Jens-Kristian Krogager, Johan P. U. Fynbo, Cedric Ledoux, Lise Christensen, Anna Gallazzi, Peter Laursen, Palle Møller, Pasquier Noterdaeme, Celine Peroux, Max Pettini, Marianne Vestergaard
We present a detailed study of the emission from a z = 2:35 galaxy that causes damped Lyman-alpha absorption in the spectrum of the background QSO, SDSS J 2222-0946. We present the results of extensive analyses of the stellar continuum covering the rest frame optical-UV regime based on broad-band HST imaging, and of spectroscopy of the strong emission lines: Ly-alpha, [OII], [OIII], [NII], and the H-alpha and H-beta lines from VLT/X-Shooter. We compare the metallicity from the absorption lines in the QSO spectrum with the oxygen abundance inferred from the strong-line methods (R23 and N2). The two emission-line methods yield consistent results: [O/H] = -0.30+/-0.13. Based on the absorption lines in the QSO spectrum a metallicity of -0:52+/-0.05 is inferred at an impact parameter of 6.3 kpc from the centre of the galaxy. The star formation rates of the galaxy from the UV continuum and H-alpha line can be reconciled assuming an amount of reddening of E(B-V) = 0.06+/-0.01, giving an inferred SFR of 13+/-1 M_sun / yr (assuming a Chabrier IMF). From the HST imaging, the galaxy associated with the absorption is found to be a compact (re=1.12 kpc) object with a disclike, elongated (axis ratio 0.17) structure indicating that the galaxy is seen close to edge on. Moreover, the absorbing gas is located almost perpendicularly above the disc of the galaxy suggesting that the gas causing the absorption is not co-rotating with the disc. We investigate the stellar and dynamical masses from SED-fitting and emission-line widths, respectively, and find consistent results of 2x10^9 M_sun. We suggest that the galaxy is a young proto-disc with evidence for a galactic outflow of enriched gas which cools down at a large distance. This galaxy hints at how star-forming galaxies may be linked to the elusive population of damped Lyman-alpha absorbers.
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http://arxiv.org/abs/1304.4231
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