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Galaxy And Mass Assembly (GAMA) : the bright void galaxy population in the optical and mid IR

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Figure

Figure 1. The effect of limiting magnitude on void size. Galaxies with Mr < 20.09 are more strongly clustered than those with −18.00 < Mr < −20.09, andvoids therefore appear larger when using a brighter magnitude cut to define their limits.
Figure 2. Large-scale structure in the GAMA fields (blue points) overlaid on an 10 h−1 Mpc slice of SDSS
Table 1. The distribution of void galaxies withequatorial GAMA fields. Due to SDSS spectroscopic incompleteness in theG09 region, we remove void galaxies in this region with Mr = −18.4 over the three δ < 0◦ to removethe effect of ‘false’ voids appearing in this undersampled region.
Figure 4. Colour–mass relation for GAMA void galaxies (purple stars). The left-hand panel shows rest-frame (and corrected for foreground extinction
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