Physical properties of z > 4 submillimeter galaxies in the COSMOS field

Smolčić, Vernesa and Karim, A. and Miettinen, Oscari and Novak, Mario and Magnelli, B. and Riechers, D. A. and Schinnerer, E. and Capak, P. and Bondi, M. and Ciliegi, P. and Aravena, M. and Bertoldi, F. and Bourke, S. and Banfield, J. and Carilli, C. L. and Civano, F. and Ilbert, O. and Intema, H. T. and Le Fèvre, O. and Finoguenov, A. and Hallinan, G. and Klockner, H.-R. and Koekemoer, A. and Laigle, C. and Masters, D. and McCracken, H. J. and Mooley, K. and Murphy, E. and Navarette, F. and Salvato, M. and Sargent, M. and Sheth, K. and Toft, S. and Zamorani, G. (2015) Physical properties of z > 4 submillimeter galaxies in the COSMOS field. Astronomy and Astrophysics, 576. Art. No. A127. ISSN 0004-6361

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We investigate the physical properties of a sample of six submillimeter galaxies (SMGs) in the COSMOS field, spectroscopically confirmed to lie at redshifts z> 4. While the redshifts for four of these SMGs were previously known, we present here two newly discovered z_(spec)> 4 SMGs. For our analysis we employ the rich (X-ray to radio) COSMOS multi-wavelength datasets. In particular, we use new data from the Giant Meterwave Radio Telescope (GMRT) 325 MHz and 3 GHz Jansky Very Large Array (VLA) to probe the rest-frame 1.4 GHz emission at z = 4, and to estimate the sizes of the star formation regions of these sources, respectively. We find that only oneSMG is clearly resolved at a resolution of 0''̣6 × 0''̣7 at 3 GHz, two may be marginally resolved, while the remaining three SMGs are unresolved at this resolution. Combining this with sizes from high-resolution (sub-)mm observations available in the literature for AzTEC 1 and AzTEC 3 we infer a median radio-emitting size for our z> 4 SMGs of (0''̣63 ± 0''̣12) × (0''̣35 ± 0''̣05) or 4.1 × 2.3 kpc^2 (major × minor axis; assuming z = 4.5) or lower if we take the two marginally resolved SMGs as unresolved. This is consistent with the sizes of star formation regions in lower-redshift SMGs, and local normal galaxies, yet higher than the sizes of star formation regions of local ultraluminous infrared galaxies (ULIRGs). Our SMG sample consists of a fair mix of compact and more clumpy systems with multiple, perhaps merging, components. With an average formation time of ~280 Myr, as derived through modeling of the UV IR spectral energy distributions, the studied SMGs are young systems. The average stellar mass, dust temperature, and IR luminosity we derive are M⋆ ~ 1.4 × 10^(11) M⊙, T_(dust) ~ 43 K, and L_(IR) ~ 1.3 × 10^(13)L⊙, respectively. The average L_(IR) is up to an order of magnitude higher than for SMGs at lower redshifts. Our SMGs follow the correlation between dust temperature and IR luminosity as derived for Herschel-selected 0.1 <z< 2 galaxies. We study the IR-radio correlation for our sources and find a deviation from that derived for z< 3 ULIRGs (⟨ q_(IR) ⟩ = 1.95 ± 0.26 for our sample, compared to q ≈ 2.6 for IR luminous galaxies at z< 2). In summary, we find that the physical properties derived for our z> 4 SMGs put them at the high end of the L_(IR)–T_(dust) distribution of SMGs, and that our SMGs form a morphologically heterogeneous sample. Thus, additional in-depth analyses of large, statistical samples of high-redshift SMGs are needed to fully understand their role in galaxy formation and evolution.

Item Type: Article
Keywords: surveys – galaxies: high-redshift – galaxies: starburst – radio continuum: galaxies – submillimeter: galaxies
Date: 17 April 2015
Subjects: NATURAL SCIENCES > Physics > Astronomy and Astrophysics
Additional Information: © 2015 ESO. Article published by EDP Sciences. Received 16 September 2014; Accepted 3 December 2014; Published online 17 April 2015.
Divisions: Faculty of Science > Department of Physics
Publisher: EDP Sciences
Depositing User: Vernesa Smolčić
Date Deposited: 08 May 2016 20:44
Last Modified: 08 May 2016 20:44

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