We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

Cosmic CARNage I : on the calibration of galaxy formation models.

Knebe, A. and Pearce, F. R. and Gonzalez-Perez, V. and Thomas, P. A. and Benson, A. and Asquith, R. and Blaizot, J. and Bower, R. and Carretero, J. and Castander, F. J. and Cattaneo, A. and Cora, S. A. and Croton, D. J. and Cui, W. and Cunnama, D. and Devriendt, J. E. and Elahi, P. J. and Font, A. and Fontanot, F. and Gargiulo, I. D. and Helly, J. and Henriques, B. and Lee, J. and Mamon, G. A. and Onions, J. and Padilla, N. D. and Power, C. and Pujol, A. and Ruiz, A. N. and Srisawat, C. and Stevens, A. R. H. and Tollet, E. and Vega-Martínez, C. A. and Yi, S. K. (2018) 'Cosmic CARNage I : on the calibration of galaxy formation models.', Monthly notices of the Royal Astronomical Society., 475 (3). pp. 2936-2954.


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
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:15 December 2017
Date deposited:06 April 2018
Date of first online publication:20 December 2017
Date first made open access:06 April 2018

Save or Share this output

Look up in GoogleScholar