Extended optical line emission from 3C 293 - Radio jets propagating through a rotating gaseous disk

Breugel, Wil van; Heckman, T.; Butcher, H. R.; Miley, G. K.

doi:10.1086/161673

Cited by 43 publications

(46 citation statements)

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“…As found originally by van der Kruit & Searle (1981), the starlight distribution parallel to the disk plane in edge-on spirals, after bulge subtraction, is well expressed by the projection of a radially truncated exponential disk, with this truncation occurring at radii of several exponential scale lengths. Similar behavior is found in 0313À192 (Fig.…”

Section: Stellar Disksupporting

confidence: 57%

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The Spiral Host Galaxy of the Double Radio Source 0313?1921

Keel

White

Owen

et al. 2006

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We present new Hubble Space Telescope (HST ), Gemini South, and Chandra observations of the radio galaxy 0313À192, which hosts a 350 kpc double source and jets, even though previous data have suggested that it is a spiral galaxy. We measure the bulge scale and the luminosity, radial, and vertical profiles of disk starlight and consider the distributions of H ii regions and absorbing dust. In each case the HST data confirm its classification as an edge-on spiral galaxy, the only such system known to produce such an extended radio source of this kind. The Gemini near-IR images and Chandra spectral fit reveal a strongly obscured central active galactic nucleus (AGN), seen through the entire interstellar medium path length of the disk and showing X-ray evidence of additional absorption from warm or dense material close to the central object. We consider several possible mechanisms for producing such a rare combination of AGN and host properties, some combination of which may be at work. These include an unusually luminous bulge (suggesting a black hole of mass $8 ; 10 8 M ), the orientation of the jets near the pole of the gas-rich disk, and some evidence of a weak gravitational interaction that has warped the disk and could have enhanced fueling of the central engine. We detect an X-ray counterpart of the kiloparsec-scale radio jet emerging to the south; jet/ counterjet limits on both radio and X-ray regimes allow them to be symmetric if seen more than 15 from the plane of the sky, still consistent with the jet axes being within $30 of the poles of the gas-rich galaxy disk. A linear or disklike emission-line structure is seen around the nucleus, inclined by $20 to the stellar disk but nearly perpendicular to the jets; this may represent the aftermath of a galaxy encounter, in which gas is photoionized by a direct view of the nuclear continuum.

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Section: Stellar Disksupporting

confidence: 57%

“…Similarly, the profile of edge-on spiral disks perpendicular to the disk plane is well described by a single exponential, nearly independent of radius (van der Kruit & Searle 1981;de Grijs et al 1997). This also applies to 0313À192 (Fig.…”

Section: Stellar Diskmentioning

confidence: 99%

The Spiral Host Galaxy of the Double Radio Source 0313?1921

Keel

White

Owen

et al. 2006

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“…However, their results did not exclude ionization by shocks. Several detailed studies of individual objects have found morphological similarities between radio and line-emitting regions and kinematic evidence for shocks (e.g., van Breugel et al 1984avan Breugel et al , 1984bTadhunter 1991;Koekemoer & Bicknell 1998Villar-Martín et al 1999;Solórzano-Iñarrea et al 2001. The alignment of lineemitting regions with the axis of the radio jet in high-redshift radio galaxies has been interpreted as evidence for an anisotropic UV source and for a shock-induced continuum by the radio jet (Baum & McCarthy 2000;Best et al 1999).…”

Section: Jet Energy Fluxesmentioning

confidence: 99%

“…In powerful radio galaxies, the optical emission lines reveal the interaction between the radio plasma and the surrounding medium. Detailed studies of individual radio galaxies suggest that the radio and line-emitting regions are spatially coincident and reveal kinematic evidence for shocks and acceleration of the line-emitting material by the jet and overpressured lobes (e.g., van Breugel et al 1984avan Breugel et al , 1984bTadhunter 1991;Koekemoer & Bicknell 1998Villar-Martín et al 1999;Solórzano-Iñarrea et al 2001.…”

