AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING

By E. D. Cunha, F. Walter, I. Smail, M. Swinbank, J. Simpson, R. Decarli, J. Hodge, A. Weiss, P. Werf, F. Bertoldi and 8 more. 2015

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The ALESS survey has followed up on a sample of 122 sub-millimeter sources in the Extended Chandra Deep Field South at 870 μm with the Atacama Large Millimeter Array (ALMA), allowing us to pinpoint the positions of sub-millimeter galaxies (SMGs) to ∼0.3 arcsec and to find their precise counterparts at different wavelengths. This enabled the first compilation of the multi-wavelength spectral energy distributions (SEDs) of a statistically reliable survey of SMGs. In this paper, we present a new calibration of the magphys SED modeling code that is optimized to fit these ultraviolet-to-radio SEDs of z > 1 ?> star-forming galaxies using an energy balance technique to connect the emission from stellar populations, dust attenuation, and dust emission in a physically consistent way. We derive statistically and physically robust estimates of the photometric redshifts and physical parameters (such as stellar masses, dust attenuation, star formation rates (SFRs), and dust masses) for the ALESS SMGs. We find that the ALESS SMGs have median stellar mass M * = 8.9 ± 0.1 × 10 10 M ⊙ ?> , median SFR = 280 ± 70 M ⊙ yr − 1 ?> , median overall V-band dust attenuation A V = 1.9 ± 0.2 ?> mag, median dust mass M dust = ( 5.6 ± 1.0 ) × 10 8 M ⊙ ?> , and median average dust temperature T dust ≃ 40 ?> K. We find that the average intrinsic SED of the ALESS SMGs resembles that of local ultra-luminous infrared galaxies in the infrared range, but the stellar emission of our average SMG is brighter and bluer, indicating lower dust attenuation, possibly because they are more extended. We explore how the average SEDs vary with different parameters (redshift, sub-millimeter flux, dust attenuation, and total infrared luminosity), and we provide a new set of SMG templates that can be used to interpret other SMG observations. To put the ALESS SMGs into context, we compare their stellar masses and SFRs with those of less actively star-forming galaxies at the same redshifts. We find that at z ≃ 2 ?> , about half of the SMGs lie above the star-forming main sequence (with SFRs three times larger than normal galaxies of the same stellar mass), while half are consistent with being at the high-mass end of the main sequence. At higher redshifts ( z ≃ 3.5 ?> ), the SMGs tend to have higher SFRs and stellar masses, but the fraction of SMGs that lie significantly above the main sequence decreases to less than a third.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e0c3daf2717ac12eb1203ee0de17a1e5305822b4

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Citations in the corpus

ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “Unfortunately, all aspects of this comparison are uncertain, from source-to-source variations in Td (Elbaz et al. 2011; Genzel et al. 2015; da Cunha et al. 2015), to the conversion from MIPS 24µm luminosities to IR luminosities, to the extension of these results to fainter, lower-mass z = 2-10…”
The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “In addition, as mentioned above, we use two GALAXEV templates that represent starburst galaxies with an increasing SFH (Behroozi et al. 2013; da Cunha et al. 2015; Sparre et al. 2015).”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, background): “…Arnouts et al. 1999; Ilbert et al. 2006; KCORRECT: Blanton & Roweis 2007; EAZY: Brammer et al. 2008) or the determination of galaxy physical parameters (e.g. CIGALE: Burgarella et al. 2005; Noll et al. 2009; MAGPHYS: da Cunha et al. 2008, 2015; FAST: Kriek et al. 2009), but not both simultaneously.”
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).”
The dust content of galaxies from z = 0 to z = 9 (2016, methodology): “In our study, we will use ALMA-based dust estimates from da Cunha et al. (2015) and Mancini et al. (2015).”
Dust in the Reionization Era: ALMA Observations of a z = 8.38 Gravitationally Lensed Galaxy (2017, methodology): “We also ran an updated version of MAGPHYS (da Cunha et al. 2008) adapted for high-z galaxies (da Cunha et al. 2015).”