Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
Volume 30, Issue -, Pages -Publisher
CAMBRIDGE UNIV PRESS
DOI: 10.1017/pasa.2013.16
Keywords
dark matter; Local Group; methods: miscellaneous
Categories
Funding
- Deustche Forschungs Gemeinschaft (DFG)
- Spanish Ministerio de Ciencia e Innovacion (MICINN) in Spain [AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009-00064, CAM S2009/ESP-1496]
- Ministerio de Economia y Competitividad (MINECO) [AYA2012-31101]
- MINECO [AYA 2009-13875-C03-02, CSD2007-0050, AYA 2012-31101]
- Comunidad de Madrid through ASTROMADRID project [CAM S2009/ESP-1496]
- ISF [1013/12]
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The differences between cold dark matter (CDM) and warm dark matter (WDM) in the formation of a group of galaxies are examined by running two identical simulations, where in the WDM case the initial power spectrum has been altered to mimic a 1-keV dark matter particle. The CDM initial conditions were constrained to reproduce at z = 0 the correct local environment within which a 'Local Group' (LG) of galaxies may form. Two significant differences between the two simulations are found. While in the CDM case a group of galaxies that resembles the real LG forms, the WDM run fails to reproduce a viable LG, instead forming a diffuse group which is still expanding at z = 0. This is surprising since, due to the suppression of small-scale power in its power spectrum, WDM is naively expected to only affect the collapse of small haloes and not necessarily the dynamics on a scale of a group of galaxies. Furthermore, the concentration of baryons in halo centre is greater in CDM than in WDM and the properties of the discs differ.
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