Distant carbon atoms betray very early enrichment in the young universe
October 31, 2006
Figure 1. GNIRS infrared spectrum of one of the redshift 6 quasars. The range of redshift of the identified C IV absorption system are shown by labeled horizontal bar.
Figure 2. Evolution of the C IV abundance as a function of redshift, expressed as the C IV contribution to the closing density of the universe. The new GNIRS points from Simcoe are shown are round dots at z = 5.40 - 5.72 and z = 5.72 - 6.21. The lower z points correspond to other studies described in Simcoe's paper.
Charting the evolution of the carbon abundance is like taking a core sample of the early universe's stellar content. Since carbon nuclei are created through fusion in stellar cores, one would expect their abundance to decline at early times, approaching the formation epoch of the first stars. Simcoe's new observations show that the level of triply ionized carbon (i.e. carbon which has been stripped of three electrons, usually denoted as C IV) remains surprisingly constant as far as redshift z ~ 6. In other words, there is no evidence for a downturn in the integrated C IV abundance, even at the most distant and earliest epochs where it has now been measured.
Simcoe conducted infrared observations of the C IV spectral regions in two high redshift quasars-SDSS1306+0356 (zem = 6.002) and SDSS1030+0524 (zem = 6.272)-using the Gemini Near Infra Red Spectrograph (GNIRS) at Gemini South (Figure 1). Infrared spectrographs are essential for studying C IV absorption at z > 5, because the relevant transitions move from the optical to the infrared spectral domain. For this reason, GNIRS is a uniquely suited instrument for exploring the z ~ 6 universe and beyond.
Although the telescope was trained on the distant quasars for these observations, the actual C IV atoms under scrutiny belong to intervening gas between the quasar and Earth. These back-lit intervening clouds absorb photons from the more distant quasars, and the strength of absorption reveals the concentration of C IV at each redshift. Simcoe measured nine C IV absorption line systems between z = 5.72 and z = 6.21.
The constancy of the C IV density throughout most of the history of the universe is surprising, especially at z ~ 6 (Figure 2). Computer simulations predict that the mass density of C IV should start to turn down at these times, in contrast to what Simcoe observes.
Recent cosmic microwave background measurements indicate that light from the very first stars began to fill intergalactic space around z ~ 11-425 million years after the Big Bang. The time elapsed between z ~ 11 and z ~ 6 (where the C IV is now seen), lasted only 500 million years, barely long enough to form galaxies. This suggests that the galaxies that formed at z ~6 -10 may have been among the very first to produce the heavy elements found throughout the intergalactic medium today. The z ~ 6 CIV measurements show that they must have done so extremely vigorously and efficiently.
For more details, see the article "High Redshift Intergalactic C IV Abundance Measurements form the Near-Infrared Spectra of Two z ~ 6 QSOs", by Robert A. Simcoe, The Astrophysical Journal, in press.