Section: Introductionmentioning

confidence: 99%

Radio-ExcessIRASGalaxies. IV. Optical Spectroscopy

Buchanan¹,

McGregor²,

Bicknell³

et al. 2006

Astron J

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This is the fourth in our series of papers discussing the nature of radio-excess galaxies, which have radio emission associated with an active nucleus but do not fit into the traditional categories of either radio-loud or radio-quiet active galaxies. In this paper we present optical spectra of our sample of far-infrared (FIR)-luminous radio-excess galaxies. Optical emission-line ratio diagnostics are used to determine the dominant source of the ionizing radiation. We find that radio excess is an excellent indicator of the presence of an active nucleus. The radio-excess sample contains a much higher fraction of active galactic nuclei (AGNs) than samples selected on FIR luminosity alone or using other criteria such as warm FIR colors. Several objects have ambiguous classifications and are likely to be composite objects with mixed excitation. The type of optical spectrum appears to be associated with the radio loudness: our results suggest that radio-loud objects may be more ''pure'' AGNs than radio-intermediate objects. We find strong evidence for interaction between the radio plasma and the surrounding gas. Broad, structured optical emission lines are observed, and a relative blueshift is measured between the [O iii] k5007 and H lines in several sources. Jet energy fluxes are inferred from the [O iii] k5007 luminosities using a shock model for the interaction between the radio jet and the line-emitting gas. The jet energy fluxes of the radio-excess objects are lower than in powerful radio sources, consistent with our previous results. We conclude that the jets of radio-intermediate sources are intrinsically weaker than those in sources with more powerful radio emission. A significant fraction of the sample spectra show poststarburst stellar continua with A star absorption lines. Poststarburst stellar populations are consistent with the large fraction of merging or disturbed host galaxies in the sample. The ages of the radio sources are significantly less than those of A stars, indicating that, if the radio sources are associated with merging activity, there is a delay between the interaction and the initiation of the radio activity.

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“…It has been known for more than two decades that AGN and intensely star-forming galaxies can drive outflows of warm ionized and neutral gas (e.g., van Breugel et al 1984;Heckman et al 1990), but it has only recently been recognized that these winds can also have a molecular component (e.g., Iono et al 2007). Consequently, much of what we know about these winds comes from observations of optical line emission of warm ionized gas and radio observations of neutral hydrogen.…”

Section: A Molecular Wind As a Signature Of Agn Feedback?mentioning

confidence: 99%

Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs atz ≥ 3.4

Polletta

Nesvadba

Neri

et al. 2011

A&A

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We report on the detection of bright CO(4-3) line emission in two powerful, obscured quasars discovered in the SWIRE survey, SW022513 and SW022550 at z ≥ 3.4. We analyze the line strength and profile to determine the gas mass, dynamical mass, and the gas dynamics for both galaxies. In SW022513 we may have found the first evidence for a molecular, AGN-driven wind in the early Universe. The line profile in SW022513 is broad (FWHM = 1000 km s −1 ) and blueshifted by −200 km s −1 relative to systemic (where the systemic velocity is estimated from the narrow components of ionized gas lines, as is commonly done for AGN at low and high redshifts). SW022550 has a more regular, double-peaked profile, which is marginally spatially resolved in our data, consistent with either a merger or an extended disk. The molecular gas masses, 4×10 10 M , are large and account for <30% of the stellar mass, making these obscured QSOs as gas rich as other powerful CO emitting galaxies at high redshift, i.e., submillimeter galaxies. Our sources exhibit relatively lower star-formation efficiencies compared to other dusty, powerful starburst galaxies at high redshift. We speculate that this could be a consequence of the AGN perturbing the molecular gas.

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Extended optical line emission from 3C 293 - Radio jets propagating through a rotating gaseous disk

Cited by 43 publications

References 0 publications

The Spiral Host Galaxy of the Double Radio Source 0313?1921

The Spiral Host Galaxy of the Double Radio Source 0313?1921

Radio-ExcessIRASGalaxies. IV. Optical Spectroscopy

Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs atz ≥ 3.4

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