High angular resolution near-infrared integral field observations of young star cluster complexes in NGC1365

TL;DR

This study uses high-resolution near-infrared integral field spectroscopy with adaptive optics to analyze young star cluster complexes in NGC1365, revealing their spatial extent, age, mass, and gas dynamics, challenging previous assumptions about their mass functions.

Contribution

It provides new high-resolution observations and analysis of embedded star clusters in NGC1365, including measurements of their spatial structure, age, mass, and gas outflows, with implications for cluster formation models.

Findings

Clusters are spatially resolved and confined to ~50pc regions.

Measured ages are 5.5-6.5 Myr with masses 3-10 million solar masses.

Detected gas outflows indicated by Bracket-gamma line profiles.

Abstract

This paper presents and examines new near-infrared integral field observations of the three so-called 'embedded star clusters' located in the nuclear region of NGC1365. Adaptive-optics- corrected K-band data cubes were obtained with the ESO/VLT instrument SINFONI. The continuum in the K-band and emission lines such as HeI, Bracket-gamma, and several H2 lines were mapped at an achieved angular resolution of 0.2arcsec over a field of 3x3arcsec^2 around each source. We find that the continuum emission of the sources is spatially resolved. This means that they are indeed cluster complexes confined to regions of about 50pc extension. We performed robust measurements of the equivalent width of the CO absorption band at 2.3micro and of Bracket-gamma. For the main mid-infrared bright sources, the data only allow us to determine an upper limit to the equivalent width of the CO bands. Under the assumption of an instantaneously formed standard initial mass function Starburst99 model, the new measurements are found to be incompatible with previously published mid-infrared line ratios. We show that an upper mass limit of 25 to 30 solar masses, lower than the typically assumed 100solar masses, allows one to simply remove this inconsistency. For such a model, the measurements are consistent with ages in the range of 5.5Myr to 6.5Myr, implying masses in the range from 3 to 10 x 10^6 solar masses. We detect extended gas emission both in HII and H2. We argue that the central cluster complexes are the sources of excitation for the whole nebulae, through ionisation and shock heating. We detect a blue wing on the Bracket-gamma emission profile, suggesting the existence of gas outflows centred on the cluster complexes. We do not find any evidence for the presence of a lower mass cluster population, which would fill up a 'traditional' power law cluster mass function.