期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 466, 期 1, 页码 88-104出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw3011
关键词
methods: numerical; galaxies: evolution; galaxies: formation; galaxies: starburst; galaxies: star formation; cosmology: theory
资金
- Gordon and Betty Moore Foundation
- NSF [AST-1412836, AST-1517491, AST-1412153]
- NASA [NNX15AB22G]
- STScI [HST-AR- 14293.001-A, HST-GO-14268.022-A]
- National Science Foundation [PHYS-1066293]
- University of California San Diego
- Cottrell Scholar Award
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1517491, 1412153] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1412836, 1411920] Funding Source: National Science Foundation
Galaxy formation models are now able to reproduce observed relations such as the relation between galaxies' star formation rates (SFRs) and stellar masses (M*) and the stellar-mass-halo-mass relation. We demonstrate that comparisons of the short-time-scale variability in galaxy SFRs with observational data provide an additional useful constraint on the physics of galaxy formation feedback. We apply SFR indicators with different sensitivity time-scales to galaxies from the Feedback in Realistic Environments (FIRE) simulations. We find that the SFR-M* relation has a significantly greater scatter when the H alpha-derived SFR is considered compared with when the far-ultraviolet (FUV)-based SFR is used. This difference is a direct consequence of bursty star formation because the FIRE galaxies exhibit order-of-magnitude SFR variations over time-scales of a few Myr. We show that the difference in the scatter between the simulated Ha-and FUV-derived SFR-M* relations at z = 2 is consistent with observational constraints. We also find that the Ha/FUV ratios predicted by the simulations at z = 0 are similar to those observed for local galaxies except for a population of low-mass (M* less than or similar to 10(9.5) M-circle dot) simulated galaxies with lower H alpha/FUV ratios than observed. We suggest that future cosmological simulations should compare the H alpha/FUV ratios of their galaxies with observations to constrain the feedback models employed.
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