Extreme Gas Kinematics in the z = 2.2 Powerful Radio Galaxy MRC 1138–262: Evidence for Efficient Active Galactic Nucleus Feedback in the Early Universe?

By N. Nesvadba, M. Lehnert, F. Eisenhauer, A. Gilbert, M. Tecza, R. Abuter. 2006

213 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

AGN wind scaling relations and the co-evolution of black holes and galaxies (2017, methodology): “Nesvadba et al. (2006, 2008) found 〈ne〉 = 240−570 cm−3 and 〈ne〉 = 300−1000 cm−3 in two z ∼ 2 radio galaxies.”
Radiative Feedback from Massive Black Holes in Elliptical Galaxies: AGN Flaring and Central Starburst Fueled by Recycled Gas (2007, background): “Also, signs of star formation in high-z objects such as those detected in UV (GALEX ) and IR (Spitzer), or accompanyingAGNs (X-ray), should be common (see, e.g., Yan et al. 2006; Nesvadba et al. 2006, Simoes Lopes et al. 2007), with IR luminosity peaks of 1046 ergs s 1.”
Evidence for powerful AGN winds at high redshift: dynamics of galactic outflows in radio galaxies during the “Quasar Era” (2008, methodology): “To address the question whether MRC1138-262 is a “one-off”, or whether AGN feedback is a common phenomenon in HzRGs, we continue the analysis of Nesvadba et al. (2006b, 2007a), adding another three HzRGs with near-infrared integral-field data at z≈ 2− 3.”
Energetic galaxy-wide outflows in high-redshift ultraluminous infrared galaxies hosting AGN activity (2012, methodology): “…accretion-related outflows are predicted to bemost prevalent, integral-field unit (IFU) observations of high-redshift radio galaxies (HzRGs, atz ≈ 2–3; Nesvadba et al. 2006, 2008) have showed that kpc-scale energetic outflows are present inat least a fraction of the high-redshift galaxy population.”
Distant radio galaxies and their environments (2008, methodology): “Nesvadba et al (2006) recently carried out an important study of the Spiderweb Galaxy with an integral field spectrograph in the optical rest frame.”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “…of bright quasar hosts have now been observed in which jets or winds appear to be strongly impacting the host galaxy and halo gas (Zirm et al. 2005; Nesvadba et al. 2006; Nesvadba et al. 2007; Reuland et al. 2007), or in which BAL quasar winds are entraining gas at 103Y104 km s 1 velocities on…”
Mechanical feedback from active galactic nuclei in galaxies, groups and clusters (2012, methodology): “For example, energetic outflows have been detected using emission and absorption line features from distant radio galaxies (e.g. Nesvadba et al 2006, Morganti et al 2007, Lehnert et al 2011), quasars (e.g. de Kool et al 2001, Chartas et al 2007, Rupke and Veilleux 2011) and starburst galaxies…”
Kiloparsec-scale outflows are prevalent among luminous AGN: outflows and feedback in the context of the overall AGN population (2014, methodology): “We also consider the mass and energy injection rates assuming an energy conserving bubble in a uniform medium (e.g., Heckman et al. 1990; Veilleux et al. 2005; Nesvadba et al. 2006 and references there-in), which gives the relation: Ėout,M2 ≈ 1.5×1046r210v31000n0.”
DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, methodology): “We have compiled a set of 27 radio galaxies from the samples studied by Holt et al. (2008), Nesvadba et al. (2006, 2008, 2010), Torresi et al. (2012), Guillard et al. (2012), and the individual case of 3C 48 by Stockton et al. (2007).”
FEEDBACK IN LUMINOUS OBSCURED QUASARS (2011, background): “These values are consistent with those commonly seen in spatially resolved observations of extended NLRs and used in mass estimations (e.g., Nesvadba et al. 2006; Fu & Stockton 2009 and many others).”
Observations of feedback from radio-quiet quasars – II. Kinematics of ionized gas nebulae (2013, background): “…= 100 cm−3 (this is around the critical density of the lines and is what is inferred for the densities from [S II] in Greene et al. 2011; radio galaxies at z = 2–3 also have ne of a few 100 cm−3 as found by Nesvadba et al. 2006, 2008), we find Mgas = (0.2–1) × 109 M , with a median of 6 × 108 M .”
The realm of the galaxy protoclusters (2016, background): “The extended gas reservoirs around radio galaxies such as the Spiderweb Galaxy could perhaps in large part be explained by strong mechanical feedback from the radio jets (Nesvadba et al., 2006).”
Narrow-line region gas kinematics of 24 264 optically selected AGN: the radio connection (2013, background): “…fraction of optically selected AGNs overall, they are at least ∼10 times more common than the more radio luminous AGNs that are typically the focus of detailed studies of AGN outflows (e.g. Holt et al. 2003, 2008; Tadhunter et al. 2003; Nesvadba et al. 2006, 2008; Cano-Dı́az et al. 2012; see fig.”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, background): “We then use calculations presented in Villar-Mart́ın et al. 2008 to determine the [O iii]/Hβ ratios of such clouds (Figure 9, left panel labeled “Model 1”).”
AGN outflows and feedback twenty years on (2018, unknown): “One example is to assume a Sedov-Taylor like solution for a supernova remnant where a spherical bubble is expanding into a constant density medium[68, 57].”
Quasar feedback and the origin of radio emission in radio-quiet quasars (2014, background): “…specific examples of black-hole-driven winds have now been identified using a variety of observational techniques, both at low and at high redshifts (Nesvadba et al. 2006; Arav et al. 2008; Nesvadba et al. 2008; Moe et al. 2009; Dunn et al. 2010; Alexander et al. 2010; Harrison et al. 2012).”
Discovery of extreme [O III] λ5007 Å outflows in high-redshift red quasars (2015, methodology): “In ionized gas observations similar to ours, the median FWHM of [O III] seen by Nesvadba et al. (2006, 2007, 2008) in powerful high-redshift radio galaxies is ∼1300 km s−1, i.e. two to three times smaller than that of extremely red quasars, but in the most extreme cases such as the central regions…”
What drives the growth of black holes (2011, background): “IFU observations of powerful ( >∼ 1026 W Hz−1 at 1.4 GHz) radio-loud quasars have revealed outflows in [O iii] that are aligned with the radio jet axis over scales of ∼10 kpc, with v ∼ 1000 km s−1 and FWHM ∼ 1000 km s−1 (e.g. Nesvadba et al., 2006, 2007, 2008).”