Discovery of a Giant Molecular Loop in the Central Region of NGC 253

• Published in: The Astrophysical journal Vol. 929; no. 1; pp. 63 - 78
• Main Authors: Konishi, R., Enokiya, R., Fukui, Y., Muraoka, K., Tokuda, K., Onishi, T.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.04.2022; IOP Publishing
• Subjects: Astrophysics; Eccentric orbits; Field strength; Galactic center; Galaxies; Galaxy kinematics; Hydrodynamics; Interstellar clouds; Magnetic fields; Magnetohydrodynamic simulation; Milky Way; Molecular structure; Star clusters; Starburst galaxies
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac58f7

Abstract NGC 253 is a starburst galaxy of SAB(s)c type with increasing interest because of its high activity at unrivaled closeness. Its energetic event is manifested as the vertical gas features in its central molecular zone, for which stellar feedback was proposed as the driving engine. In order to pursue details of the activity, we have undertaken a kinematic analysis of the ALMA archive data of 12 CO( J = 3 − 2) emission at the highest resolution ∼3 pc. We revealed that one of the non-rotating gas components in the central molecular zone shows a loop-like structure of ∼200 pc radius. The loop-like structure is associated with a star cluster, whereas the cluster is not inside the loop-like structure and is not likely as the driver of the loop-like structure formation. Further, we find that the bar potential of NGC 253 seems to be too weak to drive the gas motion by the eccentric orbit. As an alternative, we frame a scenario that magnetic acceleration by the Parker instability is responsible for the creation of the loop-like structure. We show that the observed loop-like structure properties are similar to those in the Milky Way, and argue that recent magneto-hydrodynamics simulations lend support for the picture having the magnetic field strength of ≳100 μ G. We suggest that cluster formation was triggered by the falling gas to the footpoint of the loop, which is consistent with a typical dynamical timescale of the loop ∼1 Myr.