Discovery of a redshift 6.13 quasar in 
 the UKIRT infrared  deep sky survey

Mortlock, D.; Patel, M.; Warren, S. J.; Venemans, Bram; McMahon, R. G.; Hewett, Paul C.; Simpson, Chris; Sharp, Robert; Burningham, B.; Dye, S.; Ellis, S. C.; Gonzales-Solares, E.; Huélamo, N.

doi:10.1051/0004-6361/200811161

Cited by 80 publications

(71 citation statements)

References 45 publications

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“…This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2011.0.00206.S . ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA ( Taiwan Note -Column (1), name; Column (2), magnitudes at rest-frame 1450Å (Fan et al 2013, in prep;Mortlock et al 2009;Jiang et al 2008Jiang et al , 2009Fan et al 2000); Column (3), continuum flux density at 250 GHz; Column (4) and (5), redshift and FWHM line width of the CO (6-5) line; Column (6) CO (6-5) line flux of the five objects; Column (7) CO (1-0) line luminosity calculated from the CO (6-5) line emission assuming a CO excitation ladder similar to J1148+5251 ). The CO (6-5) line measurements for J2310+1855 are from this work, and from Wang et al (2010Wang et al ( , 2011a for the other four sources.…”

Section: Discussionmentioning

confidence: 99%

“…We calculate the 1µm to 8 keV quasar bolometric luminosities for the four sources using an isotropic bolometric correction of L bol = 4.2L 1450 (Runnoe et al 2012a,b), where L 1450 is the rest-frame 1450Å luminosity calculated from the 1450Å magnitudes in the discovery papers Jiang et al 2009;Mortlock et al 2009, Fan et al 2013 We here assume that the dust extinction from quasar host galaxies at 1450Å is negligible. We then derive the SMBH masses (M BH ) from the quasar luminosity assuming Eddington accretion.…”

Section: Dynamical Masses Traced By the [C Ii] Line Emissionmentioning

confidence: 99%

“…There are currently more than sixty quasars known at z∼6, selected from large optical and near-infrared surveys (e.g. the Sloan Digital Sky Survey [SDSS], Fan et al 2006;Jiang et al 2008Jiang et al , 2009; the Canada-France High Redshift Quasar Survey, Willott et al 2007Willott et al , 2009Willott et al , 2010, the UKIDSS Large Area Survey [ULAS], Mortlock et al 2009Mortlock et al , 2011, and the Panoramic Survey Telescope and Rapid Response System [Pan-STARRS], Morganson et al 2012) with optical z-band magnitudes from 18.8 to 24.4 and inferred SMBH masses from 10 8 to a few 10 9 M ⊙ (Kurk et al 2007;Jiang et al 2007;Willott et al 2010;De Rosa et al 2011). The formation of 10 9 M ⊙ SMBHs at the highest redshift suggests fast black hole accretion and significant SMBH-galaxy evolution within 1 Gyr after the Big Bang (Li et al 2007;Narayanan et al 2008;Di Matteo et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES ATz∼ 6: NEW INSIGHTS FROM ALMA

Wang¹,

Wagg²,

Carilli³

et al. 2013

ApJ

404

633

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We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the [C II] 158 µm fine structure line and dust continuum emission from the host galaxies of five redshift 6 quasars. We also report complementary observations of 250 GHz dust continuum and CO (6-5) line emission from the z=6.00 quasar SDSS J231038.88+185519.7 using the IRAM facilities. The ALMA observations were carried out in the extended array at 0. −4 , which is comparable to the values found in other high-redshift quasar-starburst systems and local ultra-luminous infrared galaxies. The sources are marginally resolved and the intrinsic source sizes (major axis FWHM) are constrained to be 0.3 ′′ to 0.6 ′′ (i.e., 1.7 to 3.5 kpc) for the [C II] line emission and 0.2 ′′ to 0.4 ′′ (i.e., 1.2 to 2.3 kpc) for the continuum. These measurements indicate that there is vigorous star formation over the central few kpc in the quasar host galaxies. The ALMA observations also constrain the dynamical properties of the star-forming gas in the nuclear region. The intensity-weighted velocity maps of three sources show clear velocity gradients. Such velocity gradients are consistent with a rotating, gravitationally bound gas component, although they are not uniquely interpreted as such. Under the simplifying assumption of rotation, the implied dynamical masses within the [C II]-emitting regions are of order 10 10 to 10 11 M ⊙ . Given these estimates, the mass ratios between the SMBHs and the spheroidal bulge are an order of magnitude higher than the mean value found in local spheroidal galaxies, which is in agreement with results from previous CO observations of high redshift quasars.

