G0.253+0.016: A centrally condensed, high-mass protocluster

Abstract

Despite their importance as stellar nurseries and the building blocks of galaxies, very little is known about the formation of the highest mass clusters. The dense clump G0.253+0.016 represents an example of a clump that may form an Arches-like, high-mass cluster. Here we present molecular line maps toward G0.253+0.016 taken as part of the MALT90 molecular line survey, complemented with APEX observations. Combined, these data reveal the global physical properties and kinematics of G0.253+0.016. Recent Herschel data show that while the dust temperature is low (~19 K) toward its centre, the dust temperature on the exterior is higher (~27 K) due to external heating. Our new molecular line data reveal that, overall, the morphology of dense gas detected toward G0.253+0.016 matches very well its IR extinction and dust continuum emission. An anti-correlation between the dust and gas column densities toward its centre indicates that the clump is centrally condensed with a cold, dense interior in which the molecular gas is chemically depleted. The velocity field shows a strong gradient along the clump's major axis, with the blue-shifted side at higher Galactic longitude. The optically thick gas tracers are systematically red-shifted with respect to the optically thin and hot gas tracers, indicating radial motions. The gas kinematics and line ratios support the recently proposed scenario in which G0.253+0.016 results from a tidal compression during a recent pericentre passage near SgrA*. Because G0.253+0.016 represents an excellent example of a clump that may form a high-mass cluster, its detailed study should reveal a wealth of knowledge about the early stages of cluster formation.

57 pages. 29 figures. Accepted ApJ

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Cited by in corpus (35)

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• The Survey of Water and Ammonia in the Galactic Center (SWAG): Molecular Cloud Evolution in the Central Molecular Zone
• The dynamical evolution of molecular clouds near the Galactic Centre - II. Spatial structure and kinematics of simulated clouds
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• Tracing the Conversion of Gas into Stars in Young Massive Cluster Progenitors
• The dynamics and star-forming potential of the massive Galactic centre cloud G0.253+0.016
• Abundant Methanol Masers but no New Evidence for Star Formation in GCM0.253+0.016
• Characterizing the properties of cluster precursors in the MALT90 survey
• Star-formation rates from young-star counts and the structure of the ISM across the NGC346/N66 complex in the SMC
• Dynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds
• Young massive star cluster formation in the Galactic Centre is driven by global gravitational collapse of high-mass molecular clouds
• The dynamical evolution of molecular clouds near the Galactic Centre -- III. Tidally--induced star formation in protocluster clouds
• Star formation in 'the Brick': ALMA reveals an active proto-cluster in the Galactic centre cloud G0.253+0.016
• CMZoom II: Catalog of Compact Submillimeter Dust Continuum Sources in the Milky Way's Central Molecular Zone
• Kinematics and properties of the Central Molecular Zone as probed with [C II]
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• The CARMA 3mm Survey of the Inner $0.7^{\circ }\times 0.4^{\circ }$ of the Central Molecular Zone
• Initial phases of high-mass star formation: A multiwavelength study towards the extended green object G12.42+0.50
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• Fiery Cores: Bursty and Smooth Star Formation Distributions across Galaxy Centers in Cosmological Zoom-in Simulations
• JWST reveals widespread CO ice and gas absorption in the Galactic Center cloud G0.253+0.016
• Prospects for Detection of Synchrotron Emission from Secondary Electrons and Positrons in Starless Cores: Application to G0.216+0.016
• HCN $J$=4-3, HNC $J$=1-0, ${\mathrm{H}}^{13}\mathrm{CN}$ $J$=1-0, and $\mathrm{H}{\mathrm{C}}_3\mathrm{N}$ $J$=10-9 Maps of Galactic Center Region II.: Physical Properties of Dense Gas Clumps and Probability of Star Formation
• Towards a multi-scale understanding of the gas-star formation cycle in the Central Molecular Zone
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• Star formation rates on global and cloud scales within the Galactic Centre
• Molecular gas kinematics of the CMZ: Great oaks from little acorns grow