The [O<scp>iii</scp>] Emission‐Line Nebula of the<i>z</i>= 3.594 Radio Galaxy 4C +19.71

Armus, L.; Soifer, B. T.; Murphy, Thomas W.; Neugebauer, G.; Evans, A. S.; Matthews, K.

doi:10.1086/305270

Cited by 17 publications

(27 citation statements)

References 62 publications

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“…We find that the [O III] λ 5007 line contributes 36% (0.5 mag) to the K S -band flux (the Hβ line is much weaker and can be safely ignored). This value is comparable to the 45% contribution in the z = 3.594 radio galaxy MG J2144+1928 (Armus et al 1998), and to the 34% average contribution in a sample four radio galaxies where the [O III] λ 5007 line falls in the K-band (Eales & Rawlings 1993). After the emission line contribution is removed, the 64 kpc K-band magnitude (K = 18.79±0.03) is consistent with those for powerful HzRGs at this redshift .…”

Section: Identification and Spectroscopy Of The Optical/near-ir Composupporting

confidence: 80%

CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

Breuck

Neri²,

Morganti³

et al. 2003

A&A

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Abstract. We present results of a comprehensive multi-frequency study of the radio galaxy B3 J2330+3927. The 1. 9 wide radio source, consisting of 3 components, is bracketed by 2 objects in our Keck K-band image. Optical and near-IR Keck spectroscopy of these two objects yield z = 3.087 ± 0.004. The brightest (K = 18.8) object has a standard type II AGN spectrum, and is the most likely location of the AGN, which implies a one-sided jet radio morphology. Deep 113 GHz observations with the IRAM Plateau de Bure Interferometer reveal CO J = 4−3 emission, which peaks at the position of the AGN. The CO line is offset by 500 km s −1 from the systemic redshift of the AGN, but corresponds very closely to the velocity shift of an associated H I absorber seen in Lyα. This strongly suggests that both originate from the same gas reservoir surrounding the AGN host galaxy. Simultaneous 230 GHz interferometer observations find a ∼3× lower integrated flux density when compared to single dish 250 GHz observations with MAMBO at the IRAM 30 m telescope. This can be interpreted as spatially resolved thermal dust emission at scales of 0. 5 to 6 . Finally, we present a τ < 1.3% limit to the H I 21 cm absorption against the radio source, which represents the seventh nondetection out of 8 z > 2 radio galaxies observed to date with the WSRT. We present mass estimates for the atomic, neutral, and ionized hydrogen, and for the dust, ranging from M(H I) = 2 × 10 7 M derived from the associated H I absorber in Lyα up to M(H 2 ) = 7 × 10 10 M derived from the CO emission. This indicates that the host galaxy is surrounded by a massive reservoir of gas and dust. The K-band companion objects may be concentrations within this reservoir, which will eventually merge with the central galaxy hosting the AGN.

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Section: Identification and Spectroscopy Of The Optical/near-ir Composupporting

confidence: 80%

CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

Breuck

Neri²,

Morganti³

et al. 2003

A&A

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“…From detailed studies of AGNs at low redshifts, it is known that the NLRs and the extended NLRs can exhibit complex morphologies over hundreds of parsecs to kiloparsec scales (e.g., Pogge 1989 ;Wilson & Tsvetanov 1994). At high redshifts, the emission-line nebula around powerful AGNs can be quite spectacular, reaching sizes of 10È100 kpc (e.g., McCarthy, Spinrad, & van Breugel 1995 ;Armus et al 1998). If the NLR of FSC 10214]4724 has similar properties, its appearance through Ðlters isolating speciÐc UV and optical emission lines should be quite di †erent from its broad band, continuum morphology.…”

Section: Future Observationsmentioning

confidence: 99%

[ITAL]Hubble Space Telescope[/ITAL] Imaging Polarimetry of the Gravitational Lens FSC 10214+4724

Nguyen

Eisenhardt

Werner

et al. 1999

The Astronomical Journal

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We present imaging polarimetry of the extremely luminous, redshift 2.3 IRAS source FSC 10214]4724. The observations were obtained with HST Ïs Faint Object Camera in the F437M Ðlter, which is free of strong emission lines. The long arc is unresolved to FWHM in the transverse 0A .7 0A .04 direction and has an integrated polarization of 28%^3%, in good agreement with ground-based observations. The polarization position angle varies along the arc by up to 35¡. The overall position angle is 62¡^3¡ east of north. No counterimage is detected to B \ 27.5 mag (3 p), giving an observed arc to counterimage Ñux ratio greater than 250, considerably greater than the Ñux ratio of 100 measured previously in the I band. This implies that the conÐguration of the object in the source plane at the B band is di †erent from that at I band and/or that the lensing galaxy is dusty.

