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A comprehensive view of a strongly lensed planck-associated submillimeter galaxy

AutorFu, Hai; Ivison, R. J.; Pérez-Fournon, I.; Baes, M.; Cava, Antonio; Clements, D. L.; Zotti, G. de; Dye, S.; Eales, S.; Herranz, D. ; Jarvis, Matt J.; Maddox, S. J.; Negrello, Mattia; Serjeant, S.; Verma, A.
Palabras claveGalaxies: individual (HATLAS J114637.9–001132)
Galaxies: formation
Galaxies: interactions
Fecha de publicación2012
EditorAmerican Astronomical Society
Institute of Physics Publishing
CitaciónAstrophysical Journal 753(2): 134 (2012)
ResumenWe present high-resolution maps of stars, dust, and molecular gas in a strongly lensed submillimeter galaxy (SMG) at z = 3.259. HATLAS J114637.9–001132 is selected from the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) as a strong lens candidate mainly based on its unusually high 500 μm flux density (~300 mJy). It is the only high-redshift Planck detection in the 130 deg2 H-ATLAS Phase-I area. Keck Adaptive Optics images reveal a quadruply imaged galaxy in the K band while the Submillimeter Array and the Jansky Very Large Array show doubly imaged 880 μm and CO(1→0) sources, indicating differentiated distributions of the various components in the galaxy. In the source plane, the stars reside in three major kpc-scale clumps extended over ~1.6 kpc, the dust in a compact (~1 kpc) region ~3 kpc north of the stars, and the cold molecular gas in an extended (~7 kpc) disk ~5 kpc northeast of the stars. The emissions from the stars, dust, and gas are magnified by ~17, ~8, and ~7 times, respectively, by four lensing galaxies at z ~ 1. Intrinsically, the lensed galaxy is a warm (T dust ~ 40-65 K), hyper-luminous (L IR ~ 1.7 × 1013 L ☉; star formation rate (SFR) ~2000 M ☉ yr–1), gas-rich (M gas/M baryon ~ 70%), young (M stellar/SFR ~ 20 Myr), and short-lived (M gas/SFR ~ 40 Myr) starburst. With physical properties similar to unlensed z > 2 SMGs, HATLAS J114637.9–001132 offers a detailed view of a typical SMG through a powerful cosmic microscope.
DescripciónFu, Hai et al.
Versión del editorhttp://dx.doi.org/10.1088/0004-637X/753/2/134
URIhttp://hdl.handle.net/10261/108598
DOI10.1088/0004-637X/753/2/134
Identificadoresdoi: 10.1088/0004-637X/753/2/134
issn: 0004-637X
e-issn: 1538-4357
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