The Direct Detection of Lyman-Continuum Emission from Star-forming Galaxies at z~3

Details The Direct Detection of Lyman-Continuum Emission from Star-forming Galaxies at z~3 The Direct Detection of Lyman-Continuum Emission from Star-forming Galaxies at z~3

2006-06-26

arxiv.org/abs/astro-ph/0606635v1

Astrophys.J.651:688-703,2006

Astronomy and Astrophysics

Astrophysics

21 pages including 10 figures. Accepted for publication in ApJ. Version with Figures 3 and 8 at full resolution available at

Scientific paper

10.1086/507511

We present the results of rest-frame ultraviolet spectroscopic observations of a sample of 14 z~3 star-forming galaxies in the SSA22a field. These spectra are characterized by unprecedented depth in the Lyman-continuum region. For the first time, we have detected escaping ionizing radiation from individual galaxies at high redshift, with two of the 14 objects showing significant emission below the Lyman limit. We also measured the ratio of emergent flux density at 1500 AA to that in the Lyman-continuum region, for the individual detections (C49 and D3) and the sample average. If a correction for the average IGM opacity is applied to the spectra of the objects C49 and D3, we find f_1500/f_900,corr(C49)=4.5 and f_1500/f_900,corr(D3)=2.9. The average emergent flux-density ratio in our sample is =22, implying an escape fraction ~4.5 times lower than inferred from the composite spectrum in Steidel et al. (2001). If this new estimate is representative of LBGs, their contribution to the metagalactic ionizing radiation field is J_nu(900)~2.6x10^{-22} erg/s/cm^2/Hz/sr, comparable to the contribution of optically-selected quasars at the same redshift. The sum of the contributions from galaxies and quasars is consistent with recent estimates of the level of the ionizing background at z~3, inferred from the HI Ly-alpha forest optical depth. There is significant variance among the emergent far-UV spectra in our sample, yet the factors controlling the detection or non-detection of Lyman-continuum emission from galaxies are not well-determined. Because we do not yet understand the source of this variance, significantly larger samples will be required to obtain robust constraints on the galaxy contribution to the ionizing background at z~3 and beyond (abridged).

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