A Survey of z > 5.7 Quasars in the Sloan Digital Sky Survey. IV. Discovery of Seven Additional Quasars

By Xiaohui Fan, M. Strauss, Gordon Richards, J. Hennawi, Robert H. Becker, R. White, A. Diamond-Stanic, Jennifer L. D onley, Linhua Jiang, J. Kim and 21 more. 2004

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We present the discovery of seven quasars at z > 5.7, selected from ∼2000 deg2 of multicolor imaging data of the Sloan Digital Sky Survey. The new quasars have redshifts z from 5.79 to 6.13. Five are selected as part of a complete flux-limited sample in the SDSS northern Galactic cap; two have larger photometric errors and are not part of the complete sample. One of the new quasars, SDSS J1335+3533 (z = 5.93), exhibits no emission lines; the 3 σ limit on the rest-frame equivalent width of the Lyα+N V line is 5 Å. It is the highest redshift lineless quasar known and could be a gravitational lensed galaxy, a BL Lac object, or a new type of quasar. Two new z > 6 quasars, SDSS 1250+3130 (z = 6.13) and SDSS J1137+3549 (z = 6.01), show deep Gunn-Peterson absorption gaps in Lyα. These gaps are narrower than the complete Gunn-Peterson absorption troughs observed among quasars at z > 6.2 and do not have complete Lyβ absorption.

Subfields: Astronomy and Astrophysics

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SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, neutral): “…progress in the quest for high-z quasars.25 The SDSS (York et al. 2000) provided the first opportunity to search for high-z quasars over wide fields (> 1000 deg2), resulting in several tens of objects published to date (Fan et al. 2000, 2001a, 2003, 2004, 2006b; Jiang et al. 2008, 2009, 2015).”
The aftermath of the first stars: massive black holes (2006, background): “The growth of the first black holes must have been rapid enough to account for the powerful quasars observed at redshifts of z >∼ 6 (e.g. Fan et al. 2004, 2006), believed to be fueled by accretion onto supermassive black holes (SMBHs) with masses ∼ 109 M⊙ (e.g. Haiman & Loeb 2001; Volonteri & Rees…”
Inside-out or outside-in: the topology of reionization in the photon-starved regime suggested by Lyα forest data (2008, background): “Studies of the Lyα forest in QSO absorption spectra have taught us that reionization probably ended at around z ∼ 6 (Fan et al. 2002; Fan et al. 2004; Fan et al. 2006;cf Becker, Rauch, & Sargent 2007).”
A SURVEY OF z ∼ 6 QUASARS IN THE SLOAN DIGITAL SKY SURVEY DEEP STRIPE. I. A FLUX-LIMITED SAMPLE AT zAB < 21 (2007, background): “The slope β = −3.1 ± 0.4 is consistent with the slope −3.2±0.7 derived from the luminous sample alone by Fan et al. (2004) and with the slope > −4.63 (3σ) constrained by the lack of lenses in four high-redshift quasars (Richards et al. 2004).”
Taxing the rich: Recombinations and bubble growth during reionization (2005, background): “Each shows saturated or nearly saturated absorption in the Lyα forest as well as a rapid decrease in the transmission at z ≈ 6 (Fan et al. E-mail: sfurlane@tapir.caltech.edu (SRF); peng@physics.ucsb.edu (SPO) 2001; Becker et al. 2001; White et al. 2003; Fan et al. 2003, 2004).”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, methodology): “Finally, at z = 6 we use the sample compiled by Willott et al. (2010), consisting of quasars from the SDSS main (Fan et al. 2001a, 2003, 2004, 2006b), SDSS deep (Jiang et al. 2008, 2009), and CFHTQS (Willott et al. 2010).”
Towards a complete census of AGN in nearby Galaxies: a large population of optically unidentified AGN (2009, background): “Sensitive blank-field surveys have traced the evolution of luminous AGN activity out to z ≈ 5–6, providing a window on the growth of SMBHs across ≈ 95% of cosmic time (e.g., Ueda et al. 2003; Croom et al. 2004; Fan et al. 2004; Hasinger et al. 2005; Richards et al. 2006).”
Observational Constraints on Cosmic Reionization (2006, methodology): “…A., White, R. L., Becker, R. H., Pentericci, L., & Rix, H.-W. 2002, A.J., 123: 1247-1257 Fan et al. 2003Fan, X., et al. 2003, A.J., 125: 1649-1659 Fan et al. 2004Fan, X., et al. 2004, A.J., 128: 515-522 Fan et al. 2006aFan et al. 2006a, AJ, in press (astro-ph/0512080) Fan et al. 2006bFan et al.…”