The jets in 3C 66B

Hardcastle, Martin; Alexander, Paul; Pooley, G. G.; Riley, J. M.

doi:10.1093/mnras/278.1.273

Cited by 53 publications

(74 citation statements)

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“…It is a large FRI radiosource of about 100 kpc total extension (Leahy et al 1986; Hardcastle et al 1996), relatively close to us (1 arcsec ≃ 420 pc for H 0 = 75 km s −1 Mpc −1 ). It shows two jets with the brightest of them being one of the 6 synchrotron optical extragalactic jets known (Butcher et al 1980;Fraix-Burnet et al 1989a, b;Fraix-Burnet 1997).…”

Section: Introductionmentioning

confidence: 65%

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EVN-merlin observations of 3C66B

Fraix-Burnet

Despringre

Baudry

1997

Vistas in Astronomy

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Section: Introductionmentioning

confidence: 65%

“…The MERLIN map at a resolution of 150 mas shows an unresolved core together with the brightest component of the jet, i.e. knot B at 2.9 arcsec from the nucleus (Fraix-Burnet et al 1989a; Hardcastle et al 1996). An over-resolved MERLIN map at a resolution of 20 mas shows a NE 35 mas (≃ 15 pc) extension in the nucleus.…”

Section: Resultsmentioning

confidence: 99%

EVN-merlin observations of 3C66B

Fraix-Burnet

Despringre

Baudry

1997

Vistas in Astronomy

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“…At the shortest wavelengths of the MIR spectrum the stellar population of the host galaxy can be seen. 3C66B has an arcsecond-scale jet (Hardcastle et al 1996) which is also seen in the optical (Butcher et al 1980;Macchetto et al 1991;Perlman et al 2006), in X-rays (Hardcastle et al 2001), and even at MIR wavelengths a detection with Infrared Space Observatory (ISO) is claimed (Tansley et al 2000). However, unlike the case of 3C15, the jet in 3C66B is weaker than the core.…”

Section: Notesmentioning

confidence: 98%

“…For the variable 5 GHz core flux, we here give the average of all measurements available from NED. Giovannini et al 1988;(13) Giovannini et al 2005; (14) Hardcastle et al 1996;(15) Hines et al 1989;(16) Jones et al 1986; (17) Kollatschny et al 2006;(18) Laing & Bridle 1987;(19) Laing et al 2008;(20) Lawrence et al 1996; (21) Leahy & Perley 1991;(22) Leahy et al 1997;(23) Miley & Osterbrock 1979;(24) Morganti et al 1993;(25) Morganti et al 1999;(26) Taylor et al 2006;(27) O'Dea & Owen 1986;(28) Owen et al 1996;(29) Pedlar et al 1990;(30) Perley et al 1984;(31) Simpson et al 1996;(32) Strom et al 1978;(33) Tadhunter et al 1993;(34) Tadhunter et al 2005;(35) Taylor et al 1990;(36) Taylor et al 2001;(37) Vallee 1982;(38) van Breugel & Jägers 1982;(39) Walker et al 1987;(40) Wills et al 2004;(41) see http://www.jb.man.ac.uk/atlas/; (42) Kellermann et al (1969), on Baars et al (1977) scale using Laing & Peacock (1980); (43) taken from http://3crr.extragalactic.info/; (44) estimated using GMRT measurements (Lal & Rao 2004); (45) Kuehr et al 1981;(46) estimated using the 160 MHz flux (Kuehr et al 1981) and α = −0.8; (47) estimated from low-frequency measurements in NED; (48) …”

Section: The Main Samplementioning

confidence: 99%

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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“…2.2. Our models also do not take into account any intrinsic spread in the Lorentz factors, nor the possibility that the relevant Lorentz factor for the highly beamed and mildly beamed subclasses may be systematically different due to a "spine-sheath" type structure of the jet (e.g., Hardcastle et al 1996;Laing et al 1999). However, as the multiple linear regression tests discussed in Sect.…”

Section: Model-fitting the L O − R C Datamentioning

confidence: 99%

Optical nuclei of radio-loud AGN and the Fanaroff-Riley divide

Kharb¹,

Shastri²

2004

A&A

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Abstract. We investigate the nature of the point-like optical nuclei that have been found in the centres of the host galaxies of a majority of radio galaxies by the Hubble Space Telescope. We examine the evidence that these optical nuclei are relativistically beamed, and look for differences in the behaviour of the nuclei found in radio galaxies of the two Fanaroff-Riley types. We also attempt to relate this behaviour to the properties of the optical nuclei in their highly beamed counterparts (the BL Lac objects and radio-loud quasars) as hypothesized by the simple Unified Scheme. Simple model-fitting of the data suggests that the emission may be coming from a non-thermal relativistic jet. It is also suggestive that the contribution from an accretion disk is not significant for the FRI objects and for the narrow-line radio galaxies of FRII type, while it may be significant for the Broad-line objects, and consistent with the idea that the FRII optical nuclei seem to suffer from extinction due to an obscuring torus while the FRI optical nuclei do not. These results are broadly in agreement with the Unified Scheme for radio-loud AGNs.

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The jets in 3C 66B

Cited by 53 publications

References 1 publication

EVN-merlin observations of 3C66B

EVN-merlin observations of 3C66B

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

Optical nuclei of radio-loud AGN and the Fanaroff-Riley divide

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