Universität zu Köln

Hislop, Jessica M., Naab, Thorsten, Steinwandel, Ulrich P., Lahen, Natalia ORCID: 0000-0003-2166-1935, Irodotou, Dimitrios ORCID: 0000-0003-2946-8080, Johansson, Peter H. and Walch, Stefanie (2022). The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium. Mon. Not. Roy. Astron. Soc., 509 (4). S. 5938 - 5955. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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Abstract

We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarf galaxies as part of the GRIFFIN project. The simulations at sub-parsec spatial resolution and a minimum particle mass of 4 M-circle dot incorporate non-equilibrium heating, cooling, and chemistry processes, and realize individual massive stars. The simulations follow feedback channels of massive stars that include the interstellar-radiation field variable in space and time, the radiation input by photo-ionization and supernova explosions. Varying the star formation efficiency per free-fall time in the range epsilon(ff) = 0.2-50 per cent neither changes the star formation rates nor the outflow rates. While the environmental densities at star formation change significantly with epsilon(ff), the ambient densities of supernovae are independent of epsilon(ff) indicating a decoupling of the two processes. At low epsilon(ff), gas is allowed to collapse more before star formation, resulting in more massive, and increasingly more bound star clusters are formed, which are typically not destroyed. With increasing epsilon(ff), there is a trend for shallower cluster mass functions and the cluster formation efficiency Gamma for young bound clusters decreases from 50 per cent to similar to 1 per cent showing evidence for cluster disruption. However, none of our simulations form low mass (<10(3) M-circle dot) clusters with structural properties in perfect agreement with observations. Traditional star formation models used in galaxy formation simulations based on local free-fall times might therefore be unable to capture star cluster properties without significant fine tuning.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Hislop, Jessica M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Naab, Thorsten UNSPECIFIED UNSPECIFIED UNSPECIFIED Steinwandel, Ulrich P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Lahen, Natalia UNSPECIFIED orcid.org/0000-0003-2166-1935 UNSPECIFIED Irodotou, Dimitrios UNSPECIFIED orcid.org/0000-0003-2946-8080 UNSPECIFIED Johansson, Peter H. UNSPECIFIED UNSPECIFIED UNSPECIFIED Walch, Stefanie UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-681121
DOI:	10.1093/mnras/stab3347
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	509
Number:	4
Page Range:	S. 5938 - 5955
Date:	2022
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language SMOOTHED PARTICLE HYDRODYNAMICS; ADAPTIVE MESH REFINEMENT; MOLECULAR CLOUDS; FORMATION EFFICIENCY; IONIZING-RADIATION; STELLAR CLUSTERS; MASS FUNCTION; EVOLUTION; GAS; FEEDBACK Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/68112