The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium

被引:36
作者
Hislop, Jessica M. [1 ]
Naab, Thorsten [1 ]
Steinwandel, Ulrich P. [2 ]
Lahen, Natalia [1 ]
Irodotou, Dimitrios [3 ,4 ]
Johansson, Peter H. [4 ]
Walch, Stefanie [5 ]
机构
[1] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany
[2] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA
[3] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England
[4] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2, FI-00014 Helsinki, Finland
[5] Univ Cologne, Phys Inst, Zulpicher Str 77, D-50937 Cologne, Germany
基金
欧洲研究理事会;
关键词
ISM: jets and outflows; ISM: structure; galaxies: dwarf; galaxies: evolution; galaxies: star clusters: ISM; galaxies: structure; SMOOTHED PARTICLE HYDRODYNAMICS; ADAPTIVE MESH REFINEMENT; MOLECULAR CLOUDS; FORMATION EFFICIENCY; IONIZING-RADIATION; STELLAR CLUSTERS; MASS FUNCTION; EVOLUTION; GAS; FEEDBACK;
D O I
10.1093/mnras/stab3347
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
引用
收藏
页码:5938 / 5954
页数:17
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