Radiative pressure feedback by a quasar in a galactic bulge

Fabian, A. C.; Celotti, A.; Erlund, Mary

doi:10.1111/j.1745-3933.2006.00234.x

Cited by 112 publications

(128 citation statements)

References 32 publications

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“…Best et al 2006Best et al , 2007Bower et al 2006;Croton et al 2006;Fabian, Celotti & Erlund 2006). This feedback can occur because the enormous energy output of the AGN can be injected into the surrounding medium, possibly also the fuel source of the AGN, via ionizing radiation and/or relativistic jets, thereby providing enough energy to affect star formation in the host galaxy.…”

Section: Introductionmentioning

confidence: 99%

Radio-AGN feedback: when the little ones were monsters

Williams

Röttgering

2015

Monthly Notices of the Royal Astronomical Society

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We present a study of the evolution of the fraction of radio-loud active galactic nuclei (AGN) as a function of their host stellar mass. We make use of two samples of radio galaxies: one in the local Universe, 0.01 < z ≤ 0.3, using a combined SDSS-NVSS (Sloan Digital Sky Survey NRAO Very Large Array Sky Survey) sample and the other at higher redshifts, 0.5 < z ≤ 2, constructed from the VLA-COSMOS_DEEP Radio Survey at 1.4 GHz and a K s -selected catalogue of the COSMOS/UltraVISTA field. We observe an increase of more than an order of magnitude in the fraction of lower mass galaxies (M * < 10 10.75 M ) which host radio-loud AGN with radio powers P 1.4 GHz > 10 24 W Hz −1 at z ∼ 1-2 while the radio-loud fraction for higher mass galaxies (M * > 10 11.25 M ) remains the same. We argue that this increase is driven largely by the increase in cold or radiative mode accretion with increasing cold gas supply at earlier epochs. The increasing population of low-mass radio-loud AGN can thus explain the upturn in the radio luminosity function at high redshift which is important for understanding the impact of AGN feedback in galaxy evolution.

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Section: Introductionmentioning

confidence: 99%

Radio-AGN feedback: when the little ones were monsters

Williams

Röttgering

2015

Monthly Notices of the Royal Astronomical Society

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“…The growth phase ends when no gas remains, if, for example, star formation consumes all the gas. Alternatively, the AGN may blow the gas outside its host galaxy (Fabian et al 2006), curtailing star formation. In this case, the AGN must have sufficient luminosity for Tables 1 and 2 are available in electronic form at http://www.aanda.org the radiation-pressure force outwards to exceed the gravitational force inwards.…”

Section: Introductionmentioning

confidence: 99%

A glance at the host galaxy of high-redshift quasars using strong damped Lyman-αsystems as coronagraphs

Finley

Petitjean

Pâris

et al. 2013

A&A

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We searched quasar spectra from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) for the rare occurrences where a strong damped Lyman-α absorber (DLA) blocks the Broad Line Region emission from the quasar and acts as a natural coronagraph to reveal narrow Lyα emission from the host galaxy. We define a statistical sample of 31 DLAs in Data Release 9 (DR9) with log N(H i) ≥ 21.3 cm −2 located at less than 1500 km s −1 from the quasar redshift. In 25% (8) of these DLAs, a strong narrow Lyα emission line is observed with flux ∼25 × 10 −17 erg s −1 cm −2 on average. For DLAs without this feature in their troughs, the average 3-σ upper limit is <0.8 × 10 −17 erg s −1 cm −2 . Our statistical sample is nearly 2.5 times larger than the anticipated number of intervening DLAs in DR9 within 1 500 km s −1 of the quasar redshift. We also define a sample of 26 DLAs from DR9 and DR10 with narrow Lyα emission detected and no limit on the H i column density to better characterize properties of the host galaxy emission. Analyzing the statistical sample, we do not find substantial differences in the kinematics, metals, or reddening for the two populations with and without emission detected. The highly symmetric narrow Lyα emission line profile centered in the HI trough indicates that the emitting region is separate from the absorber. The luminosity of the narrow Lyα emission peaks is intermediate between that of Lyα emitters and radio galaxies, implying that the Lyα emission is predominantly due to ionizing radiation from the AGN. Galaxies neighboring the quasar host are likely responsible for the majority (>75%) of these DLAs, with only a minority (<25%) arising from H i clouds located in the AGN host galaxy.

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“…However, it was also found that more massive galaxies should be in the high-luminosity, permanent cooling-flow regime, so that for massive systems, putative hosts of luminous cooling flows, the mass problem was still unsolved; in addition, if this gas is accreted on the central SMBH, then a bright QSO should be observed in all X-ray luminous elliptical galaxies. These considerations lead naturally to the study of gas accretion on SMBHs at the center of elliptical galaxies, to explore the possibility that radiative and mechanical feedback due to accretion is the solution of the mass disposal problem in cooling flow, and it is the explanation of the maintenance of "small" SMBH masses in presence of very large amounts of recycled gas, and of the shut down of QSO activity in massive ellitpicals (e.g., see [176,28,55]). …”

Section: Introductionmentioning

confidence: 99%

AGN Feedback in Elliptical Galaxies: Numerical Simulations

Ciotti

Ostriker

2011

Hot Interstellar Matter in Elliptical Galaxies

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The importance of feedback (radiative and mechanical) from massive black holes at the centers of elliptical galaxies is not in doubt, given the well established relation among black hole mass and galaxy optical luminosity. Here, with the aid of high-resolution hydrodynamical simulations, we discuss how this feedback affects the hot ISM of isolated elliptical galaxies of different mass. The cooling and heating functions include photoionization plus Compton heating, the radiative transport equations are solved, and the mechanical feedback due to the nuclear wind is also described on a physical basis; star formation is considered. In the medium-high mass galaxies the resulting evolution is highly unsteady. At early times major accretion episodes caused by cooling flows in the recycled gas produced by stellar evolution trigger AGN flaring: relaxation instabilities occur so that duty cycles are small enough to account for the very small fraction of massive ellipticals observed to be in the QSO-phase, when the accretion luminosity approaches the Eddington luminosity. At low redshift all models are characterized by smooth, very sub-Eddington mass accretion rates. The mass accumulated by the central black hole is limited to range observed today, even though the mass lost by the evolving stellar population is roughly two order of magnitude larger than the black hole masses observed in elliptical galaxies.

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Radiative pressure feedback by a quasar in a galactic bulge

Cited by 112 publications

References 32 publications

Radio-AGN feedback: when the little ones were monsters

Radio-AGN feedback: when the little ones were monsters

A glance at the host galaxy of high-redshift quasars using strong damped Lyman-αsystems as coronagraphs

AGN Feedback in Elliptical Galaxies: Numerical Simulations

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