4.1 Article

Hyper-luminous dust-obscured galaxies discovered by the Hyper Suprime-Cam on Subaru and WISE

Journal

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/pasj/psv057

Keywords

catalogs; galaxies: active; galaxies: luminosity function, mass function; infrared: galaxies; methods: statistical

Funding

  1. National Aeronautics and Space Administration
  2. Research Coordination Committee, National Astronomical Observatory of Japan (NAOJ)
  3. National Aeronautics and Space Administration [NNX08AR22G]
  4. National Science Foundation [AST-1238877]
  5. Japan Society for the Promotion of Science [25707010]
  6. Yamada Science Foundation
  7. World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan
  8. Grants-in-Aid for Scientific Research [15K05030, 15H02070, 26400228, 23540273, 25707010] Funding Source: KAKEN

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We present the photometric properties of a sample of infrared (IR) bright dust-obscured galaxies (DOGs). Combining wide and deep optical images obtained with the Hyper Suprime-Cam on the Subaru Telescope and all-skymid-IR (MIR) images taken with Wide-Field Infrared Survey Explorer, we discovered 48 DOGs with i-K-s > 1.2 and i-[22] > 7.0, where i, K-s, and [22] represent AB magnitude in the i-band, K-s-band, and 22 mu m, respectively, in the GAMA 14 hr field (similar to 9 deg(2)). Among these objects, 31 (similar to 65%) show power-law spectral energy distributions (SEDs) in the near-IR (NIR) and MIR regime, while the remainder show an NIR bump in their SEDs. Assuming that the redshift distribution for our DOGs sample is Gaussian, with mean and sigma z = 1.99 +/- 0.45, we calculated their total IR luminosity using an empirical relation between 22 mu m luminosity and total IR luminosity. The average value of the total IR luminosity is (3.5 +/- 1.1) x 10(13) L circle dot, which classifies them as hyper-luminous infrared galaxies. We also derived the total IR luminosity function (LF) and IR luminosity density (LD) for a flux-limited subsample of 18 DOGs with 22 mu m flux greater than 3.0 mJy and with i-band magnitude brighter than 24 AB magnitude. The derived space density for this subsample is log phi = -6.59 +/- 0.11 [Mpc(-3)]. The IR LF for DOGs including data obtained from the literature is fitted well by a double-power law. The derived lower limit for the IR LD for our sample is rho(IR) similar to 3.8 x 10(7) [L circle dot Mpc(-3]) and its contributions to the total IR LD, IR LD of all ultra-luminous infrared galaxies, and that of all DOGs are > 3%, > 9%, and > 15%, respectively.

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