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Section: Discussionmentioning

confidence: 99%

Section: Dynamical Masses Traced By the [C Ii] Line Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES ATz∼ 6: NEW INSIGHTS FROM ALMA

Wang¹,

Wagg²,

Carilli³

et al. 2013

ApJ

404

633

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“…Finally, we also include the NIR spectrum of CFHQS J1509-1749 (z = 6.12) obtained by Willott et al (2007) at GEMINI South by using GNIRS and the NIR spectrum of ULAS J0203+0012 (z = 5.72) by Mortlock et al (2009) at GEMINI North with GNIRS.…”

Section: Spectroscopic Data and Samplementioning

confidence: 99%

The extinction law at high redshift and its implications

Gallerani

Maiolino

Juárez

et al. 2010

A&A

156

171

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We analyze the optical-near infrared spectra of 33 quasars with redshifts 3.9 ≤ z ≤ 6.4 to investigate the properties of dust extinction at these cosmic epochs. The SMC extinction curve has been shown to reproduce the dust reddening of most quasars at z < 2.2; we investigate whether this curve also provides a good description of dust extinction at higher redshifts. We fit the observed spectra with synthetic absorbed quasar templates obtained by varying the intrinsic slope (α λ ), the absolute extinction (A 3000 ), and by using a grid of empirical and theoretical extinction curves. We find that seven quasars in our sample are affected by substantial extinction (A 3000 ≥ 0.8), and characterized by very steep intrinsic slopes (α λ ≤ −2.3). All of the individual quasars require extinction curve deviating from that of the SMC, with a tendency to flatten at λ ≤ 2000 Å (in the rest frame of the source). However, due to the uncertainties in the individual extinction curves the SMC is still (marginally) consistent with the data in most cases. We obtain a mean extinction curve at z > 4, both by performing a simultaneous fit of all quasars and by averaging the extinction curves inferred for individual quasars. In the case of broad absorption line quasars (which are generally more absorbed by dust and possibly in a younger evolutionary stage), the mean extinction curve deviates from the SMC at a confidence level ≥95%. The difference between extinction curves in quasars at z > 4 and in quasars at lower redshift is indicative of either a different dust production mechanism at high redshift, or a different mechanism for processing dust into the ISM. We suggest that the same transitions may also apply to normal, star-forming galaxies at z > 4. In particular, the observed change in the average spectral slope of galaxies at z > 4 may be partially ascribed to a variation in the extinction curve, rather than a lower dust content at high redshift. In this scenario, the extinction curve inferred at z > 4 would imply a cosmic star-formation corrected for dust attenuation a factor of ∼2 higher than estimated in the past.

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“…The discovery of luminous quasar populations at z > 6 (Fan et al 2006;Willott et al 2010;Mortlock et al 2009) enables studies of the C iv density at higher redshift, but above z ∼ 5.5 observations become challenging as the C iv transition moves into the Y and J bands. For this reason, the earliest pilot studies in this region focused on very small (i.e., N = 2) samples of quasar sight lines.…”

Section: Introductionmentioning

confidence: 99%

CONSTRAINTS ON THE UNIVERSAL C IV MASS DENSITY ATz∼ 6 FROM EARLY INFRARED SPECTRA OBTAINED WITH THE MAGELLAN FIRE SPECTROGRAPH

Simcoe

Cooksey

Matejek

et al. 2011

ApJ

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We present a new determination of the intergalactic C iv mass density at 4.3 < z < 6.3. Our constraints are derived from high signal-to-noise spectra of seven quasars at z > 5.8 obtained with the newly commissioned Folded-Port Infrared Echellette (FIRE) spectrograph on the Magellan Baade telescope, coupled with six observations of northern objects taken from the literature. We confirm the presence of a downturn in the C iv abundance at z = 5.66 by a factor of 4.1 relative to its value at z = 4.96, as measured in the same sight lines. In the FIRE sample, a strong system previously reported in the literature as C iv at z = 5.82 is re-identified as Mg ii at z = 2.78, leading to a substantial downward revision in Ω C iv for these prior studies. Additionally, we confirm the presence of at least two systems with low-ionization C ii, Si ii, and O i absorption but relatively weak signal from C iv. The latter systems may be of interest if the downward trend in Ω C iv at high redshift is driven in part by ionization effects.

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Discovery of a redshift 6.13 quasar in the UKIRT infrared deep sky survey

Cited by 80 publications

References 45 publications

STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES ATz∼ 6: NEW INSIGHTS FROM ALMA

STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES ATz∼ 6: NEW INSIGHTS FROM ALMA

The extinction law at high redshift and its implications

CONSTRAINTS ON THE UNIVERSAL C IV MASS DENSITY ATz∼ 6 FROM EARLY INFRARED SPECTRA OBTAINED WITH THE MAGELLAN FIRE SPECTROGRAPH

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