Mass Loss, Kinematics and the Evolution of Super Star Clusters in the Antennae

Details Mass Loss, Kinematics and the Evolution of Super Star Clusters in the Antennae Mass Loss, Kinematics and the Evolution of Super Star Clusters in the Antennae

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..373g&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

Scientific paper

The youngest super star clusters (SSCs) in the merging Antennae Galaxies (NGC 4038/39) drive supersonic mass-loaded outflows from the HII regions in which they are embedded. High-resolution K-band NIRSPEC spectroscopy reveals broad spatially extended Br-gamma emission in 16 targets. The radial velocity field of young clusters resembles that of the surrounding molecular gas. Simple wind models for the line profiles provide good fits and imply cluster mass-loss rates of up to 1.5 Msun/year and terminal velocities of up to 205 km/s. The emission-line clusters (ELCs) that drive these outflows constitute at least 15% of the star-formation rate in the Antennae and their high star-formation efficiencies imply that they will evolve into bound SSCs. Comparison with population synthesis model predictions suggests that the youngest ELC outflows which are driven primarily by stellar winds very efficiently entrain ambient matter. The cluster winds transfer or dissipate a large fraction of their energy and momentum in a coronal or cool medium that does not emit Br-gamma. ELCs are the individual engines that power galactic-scale superwinds viewed in their earliest evolutionary stage. About half of the Chandra sources in the Antennae have IR cluster counterparts in which colliding-wind binaries could produce super-Eddington X-ray luminosities.

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