A comparison of galaxy group luminosity functions from semi-analytic models
Entity
UAM. Departamento de Física TeóricaPublisher
Royal Astronomical Society; Oxford University PressDate
2011-08-01Citation
10.1111/j.1365-2966.2011.18907.x
Monthly Notices of the Royal Astronomical Society 415.3 (2011): 2798-2811
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1111/j.1365-2966.2011.18907.xFunded by
ONS acknowledges the support of the STFC through its PhD Studentship Programme. BKG and CBB acknowledge the support of the UK Science & Technology Facilities Council (STFC Grant ST/F002432/1) and the Commonwealth Cosmology Initiative; visitor support (PS-B, DK, AK and LVS) from the STFC (ST/G003025/1) is similarly acknowledged. PS-B acknowledges the support of a Marie Curie Intra-European Fellowship within the 6th European Community Framework Programme. AK and PS-B are supported by the Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramón y Cajal programme. The Millennium Simulation data bases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. Access to the University of Central Lancashire’s High Performance Computing Facility is gratefully acknowledged. We acknowledge the computational support provided by the UK National Cosmology Supercomputer, COSMOS. We thank the DEISA consortium, cofunded through EU FP6 project RI-031513 and the FP7 project RI-222919, for support within the DEISA Extreme Computing InitiativeProject
info:eu-repo/grantAgreement/EC/FP7/222919Editor's Version
http://dx.doi.org/10.1111/j.1365-2966.2011.18907.xSubjects
Galaxies: clusters; Galaxies: formation; Galaxies: groups; Galaxies: haloes; Galaxies: luminosity function, mass function; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedRights
© 2011 RAS; © 2011 The Authors Monthly Notices of the Royal Astronomical SocietyAbstract
Semi-analytic models (SAMs) are currently one of the primary tools with which we model statistically significant ensembles of galaxies. The underlying physical prescriptions inherent to each SAM are, in many cases, different from one another. Several SAMs have been applied to the dark matter merger trees extracted from the Millennium Run, including those associated with the well-known Munich and Durham lineages. We compare the predicted luminosity distributions of galaxy groups using four publicly available SAMs, in order to explore a galactic environment in which the models have not been explored to the same degree as they have in the field or in rich clusters. We identify a characteristic 'wiggle' in the group galaxy luminosity function generated using the De Lucia et al. SAM, which is not present in the Durham-based models, consistent to some degree with observations. However, a comparison between conditional luminosity functions of groups between the models and observations suggests that neither model is a particularly good match. The luminosity function wiggle is interpreted as the result of the two-mode active galactic nucleus feedback implementation used in the Munich models, which itself results in flattened magnitude gap distribution. An associated analysis of the magnitude gap distribution between first- and second-ranked group galaxies shows that while the Durham models yield distributions with approximately equal luminosity first- and second-ranked galaxies, in agreement with observations, the De Lucia et al. models favour the scenario in which the second-ranked galaxy is approximately 1 mag fainter than the primary, especially when the dynamic range of the mock data is limited to 3 mag.
Files in this item
Google Scholar:Snaith, Owain N.
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Gibson, Brad K.
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Brook, Chris B.
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Courty, Stéphanie
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Sánchez-Blázquez, Patricia
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Kawata, Daisuke
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Knebe, Alexander
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Sales, Laura V.
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