Barnard 59: No Evidence for Further Fragmentation

Abstract

The dense molecular clump at the center of the Barnard 59 (B59) complex is the only region in the Pipe Nebula that has formed a small,stellar cluster. The previous analysis of a high resolution near-IR dust extinction map revealed that the nuclear region in B59 is a massive, mostly quiescent clump of 18.9 solar masses. The clump shows a monolithic profile, possibly indicating that the clump is on the way to collapse, with no evident fragmentation that could lead to another group of star systems. In this paper we present new analysis that compares the dust extinction map with a new dust emission radio-continuum map of higher spatial resolution. We confirm that the clump does not show any significant evidence for prestellar fragmentation at scales smaller than those probed previously.

15 pages, 2 figures, 2 tables. Accepted by The Astrophysical Journal

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Cited by in corpus (9)

• A case of simultaneous star and planet formation
• The molecular gas content of the Pipe Nebula I. Direct evidence of outflow-generated turbulence in B59?
• The Rotating Outflow, Envelope and Disk in Class-0/I protostar [BHB2007] 11 in the Pipe Nebula
• Optical/Near-IR Polarization Survey of Sh 2-29: Magnetic Fields, Dense Cloud Fragmentations and Anomalous Dust Grain Sizes
• Two-Stage Fragmentation for Cluster Formation: Analytical Model and Observational Considerations
• Not so different after all: Properties and Spatial Structure of Column Density Peaks in the Pipe and Orion A Clouds
• Young starless cores embedded in the magnetically dominated Pipe Nebula. II. Extended dataset
• The Green Bank Ammonia Survey: Unveiling the Dynamics of the Barnard 59 star-forming Clump
• FORCAST imaging of two small nearby Clusters: The Coronet and B59