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Gas flows in the circumgalactic medium around simulated high-redshift galaxies
Mitchell, Peter D,Blaizot, Jé,ré,my,Devriendt, Julien,Kimm, Taysun,Michel-Dansac, Lé,o,Rosdahl, Joakim,Slyz, Adrianne Blackwell Publishing Ltd 2018 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.474 No.4
nIFTy cosmology: comparison of galaxy formation models
Knebe, Alexander,Pearce, Frazer R.,Thomas, Peter A.,Benson, Andrew,Blaizot, Jeremy,Bower, Richard,Carretero, Jorge,Castander, Francisco J.,Cattaneo, Andrea,Cora, Sofia A.,Croton, Darren J.,Cui, Weigua Oxford University Press 2015 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.451 No.4
Cosmic CARNage I: on the calibration of galaxy formation models
Knebe, Alexander,Pearce, Frazer R,Gonzalez-Perez, Violeta,Thomas, Peter A,Benson, Andrew,Asquith, Rachel,Blaizot, Jeremy,Bower, Richard,Carretero, Jorge,Castander, Francisco J,Cattaneo, Andrea,Cora, S Oxford University Press 2018 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.475 No.3
<P>We present a comparison of nine galaxy formation models, eight semi-analytical, and one halo occupation distribution model, run on the same underlying cold dark matter simulation (cosmological box of comoving width 125h(-1) Mpc, with a dark-matter particle mass of 1.24 x 10(9) h(-1)M(circle dot)) and the same merger trees. While their free parameters have been calibrated to the same observational data sets using two approaches, they nevertheless retain some 'memory' of any previous calibration that served as the starting point (especially for the manually tuned models). For the first calibration, models reproduce the observed z = 0 galaxy stellar mass function (SMF) within 3 sigma The second calibration extended the observational data to include the z = 2 SMF alongside the z similar to 0 star formation rate function, cold gas mass, and the black hole bulge mass relation. Encapsulating the observed evolution of the SMF from z = 2 to 0 is found to be very hard within the context of the physics currently included in the models. We finally use our calibrated models to study the evolution of the stellar-to-halo mass (SHM) ratio. For all models, we find that the peak value of the SHM relation decreases with redshift. However, the trends seen for the evolution of the peak position as well as the mean scatter in the SHM relation are rather weak and strongly model dependent. Both the calibration data sets and model results are publicly available.</P>