Details

Autor(en) / Beteiligte

• Cowie, L. L.
• Barger, A. J.
• Hsu, L.-Y.
• Chen, Chian-Chou
• Owen, F. N.
• Wang, W.-H.

Titel

A Submillimeter Perspective on the GOODS Fields (SUPER GOODS). I. An Ultradeep SCUBA-2 Survey of the GOODS-N

Ist Teil von

• The Astrophysical journal, 2017-03, Vol.837 (2), p.139

Ort / Verlag

Philadelphia: IOP Publishing

Erscheinungsjahr

2017

Quelle

EZB Free E-Journals

Beschreibungen/Notizen

• Abstract In this first paper in the SUPER GOODS series on powerfully star-forming galaxies in the two GOODS fields, we present a deep SCUBA-2 survey of the GOODS-N at both 850 and 450 μ m (central rms noise of 0.28 mJy and 2.6 mJy, respectively). In the central region, the 850 μ m observations cover the GOODS-N to near the confusion limit of ∼1.65 mJy, while over a wider 450 arcmin 2 region—well complemented by Herschel far-infrared imaging—they have a median limit of 3.5 mJy. We present catalogs of 186 850 μ m and 31 450 μ m selected sources. We use interferometric observations from the Submillimeter Array (SMA) and the Karl G. Jansky Very Large Array (VLA) to obtain precise positions for 114 SCUBA-2 sources (28 from the SMA, all of which are also VLA sources). We present new spectroscopic redshifts and include all existing spectroscopic or photometric redshifts. We also compare redshifts estimated using the 20 cm/850 μ m and the 250 cm/850 μ m flux ratios. We show that the redshift distribution increases with increasing flux, and we parameterize the dependence. We compute the star formation history and the star formation rate (SFR) density distribution functions in various redshift intervals, finding that they reach a peak at before dropping to higher redshifts. We show that the number density per unit volume of galaxies measured from the SCUBA-2 sample does not change much relative to that of lower SFR galaxies from UV selected samples over , suggesting that, apart from changes in the normalization, the shape in the number density as a function of SFR is invariant over this redshift interval.