Iron Emission in the z = 6.4 Quasar SDSS J114816.64+525150.3

By A. Barth, P. Martini, C. Nelson, Luis C. Ho. 2003

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We present near-infrared J- and K-band spectra of the z = 6.4 quasar SDSS J114816.64+525150.3 obtained with the NIRSPEC spectrograph at the Keck II telescope, covering the rest-frame spectral regions surrounding the C IV λ1549 and Mg II λ2800 emission lines. The iron emission blend at rest wavelength 2900-3000 Å is clearly detected, and its strength appears nearly indistinguishable from that of typical quasars at lower redshifts. The Fe II/Mg II ratio is also similar to values found for lower redshift quasars, demonstrating that there is no strong evolution in Fe/α broad-line emission ratios even out to z = 6.4. In the context of current models for iron enrichment from Type Ia supernovae (SNe Ia), this implies that the SN Ia progenitor stars formed at z ≳ 10. We apply the scaling relations of Vestergaard and of McLure & Jarvis to estimate the black hole mass from the widths of the C IV and Mg II emission lines and the ultraviolet continuum luminosity. The derived mass is in the range (2-6) × 109 M☉, with an additional uncertainty of a factor of 3 due to the intrinsic scatter in the scaling relations. This result is in agreement with the previous mass estimate of 3 × 109 M☉ by Willott, McLure, & Jarvis and supports their conclusion that the quasar is radiating close to its Eddington luminosity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a770dd1906344489e6955483a667d3303c65b903

