Major Contributor to Agn Feedback: VLT X-Shooter Observations of S Iv Balqso Outflows

Borguet, B.; Arav, Nahum; Edmonds, Doug; Chamberlain, Carter; Benn, Chris

doi:10.1088/0004-637x/762/1/49

Cited by 136 publications

(166 citation statements)

References 57 publications

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“…In fact, massive outflows have been confirmed in such objects by many X-ray observations (see Brandt & Gallagher 2000;Chartas et al 2003Chartas et al , 2009. Recently, Borguet et al (2013) detected the most energetic QSO outflow to date with a kinetic power of ∼ 10 46 erg s −1 and an associated mass flow rate of ∼ 400 M ⊙ yr −1 .…”

Section: Large Scale Qso Outflowsmentioning

confidence: 95%

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Lapi

Raimundo

Aversa

et al. 2014

ApJ

114

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We exploit the recent, wide samples of far-infrared (FIR) selected galaxies followed-up in X rays and of X-ray/optically selected active galactic nuclei (AGNs) followed-up in the FIR band, along with the classic data on AGN and stellar luminosity functions at high redshift z 1.5, to probe different stages in the coevolution of supermassive black holes (BHs) and host galaxies. The results of our analysis indicate the following scenario: (i) the star formation in the host galaxy proceeds within a heavily dust-enshrouded medium at an almost constant rate over a timescale 0.5 − 1 Gyr, and then abruptly declines due to quasar feedback; over the same timescale, (ii) part of the interstellar medium loses angular momentum, reaches the circum-nuclear regions at a rate proportional to the star formation and is temporarily stored into a massive reservoir/proto-torus wherefrom it can be promptly accreted; (iii) the BH grows by accretion in a self-regulated regime with radiative power that can slightly exceed the Eddington limit L/L Edd 4, particularly at the highest redshifts; (iv) for massive BHs the ensuing energy feedback at its maximum exceeds the stellar one and removes the interstellar gas, thus stopping the star formation and the fueling of the reservoir; (v) afterwards, if the latter has retained enough gas, a phase of supply-limited accretion follows exponentially declining with a timescale of about 2 e-folding times. We also discuss how the detailed properties and the specific evolution of the reservoir can be investigated via coordinated, high-resolution observations of starforming, strongly-lensed galaxies in the (sub-)mm band with ALMA and in the X-ray band with Chandra and the next generation X-ray instruments.

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Section: Large Scale Qso Outflowsmentioning

confidence: 95%

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Lapi

Raimundo

Aversa

et al. 2014

ApJ

114

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“…In this paper, we use the most conservativeṀ out ,Ṗ out , andĖ out values to characterize the outflows. These are the "timeaveraged thin shell" values in Rupke et al (2005c), which have also been used by a number of authors describing the energetics of the ionized and neutral phases of outflows (e.g., Rupke & Veilleux 2013a;Arav et al 2013;Borguet et al 2013;Heckman et al 2015), and are most appropriate for comparison with outflow models (e.g., Faucher-Giguère & Quataert 2012; Stern et al 2016;Thompson et al 2015).…”

