Massive Star Formation in a Gravitationally Lensed H II Galaxy at z = 3.357

October 2003 • 2003ApJ...596..797F

Authors • Fosbury, R. A. E. • Villar-Martín, M. • Humphrey, A. • Lombardi, M. • Rosati, P. • Stern, D. • Hook, R. N. • Holden, B. P. • Stanford, S. A. • Squires, G. K. • Rauch, M. • Sargent, W. L. W.

Abstract • The Lynx arc, with a redshift of 3.357, was discovered during spectroscopic follow-up of the z=0.570 cluster RX J0848+4456 from the ROSAT Deep Cluster Survey. The arc is characterized by a very red R-K color and strong, narrow emission lines. Analysis of HST WFPC2 imaging and Keck optical and infrared spectroscopy shows that the arc is an H II galaxy magnified by a factor of ~10 by a complex cluster environment. The high intrinsic luminosity, the emission-line spectrum, the absorption components seen in Lyα and C IV, and the rest-frame ultraviolet continuum are all consistent with a simple H II region model containing ~10⁶ hot O stars. The best-fit parameters for this model imply a very hot ionizing continuum (T_BB~=80,000 K), a high ionization parameter (logU~=-1), and a low nebular metallicity (Z/Z_solar~=0.05). The narrowness of the emission lines requires a low mass-to-light ratio for the ionizing stars, suggestive of an extremely low metallicity stellar cluster. The apparent overabundance of silicon in the nebula could indicate enrichment by past pair-instability supernovae, requiring stars more massive than ~140 M_solar.

Based partly on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS 5-26555.

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Gordon Squires

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