期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 434, 期 4, 页码 3348-3367出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt1245
关键词
methods: numerical; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: fundamental parameters; galaxies: haloes; galaxies: structure
资金
- National Natural Science Foundation of China [11250110509]
- ERC [267291]
- STFC [246797]
- Southern California Center for Galaxy Evolution, a multicampus research programme
- University of California Office of Research
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- European Research Council (ERC) [267291] Funding Source: European Research Council (ERC)
- STFC [ST/I00162X/1, ST/I001166/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/I00162X/1, ST/I001166/1] Funding Source: researchfish
We have combined the semi-analytic galaxy formation model of Guo et al. with the particle-tagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of similar to 1900 massive dark matter haloes (10(12)-10(14)M(circle dot)) from the Millennium II Lambda cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of Milky Way-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a Sersic profile, the radial scale and amplitude of which vary systematically with halo mass (M-200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M-200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M-star and M-200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z approximate to 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly.
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