The Discovery of a Luminous [CLC][ITAL]z[/ITAL][/CLC] = 5.80 Quasar from the Sloan Digital Sky Survey

Fan, Xiaohui; White, R. L.; Davis, Marc; Becker, R. H.; Strauss, Michael A.; Haiman, Zoltán; Schneider, Donald P.; Gregg, Michael D.; Gunn, James E.; Knapp, G. R.; Lupton, Robert H.; Anderson, John E.; Anderson, Scott F.; Annis, J.; Bahcall, Neta A.; Boroski, William N.; Brunner, Róbert; Chen, Bing; Connolly, Andrew J.; Csabai, István; Doi, Mamoru; Fukugita, M.; Hennessy, G. S.; Hindsley, Robert B.; Ichikawa, Takashi; Ivezić, Eljko; Loveday, Jon; Meiksin, Avery; McKay, Timothy A.; Munn, Jeffrey A.; Newberg, Heidi Jo; Nichol, R. C.; Okamura, S.; Pier, Jeffrey R.; Sekiguchi, M.; Shimasaku, Kazuhiro; Stoughton, Chris; Szalay, Alexander S.; Szokoly, G.; Thakar, Aniruddha R.; Vogeley, Michael S.; York, Donald G.

doi:10.1086/301534

Cited by 265 publications

(42 citation statements)

References 59 publications

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“…The quasar flux at wavelengths shorter than the Lyα emission line (at rest-frame 1215.67 rf l = Å) is absorbed by the intervening neutral medium, causing an extremely red (i − z) or (z − y) color if the source is at z 6  (i-dropouts) or z 6.4  (z-dropouts), respectively. In the past two decades ∼200 quasars have been discovered at z 5.4 6.4 < < , mainly thanks to the advent of large-area surveys, e.g., the Sloan Digital Sky Survey (SDSS; Fan et al 2000, Fan et al 2003, Jiang et al 2016Wang et al 2016, the Canada-France Highredshift Quasar Survey (CFHQS; Willott et al 2007Willott et al , 2009Willott et al , 2010bWillott et al , 2013, the UK Infrared Deep Sky Server (UKIDSS; Venemans et al 2007;Mortlock et al 2009), the Dark Energy Survey (DES; Reed et al 2015, Reed et al 2017, the Very Large Telescope Survey Telescope (VST) ATLAS Survey (Carnall et al 2015), the ESO public Kilo-Degree Survey (KiDS; Venemans et al 2015b), and the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS1 or PS1; Morganson et al 2012; Bañados et al 2014Bañados et al , 2015bBañados et al , 2016. However, the search for sources at even higher redshift (z 6.4  ; age of the universe <0.80 Gyr) has been extremely challenging, and only a few quasars have been discovered at such a distance prior to the results presented here: three from the VISTA Kilo-Degree Infrared Galaxy Survey (VIKING; Venemans et al 2013), four from PS1 (Venemans et al 2015a;Tang et al 2017), and one from the Subaru Hyper Suprime-Cam-SPP Survey (HSC-SPP; Matsuoka et al 2016, Matsuoka et al 2017; so far, only one quasar has been found at z 7 > in the UKIDSS (Mortlock et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Physical Properties of 15 Quasars at z ≳ 6.5

Mazzucchelli

Bañados

Venemans

et al. 2017

ApJ

328

444

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Quasars are galaxies hosting accreting supermassive black holes; due to their brightness, they are unique probes of the early universe. To date, only a few quasars have been reported at (<800 Myr after the big bang). In this work, we present six additional quasars discovered using the Pan-STARRS1 survey. We use a sample of 15 quasars to perform a homogeneous and comprehensive analysis of this highest-redshift quasar population. We report four main results: (1) the majority of quasars show large blueshifts of the broad C iv λ1549 emission line compared to the systemic redshift of the quasars, with a median value ∼3× higher than a quasar sample at ; (2) we estimate the quasars’ black hole masses ( (0.3–5) × 109 M ⊙) via modeling of the Mg ii λ2798 emission line and rest-frame UV continuum and find that quasars at high redshift accrete their material (with ) at a rate comparable to a luminosity-matched sample at lower redshift, albeit with significant scatter (0.4 dex); (3) we recover no evolution of the Fe ii/Mg ii abundance ratio with cosmic time; and (4) we derive near-zone sizes and, together with measurements for quasars from recent work, confirm a shallow evolution of the decreasing quasar near-zone sizes with redshift. Finally, we present new millimeter observations of the [C ii] 158 μm emission line and underlying dust continuum from NOEMA for four quasars and provide new accurate redshifts and [C ii]/infrared luminosity estimates. The analysis presented here shows the large range of properties of the most distant quasars.

