期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 432, 期 2, 页码 1367-1374出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt556
关键词
methods: data analysis; large-scale structure of Universe; galaxies: statistics
资金
- Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET)
- Secretaria de Ciencia y Tecnologia, Universidad Nacional de Cordoba, Argentina
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
We analyse properties of galaxy groups and their dependence on the large-scale environment as defined by superstructures. We find that group-galaxy cross-correlations depend only on group properties regardless the groups reside in superstructures. This indicates that the total galaxy density profile around groups is independent of the global environment. At a given global luminosity, a proxy to group total mass, groups have a larger stellar mass content by a factor of 1.3, a relative excess independent of the group luminosity. Groups in superstructures have 40 per cent higher velocity dispersions and systematically larger minimal enclosing radii. We also find that the stellar population of galaxies in groups in superstructures is systematically older as inferred from the galaxy spectra Dn(4000) parameter. Although the galaxy number density profile of groups is independent of environment, the star formation rate and stellar mass profile of the groups residing in superstructures differ from groups elsewhere. For groups residing in superstructures, the combination of a larger stellar mass content and star formation rate produces a larger time-scale for star formation regardless the distance to the group centre. Our results provide evidence that groups in superstructures formed earlier than elsewhere, as expected in the assembly bias scenario.
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