shifts at the position of the observed high-excitation CH3 OH spots correspond well to the expected Keplerian velocity around a central object with 15 M☉ consistent with the mass estimate based on the bolometric luminosity of the source. We propose a picture where the CH3