The absorption spectrum of nuclear gas in Q0059-2735

Wampler, E. J.; Чугай, Н. Н.; Petitjean, P.

doi:10.1086/175551

Cited by 82 publications

(98 citation statements)

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“…Using this method, r ∼ 310 pc has been measured for the low-velocity system in FIRST J084044.5+363328, whereas r ∼ 1.35 pc is found for the high-velocity system in the same object using different diagnostic (de Kool et al 2002b). However, analysis of the similar NAL in FIRST J121442.3+280329 yielded a small distance range ∼1−30 pc for the entire outflow (de Kool et al 2002a), similar to that found for LBQS 0059-2735 (Wampler et al 1995). The largest distance found by this method has been for the low-ionization BAL in FIRST J104459.6+365605…”

Section: Discussionsupporting

confidence: 75%

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: Discussionsupporting

confidence: 75%

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

Hutsemékers

Brinkmann²

2004

A&A

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“…Williams et al (1975) already estimated a density of n e D cm~3 and a radial distance of R D 10 kpc for the AAL 1000 region in 3C 191. We reobserved 3C 191 with higher spectral resolution and wider wavelength coverage to (1) obtain more reliable densities as a function of velocity, (2) search for Fe II* AALs, which might be revealing of a much higher density environment (Wampler et al 1995 ;Halpern et al 1996), (3) revisit the question of this absorberÏs origin and location, and (4) obtain better constraints on the AAL region dynamics, abundances, and overall physical structure.…”

Section: Introductionmentioning

confidence: 99%

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

Hamann

Barlow

Chaffee

et al. 2001

ApJ

149

182

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Associated absorption lines (AALs) are valuable probes of the gaseous environments near quasars. Here we discuss high-resolution (6.7 km s~1) spectra of the AALs in the radio-loud quasar 3C 191 (redshift z \ 1.956). The measured AALs have ionizations ranging from Mg I to N V and multicomponent proÐles that are blueshifted by D400 to D1400 km s~1 relative to the quasarÏs broad emission lines. These data yield the following new results : (1) The strengths of excited-state Si II* AALs indicate a density of D300 cm~3 in the Si`gas. (2) If the gas is photoionized, this density implies a distance of D28 kpc from the quasar. Several arguments suggest that all of the lines form at approximately this distance. (3) The characteristic Ñow time from the quasar is thus D3 ] 107 yr. (4) Strong Mg I AALs identify neutral gas with very low ionization parameter and high density. We estimate n HZ 5 ] 104 cm~3 in this region, compared to D15 cm~3 where the N V lines form. (5) The total column density is cm~2 in the neutral gas and cm~2 in the moderately ionized] 1020 regions. These column densities are consistent with 3C 191Ïs strong soft X-ray Ñux and the implied absence of soft X-ray absorption. (6) The total mass in the AAL outÑow is M D 2 ] 109 assuming M _ , a global covering factor (as viewed from the quasar) of D10%. (7) The absorbing gas only partially covers the background light source(s) along our line(s) of sight, requiring absorption in small clouds or Ðlaments less than 0.01 pc across. The ratio implies that the clouds have radial (line-of-sight) N H /n H thicknesses pc. These properties might characterize a subclass of AALs that are physically related [0.2 to quasars but form at large distances. We propose a model for the absorber in which pockets of dense neutral gas are surrounded by larger clouds of generally lower density and higher ionization. This outÑowing material might be leftover from a blowout associated with a nuclear starburst, the onset of quasar activity, or a past broad absorption line (BAL) wind phase.

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“…Prior to our program, only five analyses in the literature had some handle on these two quantities, with uncertainties of 1-3 orders of magnitude (Wampler et al 1995;de Kool et al 2001de Kool et al , 2002aHamann et al 2001). Our research group developed analysis techniques that greatly improve the accuracy in extractingṀ andĖ k .…”

Section: Quantifying the Contribution Of Bal Outflows To Agn Feedbackmentioning

confidence: 99%

The Impact of BAL Outflows on Cosmological Structure Formation

Arav

2009

Proc. IAU

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Abstract. Quasar feedback has been invoked as a major mechanism for influencing large-scale cosmological structure. To quantify to what extent they affect the real universe, one needs to measure the mechanical energy output of quasars and assess the ability of this energy to produce the feedback. We have developed an observational/modeling program that has yielded the first reliable kinetic luminosity determinations of quasar broad absorption line (BAL) outflows, and have demonstrated that energetically they are indeed a major contributor to AGN feedback.

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The absorption spectrum of nuclear gas in Q0059-2735

Cited by 82 publications

References 0 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

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

The Impact of BAL Outflows on Cosmological Structure Formation

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