Young Star Cluster Complexes in NGC 4038/39: Integral field spectroscopy using VIMOS-VLT

TL;DR

This study uses integral field spectroscopy and archival imaging to analyze young star cluster complexes in NGC 4038/39, revealing their properties, dynamics, and star formation activity, and suggesting they are akin to starburst regions.

Contribution

First detailed spectroscopic analysis of star cluster complexes in the Antennae galaxies, combining optical spectroscopy with archival imaging to assess their physical properties and dynamics.

Findings

Complexes are young (3-5 Myr) with Wolf-Rayet features.

Ionized gas expands at 20-40 km/s, indicating bubble formation.

Star formation rates are comparable to starburst regions.

Abstract

We present the first results of a survey to obtain Integral Field Spectroscopy of merging galaxies along the Toomre Sequence. In the present work, we concentrate on the star cluster complexes in the Antennae galaxies (NGC 4038/39) in the overlap region as well as the nuclear region of NGC 4038. Using optical spectroscopy we derive the extinction age, metallicity, velocity, velocity dispersion of the gas and star formation rate for each of the eight complexes detected. We supplement this study with archival HST-WFPC2 U, B, V, H$\alpha$, and I band imaging. Correcting the observed colours of the star clusters within the complexes for extinction, measured through our optical spectra, we compare the clusters with simple stellar population models, with which we find an excellent agreement. In five of the complexes we detect strong Wolf-Rayet emission features, indicating young ages (3-5 Myr). The ionized gas surrounding the complexes is expanding at speeds of 20-40 km/s. This slow expansion can be understood as a bubble, caused by the stellar winds and supernovae within the complexes, expanding into the remnant of the progenitor giant molecular cloud. We also find that the complexes themselves are grouped, at about the largest scale of which young star clusters are correlated, representing the largest coherent star forming region. We show that the area normalized star formation rates of these complexes clearly place them in the regime of star forming regions in starburst galaxies, thereby justifying the label of localized starbursts. Finally, we estimate the stability of the complexes, and find that they will probably loose a large fraction of their mass to the surrounding environment, although the central regions may merge into a single large star cluster.