The CfA Seyfert Sample at 8.4 GHz

Kukula, M. J.; Pedlar, A.; Baum, S.; O’Dea, C.; Unger, Scott

doi:10.1007/978-94-010-9537-2_210

Cited by 102 publications

(238 citation statements)

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“…2, left panel), as is reported by Kukula et al (1995) for VLA C configuration data at 8.4 GHz. The largest angular size of the source is ∼2.0 arcsec (Kukula et al 1995). G: Our image shows a compact source with some signs of weak extensions toward the east or north-east, along PA ∼ 50 • .…”

Section: Ngc 5929 (1524+418)supporting

confidence: 73%

“…The radio peak and the optical nucleus (Clements 1981) are coincident within the errors. The spectral indices derived using our observations along with the 8.4 GHz observations of Kukula et al (1995) (obtained in June 1991) and the 1.5 GHz observations of Ulvestad & Wilson (1989) (obtained in February 1985 are α 5 GHz 1.5 GHz = 0.8, and α 8.4 GHz 5 GHz = 1.1. G: Our slightly resolved image shows a slight extension towards the south (PA ∼ 160 • ), which we were not able to adequately model-fit; our model contains about 60% of the total flux density on VLBI scales.…”

Section: Mrk 766 (1215+300)mentioning

confidence: 63%

“…Y: This source was reported to be a compact point source by Kukula et al (1995) at 8.4 GHz, whereas our 5 GHz map shows a compact source and a faint (3σ) extension to the north (PA ∼ −10 • ). Comparing our total flux density with the 3.26 mJy found by Kukula et al (1995) at 8.4 GHz in June 1991, we derive the spectral index α 8.4 GHz 5 GHz = 2.…”

Section: Mrk 530 (2316−000)mentioning

confidence: 65%

“…Comparing our total flux density with the 3.26 mJy found by Kukula et al (1995) at 8.4 GHz in June 1991, we derive the spectral index α 8.4 GHz 5 GHz = 2. Our total flux density is consistent with the measurements of Edelson (1987) (11.5 mJy), and Roy et al (1994), viz., a correlated flux density of 11 mJy obtained using a single 275 km baseline at 2.3 GHz.…”

Section: Mrk 530 (2316−000)mentioning

confidence: 83%

“…The spectral indices of the north-east and south-west components are steep, with α 15 GHz 1.6 GHz = 0.9 and 0.8, respectively. The central component has a flatter spectrum, with α 15 GHz 1.6 GHz = 0.3 (Su et al 1996;Kukula et al 1995;Wilson & Keel 1989) and is close to the position of the optical nucleus, and hence is likely to be the core. The epochs of these observations are August 1993 (1.6 GHz), November 1992 (5 GHz), June 1990 (8.4 GHz) and March 1989 (15 GHz).…”

Section: Ngc 5929 (1524+418)mentioning

confidence: 99%

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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 5929 (1524+418)supporting

confidence: 73%

Section: Mrk 766 (1215+300)mentioning

confidence: 63%

Section: Mrk 530 (2316−000)mentioning

confidence: 65%

Section: Mrk 530 (2316−000)mentioning

confidence: 83%

Section: Ngc 5929 (1524+418)mentioning

confidence: 99%

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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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The Radio Properties of Radio-Quiet Quasars

Kukula

Dunlop

Hughes

et al. 1997

ESO Astrophysics Symposia

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A B S T R A C TAlthough radio-quiet quasars (RQQs) constitute տ 90 per cent of optically identified quasar samples, their radio properties are only poorly understood. In this paper we present the results of a multi-frequency VLA study of 27 low-redshift RQQs. We detect radio emission from 20 objects, half of which are unresolved (Յ 0:24 arcsec). In cases where significant structure can be resolved, double, triple and linear radio sources on scales of a few kpc are found. The radio emission (typically) has a steep spectrum (a ϳ 0:7, where S ϰ n ¹a ), and high brightness temperatures (T B Ն 10 5 K) are measured in some of the radio components. The RQQs form a natural extension to the radio luminosity-absolute magnitude distribution of nearby Seyfert 1s. We conclude that a significant fraction of the radio emission in RQQs originates in a compact nuclear source directly associated with the quasar. There are no significant differences between the radio properties of RQQs with elliptical hosts and those in disc galaxies within the current sample.

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Status of AGN Unification Models

Barthel¹

1995

Highlights of Astronomy

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The CfA Seyfert Sample at 8.4 GHz

Cited by 102 publications

References 0 publications

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

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

The Radio Properties of Radio-Quiet Quasars

Status of AGN Unification Models

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