Kiloparsec-Scale Radio Emission in Seyfert Galaxies: Evidence for Starburst-driven Superwinds?

Baum, S. A.; O'dea, C. P.; Dallacassa, D.; Bruyn, A. G. de; Pedlar, A.

doi:10.1086/173508

Cited by 165 publications

(274 citation statements)

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“…Y: Our map has similar features to those seen previously by Nagar et al (1999) The WSRT image of this source at 5 GHz reported by Baum et al (1993) shows amorphous structure on larger scales (>2.5 arcsec). Our central-component flux density and total flux density are slightly higher than those in the 5 GHz image of Ulvestad & Wilson (1984b) with a similar resolution.…”

Section: Ngc 2273 (0645+609)supporting

confidence: 86%

Milliarcsec-scale radio structure of a matched sample of Seyfert 1 and Seyfert 2 galaxies

Lal

Shastri²,

Gabuzda

2004

A&A

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Abstract.We have obtained mas-scale resolution very long baseline interferometry (VLBI) images of a sample of Seyfert 1 and Seyfert 2 galaxies at 5 GHz (wavelength, λ = 6 cm). The Seyferts of the two types were chosen to be matched in several orientation-independent properties, primarily in order to rigorously test predictions of the unified scheme. We detected all the 15 objects that we observed. In this paper we describe the observations and data reduction procedures, and present the VLBI radio images as well as simultaneous Very Large Array images that we obtained for these 15 Seyferts.

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Section: Ngc 2273 (0645+609)supporting

confidence: 86%

Milliarcsec-scale radio structure of a matched sample of Seyfert 1 and Seyfert 2 galaxies

Lal

Shastri²,

Gabuzda

2004

A&A

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“…We have recently shown (Schmitt et al 1997 ;Clarke, Kinney, & Pringle 1998 ; see also that there is no correlation between the position angles of radio jets and disk major axes in Seyfert galaxies, conÐrm-ing previous results based on smaller samples (Ulvestad & Wilson 1984 ;Brindle et al 1990 ;Baum et al 1993). Clarke et al (1998) and showed, using a statistical inversion technique, that the observed values of d (the di †erence between the position angle of the jet and the host galaxy disk major axis) and i (inclination of the galaxy disk relative to the line of sight) can be reproduced by a homogeneous distribution of angles b between the jet and the galaxy disk axis.…”

Section: Introductionsupporting

confidence: 79%

Jet Directions in Seyfert Galaxies: B and I Imaging Data

Schmitt

Kinney

2000

ASTROPHYS J SUPPL S

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We present the results of broadband B and I imaging observations for a sample of 88 Seyfert galaxies (29 Seyfert 1s and 59 Seyfert 2s), selected from a mostly isotropic property, the Ñux at 60 km. We also present the B and I imaging results for an additional sample of 20 Seyfert galaxies (7 Seyfert 1s and 13 Seyfert 2s), selected from the literature and known to have extended radio emission. The I-band images are Ðtted with ellipses to determine the position angle and ellipticity of the host galaxy major axis. This information will be used in a future paper, combined with information from radio observations, to study the orientation of radio jets relative to the planes of their host galaxies. Here we present surface brightness proÐles and magnitudes in the B and I bands, as well as mean ellipticities and major axis position angles.

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“…This might indeed be the case for some objects (e.g. 0108+388, Baum et al 1990), but in many others such faint features are instead the continuation of the inner jet in cJ structures. Thus these sources cannot be considered CSOs.…”

Section: Morphology and Other Propertiesmentioning

confidence: 88%