The Void Galaxy Survey: Photometry, structure and identity of void galaxies

Abstract

We analyze photometry from deep B-band images of 59 void galaxies in the Void Galaxy Survey (VGS), together with their near-infrared 3.6$\mu$m and 4.5$\mu$m Spitzer photometry. The VGS galaxies constitute a sample of void galaxies that were selected by a geometric-topological procedure from the SDSS DR7 data release, and which populate the deep interior of voids. Our void galaxies span a range of absolute B-magnitude from ${\mathrm{M}}_{\mathrm{B}}=-15.5$ to ${\mathrm{M}}_{\mathrm{B}}=-20$, while at the 3.6$\mu$m band their magnitudes range from ${\mathrm{M}}_{3.6}=-18$ to ${\mathrm{M}}_{3.6}=-24$. Their B-[3.6] colour and structural parameters indicate these are star forming galaxies. A good reflection of the old stellar population, the near-infrared band photometry also provide a robust estimate of the stellar mass, which for the VGS galaxies we confirm to be smaller than $3\times 10^{10}$ M${}_{\odot }$. In terms of the structural parameters and morphology, our findings align with other studies in that our VGS galaxy sample consists mostly of small late-type galaxies. Most of them are similar to Sd-Sm galaxies, although a few are irregularly shaped galaxies. The sample even includes two early-type galaxies, one of which is an AGN. Their Sérsic indices are nearly all smaller than $n=2$ in both bands and they also have small half-light radii. In all, we conclude that the principal impact of the void environment on the galaxies populating them mostly concerns their low stellar mass and small size.

Accepted for publication in MNRAS, 16 pages, 11 figures

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