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Section: Introductionmentioning

confidence: 99%

Physical Properties of 15 Quasars at z ≳ 6.5

Mazzucchelli

Bañados

Venemans

et al. 2017

ApJ

328

444

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“…About fifteen years ago the first quasars at > z 5.6 (i.e., within the first gigayear of the universe) were discovered (Fan et al 2000). By 2011 the number of quasars at > z 5.6 had reached 60, with most of the contributions coming from large surveys, such as the SDSS (e.g., Fan et al 2006;Jiang et al 2008), CFHQS (e.g., Willott et al 2007Willott et al , 2010b, and UKIDSS (e.g., Venemans et al 2007;Mortlock et al 2011).…”

Section: Introductionmentioning

confidence: 99%

THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE

Bañados

Venemans

Decarli

et al. 2016

ApJS

337

282

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Luminous quasars at > z 5.6 can be studied in detail with the current generation of telescopes and provide us with unique information on the first gigayear of the universe. Thus far, these studies have been statistically limited by the number of quasars known at these redshifts. Such quasars are rare, and therefore, wide-field surveys are required to identify them, and multiwavelength data are required to separate them efficiently from their main contaminants, the far more numerous cool dwarfs. In this paper, we update and extend the selection for thez 6 quasars presented in Bañados et al. (2014) using the Pan-STARRS1 (PS1) survey. We present the PS1 distant quasar sample, which currently consists of 124 quasars in the redshift range   z 5.6 6.7 that satisfy our selection criteria. Of these quasars, 77 have been discovered with PS1, and 63 of them are newly identified in this paper. We present the composite spectra of the PS1 distant quasar sample. This sample spans a factor of ∼20 in luminosity and shows a variety of emission line properties. The number of quasars at > z 5.6 presented in this work almost doubles the previously known quasars at these redshifts, marking a transition phase from studies of individual sources to statistical studies of the high-redshift quasar population, which was impossible with earlier, smaller samples.

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“…22 The SDSS (York et al 2000) provided the first opportunity to search for high-z quasars over wide fields (>1000 deg 2 ), resulting in several tens of objects published to date (Fan et al 2000(Fan et al , 2001a(Fan et al , 2003(Fan et al , 2004(Fan et al , 2006bJiang et al 2008Jiang et al , 2009Jiang et al , 2015. The Canada-France High-z Quasar Survey (CFHQS; Willott et al 2005Willott et al , 2007Willott et al , 2009Willott et al , 2010aWillott et al , 2010b explored fainter magnitudes than the SDSS and found a few tens of new quasars, including one very faint object (CFHQS J0216-0455; z AB =24.4 mag at z = 6.01) discovered in the Subaru XMM-Newton Deep Survey (Furusawa et al 2008) area.…”

Section: Introductionmentioning

confidence: 99%

SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9^∗ †

Matsuoka

Onoue

Kashikawa

et al. 2016

ApJ

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200

190

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We report the discovery of 15 quasars and bright galaxies at 5.7<z<6.9. This is the initial result from the Subaru High-z Exploration of Low-Luminosity Quasars project, which exploits the exquisite multiband imaging data produced by the Subaru Hyper Suprime-Cam (HSC) Strategic Program survey. The candidate selection is performed by combining several photometric approaches including a Bayesian probabilistic algorithm to reject stars and dwarfs. The spectroscopic identification was carried out with the Gran Telescopio Canarias and the Subaru Telescope for the first 80 deg 2 of the survey footprint. The success rate of our photometric selection is quite high, approaching 100% at the brighter magnitudes (z AB <23.5 mag). Our selection also recovered all the known high-z quasars on the HSC images. Among the 15 discovered objects, six are likely quasars, while the other six with interstellar absorption lines and in some cases narrow emission lines are likely bright Lyman-break galaxies. The remaining three objects have weak continua and very strong and narrow Lyα lines, which may be excited by ultraviolet light from both young stars and quasars. These results indicate that we are starting to see the steep rise of the luminosity function of z6 galaxies, compared with that of quasars, at magnitudes fainter than M 1450 ∼−22 mag or z AB ∼24 mag. Follow-up studies of the discovered objects as well as further survey observations are ongoing.

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The Discovery of a Luminous [CLC][ITAL]z[/ITAL][/CLC] = 5.80 Quasar from the Sloan Digital Sky Survey

Cited by 265 publications

References 59 publications

Physical Properties of 15 Quasars at z ≳ 6.5

Physical Properties of 15 Quasars at z ≳ 6.5

THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE

SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9^∗ †

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The Discovery of a Luminous [CLC][ITAL]z[/ITAL][/CLC] = 5.80 Quasar from the Sloan Digital Sky Survey

Cited by 265 publications

References 59 publications

Physical Properties of 15 Quasars at z ≳ 6.5

Physical Properties of 15 Quasars at z ≳ 6.5

THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE

SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9∗ †

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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^∗ †