The Carbon Content of Intergalactic Gas at Z=4.25 and Its Evolution toward Z=2.4

• Main Author: Simcoe, Robert A. (Contributor)
• Other Authors: Massachusetts Institute of Technology. Department of Physics (Contributor), MIT Kavli Institute for Astrophysics and Space Research (Contributor)
• Format: Article
• Language: English
• Published: IOP Publishing, 2013-01-24T16:36:31Z.
• Subjects: Article
• Online Access: Get fulltext

 This paper presents ionization-corrected measurements of the carbon abundance in intergalactic gas at 4.0 < z < 4.5, using spectra of three bright quasars obtained with the Magellan Inamori Kycocera Echelle spectrograph on Magellan. By measuring the C IV strength in a sample of 131 discrete H I-selected quasar absorbers with p/[bar over p] [> over /] 1.6, we derive a median carbon abundance of [C/H]=-3.55, with lognormal scatter of approximately σ ≈ 0.8 dex. This median value is a factor of two to three lower than similar measurements made at z ~ 2.4 using C IV and O VI. The strength of evolution is modestly dependent on the choice of UV background spectrum used to make ionization corrections, although our detection of an abundance evolution is generally robust with respect to this model uncertainty. We present a framework for analyzing the effects of spatial fluctuations in the UV ionizing background at frequencies relevant for C IV production. We also explore the effects of reduced flux between 3 and 4 Rydbergs (as from He II Lyman series absorption) on our abundance estimates. At He II line absorption levels similar to published estimates, the effects are very small, although a larger optical depth could reduce the strength of the abundance evolution. Our results imply that ~50% of the heavy elements seen in the intergalactic medium at z ~ 2.4 were deposited in the 1.3 Gyr between z ~ 4.3 and z ~ 2.4. The total implied mass flux of carbon into the Lyα forest would constitute ~30% of the IMF-weighted carbon yield from known star-forming populations over this period.