Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models

Q. Guo, V. Gonzalez-Perez, M. Schaller, M. Furlong, R.G. Bower, S. Cole, R.A. Crain, C.S. Frenk, J.C. Helly, C.G. Lacey, Claudia Lagos Urbina, P. Mitchell, J. Schaye, T. Theuns

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Abstract

© 2016 The Authors.We compare global predictions from the EAGLE hydrodynamical simulation, and two semianalytic (SA) models of galaxy formation, L-GALAXIES and GALFORM. All three models include the key physical processes for the formation and evolution of galaxies and their parameters are calibrated against a small number of observables at z ˜ 0. The two SA models have been applied to merger trees constructed from the EAGLE dark matter only simulation. We find that at z = 2, both the galaxy stellar mass functions for stellar masses M* <1010.5M? and the median specific star formation rates (sSFRs) in the three models agree to better than 0.4 dex. The evolution of the sSFR predicted by the three models closely follows the mass assembly history of dark matter haloes. In both EAGLE and L-GALAXIES there are more central passive galaxies with M* <109.5M? than in GALFORM. This difference is related to galaxies that have entered and then left a larger halo and which are treated as satellites in GALFORM. In the range 0 <z <1, the slope of the evolution of the star formation rate density in EAGLE is a factor of ˜1.5 steeper than for the two SA models. The median sizes for galaxies with M* > 109.5M? differ in some instances by an order of magnitude, while the stellar mass-size relation in EAGLE is a factor of ˜2 tighter than for the two SA models. Our results suggest the need for a revision of how SA models treat the effect of baryonic self-gravity on the underlying dark matter. The treatment of gas flows in the models needs to be revised based on detailed comparison with observations to understand in particular the evolution of the stellar mass-metallicity relation.
Original languageEnglish
Pages (from-to)3457-3482
Number of pages26
JournalMonthly Notices of the Royal Astronomical Society
Volume461
Issue number4
DOIs
Publication statusPublished - 2016

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galaxies
stellar mass
simulation
dark matter
galactic evolution
gas flow
merger
metallicity
gravity
gravitation
prediction
predictions

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Guo, Q., Gonzalez-Perez, V., Schaller, M., Furlong, M., Bower, R. G., Cole, S., ... Theuns, T. (2016). Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models. Monthly Notices of the Royal Astronomical Society, 461(4), 3457-3482. https://doi.org/10.1093/mnras/stw1525
Guo, Q. ; Gonzalez-Perez, V. ; Schaller, M. ; Furlong, M. ; Bower, R.G. ; Cole, S. ; Crain, R.A. ; Frenk, C.S. ; Helly, J.C. ; Lacey, C.G. ; Lagos Urbina, Claudia ; Mitchell, P. ; Schaye, J. ; Theuns, T. / Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 461, No. 4. pp. 3457-3482.
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author = "Q. Guo and V. Gonzalez-Perez and M. Schaller and M. Furlong and R.G. Bower and S. Cole and R.A. Crain and C.S. Frenk and J.C. Helly and C.G. Lacey and {Lagos Urbina}, Claudia and P. Mitchell and J. Schaye and T. Theuns",
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Guo, Q, Gonzalez-Perez, V, Schaller, M, Furlong, M, Bower, RG, Cole, S, Crain, RA, Frenk, CS, Helly, JC, Lacey, CG, Lagos Urbina, C, Mitchell, P, Schaye, J & Theuns, T 2016, 'Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models' Monthly Notices of the Royal Astronomical Society, vol. 461, no. 4, pp. 3457-3482. https://doi.org/10.1093/mnras/stw1525

Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models. / Guo, Q.; Gonzalez-Perez, V.; Schaller, M.; Furlong, M.; Bower, R.G.; Cole, S.; Crain, R.A.; Frenk, C.S.; Helly, J.C.; Lacey, C.G.; Lagos Urbina, Claudia; Mitchell, P.; Schaye, J.; Theuns, T.

In: Monthly Notices of the Royal Astronomical Society, Vol. 461, No. 4, 2016, p. 3457-3482.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Galaxies in the EAGLE hydrodynamical simulation and in the Durham and Munich semi-analytical models

AU - Guo, Q.

AU - Gonzalez-Perez, V.

AU - Schaller, M.

AU - Furlong, M.

AU - Bower, R.G.

AU - Cole, S.

AU - Crain, R.A.

AU - Frenk, C.S.

AU - Helly, J.C.

AU - Lacey, C.G.

AU - Lagos Urbina, Claudia

AU - Mitchell, P.

AU - Schaye, J.

AU - Theuns, T.

PY - 2016

Y1 - 2016

N2 - © 2016 The Authors.We compare global predictions from the EAGLE hydrodynamical simulation, and two semianalytic (SA) models of galaxy formation, L-GALAXIES and GALFORM. All three models include the key physical processes for the formation and evolution of galaxies and their parameters are calibrated against a small number of observables at z ˜ 0. The two SA models have been applied to merger trees constructed from the EAGLE dark matter only simulation. We find that at z = 2, both the galaxy stellar mass functions for stellar masses M* <1010.5M? and the median specific star formation rates (sSFRs) in the three models agree to better than 0.4 dex. The evolution of the sSFR predicted by the three models closely follows the mass assembly history of dark matter haloes. In both EAGLE and L-GALAXIES there are more central passive galaxies with M* <109.5M? than in GALFORM. This difference is related to galaxies that have entered and then left a larger halo and which are treated as satellites in GALFORM. In the range 0 109.5M? differ in some instances by an order of magnitude, while the stellar mass-size relation in EAGLE is a factor of ˜2 tighter than for the two SA models. Our results suggest the need for a revision of how SA models treat the effect of baryonic self-gravity on the underlying dark matter. The treatment of gas flows in the models needs to be revised based on detailed comparison with observations to understand in particular the evolution of the stellar mass-metallicity relation.

AB - © 2016 The Authors.We compare global predictions from the EAGLE hydrodynamical simulation, and two semianalytic (SA) models of galaxy formation, L-GALAXIES and GALFORM. All three models include the key physical processes for the formation and evolution of galaxies and their parameters are calibrated against a small number of observables at z ˜ 0. The two SA models have been applied to merger trees constructed from the EAGLE dark matter only simulation. We find that at z = 2, both the galaxy stellar mass functions for stellar masses M* <1010.5M? and the median specific star formation rates (sSFRs) in the three models agree to better than 0.4 dex. The evolution of the sSFR predicted by the three models closely follows the mass assembly history of dark matter haloes. In both EAGLE and L-GALAXIES there are more central passive galaxies with M* <109.5M? than in GALFORM. This difference is related to galaxies that have entered and then left a larger halo and which are treated as satellites in GALFORM. In the range 0 109.5M? differ in some instances by an order of magnitude, while the stellar mass-size relation in EAGLE is a factor of ˜2 tighter than for the two SA models. Our results suggest the need for a revision of how SA models treat the effect of baryonic self-gravity on the underlying dark matter. The treatment of gas flows in the models needs to be revised based on detailed comparison with observations to understand in particular the evolution of the stellar mass-metallicity relation.

U2 - 10.1093/mnras/stw1525

DO - 10.1093/mnras/stw1525

M3 - Article

VL - 461

SP - 3457

EP - 3482

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -