2013/08/31 by Chian-Chou Chen, Lennox L. Cowie, L. L. Cowie +9
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #COSMIC cancer database #Cosmic infrared background #Cosmic microwave background #Extragalactic background light #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Infrared #James Clerk Maxwell Telescope #Optics #Physics #Range (aeronautics) #Redshift #Star formation #Telescope #Wavelength #astro-ph.CO
paper · pdf · doi:10.1088/0004-637x/776/2/131
update fig14 with bugs fixed, 14 pages, 14 figures, ApJ in press
arxiv created 2013/09/12 · openalex publication_date 2013/10/07 · arxiv updated 2015/06/17 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We use the SCUBA-2 submillimeter camera mounted on the James Clerk Maxwell Telescope to obtain extremely deep number counts at 450 and 850 μm. We combine data on two cluster lensing fields, A1689 and A370, and three blank fields, CDF-N, CDF-S, and COSMOS, to measure the counts over a wide flux range at each wavelength. We use statistical fits to broken power law representations to determine the number counts. This allows us to probe to the deepest possible level in the data. At both wavelengths our results agree well with the literature in the flux range over which they have been measured, with the exception of the 850 μm counts in CDF-S, where we do not observe the counts deficit found by previous single-dish observations. At 450 μm, we detect significant counts down to ∼1 mJy, an unprecedented depth at this wavelength. By integrating the number counts above this flux limit, we measure Jy deg −2 of the 450 μm extragalactic background light (EBL). The majority of this contribution is from sources with S 450 μm between 1–10 mJy, and these sources are likely to be the ones that are analogous to the local luminous infrared galaxies. At 850 μm, we measure Jy deg −2 of the EBL. Because of the large systematic uncertainties on the COBE measurements, the percentage of the EBL we resolve could range from 48%–153% (44%–178%) at 450 (850) μm. Based on high-resolution Submillimeter Array observations of around half of the 4 σ 850 μm sample in CDF-N, we find that 12.5 % of the sources are blends of multiple fainter sources. This is a low multiple fraction, and we find no significant difference between our original SCUBA-2 850 μm counts and the multiplicity-corrected counts.