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Binary active galactic nuclei (AGNs) provide clues to how gas-rich mergerstrigger and fuel AGNs and how supermassive black hole (SMBH) pairs evolve in agas-rich environment. While significant effort has been invested in theiridentification, the detailed properties of binary AGNs and their host galaxiesare still poorly constrained. In a companion paper, we examined the nature ofionizing sources in the double nuclei of four kpc-scale binary AGNs withredshifts between 0.1~0.2. Here, we present their host galaxy morphology basedon F336W (U-band) and F105W (Y-band) images taken by the Wide Field Camera 3(WFC3) onboard the Hubble Space Telescope. Our targets have double-peakednarrow emission lines and were confirmed to host binary AGNs with follow upobservations. We find that kpc-scale binary AGNs occur in galaxy mergers withdiverse morphological types. There are three major mergers with intermediatemorphologies and a minor merger with a dominant disk component. We estimate themasses of the SMBHs from their host bulge stellar masses and obtain Eddingtonratios for each AGN. Compared with a representative control sample drawn at thesame redshift and stellar mass, the AGN luminosities and Eddington ratios ofour binary AGNs are similar to those of single AGNs. The U-Y color mapsindicate that clumpy star forming regions could significantly affect the X-raydetection of binary AGNs, e.g., the hardness ratio. Considering the weak X-rayemission in AGNs triggered in merger systems, we suggest that samples of X-rayselected AGNs may be biased against gas-rich mergers.

astrophysical journal/the astrophysical journal

Chandra X-ray and Hubble Space Telescope Imaging of Optically Selected  Kiloparsec-Scale Binary Active Galactic Nuclei II: Host Galaxy Morphology and  AGN Activity