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Near Infrared Spectroscopy of High Redshift Active Galactic Nuclei. I. A Metallicity-Accretion Rate Relationship
Astrophysics · Submitted 24 Jun 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that metallicity, indicated by the N V/C IV line ratio, is primarily correlated with accretion rate, which is a function of luminosity and H_beta line-width.
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The abstract, sentence by sentence
We present new near infrared spectroscopic measurements of the H_beta region for a sample of 29 luminous high redshift quasars. We have measured the width of H_beta in those sources, and added archival H_beta width measurements, to create a sample of 92 active galactic nuclei (AGNs) for which H_beta width and rest-frame UV measurements of N V \lambda 1240 and C IV \lambda 1549 emission-lines are available. Our sample spans six orders of magnitude in luminosity and includes 31 radio-loud AGNs. It also includes 10 narrow-line Seyfert 1 galaxies and one broad absorption-line quasar. We find that metallicity, indicated by the N V/C IV line ratio, is primarily correlated with accretion rate, which is a function of luminosity and H_beta line-width. This may imply an intimate relation between starburst, responsible for the metal enrichment of the nuclear gas, and AGN fueling, represented by the accretion rate. The correlation of metallicity with luminosity, or black hole (BH) mass, is weaker in contrast with recent results which were based on measurements of the width of C IV. We argue that using C IV as a proxy to H_beta in estimating M_BH might be problematic and lead to spurious BH mass and accretion rate estimates in individual sources. We discuss the potential implications of our new result in the framework of the starburst-AGN connection and theories of BH growth.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present new near infrared spectroscopic measurements of the H_beta region for a sample of 29 luminous high redshift quasars. | contribution 0.96 | 0.97 | 0.02 | asserted 0.99 |
| s1 | We have measured the width of H_beta in those sources, and added archival H_beta width measurements, to create a sample of 92 active galactic nuclei (AGNs) for which H_beta width and rest-frame UV measurements of N V \lambda 1240 and C IV \lambda 1549 emission-lines are available. | method 0.78 | 0.91 | 0.02 | asserted 1.00 |
| s2 | Our sample spans six orders of magnitude in luminosity and includes 31 radio-loud AGNs. | contribution 0.69 | 0.70 | 0.02 | asserted 1.00 |
| s3 | It also includes 10 narrow-line Seyfert 1 galaxies and one broad absorption-line quasar. | contribution 0.71 | 0.52 | 0.02 | asserted 1.00 |
| s4 | We find that metallicity, indicated by the N V/C IV line ratio, is primarily correlated with accretion rate, which is a function of luminosity and H_beta line-width. | result 1.00 | 0.97 | 0.92 | asserted 1.00 |
| s5 | This may imply an intimate relation between starburst, responsible for the metal enrichment of the nuclear gas, and AGN fueling, represented by the accretion rate. | interpretation 1.00 | 0.25 | 0.08 | hedged possibility 1.00 |
| s6 | The correlation of metallicity with luminosity, or black hole (BH) mass, is weaker in contrast with recent results which were based on measurements of the width of C IV. | result 0.99 | 0.82 | 0.08 | asserted 1.00 |
| s7 | We argue that using C IV as a proxy to H_beta in estimating M_BH might be problematic and lead to spurious BH mass and accretion rate estimates in individual sources. | interpretation 0.95 | 0.39 | 0.09 | hedged possibility 0.53 |
| s8 | We discuss the potential implications of our new result in the framework of the starburst-AGN connection and theories of BH growth. | interpretation 0.89 | 0.36 | 0.04 | unclear 0.83 |
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The paper
Original abstract
We present new near infrared spectroscopic measurements of the H_beta region for a sample of 29 luminous high redshift quasars. We have measured the width of H_beta in those sources, and added archival H_beta width measurements, to create a sample of 92 active galactic nuclei (AGNs) for which H_beta width and rest-frame UV measurements of N V \lambda 1240 and C IV \lambda 1549 emission-lines are available. Our sample spans six orders of magnitude in luminosity and includes 31 radio-loud AGNs. It also includes 10 narrow-line Seyfert 1 galaxies and one broad absorption-line quasar. We find that metallicity, indicated by the N V/C IV line ratio, is primarily correlated with accretion rate, which is a function of luminosity and H_beta line-width. This may imply an intimate relation between starburst, responsible for the metal enrichment of the nuclear gas, and AGN fueling, represented by the accretion rate. The correlation of metallicity with luminosity, or black hole (BH) mass, is weaker in contrast with recent results which were based on measurements of the width of C IV. We argue that using C IV as a proxy to H_beta in estimating M_BH might be problematic and lead to spurious BH mass and accretion rate estimates in individual sources. We discuss the potential implications of our new result in the framework of the starburst-AGN connection and theories of BH growth.
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References
How the literature uses it
11 arXiv papers cite this in 13 sentences
Papers citing it · 6 sentences without a confident label
Uses its data or values 7 papers
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TON–618 is widely cited as one of the most massive BH candidates known, with a virial mass estimate of order $6.6×10^10 M_⊙$ [ref] .
G(2) Glueball Boson Stars as Restricted Kerr Mimickers in the Thomas--Fermi Limit · TON–618 bound as a decisive selection criterion · 0.93
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The current heaviest BH is associated with the quasar TON 618 and has a mass of $7 ×10^10 M_⊙$ [ref] , while the second heaviest, at the centre of the galaxy IC 1101, has a mass inferred from its radio emission of $4 ×10^10 M_⊙$ [ref] .
Constraints on Stupendously Large Black Holes · Introduction · 0.97
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In addition, there exist more massive black holes, such as Ton 618, whose mass is estimated to be $M = 6.6 ×10^10 M_⊙$, with a dark matter halo's characteristic density of $1.4 ×10^7 M_⊙/kpc^3$ and a characteristic scale of $500 kpc$ [ref] ; the dark matter halo parameters satisfy $k ≈10^4 M$ and $h ≈10^8 M$.
Periodic orbits and their gravitational waves in EMRIs: supermassive black hole affected by galactic dark matter halos · Spacetime Metric · 0.98
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