High‐Resolution Keck Spectra of the Associated Absorption Lines in 3C 191

Hamann, F.; Barlow, Tom A.; Chaffee, F.; Foltz, C. B.; Weymann, R. J.

doi:10.1086/319733

Cited by 149 publications

(199 citation statements)

References 65 publications

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“…Velocity and ionization dependent partial covering is often seen in NALs Hamann et al 2001), and has also been reported for mini-BAL and BAL QSOs (Arav et al 1999;Srianand & Petitjean 2000;de Kool et al 2001de Kool et al , 2002bHall et al 2003). The partial covering proves the intrinsic nature of the absorbers.…”

Section: Discussionmentioning

confidence: 56%

“…Large distances have been inferred from the presence of C  or Si  absorption in two other NALs which are known to be intrinsic absorbers due to partial covering: 20 kpc for 3C 191 (Hamann et al 2001) 2 , and >570 pc for APM 08279+5255 (Srianand & Petitjean 2000). A related but distinct technique is the use of numerous Fe  absorption lines to estimate absorber distances.…”

Section: Discussionmentioning

confidence: 99%

“…The ionization parameter U is constrained by the simultaneous presence of Mg  and N  in the narrow component A1, which requires −2.8 < ∼ log U < ∼ −2.5 for ionization fractions >1% for both ions, according to the calculations of Hamann & Ferland (1999). We adopt log U = −2.8 for ease of comparison with Hamann et al (2001). We estimate L LL ≈ 2.5 × 10 30 ergs s −1 Hz −1 by extrapolating the flux measured in the low-resolution SDSS spectrum (assuming a cosmology with H 0 = 70 km s −1 Mpc −1 , Ω M = 0.3, and Ω Λ = 0.7, Pen et al 1999).…”

Section: Absorption From Excited Levels: Electron Density and Distancmentioning

confidence: 99%

“…We estimate L LL ≈ 2.5 × 10 30 ergs s −1 Hz −1 by extrapolating the flux measured in the low-resolution SDSS spectrum (assuming a cosmology with H 0 = 70 km s −1 Mpc −1 , Ω M = 0.3, and Ω Λ = 0.7, Pen et al 1999). Adopting n H ≈ n e , and α = −1.6, again for ease of comparison with Hamann et al (2001), we find a distance 9 kpc ≤ r ≤ 37 kpc. This range of values reflects only the uncertainties on n e ; the distance would be 30% smaller if we had used log U = −2.5.…”

Section: Absorption From Excited Levels: Electron Density and Distancmentioning

confidence: 99%

“…While it is known that NALs may form in various environments (Hamann et al 2001 and references therein), it is not clear whether at least some of them are directly related to the BAL phenomenon. In some rare cases, NALs and BALs may be observed in the same quasar, providing an opportunity to directly investigate this issue.…”

Section: Introductionmentioning

confidence: 99%

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VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

Hutsemékers

Brinkmann²

2004

A&A

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Abstract. We analyse high-resolution VLT+UVES spectra of the low-ionization intrinsic absorber observed in the BAL QSO SDSS J001130.56+005550.7. Two narrow absorption systems at velocities −600 km s −1 and −22 000 km s −1 are detected. The low-velocity system is part of the broad absorption line (BAL), while the high-velocity one is well detached. While most narrow absorption components are only detected in the high-ionization species, the lowest velocity component is detected in both highand low-ionization species, including in the excited Si  and C  lines. From the analysis of doublet lines, we find that the narrow absorption lines at the low-velocity end of the BAL trough are completely saturated but do not reach zero flux, their profiles being dominated by a velocity-dependent covering factor. The covering factor is significantly smaller for Mg  than for Si  and N , which demonstrates the intrinsic nature of absorber. From the analysis of the excited Si  and C  lines in the lowest velocity component, we find an electron density 10 3 cm −3 . Assuming photoionization equilibrium, we derive a distance 20 kpc between the low-ionization region and the quasar core. The correspondence in velocity of the high-and low-ionization features suggests that all these species must be closely associated, hence formed at the same distance of ∼20 kpc, much higher than the distance usually assumed for BAL absorbers.

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Section: Discussionmentioning

confidence: 56%

Section: Discussionmentioning

confidence: 99%

Section: Absorption From Excited Levels: Electron Density and Distancmentioning

confidence: 99%

Section: Absorption From Excited Levels: Electron Density and Distancmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

Hutsemékers

Brinkmann²

2004

A&A

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Metal Enrichment Processes

Schindler

Diaferio

Clusters of Galaxies

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Active Galaxies in the UV

Kollatschny

Wang

Fundamental Questions in Astrophysics: Guidelines for Future UV Observatories

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In this article we present different aspects of AGN studies demonstrating the importance of the UV spectral range. Most important diagnostic lines for studying the general physical conditions as well as the metalicities in the central broad line region in AGN are emitted in the UV. The UV/FUV continuum in AGN excites not only the emission lines in the immediate surrounding but it is responsible for the ionization of the intergalactic medium in the early stages of the universe. Variability studies of the emission line profiles of AGN in the UV give us information on the structure and kinematics of the immediate surrounding of the central supermassive black hole as well as on its mass itself. 2 Wolfram Kollatschny, Wang Ting-GuiActive Galactic Nuclei (AGN) are the most luminous objects in the universe.Their luminosities, their spectral energy distribution from the radio to the γray range, as well as their emission line ratios cannot be generated by normal stars. Galaxies containing an active nucleus are called active galaxies. We divide the AGN in different subclasses such as Quasars, Seyfert galaxies and Liners.Many aspects of the generation of the energy in AGN are still unknown. Accretion of gas onto a central supermassive black hole (SMBH) is generally accepted to be the dominant physical process generating the enormous energies we are observing (Rees [Rees (1984)]). The accretion flow is the source of the non-thermal continuum emission in the UV, X-ray and optical. The spectral energy distribution (SED) of the non-thermal continuum emission in typical AGN has its maximum in the UV. The central continuum source ionizes the circumnuclear gas in the so called broad line region (BLR) and narrow line region (NLR). The majority of the most important emission lines are emitted in the UV spectral range.The overall continuum distribution as well as the UV spectral lines (narrow emission lines, broad emission lines, absorption lines) are tracers of the physical conditions of those regions where these emission lines originate.Active Galaxies in the UV 3

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High‐Resolution Keck Spectra of the Associated Absorption Lines in 3C 191

Cited by 149 publications

References 65 publications

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

Metal Enrichment Processes

Active Galaxies in the UV

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