A deep ALMA image of the Hubble Ultra Deep Field

By J. Dunlop, R. McLure, A. Biggs, James E. Geach, M. Michałowski, R. Ivison, W. Rujopakarn, E. V. Kampen, A. Kirkpatrick, Adrian Pope and 26 more. 2016

293 citations recorded by the source corpus.

We present the results of the first, deep Atacama Large Millimeter Array (ALMA) imaging covering the full ≃4.5 arcmin2 of the Hubble Ultra Deep Field (HUDF) imaged with Wide Field Camera 3/IR on HST. Using a 45-pointing mosaic, we have obtained a homogeneous 1.3-mm image reaching σ1.3 ≃ 35 μJy, at a resolution of ≃0.7 arcsec. From an initial list of ≃50 > 3.5σ peaks, a rigorous analysis confirms 16 sources with S1.3 > 120 μJy. All of these have secure galaxy counterparts with robust redshifts (〈z〉 = 2.15). Due to the unparalleled supporting data, the physical properties of the ALMA sources are well constrained, including their stellar masses (M*) and UV+FIR star formation rates (SFR). Our results show that stellar mass is the best predictor of SFR in the high-redshift Universe; indeed at z ≥ 2 our ALMA sample contains seven of the nine galaxies in the HUDF with M* ≥ 2 × 1010 M⊙, and we detect only one galaxy at z > 3.5, reflecting the rapid drop-off of high-mass galaxies with increasing redshift. The detections, coupled with stacking, allow us to probe the redshift/mass distribution of the 1.3-mm background down to S1.3 ≃ 10 μJy. We find strong evidence for a steep star-forming ‘main sequence’ at z ≃ 2, with SFR ∝M* and a mean specific SFR ≃ 2.2 Gyr−1. Moreover, we find that ≃85 per cent of total star formation at z ≃ 2 is enshrouded in dust, with ≃65 per cent of all star formation at this epoch occurring in high-mass galaxies (M* > 2 × 1010 M⊙), for which the average obscured:unobscured SF ratio is ≃200. Finally, we revisit the cosmic evolution of SFR density; we find this peaks at z ≃ 2.5, and that the star-forming Universe transits from primarily unobscured to primarily obscured at z ≃ 4.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7ccb9855f07f99d323d4f0523fefb51654db84ea

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Citations in the corpus

An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, methodology): “…ALMA has been used to undertake a number of typically deep continuum surveys of small contiguous fields (Hatsukade et al. 2016; Walter et al. 2016; Dunlop et al. 2017; Franco et al. 2018; Hatsukade et al. 2018; Muñoz Arancibia et al. 2018; Umehata et al. 2018), with areas of tens of arcmin2…”
Full-data Results of Hubble Frontier Fields: UV Luminosity Functions at z ∼ 6–10 and a Consistent Picture of Cosmic Reionization (2017, unknown): “In Figure 8, we include total ρUV at z ∼ 0 − 3 (Steidel et al. 1999; Wyder et al. 2005; Schiminovich et al. 2005; Reddy & Steidel 2009), and cosmic SFRDs at z ∼ 1 − 4 based on ρUV (Mtrunc = −15.0) and IR luminosity densities (the sensitivity corresponding to ≃ 30 µJy) (Dunlop et al. 2017).”
The MUSE Hubble Ultra Deep Field Survey: I. Survey description, data reduction and source detection (2017, background): “…Sciences A1, page 1 of 20 including for example Chandra (Xue et al. 2011; Luo et al. 2017), XMM (Comastri et al. 2011), ALMA (Walter et al. 2016; Dunlop et al. 2017), Spitzer/IRAC (Labbé et al. 2015), and the VLA (Kellermann et al. 2008; Rujopakarn et al. 2016), the field is also covered at all…”
PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, methodology): “For the 1mm photometry samples (Scoville et al. 2016, DeCarli et al. 2016, Dunlop et al. 2017, Barro et al. 2016, Tadaki et al. 2017, S. Lilly, priv.comm.) the detection fractions are about 0.65, 0.53 and 0.4 for ≥3, ≥4 and ≥5σ significance.”
An Extreme Protocluster of Luminous Dusty Starbursts in the Early Universe (2017, background): “…ultra-deep ALMA continuum map at 2 mm represents a significant overdensity of DSFGs when compared with the most recent ALMA counts (Aravena et al. 2016; Oteo et al. 2016a; Dunlop et al. 2017) because only 1-2 DSFGs brighter than the faintest DRC component would be expected, and we have 11 of them.”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, background): “Several studies have reported spatial offsets between ALMA-detected objects and their HST-counterparts either due to astrometry uncertainties or physical offsets in different wavelengths (e.g., Laporte et al. 2017; González-López et al. 2017; Carniani et al. 2018b; Dunlop et al. 2017).”
GOODS-ALMA: 1.1 mm galaxy survey (2018, methodology): “As the GOODS–South Field encompasses the Hubble Ultra Deep Field (HUDF), we take advantage of deep 1.3-mm ALMA data of the HUDF.”
The Star Formation Main Sequence in the Hubble Space Telescope Frontier Fields (2017, background): “Recently, the analysis of Dunlop et al. (2017) (see also Koprowski et al. 2016) ascribes the observed flattening at z & 2 to the inability of correctly recovering the SFR in deeply obscured high-mass galaxies when rest-frame optical/UV tracers are adopted (although some of the works above are based…”
The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, methodology): “…galaxies have been made possible with facilities such as the Atacama Large Millimeter Array (ALMA), allowing for direct measurements of either the dust continuum or far-IR spectral features for more typical star-forming galaxies in the distant universe (Carilli & Walter 2013; Dunlop et al. 2017).”