A bright z=5.2 lensed submillimeter galaxy in the field of Abell 773 HLSJ091828.6+514223

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 d...

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Detalhes bibliográficos
Autores: 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, Pablo Guillermo, Schaerer, D., Smith, G. P., Swinbank, A. M., van der Werf, P.
Tipo de documento: artigo
Data de publicação:2012
País:España
Recursos:Universidad Complutense de Madrid (UCM)
Repositório:Docta Complutense
Idioma:inglês
OAI Identifier:oai:docta.ucm.es:20.500.14352/45096
Acesso em linha:https://hdl.handle.net/20.500.14352/45096
Access Level:Acceso aberto
Palavra-chave:52
Star-formation history
Ultraluminous infrared galaxies
Molecular gas
Herschel-atlas
APM 08279+5255
Markarian 231
Water-vapor
Interstellar-medium
Massive galaxy
Dark-matter
Astrofísica
Astronomía (Física)
Descrição
Resumo: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 CI(^3P_2−^3 P_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.

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