Star Clusters Near and Far
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Star Clusters Near and Far Tracing Star Formation Across Cosmic Time Angela Adamo1 · Peter Zeidler2,3 · J.M. Diederik Kruijssen4 · Mélanie Chevance4 · Mark Gieles5,6 · Daniela Calzetti7 · Corinne Charbonnel8,9 · Hans Zinnecker10 · Martin G.H. Krause11
Received: 31 January 2020 / Accepted: 11 May 2020 © The Author(s) 2020
Abstract Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e. detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we Star Formation Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger
B A. Adamo
[email protected] P. Zeidler [email protected] J.M.D. Kruijssen [email protected]
1
Department of Astronomy, Oskar Klein Centre, Stockholm University, AlbaNova University Centre, 106 91 Stockholm, Sweden
2
Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
3
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120 Heidelberg, Germany
5
Institut de Ciències del Cosmos (ICCUB-IEEC), Universitat de Barcelona, Martí i Franquès 1, 08028 Barcelona, Spain
6
ICREA, Pg. Lluis Companys 23, 08010 Barcelona, Spain
7
Departement of Astronomy, University of Massachusetts, LGRT-B 619J, 710 North Pleasant Street, Amherst, USA
8
Department of Astronomy, University of Geneva, Chemin de Pegase 51, 1290 Versoix, Switzerland
9
IRAP, CNRS & Univ. of Toulouse, 14, av.E.Belin, 31400 Toulouse, France
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believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations. Keywords Young star clusters · Cluster mass function · Stellar mass function · Resolved and unresolved stellar populations · Galaxy formation · Galaxy evolution
1 Introduction Deciding if a grouping of stars is a gravitationally bound star cluster is very challenging when the kinematics of the single stars cannot be traced. To use star clusters as tracers of galaxy evolution, it requires the understanding of the formation and evolution of gravitationally bound stellar systems; i.e. star clusters that are likely to survive for
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