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“…Interestingly, longslit spectroscopy of powerful radio galaxies at z ≥ 1 (and in a few cases at lower redshifts) revealed strongly distorted emission line kinematics, with velocities often exceeding ∼1000 km s −1 along the axis of the radio jet (e.g., Tadhunter 1991;McCarthy et al 1996;Evans 1998;Baum & McCarthy 2000;Villar-Martín et al 1999;Inskip et al 2002;Clark et al 1998;Best et al 1997). Similarly, [OIII]λ5007 narrow-band imaging of 4C 19.71 at z ∼ 3.6 revealed a giant emission line region extending over ∼74 kpc (Armus et al 1998). This emission line region, corresponding to an ionized gas mass of 10 8−9 M aligns roughly with the axis of the radio jet, which led Armus et al to suspect that the jet and the nebulosity may be physically related.…”

Section: Introductionmentioning

confidence: 98%

Evidence for powerful AGN winds at high redshift: dynamics of galactic outflows in radio galaxies during the “Quasar Era”

Nesvadba

Lehnert²,

Breuck

et al. 2008

A&A

342

449

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AGN feedback now appears as an attractive mechanism to resolve some of the outstanding problems with the "standard" cosmological models, in particular those related to massive galaxies. At low redshift, evidence is growing that gas cooling and star formation may be efficiently suppressed by mechanical energy input from radio sources. To directly constrain how this may influence the formation of massive galaxies near the peak in the redshift distribution of powerful quasars, z ∼ 2, we present an analysis of the emission-line kinematics of 3 powerful radio galaxies at z ∼ 2−3 (HzRGs) based on rest-frame optical integral-field spectroscopy obtained with SINFONI on the VLT. The host galaxies of powerful radio-loud AGN are among the most massive galaxies, and thus AGN feedback may have a particularly clear signature in these galaxies. We find evidence for bipolar outflows in all HzRGs, with kinetic energies that are equivalent to 0.2% of the rest-mass of the supermassive black hole. Observed total velocity offsets in the outflows are ∼800−1000 km s −1 between the blueshifted and redshifted line emission, and FWHMs ∼ 1000 km s −1 suggest strong turbulence. Line ratios allow to measure electron temperatures, ∼10 4 K from [OIII]λλλ4363, 4959, 5007 at z ∼ 2, electron densities (∼500 cm −3 ) and extinction (A V ∼ 1−4 mag). Ionized gas masses estimated from the Hα luminosity are of order 10 10 M , similar to the molecular gas content of HzRGs, underlining that these outflows may indicate a significant phase in the evolution of the host galaxy. The total energy release of ∼10 60 erg during a dynamical time of ∼10 7 yrs corresponds to about the binding energy of a massive galaxy, similar to the prescriptions adopted in galaxy evolution models. Geometry, timescales and energy injection rates of order 10% of the kinetic energy flux of the jet suggest that the outflows are most likely driven by the radio source. The global energy density release of ∼10 57 erg s −1 Mpc −3 may also influence the subsequent evolution of the HzRG by enhancing the entropy and pressure in the surrounding halo and facilitating ram-pressure stripping of gas in satellite galaxies that may contribute to the subsequent mass assembly of the HzRG through low-dissipation "dry" mergers.

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The [Oiii] Emission‐Line Nebula of thez= 3.594 Radio Galaxy 4C +19.71

Cited by 17 publications

References 62 publications

CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

[ITAL]Hubble Space Telescope[/ITAL] Imaging Polarimetry of the Gravitational Lens FSC 10214+4724

Evidence for powerful AGN winds at high redshift: dynamics of galactic outflows in radio galaxies during the “Quasar Era”

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