An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs

By M. Swinbank, J. Simpson, I. Smail, C. Harrison, J. Hodge, A. Karim, F. Walter, D. M. Alexander, N. Brandt, C. De Breuck and 28 more. Monthly notices of the Royal Astronomical Society, 2013

265 citations recorded by the source corpus.

We exploit Atacama Large Millimeter Array (ALMA) 870 mu m observations of sub-millimetre sources in the Extended Chandra Deep Field South to investigate the far-infrared properties of high-redshift sub-millimetre galaxies (SMGs). Using the precisely located 870 mu m ALMA positions of 99 SMGs, together with 24 mu m and radio imaging, we deblend the Herschel/SPIRE imaging to extract their far-infrared fluxes and colours. The median redshifts for ALMA LESS (ALESS) SMGs which are detected in at least two SPIRE bands increases with wavelength of the peak in their spectral energy distributions (SEDs), with z = 2.3 +/- 0.2, 2.5 +/- 0.3 and 3.5 +/- 0.5 for the 250, 350 and 500 mu m peakers, respectively. 34 ALESS SMGs do not have a >3 sigma counterpart at 250, 350 or 500 mu m. These galaxies have a median photometric redshift derived from the rest-frame UV-mid-infrared SEDs of z = 3.3 +/- 0.5, which is higher than the full ALESS SMG sample; z = 2.5 +/- 0.2. We estimate the far-infrared luminosities and characteristic dust temperature of each SMG, deriving L-IR = (3.0 +/- 0.3) x 10(12) L-circle dot (SFR = 300 +/- 30 M-circle dot yr(-1)) and T-d = 32 +/- 1 K. The characteristic dust temperature of these high-redshift SMGs is Delta T-d = 3-5K lower than comparably luminous galaxies at z = 0, reflecting the more extended star formation in these systems. We show that the contribution of S-870 mu m >= 1 mJy SMGs to the cosmic star formation budget is 20 per cent of the total over the redshift range z similar to 1-4. Adopting an appropriate gas-to-dust ratio, we estimate a typical molecular mass of the ALESS SMGs of M-H2 = (4.2 +/- 0.4) x 10(10) M-circle dot. Finally, we show that SMGs with S-870 mu m > 1 mJy (L-IR greater than or similar to 10(12) L-circle dot) contain similar to 10 per cent of the z similar to 2 volume-averaged H-2 mass density.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/14a9f47e67fb08872f1ea316d3f2c979494e542f

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In Astronomy and Astrophysics

1. D. M. Alexander
2. P. Hopkins
3. L. Hernquist
4. D. Narayanan
5. C. Casey
6. R. Dav'e
7. F. Walter
8. E. Daddi

In Instrumentation

1. D. M. Alexander
2. P. Hopkins
3. Mark Dickinson
4. D. Narayanan
5. E. Daddi
6. C. Casey
7. R. Dav'e
8. L. Hernquist

Citations in the corpus

• AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “…the redshifts and physical properties of the ALESS SMGs, and also highlight the effect of fitting the whole SED simultaneously versus fitting only the stellar emission or only the infrared emission as done in previous studies of these SMGs (e.g., Simpson et al. 2014; Swinbank et al. 2014).”
• An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, methodology): “The uncertainties on the flux densities (and limits) are found by attempting to recover fake sources injected into the maps (see Swinbank et al. 2014 for details), and the typical 3σ detection limits are 7.0, 8.0, and 10.6 mJy at 250, 350, and 500 μm, respectively.”
• Dusty Star Forming Galaxies at High Redshift (2014, methodology): “A few high-z SMGs which have CO(1–0) observations (Ivison et al., 2011) have also been used to calibrate galaxies’ gas-to-dust ratio ∼100, which has been subsequently used to estimate some high-z DSFGs’ gas masses (e.g. Swinbank et al., 2014).”
• GOODS-ALMA: 1.1 mm galaxy survey (2018, background): “…gas-rich (fgas > 50%; e.g. Daddi et al. 2010), with huge star formation rates (SFR) - often greater than 100 M year−1 (e.g. Magnelli et al. 2012; Swinbank et al. 2014) - making them significant contributors to the cosmic star formation (e.g. Casey et al. 2013), often driven by mergers (e.g.…”
• Molecular hydrogen abundances of galaxies in the EAGLE simulations (2015, methodology): “There is also a wealth of literature using dust mass as a proxy for H2 mass through the dust-to-gas mass ratio dependence on metallicity (e.g. Boselli, Lequeux & Gavazzi 2002; Santini et al. 2014; Swinbank et al. 2014; Béthermin et al. 2015).”
• The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “…et al. 2013; De Breuck et al. 2014; Carniani et al. 2013; Carilli et al. 2013; Willott et al. 2013, 2015) to trace obscured star formation (e.g. Swinbank et al. 2014; Gallerani et al. 2012; Negrello et al. 2010; Hezaveh et al. 2013; Schaerer et al. 2015a), and even to trace AGNs and their…”
• AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES (2013, methodology): “These data are described in Swinbank et al. (2014), the companion paper to this work studying the far-infrared properties of the ALESS SMGs.”
• A remarkably flat relationship between the average star formation rate and AGN luminosity for distant X-ray AGN. (2015, methodology): “Therefore for the 24 μm undetected sources, we extracted the FIR photometry at the optical counterpart positions following the method described in Swinbank et al. (2014).”