Capak, PCarilli, CLLee, NAldcroft, TAussel, HSchinnerer, EWilson, GWYun, MinBlain, AGiavalisco, MIlbert, OKartaltepe, JLee, KSMcCracken, HMobasher, BSalvato, MSasaki, SScott, KSSheth, KShioya, YThompson, DElvis, MSanders, DBScoville, NZTanaguchi, Y2024-04-262024-04-262008-0110.1086/590555https://hdl.handle.net/20.500.14394/2872<p>This is the pre-published version harvested from ArXiv. The published version is located at <a href="http://iopscience.iop.org/1538-4357/681/2/L53/">http://iopscience.iop.org/1538-4357/681/2/L53/</a></p>We report the spectroscopic confirmation of a submillimeter galaxy (SMG) at z = 4.547 with an estimated LIR = (0.5-2.0) × 1013 L. The spectra, mid-IR, and X-ray properties indicate the bolometric luminosity is dominated by star formation at a rate of >1000 M yr−1. Multiple, spatially separated components are visible in the Lyα line with an observed velocity difference of up to 380 km s−1 and the object morphology indicates a merger. The best-fit spectral energy distribution and spectral line indicators suggest the object is 2-8 Myr old and contains >1010 M of stellar mass. This object is a likely progenitor for the massive early-type systems seen at z ~ 2.galaxies : evolutiongalaxies : formationgalaxies : high-redshiftgalaxies : interactionsgalaxies : starburstsubmillimeterAstrophysics and Astronomyarticle