The Physical Conditions in a Pre Super Star Cluster Molecular Cloud in the Antennae Galaxies

K. E. Johnson; A. K. Leroy; R. Indebetouw; C. L. Brogan; B. C. Whitmore; J. Hibbard; K. Sheth; A. Evans

doi:10.1088/0004-637X/806/1/35

paper

The Physical Conditions in a Pre Super Star Cluster Molecular Cloud in the Antennae Galaxies

arXiv:1503.06477 · doi:10.1088/0004-637X/806/1/35

Abstract

We present an analysis of the physical conditions in an extreme molecular cloud in the Antennae merging galaxies. This cloud has properties consistant with those required to form a globular cluster. We have obtained ALMA CO and 870 $μ$ m observations of the Antennae galaxy system with $\sim 0".5$ resolution. This cloud stands out in the data with a radius of $≲ 24$ ~pc and mass of $> 5 \times 1 0^{6}$ ~M $_{⊙}$ . The cloud appears capable of forming a globular cluster, but the lack of associated thermal radio emission indicates that star formation has not yet altered the environment. The lack of thermal radio emission places the cloud in an early stage of evolution, which we expect to be short-lived ( $≲ 1$ ~Myr) and thus rare. Given its mass and kinetic energy, for the cloud to be confined (as its appearance strongly suggests) it must be subject to an external pressure of P/ $k_{B} ≳ 1 0^{8}$ ~K~cm $^{- 3}$ -- 10,000 times higher than typical interstellar pressure. This would support theories that high pressures are required to form globular clusters and may explain why extreme environments like the Antennae are preferred environments for generating such objects. Given the cloud temperature of $\sim 25$ ~K, the internal pressure must be dominated by non-thermal processes, most likely turbulence. We expect the molecular cloud to collapse and begin star formation in $≲ 1$ ~Myr.

9 pages, 6 figures

The Physical Conditions in a Pre Super Star Cluster Molecular Cloud in the Antennae Galaxies

Abstract

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