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Home List of Titles The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation
Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/223401
- The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation
- Scannapieco, C.; Wadepuhl, M.; Parry, O. H.; Navarro, J. F.; Jenkins, A.; Springel, V.; Teyssier, R.; Carlson, E.; Couchman, H. M. P.; Crain, R. A.; Dalla Vecchia, C.; Frenk, C. S.; Kobayashi, C.; Monaco, P.; Murante, G.; Okamoto, T.; Quinn, T.; Schaye, J.; Stinson, G. S.; Theuns, T.; Wadsley, J.; White, S. D. M.; Woods, R.
- We compare the results of various cosmological gas-dynamical codes used to simulate the formation of a galaxy in the Λ cold dark matter structure formation paradigm. The various runs (13 in total) differ in their numerical hydrodynamical treatment [smoothed particle hydrodynamics (SPH), moving mesh and adaptive mesh refinement] but share the same initial conditions and adopt in each case their latest published model of gas cooling, star formation and feedback. Despite the common halo assembly history, we find large code-to-code variations in the stellar mass, size, morphology and gas content of the galaxy at z= 0, due mainly to the different implementations of star formation and feedback. Compared with observation, most codes tend to produce an overly massive galaxy, smaller and less gas rich than typical spirals, with a massive bulge and a declining rotation curve. A stellar disc is discernible in most simulations, although its prominence varies widely from code to code. There is a well-defined trend between the effects of feedback and the severity of the disagreement with observed spirals. In general, models that are more effective at limiting the baryonic mass of the galaxy come closer to matching observed galaxy scaling laws, but often to the detriment of the disc component. Although numerical convergence is not particularly good for any of the codes, our conclusions hold at two different numerical resolutions. Some differences can also be traced to the different numerical techniques; for example, more gas seems able to cool and become available for star formation in grid-based codes than in SPH. However, this effect is small compared to the variations induced by different feedback prescriptions. We conclude that state-of-the-art simulations cannot yet uniquely predict the properties of the baryonic component of a galaxy, even when the assembly history of its host halo is fully specified. Developing feedback algorithms that can effectively regulate the mass of a galaxy without hindering the formation of high angular momentum stellar discs remains a challenge.
- Publication type
- Journal article
- Research centre
- Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing
- Monthly Notices of the Royal Astronomical Society, Vol. 423, no. 2 (Jun 2012), pp. 1726-1749
- Publication year
- FOR Code(s)
- 0201 Astronomical and Space Sciences
- Cosmology theory; Galaxy evolution; Galaxy formation; Numerical methods
- Wiley-Blackwell Publishing
- Publisher URL
- Copyright © 2012 The Authors. Monthly Notices of the Royal Astronomical Society copyright © 2012 RAS.
- Peer reviewed