Strong candidate for AGN feedback: VLT/X-shooter observations of BALQSO SDSS J0831+0354

Chamberlain, Carter; Arav, Nahum; Benn, Chris

doi:10.1093/mnras/stv572

Cited by 65 publications

(62 citation statements)

References 62 publications

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“…This is an order-ofmagnitude calculation given the approximations in the jet luminosity, the lifetime (t) of the jet, and the volume. Observations of other BAL quasars indicate that the kinetic luminosity of outflows can become as high as 10 46 erg s 1 - (Chamberlain et al 2015), which is close to the kinetic luminosity for the 3C 298 jet and would exert a pressure of 10 −8 dynes cm −2 . This means that a BAL-type wind could potentially drive the extended 3C 298 outflow.…”

Section: Virial Parameters and Gas Pressurementioning

confidence: 71%

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Vayner

Wright

Murray

et al. 2017

ApJ

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We present high angular resolution multiwavelength data of the 3C 298 radio-loud quasar host galaxy (z = 1.439) taken using the W.M. Keck Observatory OSIRIS integral field spectrograph (IFS) with adaptive optics, the Atacama Large Millimeter/submillimeter Array (ALMA), the Hubble Space Telescope (HST) WFC3, and the Very Large Array (VLA). Extended emission is detected in the rest-frame optical nebular emission lines Hβ, [O III], Hα, [N II], and [S II], as well as in the molecular lines CO (J = 3−2) and (J = 5−4). Along the path of the relativistic jets of 3C 298, we detect conical outflows in ionized gas emission with velocities of up to 1700 km s 1 -and an outflow rate of 450-1500 M yr 1 - extended over 12 kpc. Near the spatial center of the conical outflow, CO (J = 3−2) emission shows a molecular gas disk with a rotational velocity of±150 km s 1 -and total molecular mass (M H 2 ) of M 6.6 0.36 10 9 ´. On the blueshifted side of the molecular disk, we observe broad extended emission that is due to a molecular outflow with a rate of 2300 M yr 1 - and depletion timescale of 3 Myr. We detect no narrow Hαemission in the outflow regions, suggesting a limit on star formation of 0.3 M yr kpc. Quasardriven winds are evacuating the molecular gas reservoir, thereby directly impacting star formation in the host galaxy. The observed mass of the supermassive black hole is M 10 9.37 9.56  -,and we determine a dynamical bulge mass of M M 1 1.7 10 R bulge 10 1.6 kpc =´ -. The bulge mass of 3C 298 lies 2-2.5 orders of magnitude below the expected value from the local galactic bulge-supermassive black hole mass (M M bulge BH -) relationship. A second galactic disk observed in nebular emission is offset from the quasar by 9 kpc, suggesting that the system is an intermediate-stage merger. These results show that galactic-scale negative feedback is occurring early in the merger phase of 3C 298, well before the coalescence of the galactic nuclei and assembly on the local M M bulge BH -relationship.

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Section: Virial Parameters and Gas Pressurementioning

confidence: 71%

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Vayner

Wright

Murray

et al. 2017

ApJ

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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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“…This is one of the reasons we use slow jets (Sternberg et al 2007). Another reason is recent observations of such outflows from AGN (e.g., Chamberlain et al 2015). …”

Section: Heating the Icmmentioning

confidence: 99%

Heating the intracluster medium by jet-inflated bubbles

Hillel

Soker

2015

Mon. Not. R. Astron. Soc.

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We examine the heating of the intra-cluster medium (ICM) of cooling flow clusters of galaxies by jet-inflated bubbles and conclude that mixing of hot bubble gas with the ICM is more important than turbulent heating and shock heating. We use the pluto hydrodynamical code in full 3D to properly account for the inflation of the bubbles and to the multiple vortices induced by the jets and bubbles. The vortices mix some hot shocked jet gas with the ICM. For the parameters used by us the mixing process accounts for about four times as much heating as that by the kinetic energy in the ICM, namely, turbulence and sound waves. We conclude that turbulent heating plays a smaller role than mixing. Heating by shocks is even less efficient.

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Strong candidate for AGN feedback: VLT/X-shooter observations of BALQSO SDSS J0831+0354

Cited by 65 publications

References 62 publications

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

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

Heating the intracluster medium by jet-inflated bubbles

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