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Physical properties of z>4 submillimeter galaxies in the COSMOS field | | V. Smolcic
; A. Karim
; O. Miettinen
; M. Novak
; B. Magnelli
; D. A. Riechers
; E. Schinnerer
; P. Capak
; M. Bondi
; P. Ciliegi
; M. Aravena
; F. Bertoldi
; S. Bourke
; J. Banfield
; C. L. Carilli
; F. Civano
; O. Ilbert
; O. Le Fevre
; A. Finoguenov
; G. Hallinan
; H.-R. Kloeckner
; C. Laigle
; D. Masters
; H. J. McCracken
; K. Mooley
; E. Murphy
; F. Navarette
; M. Salvato
; M. Sargent
; K. Sheth
; S. Toft
; G. Zamorani
; | | Date: |
11 Dec 2014 | | Abstract: | We study the physical properties of a sample of 6 SMGs in the COSMOS field,
spectroscopically confirmed to lie at z>4. We use new GMRT 325 MHz and 3 GHz
JVLA data to probe the rest-frame 1.4 GHz emission at z=4, and to estimate the
sizes of the star-forming (SF) regions of these sources, resp. Combining our
size estimates with those available in the literature for AzTEC1 and AzTEC3 we
infer a median radio-emitting size for our z>4 SMGs of
(0.63"+/-0.12")x(0.35"+/-0.05") or 4.1x2.3 kpc^2 (major times 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 SF regions in lower-redshift
SMGs, and local normal galaxies, yet higher than the sizes of SF regions of
local 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, derived through modeling of the UV-IR SEDs, the studied SMGs
are young systems. The average stellar mass, dust temperature, and IR
luminosity we derive are M*~1.4x10^11 M_sun, T_dust~43 K, and
L_IR~1.3x10^13L_sun, resp. 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, further in-depth analyses of large, statistical
samples of high-redshift SMGs are needed to fully understand their role in
galaxy formation and evolution. | | Source: | arXiv, 1412.3799 | | Services: | Forum | Review | PDF | Favorites | |
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