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(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. IV. Physical properties derived from spectral energy distributions

Miettinen, O. and Delvecchio, I. and Smolčić, V. and Novak, M. and Aravena, M. and Karim, A. and Murphy, E. J. and Schinnerer, E. and Capak, P. and Ilbert, O. and Intema, H. T. and Laigle, C. and McCracken, H. J. (2017) (Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies. IV. Physical properties derived from spectral energy distributions. Astronomy and Astrophysics, 597 . Art. No. A5. ISSN 0004-6361.

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Context. Submillimetre galaxies (SMGs) in the early Universe are potential antecedents of the most massive galaxies we see in the present-day Universe. An important step towards quantifying this galactic evolutionary connection is to investigate the fundamental physical properties of SMGs, such as their stellar mass content (M⋆) and star formation rate (SFR). Aims. We attempt to characterise the physical nature of a 1.1 mm selected, flux-limited, and interferometrically followed up sample of SMGs in the COSMOS field. Methods. We used the latest release of the MAGPHYS code to fit the multiwavelength (UV to radio) spectral energy distributions (SEDs) of 16 of the target SMGs, which lie at redshifts z ≃ 1.6−5.3. We also constructed the pure radio SEDs of our SMGs using three different radio bands (325 MHz, 1.4 GHz, and 3 GHz). Moreover, since two SMGs in our sample, AzTEC 1 and AzTEC 3, benefit from previous ^(12)C^(16)O line observations, we studied their properties in more detail. Results. The median and 16th–84th percentile ranges of M⋆, infrared (8−1000 μm) luminosity (L_(IR)), SFR, dust temperature (T_(dust)), and dust mass (M_(dust)) were derived to be log (M⋆/M⊙) = 10.96^(+0.34)_(-0.19), log (L_(IR)/L⊙) = 12.93^(+0.09)_(-0.19), SFR = 856^(+191)_(-310)M⊙ yr^(-1), T_(dust) = 40.6^(+7.5)_(-8.1) K, and log (M_(dust)/M⊙) = 9.17^(+0.03)_(-0.33), respectively. We found that 63% of our target SMGs lie above the galaxy main sequence by more than a factor of 3 and, hence, are starbursts. The 3 GHz radio sizes we have previously measured for the target SMGs were compared with the present M⋆ estimates, and we found that the z > 3 SMGs are fairly consistent with the mass–size relationship of z ~ 2 compact, quiescent galaxies (cQGs). The median radio spectral index is found to be α = −0.77^(+0.28)_(-0.42). The median IR-radio correlation parameter is found to be q = 2.27^(+0.27)_(-0.13), which is lower than was measured locally (median q = 2.64). The gas-to-dust mass ratio for AzTEC 1 is derived to be δ_(gdr) = 90^(+23)_(-19), while that for AzTEC 3 is 33^(+28)_(-18). AzTEC 1 is found to have a sub-Eddington SFR surface density (by a factor of 2.6^(+0.2)_(-0.1)), while AzTEC 3 appears to be an Eddington-limited starburster. The gas reservoir in these two high-z SMGs would be exhausted in only ~ 86 and 19 Myr at the current SFR, respectively. Conclusions. A comparison of the MAGPHYS-based properties of our SMGs with those of equally bright SMGs in the ECDFS field (the ALESS SMGs) that are 870 μm selected and followed up by ALMA, suggests that the two populations share fairly similar physical characteristics, including the q parameter. The somewhat higher L_(dust) for our sources (factor of 1.9^(+9.3)_(-1.6) on average) can originate in the longer selection wavelength of 1.1 mm. Although the derived median α is consistent with a canonical synchrotron spectral index, some of our SMGs exhibit spectral flattening or steepening, which can be attributed to different cosmic-ray energy gain and loss mechanisms. A hint of negative correlation is found between the 3 GHz size and the level of starburstiness and, hence, cosmic-ray electrons in more compact starbursts might be more susceptible to free-free absorption. Some of the derived low and high q values (compared to the local median) could be the result of a specific merger or post-starburst phase of galaxy evolution. Overall, our results, such as the M⋆–3 GHz radio size analysis and comparison with the stellar masses of z ~ 2 cQGs in concert with the star formation properties of AzTEC 1 and 3, support the scenario where z > 3 SMGs evolve into the present day giant, gas-poor ellipticals.

Item Type:Article
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URLURL TypeDescription Paper
Schinnerer, E.0000-0002-3933-7677
McCracken, H. J.0000-0002-9489-7765
Additional Information:© 2016 ESO. Received: 14 January 2016; Accepted: 2 September 2016; Published online 19 December 2016. We would like to thank the anonymous referee for  providing us with comments and suggestions. This research was funded by the European Union’s Seventh Framework programme under grant agreement 337595 (ERC Starting Grant, “CoSMass”). This work was completed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. This work was partially supported by a grant from the Simons Foundation. M.A. acknowledges partial support from FONDECYT through grant 1140099. A.K. acknowledges support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00978.S and ADS/JAO.ALMA#2013.1.00118.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This paper is also partly based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This research has made use of NASA’s Astrophysics Data System, and the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the NASA. We greatfully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information on the COSMOS survey is available at PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
European Research Council (ERC)337595
Simons FoundationUNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1140099
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
Subject Keywords:galaxies: evolution – galaxies: formation – galaxies: starburst – galaxies: star formation – radio continuum: galaxies – submillimeter: galaxies
Record Number:CaltechAUTHORS:20170310-104204574
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Official Citation:(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies - IV. Physical properties derived from spectral energy distributions O. Miettinen, I. Delvecchio, V. Smolčić, M. Novak, M. Aravena, A. Karim, E. J. Murphy, E. Schinnerer, P. Capak, O. Ilbert, H. T. Intema, C. Laigle and H. J. McCracken A&A, 597 (2017) A5 DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75025
Deposited By: Tony Diaz
Deposited On:10 Mar 2017 19:21
Last Modified:10 Mar 2017 19:21

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