A Galactic Wind at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $z=5.190$ \end{document}

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Abstract

We report the serendipitous detection in high-resolution optical spectroscopy of a strong, asymmetric Lyα emission line at z = 5.190. The detection was made in a 2.25 hr exposure with the Echelle Spectrograph and Imager on the Keck II telescope through a spectroscopic slit of dimensions 1'' × 20''. The progenitor of the emission line, J123649.2+621539 (hereafter ES1), lies in the Hubble Deep Field-North northwest flanking field, where it appears faint and compact, subtending just 03 (FWHM) with IAB = 25.4. The ES1 Lyα line flux of 3.0 × 10-17 ergs cm-2 s-1 corresponds to a luminosity of 9.0 × 1042 ergs s-1, and the line profile shows the sharp blue cutoff and broad red wing commonly observed in star-forming systems and expected for radiative transfer in an expanding envelope. We find that the Lyα profile is consistent with a galaxy-scale outflow with a velocity of v > 300 km s-1. This value is consistent with wind speeds observed in powerful local starbursts (typically 102-103 km s-1) and compares favorably to simulations of the late-stage evolution of Lyα emission in star-forming systems. We discuss the implications of this high-redshift galactic wind for the early history of the evolution of galaxies and the intergalactic medium and for the origin of the UV background at z > 3.

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