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Published July 20, 2014 | Submitted + Published
Journal Article Open

HerMES: The Rest-Frame UV Emission and A Lensing Model for the z=6.34 Luminous Dusty Starburst Galaxy HFLS3


We discuss the rest-frame ultraviolet emission from the starbursting galaxy HFLS3 at a redshift of 6.34. The galaxy was discovered in Herschel/SPIRE data due to its red color in the submillimeter wavelengths from 250 to 500 μm. Keck/NIRC2 K s -band adaptive optics imaging data showed two potential near-IR counterparts near HFLS3. Previously, the northern galaxy was taken to be in the foreground at z = 2.1, while the southern galaxy was assumed to be HFLS3's near-IR counterpart. The recently acquired Hubble/WFC3 and Advanced Camera for Surveys (ACS) imaging data show conclusively that both optically bright galaxies are in the foreground at z < 6. A new lensing model based on the Hubble imaging data and the millimeter-wave continuum emission yields a magnification factor of 2.2 ± 0.3, with a 95% confidence upper limit on the magnification of 3.5. When corrected for lensing, the instantaneous star formation rate is 1320 M_☉ yr^(–1), with the 95% confidence lower limit around 830 M_☉ yr^(–1). The dust and stellar masses of HFLS3 from the same spectral energy distribution (SED) models are at the level of 3 × 10^8 M_☉ and ~5 × 10^(10) M_☉, respectively, with large systematic uncertainties on assumptions related to the SED model. With Hubble/WFC3 images, we also find diffuse near-IR emission about 0.5 arcsec (~3 kpc) to the southwest of HFLS3 that remains undetected in the ACS imaging data. The emission has a photometric redshift consistent with either z ~ 6 or a dusty galaxy template at z ~ 2.

Additional Information

© 2014 American Astronomical Society. Received 2014 April 6; accepted 2014 May 16; published 2014 July 1. Financial support for this work was provided by NASA through grant HST-GO-13045 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Additional support for A.C., W.O., J.C., J.L.W., and C.M.C. was from NSF with AST-1313319. We thank E. da Cunha for help with Magphys. Dark Cosmology Centre is funded by the Danish National Research Foundation (J.L.W. and D.W.). S.O. acknowledges support from the Science and Technology Facilities Council [grant No. ST/I000976/1]. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES).

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Published - 0004-637X_790_1_40.pdf

Submitted - 1404.1378v1.pdf


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