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|Title:||The definition of environment and its relation to the quenching of galaxies at z = 1-2 in a hierarchical Universe||Authors:||Fossati, M.
Wilman, D. J.
DE LUCIA, GABRIELLA
Mendel, J. T.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||446||Issue:||3||First Page:||2582||Abstract:||A well-calibrated method to describe the environment of galaxies at all redshifts is essential for the study of structure formation. Such a calibration should include well-understood correlations with halo mass, and the possibility to identify galaxies which dominate their potential well (centrals), and their satellites. Focusing on z ̃ 1 and 2, we propose a method of environmental calibration which can be applied to the next generation of low- to medium-resolution spectroscopic surveys. Using an up-to-date semi-analytic model of galaxy formation, we measure the local density of galaxies in fixed apertures on different scales. There is a clear correlation of density with halo mass for satellite galaxies, while a significant population of low-mass centrals is found at high densities in the neighbourhood of massive haloes. In this case, the density simply traces the mass of the most massive halo within the aperture. To identify central and satellite galaxies, we apply an observationally motivated stellar mass rank method which is both highly pure and complete, especially in the more massive haloes where such a division is most meaningful. Finally, we examine a test case for the recovery of environmental trends: the passive fraction of galaxies and its dependence on stellar and halo mass for centrals and satellites. With careful calibration, observationally defined quantities do a good job of recovering known trends in the model. This result stands even with reduced redshift accuracy, provided the sample is deep enough to preserve a wide dynamic range of density.||Acknowledgments:||MF and DJW acknowledge the support of the Deutsche Forschungsgemeinschaft via Project ID 387/1-1. FF acknowledges financial contribution from the grants PRIN MIUR 2009 ‘The Intergalactic Medium as a probe of the growth of cosmic structures’ and PRIN INAF 2010 ‘From the dawn of galaxy formation’. GDL, MH and EC acknowledge financial support from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant under agreement no. 202781. PM has been supported by a FRA2012 grant of the University of Trieste and PRIN MIUR 2010-2011 J91J12000450001 ‘The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid’. MF thanks Gerard Lemson for help and advices in handling the G13 models, and Olga Cucciati, Michael Balogh, and Michael Cooper for comments which helped to improve the manuscript. We thank the anonymous referee for his/her comments that helped improving the quality of the paper.||URI:||http://hdl.handle.net/20.500.12386/23426||URL:||https://academic.oup.com/mnras/article/446/3/2582/2892436||ISSN:||0035-8711||DOI:||10.1093/mnras/stu2255||Bibcode ADS:||2015MNRAS.446.2582F||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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