Star Cluster Formation in Cosmological Simulations. II. Effects of Star Formation Efficiency and Stellar Feedback [electronic resource]
Galaxies: Formation; Galaxies: High-Redshift; Galaxies: Star Clusters: General; Galaxies: Star Formation; Methods: Numerical.
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| Format: | Government Document Electronic eBook |
| Language: | English |
| Published: |
Washington, D.C. : Oak Ridge, Tenn. :
United States. Department of Energy. High Energy Physics Division ; distributed by the Office of Scientific and Technical Information, U.S. Department of Energy,
2018.
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| Subjects: |
MARC
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| 245 | 0 | 0 | |a Star Cluster Formation in Cosmological Simulations. II. Effects of Star Formation Efficiency and Stellar Feedback |h [electronic resource] |
| 260 | |a Washington, D.C. : |b United States. Department of Energy. High Energy Physics Division ; |a Oak Ridge, Tenn. : |b distributed by the Office of Scientific and Technical Information, U.S. Department of Energy, |c 2018. | ||
| 300 | |a Article No. 107 : |b digital, PDF file. | ||
| 336 | |a text |b txt |2 rdacontent. | ||
| 337 | |a computer |b c |2 rdamedia. | ||
| 338 | |a online resource |b cr |2 rdacarrier. | ||
| 500 | |a Published through SciTech Connect. | ||
| 500 | |a 07/10/2018. | ||
| 500 | |a "arxiv:1712.01219" | ||
| 500 | |a " fermilab-pub--18-366-a" | ||
| 500 | |a "1684467" | ||
| 500 | |a The Astrophysical Journal (Online) 861 2 ISSN 1538-4357 AM. | ||
| 500 | |a Hui Li; Oleg Y. Gnedin; Nickolay Y. Gnedin. | ||
| 520 | 3 | |a Here, the implementation of star formation and stellar feedback in cosmological simulations plays a critical role in shaping galaxy properties. In the first paper of the series, we presented a new method to model star formation as a collection of star clusters. In this paper, we improve the algorithm by eliminating accretion gaps, boosting momentum feedback, and introducing a subgrid initial bound fraction, $f_i$, that distinguishes cluster mass from stellar particle mass. We perform a suite of simulations with different star formation efficiency per freefall time $\epsilon_{\rm ff}$ and supernova momentum feedback intensity $f_{\rm boost}$. We find that the star formation history of a Milky Way-sized galaxy is sensitive to $f_{\rm boost}$, which allows us to constrain its value, $f_{\rm boost}\approx5$, in the current simulation setup. Changing $\epsilon_{\rm ff}$ from a few percent to 200\% has little effect on global galaxy properties. However, on smaller scales, the properties of star clusters are very sensitive to $\epsilon_{\rm ff}$. We find that $f_i$ increases with $\epsilon_{\rm ff}$ and cluster mass. Through the dependence on $f_i$, the shape of the cluster initial mass function varies strongly with $\epsilon_{\rm ff}$. The fraction of clustered star formation and maximum cluster mass increase with the star formation rate surface density, with the normalization of both relations dependent on $\epsilon_{\rm ff}$. The cluster formation timescale systematically decreases with increasing $\epsilon_{\rm ff}$. Local variations in the gas accretion history lead to a 0.25̃dex scatter for the integral cluster formation efficiency. Joint constraints from all the observables prefer the runs that produce a median integral efficiency of 16% | |
| 520 | 0 | |a Galaxies: Formation; Galaxies: High-Redshift; Galaxies: Star Clusters: General; Galaxies: Star Formation; Methods: Numerical. | |
| 536 | |b AC02-07CH11359. | ||
| 650 | 7 | |a Astronomy And Astrophysics. |2 edbsc. | |
| 710 | 2 | |a Fermi National Accelerator Laboratory. |4 res. | |
| 710 | 1 | |a United States. |b Department of Energy. |b High Energy Physics Division. |4 spn. | |
| 710 | 1 | |a United States. |b Department of Energy. |b Office of Scientific and Technical Information. |4 dst. | |
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