An ALCHEMI inspection of sulphur-bearing species towards the central molecular zone of NGC 253
Artikel i vetenskaplig tidskrift, 2024
Context. Sulphur-bearing species are detected in various environments within Galactic star-forming regions and are particularly abundant in the gas phase of outflow and shocked regions in addition to photo-dissociation regions. Thanks to the powerful capabilities of millimetre interferometers, studying sulphur-bearing species and their region of emission in various extreme extra-galactic environments (e.g. starburst and active galactic nuclei) and at a high-angular resolution and sensitivity is now possible. Aims. In this work, we aim to investigate the nature of the emission from the most common sulphur-bearing species observable at millimetre wavelengths towards the nuclear starburst of the nearby galaxy NGC 253. We intend to understand which type of regions are probed by sulphur-bearing species and which process(es) dominate(s) the release of sulphur into the gas phase. Methods. We used the high-angular resolution (1.600 or ∼27 pc) observations from the ALCHEMI ALMA Large Program to image several sulphur-bearing species towards the central molecular zone (CMZ) of NGC 253. We performed local thermodynamic equilibrium (LTE) and non-LTE large velocity gradient (LVG) analyses to derive the physical conditions of the gas where the sulphur-bearing species are emitted, and their abundance ratios across the CMZ. Finally, we compared our results with previous ALCHEMI studies and a few selected Galactic environments. Results. To reproduce the observations, we modelled two gas components for most of the sulphur-bearing species investigated in this work. We found that not all sulphur-bearing species trace the same type of gas: strong evidence indicates that H2S and part of the emission of OCS, H2CS, and SO are tracing shocks, whilst part of SO and CS emission rather traces the dense molecular gas. For some species, such as CCS and SO2, we could not firmly conclude on their origin of emission. Conclusions. The present analysis indicates that the emission from most sulphur-bearing species throughout the CMZ is likely dominated by shocks associated with ongoing star formation. In the inner part of the CMZ where the presence of super star clusters was previously indicated, we could not distinguish between shocks or thermal evaporation as the main process releasing the S-bearing species.
galaxies: abundances
ISM: molecules
astrochemistry
galaxies: ISM
galaxies: active
galaxies: starburst
Författare
M. Bouvier
Universiteit Leiden
Serena Viti
Universiteit Leiden
E. Behrens
University of Virginia
Joshua Butterworth
Universiteit Leiden
K. Y. Huang
Universiteit Leiden
J. G. Mangum
National Radio Astronomy Observatory
N. Harada
The Graduate University for Advanced Studies (SOKENDAI)
National Astronomical Observatory of Japan
S. Martin
Atacama Large Millimeter-submillimeter Array (ALMA)
European Southern Observatory Santiago
Víctor M. Rivilla
Centro de Astrobiologia (CAB)
Sebastien Muller
Chalmers, Rymd-, geo- och miljövetenskap, Onsala rymdobservatorium
K. Sakamoto
The Graduate University for Advanced Studies (SOKENDAI)
Y. Yoshimura
University of Tokyo
Kunihiko Tanaka
Keio University
K. Nakanishi
The Graduate University for Advanced Studies (SOKENDAI)
National Astronomical Observatory of Japan
R. Herrero-Illana
European Southern Observatory Santiago
L. Colzi
Centro de Astrobiologia (CAB)
M. Gorski
Northwestern University
C. Henkel
Xinjiang Astronomical Observatory
Max-Planck-Gesellschaft
King Abdulaziz University
Pedro Humire
Universidade de Sao Paulo (USP)
D. S. Meier
New Mexico Institute of Mining and Technology
National Radio Astronomy Observatory Socorro
P. van der Werf
Universiteit Leiden
Y. T. Yan
Max-Planck-Gesellschaft
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 689 A64Molekyler som Diagnostiska Redskap för Aktiva och Skymda Galaxer
Vetenskapsrådet (VR) (2011-4143), 2012-01-01 -- 2014-12-31.
Ämneskategorier
Astronomi, astrofysik och kosmologi
DOI
10.1051/0004-6361/202449186