Cosmic CARNage I: on the calibration of galaxy formation models

Knebe, Alexander and Pearce, Frazer R. and Gonzalez-Perez, Violeta and Thomas, Peter A. and Benson, Andrew and Asquith, Rachel and Blaizot, Jeremy and Bower, Richard and Carretero, Jorge and Castander, Francisco J. and Cattaneo, Andrea and Cora, Sofía A. and Croton, Darren J. and Cui, Weiguang and Cunnama, Daniel and Devriendt, Julien E. and Elahi, Pascal J. and Font, Andreea and Fontanot, Fabio and Gargiulo, Ignacio D. and Helly, John and Henriques, Bruno and Lee, Jaehyun and Mamon, Gary A. and Onions, Julian and Padilla, Nelson D. and Power, Chris and Pujol, Arnau and Ruiz, Andrés N. and Srisawat, Chaichalit and Stevens, Adam R H and Tollet, Edouard and Vega-Martínez, Cristian A. and Yi, Sukyoung K. (2018) Cosmic CARNage I: on the calibration of galaxy formation models. Monthly Notices of the Royal Astronomical Society, 475 (3). pp. 2936-2954. ISSN 1365-2966

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Abstract

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 × 109h−1M ) 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 3σ. The second calibration extended the observational data to include the z = 2 SMF alongside the z ∼ 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.

Item Type: Article
Keywords: methods: analytical ; methods: numerical ; galaxies: evolution ; galaxies: haloes ; dark matter ; cosmology: theory.
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number: https://doi.org/10.1093/mnras/stx3274
Depositing User: Eprints, Support
Date Deposited: 13 Feb 2018 13:16
Last Modified: 14 Feb 2018 08:00
URI: http://eprints.nottingham.ac.uk/id/eprint/49764

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