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A Survey of z>5.7 Quasars in the Sloan Digital Sky Survey III: Discovery of Five Additional Quasars
Journal article   Open access

A Survey of z>5.7 Quasars in the Sloan Digital Sky Survey III: Discovery of Five Additional Quasars

Xiaohui Fan, Joseph F Hennawi, Gordon T Richards, Michael A Strauss, Donald P Schneider, Jennifer L Donley, Jason E Young, James Annis, Huan Lin, Hubert Lampeitl, …
The Astronomical journal, v 128(2), pp 515-522
07 May 2004
DOI: https://doi.org/10.1086/422434
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https://doi.org/10.1086/422434View
Published, Version of Record (VoR)Maybe Open Access (Publisher Bronze),  Open

Abstract

Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics
Astron.J.128:515,2004 We present the discovery of five new quasars at z>5.7, selected from the multicolor imaging data of the Sloan Digital Sky Survey (SDSS). Three of them, at redshifts 5.93, 6.07, and 6.22, were selected from ~1700 deg^2 of new SDSS Main Survey imaging in the Northern Galactic Cap. An additional quasar, at redshift 5.85, was discovered by coadding the data obtained in the Fall Equatorial Stripe in the SDSS Southern Survey Region. The fifth object, at redshift 5.80, is selected from a non-standard SDSS scan in the Southern Galactic Cap outside the Main Survey area. The spectrum of SDSS J162331.81+311200.5 (z=6.22) shows a complete Gunn-Peterson trough at z_abs > 5.95, similar to the troughs detected in other three z>6.2 quasars known. We present a composite spectrum of the z>5.7 quasars discovered in the SDSS to date. The average emission line and continuum properties of z~6 quasars exhibit no significant evolution compared to those at low redshift. Using a complete sample of nine z>5.7 quasars, we find that the density of quasars with M_1450 < -26.7 at z~6 is (6+/-2) x 10^-10 per Mpc^3 consistent with our previous estimates. The luminosity distribution of the sample is fit with a power law luminosity function Psi(L) ~ L^(-3.2+/-0.7), somewhat steeper than but consistent with our previous estimates.

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