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Durham University

Department of Physics

Staff profile

Publication details for Professor Ian Smail

Combes, F., Rex, M., Rawle, T.D. Egami, E. Boone, F. Smail, I. , Richard, J. Ivison, R.J. Gurwell, M. Casey, C M. Omont, A. Berciano Alba, A. Dessauges-Zavadsky, M. Edge, A.C. , Fazio, G.G. Kneib, J.-P. Okabe, N. Pelló, R. Pérez-González, P.G., Schaerer, D. Smith, G. P. Swinbank, A.M. & van der Werf, P. (2012). A bright z = 5.2 lensed submillimeter galaxy in the field of Abell 773 HLSJ091828.6+514223. Astronomy & astrophysics 538: L4.

Author(s) from Durham

Abstract

g our Herschel Lensing Survey (HLS) of massive galaxy clusters, we have discovered an exceptionally bright source behind the z = 0.22 cluster Abell 773, which appears to be a strongly lensed submillimeter galaxy (SMG) at z = 5.2429. This source is unusual compared to most other lensed sources discovered by Herschel so far, because of its higher submm flux (~200 mJy at 500 μm) and its high redshift. The dominant lens is a foreground z = 0.63 galaxy, not the cluster itself. The source has a far-infrared (FIR) luminosity of LFIR = 1.1 × 1014/μ L⊙, where μ is the magnification factor, likely ~11. We report here the redshift identification through CO lines with the IRAM-30 m, and the analysis of the gas excitation, based on CO(7–6), CO(6–5), CO(5–4) detected at IRAM and the CO(2–1) at the EVLA. All lines decompose into a wide and strong red component, and a narrower and weaker blue component, 540 km s-1 apart. Assuming the ultraluminous galaxy (ULIRG) CO-to-H2 conversion ratio, the H2  mass is 5.8 × 1011/μ M⊙, of which one third is in a cool component. From the C I(3P2-3P1) line we derive a C I/H2  number abundance of 6 × 10-5 similar to that in other ULIRGs. The H2Op(2,0,2−1,1,1) line is strong only in the red velocity component, with an intensity ratio I(H2O)/I(CO) ~ 0.5, suggesting a strong local FIR radiation field, possibly from an active nucleus (AGN) component. We detect the [NII]205 μm line for the first time at high-z. It shows comparable blue and red components, with a strikingly broad blue one, suggesting strong ionized gas flows.