Journal Article

Ultraviolet Fe <span class="smallCaps">ii</span> emission in <i>z</i>∼ 2 quasars

H. Sameshima, J. Maza, Y. Matsuoka, S. Oyabu, K. Kawara, Y. Yoshii, N. Asami, N. Ienaka and Y. Tsuzuki

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 395, issue 2, pages 1087-1091
Published in print May 2009 | ISSN: 0035-8711
Published online April 2009 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2009.14605.x
Ultraviolet Fe ii emission in z∼ 2 quasars

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We present spectra of six luminous quasars at z∼ 2, covering rest wavelengths 1600−3200 Å. The fluxes of the UV Fe ii emission lines and Mg iiλ2798 doublet, the line widths of Mg ii and the 3000 Å luminosity were obtained from the spectra. These quantities were compared with those of low-redshift quasars at z= 0.06–0.55 studied by Tsuzuki et al. In a plot of the Fe ii(UV)/Mg ii flux ratio as a function of the central black hole mass, Fe ii(UV)/Mg ii in our z∼ 2 quasars is systematically greater than in the low-redshift quasars. We confirmed that luminosity is not responsible for this excess. It is unclear whether this excess is caused by rich Fe abundance at z∼ 2 over low-redshift or by non-abundance effects such as high gas density, strong radiation field and high microturbulent velocity.

Keywords: galaxies: abundances; galaxies: active; line: formation; quasars: emission lines

Journal Article.  2406 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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