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Young massive clusters in Arp 299

Published online by Cambridge University Press:  11 March 2020

Zara Randriamanakoto Open the ORCID record for Zara Randriamanakoto [Opens in a new window]  and
Petri Väisänen
Zara Randriamanakoto
Affiliation:
South African Astronomical Observatory PO Box 9, 7935 Observatory, Cape Town, Souh Africa email: zara@saao.ac.za
Petri Väisänen
Affiliation:
South African Astronomical Observatory PO Box 9, 7935 Observatory, Cape Town, Souh Africa email: zara@saao.ac.za Southern African Large Telescope PO Box 9, 7935 Observatory, Cape Town, Souh Africa email: petri@saao.ac.za
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Abstract

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Because of their young ages and compact densities, young massive star clusters (YMCs) are widely considered as potential proto-globular clusters. They are ubiquitous in environments with ongoing star formation activity such as interacting luminous infrared galaxies. To determine the galactic environmental effects on the star cluster formation and evolution, we study the YMC population of Arp 299 (NGC 3690E/NGC 3690W) using data taken with the HST WFC3/UVIS camera. By fitting the multiband photometry with the Yggdrasil models, we derive the star cluster masses, ages and extinction. While the cluster mass-galactocentric radius relation of NGC 3690E indicates that there could be an influence of the gas density distribution on the cluster formation, the age distribution of the western component suggests that YMCs in that galaxy endure stronger disruption mechanisms. With a cluster formation efficiency of 19 percent, star formation happening in bound clusters in Arp 299 is 3–5 times higher than that of a typical normal spiral.

Keywords

galaxies: interactionsgalaxies: individual: Arp 299NGC 3690ENGC 3690Wgalaxies: star clustersinfrared: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 143 - 146
Copyright
© International Astronomical Union 2020

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