<i>HST</i>and Merlin Observations of 3C 264—A Laboratory for Jet Physics and Unified Schemes

Baum, Stefi A.; O’Dea, C. P.; Giovannini, G.; Cotton, William B.; Koff, S. de; Feretti, L.; Golombek, Daniel; Lara, L.; Macchetto, F.; Miley, G. K.; Sparks, W. B.; Venturi, T.; Komissarov, S. S.

doi:10.1086/304221

Cited by 75 publications

(94 citation statements)

References 31 publications

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“…We note that this source has an arcsecond-scale radio jet (e.g., Lara et al 2004) which is also detected at optical wavelengths (Crane et al 1993;Baum et al 1997). However, in the radio the core is stronger than the total jet emission and has a significantly flatter spectrum (Lara et al 2004).…”

Section: Sources Without Residual Mir Emissionmentioning

confidence: 68%

THESPITZERVIEW OF FR I RADIO GALAXIES: ON THE ORIGIN OF THE NUCLEAR MID-INFRARED CONTINUUM

Leipski

Antonucci

Ogle

et al. 2009

ApJ

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We present Spitzer mid-infrared (MIR) spectra of 25 FR I radio galaxies and investigate the nature of their MIR continuum emission. MIR spectra of star-forming galaxies and quiescent elliptical galaxies are used to identify host galaxy contributions while radio/optical core data are used to isolate the nuclear nonthermal emission. Out of the 15 sources with detected optical compact cores, four sources are dominated by emission related to the host galaxy. Another four sources show signs of warm, nuclear dust emission: 3C15, 3C84, 3C270, and NGC 6251. It is likely that these warm dust sources result from hidden active galactic nuclei of optical spectral type 1. The MIR spectra of seven sources are dominated by synchrotron emission, with no significant component of nuclear dust emission. In parabolic spectral energy distribution fits of the nonthermal cores FR Is tend to have lower peak frequencies and stronger curvature than blazars. This is roughly consistent with the common picture in which the core emission in FR Is is less strongly beamed than in blazars.

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Section: Sources Without Residual Mir Emissionmentioning

confidence: 68%

THESPITZERVIEW OF FR I RADIO GALAXIES: ON THE ORIGIN OF THE NUCLEAR MID-INFRARED CONTINUUM

Leipski

Antonucci

Ogle

et al. 2009

ApJ

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“…Both the jet and counterjet are embedded in a vast and diffuse region of low surface brightness emission, which seems to have been dragged toward the north, possibly revealing the existence of a high density intracluster medium. Simultaneous EVN and MERLIN observations at 5.0 GHz by Lara et al (1999); Baum et al (1997) showed for the first time the detailed structure of 3C 264 on sub-kiloparsec scales. It consists of a one-sided jet with evident variations in its morphological properties with distance: i) the strong core and innermost jet (0−10 pc); ii) a wellcollimated and narrow region (10−100 pc); iii) a region with strong widening, kinks, and filaments (100−300 pc); and iv) a faint and narrow region after a jet deflection (300−400 pc from the core).…”

Section: Notes On Individual Sourcesmentioning

confidence: 95%

“…In Col. 8 we give the angular resolution of maps used to estimate the core coordinates. We use (v) for the detected objects whose coordinates are taken by the VLBA maps and (!n) for well known radiosources with public VLBI data: (!1) from Taylor et al (2006a), (!2) from Lara et al (1997); Baum et al (1997); Lara et al (1999), (!3) from Gentile et al (2007) and (!4) from Venturi et al (1995). We use (xn) for undetected radiosources for which coordinates are taken from: (x1) , from NVSS ; (x2) from NED; (x3) from FIRST; (x4) from radio data of ; (x5) from Ledlow & Owen (1995).…”

Section: Notes On Individual Sourcesmentioning

confidence: 99%

Parsec-scale properties of brightest cluster galaxies

Liuzzo

Giovannini

Giroletti³

et al. 2010

A&A

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We present new VLBI observations at 5 GHz of a complete sample of brightest cluster galaxies (BCGs) in nearby Abell clusters (distance class <3). Combined with data from the literature, we provide parsec-scale information for 34 BCGs. Our analysis of the parsec-scale radio emission of BCGs and the cluster X-ray properties finds a possible dichotomy between BCGs in cool-core clusters and those in non-cool-core clusters. Among resolved sources, those in cool-core clusters tend to have two-sided parsec-scale jets, while those in less relaxed clusters have predominantly one-sided parsec-scale jets. We suggest that this difference is caused by the interplay between the jets and the surrounding medium. The one-sided structure in non-cool-core clusters may be due to Doppler boosting effects in relativistic, intrinsically symmetric jets whereas two-sided morphology in cool core clusters is probably related to the presence of heavy and mildly relativistic jets that have been decelerated on the parsec-scale. Evidence of recurrent activity is also found in BCGs in cool-core clusters.

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“…Besides this rich radio structure, another peculiarity of 3C 264 is the existence of an optical jet coincident with the radio jet, most possibly of synchrotron nature (Lara et al 1999) and extending up to 2 (0.82 kpc) (Crane et al 1993;Baum et al 1997). There is also evidence of a "ring" around the host galaxy core with a radius between 0.…”

Section: Introductionmentioning

confidence: 96%

“…There is also evidence of a "ring" around the host galaxy core with a radius between 0. 75 and 1 (300-400 pc) (Baum et al 1997).…”

Section: Introductionmentioning

confidence: 99%

The inner kiloparsec of the jet in 3C 264

Lara

Giovannini

Cotton

et al. 2004

A&A

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Abstract. We present new multi-frequency EVN, MERLIN and VLA observations of the radio source 3C 264, sensitive to linear scales ranging from parsec to several kiloparsecs. The observations confirm the existence of regions with different properties in the first kiloparsec of the jet. The most remarkable feature is the transition between a well collimated narrow jet at distances from the core below 80 pc, to a conical-shaped wide jet, with an opening angle of 20• . Another change of properties, consisting of an apparent deflection of the jet ridge line and a diminution of the surface brightness, occurs at a distance of ∼300 pc from the core, coincident with the radius of a ring observed at optical wavelengths. Our observations add new pieces of information on the spectrum of the radio-optical jet of 3C 264, with results consistent with a synchrotron emission mechanism and a spectrum break frequency in the infrared. Brightness profiles taken perpendicularly to the jet of 3C 264 are consistent with a spine brightened jet at distances below 100 pc from the core, and an edge-brightened jet beyond, which can be interpreted as evidence of a transverse jet velocity structure. Our observations do not allow us to distinguish between the presence of a face-on dust and gas disk at the center of the host galaxy of 3C 264, or rather an evacuated bubble. However, the properties of the jet structure, the changes in the polarization angle, and the plausible jet orientation can be naturally brought into agreement in the bubble scenario.

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HSTand Merlin Observations of 3C 264—A Laboratory for Jet Physics and Unified Schemes

Cited by 75 publications

References 31 publications

THESPITZERVIEW OF FR I RADIO GALAXIES: ON THE ORIGIN OF THE NUCLEAR MID-INFRARED CONTINUUM

THESPITZERVIEW OF FR I RADIO GALAXIES: ON THE ORIGIN OF THE NUCLEAR MID-INFRARED CONTINUUM

Parsec-scale properties of brightest cluster galaxies

The inner kiloparsec of the jet in 3C 264

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