Section: Estimating the Energeticsmentioning

confidence: 99%

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

González-Alfonso

Fischer

Spoon

et al. 2017

ApJ

143

204

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We report on the energetics of molecular outflows in 14 local Ultraluminous Infrared Galaxies (ULIRGs) that show unambiguous outflow signatures (P-Cygni profiles or high-velocity absorption wings) in the far-infrared lines of OH measured with the Herschel/PACS spectrometer. All sample galaxies are gas-rich mergers at various stages of the merging process. Detection of both ground-state (at 119 and 79 µm) and one or more radiatively-excited (at 65 and 84 µm) lines allows us to model the nuclear gas ( 300 pc) as well as the more extended components using spherically symmetric radiative transfer models. Reliable models and the corresponding energetics are found in 12 of the 14 sources. The highest molecular outflow velocities are found in buried sources, in which slower but massive expansion of the nuclear gas is also observed. With the exception of a few outliers, the outflows have momentum fluxes of (2 − 5) × L IR /c and mechanical luminosities of (0.1 − 0.3)% of L IR . The moderate momentum boosts in these sources ( 3) suggest that the outflows are mostly momentum-driven by the combined effects of AGN and nuclear starbursts, as a result of radiation pressure, winds, and supernovae remnants. In some sources (∼ 20%), however, powerful (10 10.5−11 L ⊙ ) AGN feedback and (partially) energy-conserving phases are required, with momentum boosts in the range 3 − 20. These outflows appear to be stochastic, strong-AGN feedback events that occur throughout the merging process. In a few sources, the outflow activity in the innermost regions has subsided in the last ∼ 1 Myr. While OH traces the molecular outflows at sub-kpc scales, comparison of the masses traced by OH with those previously inferred from tracers of more extended outflowing gas suggests that most mass is loaded (with loading factors ofṀ /SFR = 1 − 10) from the central galactic cores (a few × 100 pc), qualitatively consistent with an ongoing inside-out quenching of star formation. Outflow depletion timescales are < 10 8 yr, shorter than the gas consumption timescales by factors of 1.1 − 15, and are anti-correlated with the AGN luminosity.

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“…Our estimates are also consistent with previous studies using photoionization models and density-sensitive absorption lines to estimate BAL-outflow locations. Arav et al (2013) utilized the O vi absorption doublet and cloudy models to estimate a BALoutflow distance of 3 kpc, while Borguet et al (2013) and Chamberlain, Arav & Benn (2015) both used the S iv doublet to estimate an outflow distance of 100 pc and between 100-2000 pc from the SMBH, respectively.…”

Section: Bal Outflows Undergoing Ionization Changesmentioning

confidence: 99%

Broad absorption line disappearance and emergence using multiple-epoch spectroscopy from the Sloan Digital Sky Survey

McGraw

Brandt

Grier

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate broad absorption line (BAL) disappearance and emergence using a 470 BAL-quasar sample over ≤ 0.10-5.25 rest-frame years with at least three spectroscopic epochs for each quasar from the Sloan Digital Sky Survey. We identify 14 disappearing BALs over ≤ 1.73-4.62 rest-frame years and 18 emerging BALs over ≤ 1.46-3.66 rest-frame years associated with the C iv λλ1548,1550 and/or Si iv λλ1393,1402 doublets, and report on their variability behavior. BAL quasars in our dataset exhibit disappearing/emerging C iv BALs at a rate of 2.3 +0.9 −0.7 and 3.0 +1.0 −0.8 per cent, respectively, and the frequency for BAL to non-BAL quasar transitions is 1.7 +0.8 −0.6 per cent. We detect four re-emerging BALs over ≤ 3.88 rest-frame years on average and three re-disappearing BALs over ≤ 4.15 rest-frame years on average, the first reported cases of these types. We infer BAL lifetimes along the line of sight to be nominally < ∼ 100-1000 yr using disappearing C iv BALs in our sample. Interpretations of (re-)emerging and (re-)disappearing BALs reveal evidence that collectively supports both transverse-motion and ionization-change scenarios to explain BAL variations. We constrain a nominal C iv/Si iv BAL outflow location of < ∼ 100 pc from the central source and a radial size of > ∼ 1×10 −7 pc (0.02 au) using the ionization-change scenario, and constrain a nominal outflow location of < ∼ 0.5 pc and a transverse size of ∼0.01 pc using the transverse-motion scenario. Our findings are consistent with previous work, and provide evidence in support of BALs tracing compact flow geometries with small filling factors.

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Major Contributor to Agn Feedback: VLT X-Shooter Observations of S Iv Balqso Outflows

Cited by 136 publications

References 57 publications

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

The Coevolution of Supermassive Black Holes and Massive Galaxies at High Redshift

Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis

Broad absorption line disappearance and emergence using multiple-epoch spectroscopy from the Sloan Digital Sky Survey

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