TY - JOUR
T1 - A bright z = 5.2 lensed submillimeter galaxy in the field of Abell 773
T2 - HLSJ091828.6+514223
AU - Combes, F.
AU - Rex, M.
AU - Rawle, T. D.
AU - Egami, E.
AU - Boone, F.
AU - Smail, I.
AU - Richard, J.
AU - Ivison, R. J.
AU - Gurwell, M.
AU - Casey, C. M.
AU - Omont, A.
AU - Berciano Alba, A.
AU - Dessauges-Zavadsky, M.
AU - Edge, A. C.
AU - Fazio, G. G.
AU - Kneib, J. P.
AU - Okabe, N.
AU - Pelló, R.
AU - Pérez-González, P. G.
AU - Schaerer, D.
AU - Smith, G. P.
AU - Swinbank, A. M.
AU - Van Der Werf, P.
N1 - Funding Information:
IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Herschel is an ESA space observatory with instruments provided by European-led PI consortia and with important participation from NASA. Support for this work was provided in part by NASA through an award issued by JPL/Caltech. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NRAO is operated by Associated Universities Inc., under a cooperative agreement with the National Science Foundation. The Keck observatory, made possible thanks to the generous support of W. M. Keck Foundation, is operated by Caltech, the University of California, and NASA.
PY - 2012
Y1 - 2012
N2 - During 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 L FIR = 1.1 × 10 14/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-H 2 conversion ratio, the H 2 mass is 5.8 × 10 11/μ M ⊙, of which one third is in a cool component. From the C I( 3P 2- 3P 1) line we derive a C I/H 2 number abundance of 6 × 10 -5 similar to that in other ULIRGs. The H 2O p(2,0,2-1,1,1) line is strong only in the red velocity component, with an intensity ratio I(H 2O)/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.
AB - During 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 L FIR = 1.1 × 10 14/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-H 2 conversion ratio, the H 2 mass is 5.8 × 10 11/μ M ⊙, of which one third is in a cool component. From the C I( 3P 2- 3P 1) line we derive a C I/H 2 number abundance of 6 × 10 -5 similar to that in other ULIRGs. The H 2O p(2,0,2-1,1,1) line is strong only in the red velocity component, with an intensity ratio I(H 2O)/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.
KW - galaxies: ISM
KW - galaxies: evolution
KW - galaxies: high-redshift
KW - galaxies: individual: HLSJ091828.6+514223
KW - infrared: galaxies
KW - submillimeter: galaxies
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U2 - 10.1051/0004-6361/201118750
DO - 10.1051/0004-6361/201118750
M3 - Review article
AN - SCOPUS:84859228366
SN - 0004-6361
VL - 538
JO - Astronomy and astrophysics
JF - Astronomy and astrophysics
M1 - L4
ER -