Herschel and Hubble Study of a Lensed Massive Dusty Starbursting Galaxy at z ∼ 3
- Department of Physics and Astronomy, University of California Irvine, Irvine, CA (United States)
- Laboratoire d’Astrophysique de Marseille, Pôle de l’Étoile Site de Château-Gombert 38, rue Frédéric Joliot-Curie F-13388 Marseille cedex 13 (France)
- Department of Astronomy, Cornell University, Ithaca, NY, 14853 (United States)
- National Radio Astronomy Observatory, Green Bank, WV, 24944 (United States)
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS 42, Cambridge, MA 02138 (United States)
- Department of Astronomy University of Maryland College Park, MD 20742 (United States)
- European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching (Germany)
- School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA (United Kingdom)
- Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA (United Kingdom)
- Department of Physics and Astronomy, Rutgers, the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019 (United States)
- Department of Physical Sciences, San Diego Miramar College, San Diego CA, 92126 (United States)
- Department of Astronomy, University of Texas at Austin, RLM 16.218 2515 Speedway, Stop C1400, Austin, TX 78712-1205 (United States)
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife (Spain)
- INAF-Osservatorio Astronomico di Padova, I-35122 Padova (Italy)
- School of Physics and Astronomy, Cardiff University, Cardiff (United Kingdom)
We present the results of combined deep Keck/NIRC2, HST/WFC3 near-infrared, and Herschel far-infrared observations of an extremely star-forming dusty lensed galaxy identified from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS J133542.9+300401). The galaxy is gravitationally lensed by a massive WISE-identified galaxy cluster at z ∼ 1. The lensed galaxy is spectroscopically confirmed at z = 2.685 from detection of CO (1→0) by GBT and from detection of CO (3→2) obtained with CARMA. We use the combined spectroscopic and imaging observations to construct a detailed model of the background dusty lensed submillimeter galaxy (SMG), which allows us to study the source plane properties of the target. The best-fit lens model provides magnifications of μ {sub star} = 2.10 ± 0.11 and μ {sub dust} = 2.02 ± 0.06 for the stellar and dust components, respectively. Multiband data yield a magnification-corrected star formation rate of 1900(±200) M {sub ⊙} yr{sup −1} and a stellar mass of 6.8{sub −2.7}{sup +0.9}×10{sup 11} M{sub ⊙}, consistent with a main sequence of star formation at z ∼ 2.6. The CO observations yield a molecular gas mass of 8.3(±1.0) × 10{sup 10} M {sub ⊙}, similar to the most massive star-forming galaxies, which together with the high star formation efficiency, are responsible for the intense observed star formation rates. The lensed SMG has a very short gas depletion timescale of ∼40 Myr. The high stellar mass and small gas fractions observed indicate that the lensed SMG likely has already formed most of its stellar mass and could be a progenitor of the most massive elliptical galaxies found in the local universe.
- OSTI ID:
- 22875987
- Journal Information:
- Astrophysical Journal, Vol. 844, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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