Iron Emission in z~6 QSOs

Details Iron Emission in z~6 QSOs Iron Emission in z~6 QSOs

2003-03-18

arxiv.org/abs/astro-ph/0303424v1

Astrophys.J. 587 (2003) L67-L70

Astronomy and Astrophysics

Astrophysics

13 pages, 3 figures, accepted for publication in ApJ Letters

Scientific paper

10.1086/375338

We have obtained low-resolution near infrared spectra of three QSOs at 5.7 < z < 6.3 using the NICMOS instrument of the Hubble Space Telescope. The spectra cover the rest-frame ultraviolet emission of the objects between lambda_rest ~ 1600A - 2800A. The Fe II emission-line complex at 2500A is clearly detected in two of the objects, and possibly detected in the third. The strength of this complex and the ratio of its integrated flux to that of Mg II lambda 2800 are comparable to values measured for QSOs at lower redshifts, and are consistent with Fe/Mg abundance ratios near or above the solar value. There thus appears to be no evolution of QSO metallicity to z~6. Our results suggest that massive, chemically enriched galaxies formed within 1 Gyr of the Big Bang. If this chemical enrichment was produced by Type Ia supernovae, then the progenitor stars formed at z ~ 20 +/- 10, in agreement with recent estimates based on the cosmic microwave background. These results also support models of an evolutionary link between star formation, the growth of supermassive black holes and nuclear activity.

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