2013ApJ...769..116H

We use Wide-field Infrared Survey Explorer (WISE), AKARI, and Galaxy Evolution Explorer (GALEX) data to select local analogs of high-redshift (z ∼ 2) dust obscured galaxies (DOGs). We identify 47 local DOGs with S_12 µm_/S0.22 µm_ ≥ 892 and S_12 µm_> 20 mJy at 0.05 < z < 0.08 in the Sloan Digital Sky Survey data release 7. The infrared (IR) luminosities of these DOGs are in the range 3.4x10¹⁰ (L_☉) ≲ L_IR ≲ 7.0x10¹¹ (L_☉) with a median L_IR of 2.1x10¹¹ (L_☉). We compare the physical properties of local DOGs with a control sample of galaxies that have lower S_12 µm_/S0.22 µm_ but have similar redshift, IR luminosity, and stellar mass distributions. Both WISE 12 µm and GALEX near-ultraviolet (NUV) flux densities of DOGs differ from the control sample of galaxies, but the difference is much larger in the NUV. Among the 47 DOGs, 36%±7% have small axis ratios in the optical (i.e., b/a < 0.6), larger than the fraction among the control sample (17%±3%). There is no obvious sign of interaction for many local DOGs. No local DOGs have companions with comparable optical magnitudes closer than ∼50 kpc. The large- and small-scale environments of DOGs are similar to the control sample. Many physical properties of local DOGs are similar to those of high-z DOGs, even though the IR luminosities of local objects are an order of magnitude lower than for the high-z objects: the presence of two classes (active galactic nuclei- and star formation-dominated) of DOGs, abnormal faintness in the UV rather than extreme brightness in the mid-IR, and diverse optical morphology. These results suggest a common underlying physical origin of local and high-z DOGs. Both seem to represent the high-end tail of the dust obscuration distribution resulting from various physical mechanisms rather than a unique phase of galaxy evolution.