The UV–optical colour dependence of galaxy clustering in the local universe

We measure the UV-optical colour dependence of galaxy clustering in the local Universe. Using the clean separation of the red and blue sequences made possible by the NUV - r colour-magnitude diagram, we segregate the galaxies into red, blue and intermediate `green' classes. We explore the clustering as a function of this segregation by removing the dependence on luminosity and by excluding edge-on galaxies as a means of a non-model dependent veto of highly extincted galaxies. We find that xi(r(p), pi) for both red and green galaxies shows strong redshift-space distortion on small scales - the `finger-of-God' effect, with green galaxies having a lower amplitude than is seen for the red sequence, and the blue sequence showing almost no distortion. On large scales, xi(r(p), pi) for all three samples show the effect of large-scale streaming from coherent infall. On scales of 1 h-1 Mpc \textless r(p) \textless 10 h-1 Mpc, the projected auto-correlation function w(p)(r(p)) for red and green galaxies fits a power law with slope gamma similar to 1.93 and amplitude r(0) similar to 7.5 and 5.3, compared with gamma similar to 1.75 and r(0) similar to 3.9 h-1 Mpc for blue sequence galaxies. Compared to the clustering of a fiducial L* galaxy, the red, green and blue have a relative bias of 1.5, 1.1 and 0.9, respectively. The w(p)(r(p)) for blue galaxies display an increase in convexity at similar to 1 h-1 Mpc, with an excess of large-scale clustering. Our results suggest that the majority of blue galaxies are likely central galaxies in less massive haloes, while red and green galaxies have larger satellite fractions, and preferentially reside in virialized structures. If blue sequence galaxies migrate to the red sequence via processes like mergers or quenching that take them through the green valley, such a transformation may be accompanied by a change in environment in addition to any change in luminosity and colour.