AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES

By J. Simpson, A. M. Swinbank, I. Smail, D. M. Alexander, W. N. Brandt, F. Bertoldi, C. De Breuck, S. Chapman, K. Coppin, E. D. Da Cunha and 14 more. 2013

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We present the first photometric redshift distribution for a large sample of 870 μm submillimeter galaxies (SMGs) with robust identifications based on observations with ALMA. In our analysis we consider 96 SMGs in the Extended Chandra Deep Field South, 77 of which have 4–19 band photometry. We model the SEDs for these 77 SMGs, deriving a median photometric redshift of zphot = 2.3 ± 0.1. The remaining 19 SMGs have insufficient photometry to derive photometric redshifts, but a stacking analysis of Herschel observations confirms they are not spurious. Assuming that these SMGs have an absolute H-band magnitude distribution comparable to that of a complete sample of z ∼ 1–2 SMGs, we demonstrate that they lie at slightly higher redshifts, raising the median redshift for SMGs to zphot = 2.5 ± 0.2. Critically we show that the proportion of galaxies undergoing an SMG-like phase at z ⩾ 3 is at most 35% ± 5% of the total population. We derive a median stellar mass of M⋆ = (8 ± 1) × 1010 M☉, although there are systematic uncertainties of up to 5 × for individual sources. Assuming that the star formation activity in SMGs has a timescale of ∼100 Myr, we show that their descendants at z ∼ 0 would have a space density and MH distribution that are in good agreement with those of local ellipticals. In addition, the inferred mass-weighted ages of the local ellipticals broadly agree with the look-back times of the SMG events. Taken together, these results are consistent with a simple model that identifies SMGs as events that form most of the stars seen in the majority of luminous elliptical galaxies at the present day.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/346a3a2bf7c69874ba72b0429f481cee0c6f47c0

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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): “We derive a median dust mass for the full AS2UDS sample of Md = (6.8 ± 0.3) × 108 M with a 68th percentile range of Md = (3.0–12.6) × 108 M , which broadly agrees with the median estimated for the ALESS sample: Md = (5.6 ± 0.1) × 108 M (da Cunha et al. 2015).”
AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “In order to account for possible zero point offsets and/or mismatches between the photometry at different wavelengths, we add a magnitude error in quadrature to the quoted errors that is proportional to the photometric offsets determined by Simpson et al. (2014).”
GOODS-ALMA: 1.1 mm galaxy survey (2018, background): “> 7× 1010M ; e.g. Chapman et al. 2005; Hainline et al. 2011; Simpson et al. 2014), 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…”
The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, background): “…optical–infrared (U, g, B, V, R, I, z, J, K and IRAC: 3.6 and 4.5 µm) imaging (Cirasuolo et al. 2007; Lawrence et al. 2007; Hambly et al. 2008; Williams et al. 2009; Cardamone et al. 2010; Kim et al. 2011a; Muzzin et al. 2013a; Simpson et al. 2014; Sobral et al. 2015 and references therein).”
KILOPARSEC-SCALE DUST DISKS IN HIGH-REDSHIFT LUMINOUS SUBMILLIMETER GALAXIES (2016, methodology): “…(corresponding to signal–to– noise (S/N) values of 3.8 and 4.2) in the Cycle 0 catalog, respectively, and based on the multi-wavelength data presented in Simpson et al. (2014), it is possible that ALESS 15.3 was spurious and ALESS 67.2 has been resolved out (see Chen et al. 2016, in preparation).”