@article{
 title = {Galaxy bimodality versus stellar mass and environment},
 type = {article},
 year = {2006},
 identifiers = {[object Object]},
 keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: luminosity function,mass function},
 pages = {469-483},
 volume = {373},
 websites = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2006.11081.x},
 month = {12},
 day = {1},
 id = {40e8a2da-8f34-3578-8646-d10afd2a494e},
 created = {2017-05-30T17:46:56.769Z},
 accessed = {2016-08-02},
 file_attached = {true},
 profile_id = {117ca603-cac1-3ce1-9f60-a761cb678261},
 group_id = {5a95a0b6-1946-397c-b16a-114c6fdf3127},
 last_modified = {2017-05-31T00:23:52.100Z},
 read = {false},
 starred = {false},
 authored = {false},
 confirmed = {true},
 hidden = {false},
 citation_key = {Baldry2006},
 folder_uuids = {a55b3938-9553-4705-9661-67c5f054d79a},
 private_publication = {false},
 abstract = {We analyse a z<0.1 galaxy sample from the Sloan Digital Sky Survey focusing on the variation of the galaxy colour bimodality with stellar mass and projected neighbour density Sigma, and on measurements of the galaxy stellar mass functions. The characteristic mass increases with environmental density from about 10^10.6 Msun to 10^10.9 Msun (Kroupa IMF, H_0=70) for Sigma in the range 0.1--10 per Mpc^2. The galaxy population naturally divides into a red and blue sequence with the locus of the sequences in colour-mass and colour-concentration index not varying strongly with environment. The fraction of galaxies on the red sequence is determined in bins of 0.2 in log Sigma and log mass (12 x 13 bins). The red fraction f_r generally increases continuously in both Sigma and mass such that there is a unified relation: f_r = F(Sigma,mass). Two simple functions are proposed which provide good fits to the data. These data are compared with analogous quantities in semi-analytical models based on the Millennium N-body simulation: the Bower et al. (2006) and Croton et al. (2006) models that incorporate AGN feedback. Both models predict a strong dependence of the red fraction on stellar mass and environment that is qualitatively similar to the observations. However, a quantitative comparison shows that the Bower et al. model is a significantly better match; this appears to be due to the different treatment of feedback in central galaxies.},
 bibtype = {article},
 author = {Baldry, I. K. and Balogh, M. L. and Bower, R. G. and Glazebrook, K. and Nichol, R. C. and Bamford, S. P. and Budavari, T.},
 journal = {Monthly Notices of the Royal Astronomical Society},
 number = {2}
}

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The characteristic mass increases with environmental density from about 10^10.6 Msun to 10^10.9 Msun (Kroupa IMF, H_0=70) for Sigma in the range 0.1--10 per Mpc^2. The galaxy population naturally divides into a red and blue sequence with the locus of the sequences in colour-mass and colour-concentration index not varying strongly with environment. The fraction of galaxies on the red sequence is determined in bins of 0.2 in log Sigma and log mass (12 x 13 bins). The red fraction f_r generally increases continuously in both Sigma and mass such that there is a unified relation: f_r = F(Sigma,mass). Two simple functions are proposed which provide good fits to the data. These data are compared with analogous quantities in semi-analytical models based on the Millennium N-body simulation: the Bower et al. (2006) and Croton et al. (2006) models that incorporate AGN feedback. 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