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Stellar sources of dust in the high-redshift Universe (2009, background): “In fact, the detection of metal lines such as Fe (Barth et al. 2003), CII (Maiolino et al. 2005), and OI (in absorption, Becker et al. 2006) indicates that the ISM of the QSO host was significantly enriched by heavy elements.”
A SURVEY OF z ∼ 6 QUASARS IN THE SLOAN DIGITAL SKY SURVEY DEEP STRIPE. I. A FLUX-LIMITED SAMPLE AT zAB < 21 (2007, background): “…Germany 10 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 the Eddington limit (e.g. Barth et al. 2003; Vestergaard 2004; Jiang et al. 2006a; Kurk et al. 2007), revealing the rapid growth of central BHs at high redshift.”
Rapid Growth of High-Redshift Black Holes (2005, background): “We do not expect, therefore, that SDSS quasars are accreting above the Eddington value, consistently with observations (Barth et al. 2003, Willott, McLure & Jarvis 2003).”
The Radio-Loud Fraction of Quasars is a Strong Function of Redshift and Optical Luminosity (2006, background): “Their emission-line strengths and UV continuum shapes are very similar to those of low-redshift quasars (e.g., Barth et al. 2003; Pentericci et al. 2003; Fan et al. 2004), the emission line ratios indicate solar or supersolar metallicity in emission-line regions as found in low-redshift quasars…”
Quasars at z = 6: The Survival of the Fittest (2006, background): “This quasar, at z = 6.4, has estimates of the SMBH mass in the range (2− 6)× 109M⊙ (Barth et al. 2003; Willott et al. 2003).”
Early Growth and Efficient Accretion of Massive Black Holes at High Redshift (2003, background): “64+525150.3 based on both Mg ii (Willott et al. 2003a) and C iv line widths (Barth et al. 2003) are in agreement (but note that individual mass estimates based on scaling relationships may be uncertain by a factor 10 (Paper I); the factor 3 uncertainty is valid for statistical samples only). ton…”
The Type Ia Supernova Rate (2005, background): “…constrain Type Ia evolution at short time scales, such as studies of the distribution of SNe Ia relative to spiral arms (Maza & van den Bergh 1976; Bartunov 1994; McMillan & Ciardullo 1996; Petrosian et al. 2005) and the Fe content of high-redshift quasars (Barth et al. 2003; Dietrich et al. 2003).”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, background): “…important regime may determine SMBH mass growth in the Universe from z ∼ 10–20 to z ∼ 6–8 leading to black holes with masses of 109 M (Collin et al. 2002; Barth et al. 2003; Willott et al. 2005; Fan et al. 2006; Willott et al. 2010; Mortlock et al. 2011; Kawakatu & Ohsuga 2011; Fabian 2012) and…”
On the evolution of the black‐hole/spheroid mass ratio (2005, background): “The highest redshift quasar currently identified(z = 6.41) by the Sloan Digital Sky Survey (SDSSJ1148+5251; Fan et al. 2003) is believed to harbour a central black-hole of mass≃ 3 × 109 M⊙ (Willott, McLure & Jarvis 2003; Barth et al. 2003).”
Massive black hole seeds from low angular momentum material (2003, background): “Consider, for example the analysis of Barth et al. (2003), who have estimated a mass of M bh = (2–6) × 109 M for a black hole powering a z = 6.4 quasar found in the Sloan Digital Sky Survey.”
Formation of z~6 Quasars from Hierarchical Galaxy Mergers (2006, background): “However, the detection of metal lines (Walter et al. 2004; Barth et al. 2003; Maiolino et al. 2005), along with dust (Bertoldi et al. 2003a; Carilli et al. 2004; Robson et al. 2004; Charmandaris et al. 2004; Hines et al. 2006; Beelen et al. 2006), indicates that the interstellar medium (ISM) of…”
Formation of supermassive black holes (2010, background): “…jointly with 8-m class telescopes and large surveys, have made important breakthroughs, and observational cosmology probed capable of putting constraints on MBHs, when shining as quasars, up to high redshift (Fan et al, 2001b,a, 2004; Barth et al, 2003; Willott et al, 2003; Walter et al, 2004).”
Black Hole Masses and Enrichment of z ~ 6 SDSS Quasars (2007, methodology): “…by us are lower by a factor of a few than some previous measurements for individual quasars at z > 5.8 reported in the literature (Maiolino et al. 2003; Freudling et al. 2003; Iwamuro et al. 2004) but are consistent with others (Barth et al. 2003; Freudling et al. 2003; Iwamuro et al. 2004).”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, background): “This does not however relieve other problems with the hier- archical formation of galaxies, as there are massive systems well formed by z ∼ 6 in the form of QSOs that contain high metallicities (Barth et al. 2003) that might also contain massive galaxies.”
Gemini Near-Infrared Spectroscopy of Luminous z ∼ 6 Quasars: Chemical Abundances, Black Hole Masses, and Mg II Absorption (2007, methodology): “—TheMg ii emission line can bewell fitted by double Gaussians (e.g., Barth et al. 2003), with a weak component located on the blue side of a much stronger component.”
Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, background): “…accretion state may be responsible for much of the SMBH mass growth in the Universe; for instance, it might explain the paradox of having 109 M BHs already at z > 6, when the Universe was less than 1 Gyr old (Barth et al. 2003; Willott et al. 2005, 2010; Fan et al. 2006; Mortlock et al. 2011).”
Physical Properties of 15 Quasars at z ≳ 6.5 (2017, methodology): “Moreover, several studies show that quasars at z ∼6 are hosted in massive, already chemically evolved galaxies (e.g., Barth et al. 2003, Stern et al. 2003, Walter et al. 2003, De Rosa et al. 2011).”
BLACK HOLE MASS ESTIMATES AND EMISSION-LINE PROPERTIES OF A SAMPLE OF REDSHIFT z > 6.5 QUASARS (2013, background): “Previous NIR-spectroscopy works that studied the Fe ii/Mg ii line ratio in samples including high-z quasars (e.g., Barth et al. 2003; Dietrich et al. 2003; Iwamuro et al. 2004; Jiang et al. 2007; Kurk et al. 2007) showed an increase in the scatter of the measured Fe ii/Mg ii line ratios at z ∼ 6.”
Growth of Structure Seeded by Primordial Black Holes (2006, background): “…of supermassive black holes at high redshifts has attracted a great deal of attention since quasars have been discovered at redshifts of z > 6, implying that black holes as massive as 109 M (Fan et al. 2003; Barth et al. 2003; Willott et al. 2003) exist when the universe is less than 1 Gyr old.”