期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 445, 期 1, 页码 581-603出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1738
关键词
stars: formation; galaxies: active; galaxies: evolution; galaxies: formation; cosmology: theory
资金
- National Science Foundation [OCI-1053575, TG-AST120025, TG-AST130039, TG-TG-AST090039]
- UC-HiPACC
- NASA issued by the Chandra X-ray Observatory Center [PF1-120083]
- NASA [NAS8-03060, NNX09AG01G]
- Gordon and Betty Moore Foundation [776]
- Fulbright/MICINN Program
- Hellman Fellowship fund at the UC San Diego
- NASA ATP grant [NNX11AI97G, 12-ATP12-0183]
- Miller Institute for Basic Research in Science
- NASA through Einstein Postdoctoral Fellowship [PF3-140106, 10-ATP10-0187]
- Simons Foundation
- David and Lucile Packard Foundation
- Thomas Alison Schneider Chair in Physics
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1412153] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009999, 1411920, 1455342] Funding Source: National Science Foundation
- NASA [118606, NNX09AG01G, 144347, NNX11AI97G] Funding Source: Federal RePORTER
We present a series of high-resolution cosmological simulations(1) of galaxy formation to z = 0, spanning halo masses similar to 10(8)-10(13) M-circle dot, and stellar masses similar to 10(4)-10(11) M-circle dot. Our simulations include fully explicit treatment of themultiphase interstellar medium and stellar feedback. The stellar feedback inputs (energy, momentum, mass, and metal fluxes) are taken directly from stellar population models. These sources of feedback, with zero adjusted parameters, reproduce the observed relation between stellar and halo mass up to M-halo similar to 10(12) M-circle dot. We predict weak redshift evolution in the M-*-M-halo relation, consistent with current constraints to z > 6. We find that the M-*-M-halo relation is insensitive to numerical details, but is sensitive to feedback physics. Simulations with only supernova feedback fail to reproduce observed stellar masses, particularly in dwarf and high-redshift galaxies: radiative feedback (photoheating and radiation pressure) is necessary to destroy giant molecular clouds and enable efficient coupling of later supernovae to the gas. Star formation rates (SFRs) agree well with the observed Kennicutt relation at all redshifts. The galaxy-averaged Kennicutt relation is very different from the numerically imposed law for converting gas into stars, and is determined by self-regulation via stellar feedback. Feedback reduces SFRs and produces reservoirs of gas that lead to rising late-time star formation histories, significantly different from halo accretion histories. Feedback also produces large short-time-scale variability in galactic SFRs, especially in dwarfs. These properties are not captured by common 'sub-grid' wind models.
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