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We discuss the restframe UV emission from the starbursting galaxy HFLS3 atz=6.34, discovered in Herschel/SPIRE data due to its red color in the submmwavelengths from 250-500 um. The apparent inst. SFR of HFLS3 inferred from thetotal FIR luminosity measured with over 15 photometric data points between 100to 1000 um is 2900 Msun/yr. Keck/NIRC2 Ks band adaptive optics imaging datashowed two potential NIR counterparts near HFLS3. Previously, the northerngalaxy was taken to be in the foreground at z=2.1 while the southern galaxy wasassumed to HFLS3's NIR counterpart. New HST/WFC3 and ACS imaging data show bothoptically bright galaxies are in the foreground at z<6. A new lensing modelbased on HST data and mm-wave continuum emission yields a magnification of2.2+/-0.3. The lack of multiple imaging constrains the lensing magnification tobe lower than either 2.7 or 3.5 at the 95% confidence level for the twoscenarios, which attribute one or two components to HFLS3 in the source plane.Correcting for gravitational lensing, the inst. SFR is 1320 Msun/yr with the95% confidence lower limit around 830 Msun/yr. Using models for the restframeUV to FIR SED, the ave. SFR over the last 100 Myr is around 660 Msun/yr. Thedust and stellar masses of HFLS3 from the same SED models are 3x10^8 Msun and~5x10^10 Msun, respectively, with large systematic uncertainties on assumptionsrelated to the SED model. With HST/WFC3 images we also find diffuse NIRemission about 0.5" (~3 kpc) SW of HFLS3 that remains undetected in the ACSdata. The emission has a photometric redshift consistent with either z~6 or adusty galaxy template at z~2. If at the same redshift as HFLS3 the detecteddiffuse emission could be part of the complex merger system that could betriggering the starburst. Alternatively, it could be part of the foregroundstructure at z~2.1 that is responsible for lensing of HFLS3.

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