TY - JOUR
T1 - What FIREs up star formation
T2 - The emergence of the Kennicutt-Schmidt law from feedback
AU - Orr, Matthew E.
AU - Hayward, Christopher C.
AU - Hopkins, Philip F.
AU - Chan, T. K.
AU - Faucher-Giguère, Claude André
AU - Feldmann, Robert
AU - Kereš, Dušan
AU - Murray, Norman
AU - Quataert, Eliot
N1 - Funding Information:
MEO is grateful for the encouragement of his late father, SRO, in studying astrophysics, and for many helpful discussions with A. Wetzel, J. Schaye, S. Dib, and I. Escala. We are grateful to the anonymous referee for providing us with constructive comments and suggestions, which have significantly improved the work. This research has made use of NASA's Astrophysics Data System. MEO was supported by the National Science Foundation Graduate Research Fellowship under grant no. 1144469. CCH is grateful to the Gordon and Betty Moore Foundation for financial support. The Flatiron Institute is supported by the Simons Foundation. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. Numerical calculations were run on the Caltech compute cluster 'Zwicky' (NSF MRI award #PHY-0960291) and allocations TG-AST120025, and TG-AST130039 granted by the Extreme Science and EngineeringDiscovery Environment (XSEDE) supported by the NSF. CAFG was supported by NSF through grants AST-1412836 and AST-1517491, by NASA through grant NNX15AB22G, and by STScI through grants HST-AR-14293.001-A and HST-GO-14268.022-A. RF was supported by the Swiss National Science Foundation (grant no. 157591). DK acknowledges support from the NSF grant AST- 1412153 and Cottrell Scholar Award from the Research Corporation for Science Advancement. EQ was supported by NASA ATP grant 12-ATP12-0183, a Simons Investigator award from the Simons Foundation, and the David and Lucile Packard Foundation.
Funding Information:
MEO is grateful for the encouragement of his late father, SRO, in studying astrophysics, and for many helpful discussions with A. Wetzel, J. Schaye, S. Dib, and I. Escala. We are grateful to the anonymous referee for providing us with constructive comments and suggestions, which have significantly improved the work. This research has made use of NASA’s Astrophysics Data System. MEO was supported by the National Science Foundation Graduate Research Fellowship under grant no. 1144469. CCH is grateful to the Gordon and Betty Moore Foundation for financial support. The Flatiron Institute is supported by the Simons Foundation. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. Numerical calculations were run on the Caltech compute cluster ‘Zwicky’ (NSF MRI award #PHY-0960291) and allocations TG-AST120025, and TG-AST130039 granted by the Extreme Science and Engineering Discovery Environment (XSEDE) supported by the NSF. CAFG was supported by NSF through grants AST-1412836 and AST-1517491, by NASA through grant NNX15AB22G, and by STScI through grants HST-AR-14293.001-A and HST-GO-14268.022-A. RF was supported by the Swiss National Science Foundation (grant no. 157591). DK acknowledges support from the NSF grant AST-1412153 and Cottrell Scholar Award from the Research Corporation for Science Advancement. EQ was supported by NASA ATP grant 12-ATP12-0183, a Simons Investigator award from the Si-mons Foundation, and the David and Lucile Packard Foundation.
Publisher Copyright:
© 2018 The Author(s).
PY - 2018/8/1
Y1 - 2018/8/1
N2 - We present an analysis of the global and spatially resolved Kennicutt-Schmidt (KS) star formation relation in the FIRE (Feedback In Realistic Environments) suite of cosmological simulations, including haloes with z = 0 masses ranging from 1010 to 1013 M⊙.We show that the KS relation emerges and is robustly maintained due to the effects of feedback on local scales regulating star-forming gas, independent of the particular small-scale star formation prescriptions employed. We demonstrate that the time-averaged KS relation is relatively independent of redshift and spatial averaging scale, and that the star formation rate surface density is weakly dependent on metallicity and inversely dependent on orbital dynamical time. At constant star formation rate surface density, the 'cold and dense' gas surface density (gas with T < 300 K and n > 10 cm-3, used as a proxy for the molecular gas surface density) of the simulated galaxies is ~0.5 dex less than observed at ~kpc scales. This discrepancymay arise from underestimates of the local column density at the particle-scale for the purposes of shielding in the simulations. Finally, we show that on scales larger than individual giant molecular clouds, the primary condition that determines whether star formation occurs is whether a patch of the galactic disc is thermally Toomre-unstable (not whether it is self-shielding): once a patch can no longer be thermally stabilized against fragmentation, it collapses, becomes self-shielding, cools, and forms stars, regardless of epoch or environment.
AB - We present an analysis of the global and spatially resolved Kennicutt-Schmidt (KS) star formation relation in the FIRE (Feedback In Realistic Environments) suite of cosmological simulations, including haloes with z = 0 masses ranging from 1010 to 1013 M⊙.We show that the KS relation emerges and is robustly maintained due to the effects of feedback on local scales regulating star-forming gas, independent of the particular small-scale star formation prescriptions employed. We demonstrate that the time-averaged KS relation is relatively independent of redshift and spatial averaging scale, and that the star formation rate surface density is weakly dependent on metallicity and inversely dependent on orbital dynamical time. At constant star formation rate surface density, the 'cold and dense' gas surface density (gas with T < 300 K and n > 10 cm-3, used as a proxy for the molecular gas surface density) of the simulated galaxies is ~0.5 dex less than observed at ~kpc scales. This discrepancymay arise from underestimates of the local column density at the particle-scale for the purposes of shielding in the simulations. Finally, we show that on scales larger than individual giant molecular clouds, the primary condition that determines whether star formation occurs is whether a patch of the galactic disc is thermally Toomre-unstable (not whether it is self-shielding): once a patch can no longer be thermally stabilized against fragmentation, it collapses, becomes self-shielding, cools, and forms stars, regardless of epoch or environment.
KW - Galaxies: evolution
KW - Galaxies: formation
KW - Galaxies: star formation
KW - Instabilities
KW - Opacity -methods: numerical
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U2 - 10.1093/MNRAS/STY1241
DO - 10.1093/MNRAS/STY1241
M3 - Article
AN - SCOPUS:85050694753
SN - 0035-8711
VL - 478
SP - 3653
EP - 3673
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -