Unusual radio and optical structures in the Seyfert galaxy Markarian 6

Kukula, M. J.; Holloway, A. J.; Pedlar, A.; Meaburn, J.; López, J. A.; Axon, D. J.; Schilizzi, R. T.; Baum, S. A.

doi:10.1093/mnras/280.4.1283

Cited by 36 publications

(83 citation statements)

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“…Like Mrk 6, both NGC 4151 and Mrk 766 are Seyfert 1.5 galaxies (see Koski 1976 andMartel 1993), and all three objects may have their active galactic nuclei (AGNs) aligned in a fairly edge-on manner (e.g.,°3.2 of Evans et al 1993). A fairly edge-on orientation of the AGN in Mrk 6 is further supported by the length and structure of its impressive radio jet (see Kukula et al 1996). The large angular size of the Mrk 6 jet when compared to jets seen in other similar type 1 Seyfert galaxies suggests that it does not su †er from signiÐ-cant foreshortening by projection e †ects (consistent with an edge-on orientation).…”

Section: Introductionmentioning

confidence: 68%

Heavy and Complex X‐Ray Absorption toward the Nucleus of Markarian 6

Feldmeier¹,

Brandt²,

Elvis³

et al. 1999

ApJ

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We have used the ASCA satellite to make the Ðrst X-ray spectra of Mrk 6, a bright Seyfert 1.5 galaxy with complex and variable permitted lines, an ionization cone, and remarkable radio structures. Our 0.6È9.5 keV spectra penetrate to the black hole core of this Seyfert and reveal heavy and complex intrinsic X-ray absorption. Both total covering and single partial covering models fail to acceptably Ðt the observed absorption, and double partial covering or partial covering plus warm absorption appears to be required. The double partial covering model provides the best statistical Ðt to the data, and we measure large column densities of B(3È20) ] 1022 cm~2 irrespective of the particular spectral model under consideration. These X-ray columns are over an order of magnitude larger than expected based on observations at longer wavelengths. Our data suggest that most of the X-ray absorption occurs either in gas that has a relatively small amount of dust or in gas that is located within the broad-line region. The X-ray absorber may well be the putative "" atmosphere ÏÏ above the torus that collimates the ionization cone. We also detect an apparently broad 6.4 keV iron Ka line, and we present optical spectra demonstrating that the optical emission lines were in a representative state during our ASCA observation.

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Section: Introductionmentioning

confidence: 68%

Heavy and Complex X‐Ray Absorption toward the Nucleus of Markarian 6

Feldmeier¹,

Brandt²,

Elvis³

et al. 1999

ApJ

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“…For example, the radio jet of NGC 1068 is diverted by interaction with molecular gas within the central 100 pc (Gallimore et al , 1996b, and at a distance of $800 pc from the central engine the jet terminates in a bow shock that plows into the surrounding ISM at >80 km s À1 , 1987. Mrk 6 shows similar bowshock-like structures on kiloparsec scales ( Baum et al 1993;Kukula et al 1996). The $800 pc jet of NGC 2110, which appears to propagate directly into the disk of the surrounding host galaxy ), seems to have been bent into a gentle S-shape by the rotating ISM .…”

Section: Jet Misalignmentsmentioning

confidence: 99%

“…For instance, while the typical jet length scale in these long-baseline surveys is $10 to a few hundred parsecs, early targeted VLA observations, obtained with shorter baselines than the later surveys, found larger scale radio outflows exceeding 1 kpc in full extent ( Wilson & Willis 1980;Hummel et al 1983). One of the more spectacular examples is Mrk 6, which displays an $600 pc nuclear jet roughly aligned with 10 kpc scale lobes ( Baum et al 1993;Kukula et al 1996). In fact, such large-scale outflows may be common: Baum et al (1993) used the Westerbork Synthesis Radio Telescope ( WSRT; $5} resolution at the ¼ 5 GHz) to observe a sample of 13 radio-bright Seyfert galaxies, and, remarkably, 12 of these sources showed extended radio lobes extending up to several kiloparsecs from the nucleus.…”

Section: Introductionmentioning

confidence: 98%

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

et al. 2006

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Seyfert galaxies commonly host compact jets spanning 10-100 pc scales, but larger structures are resolved out in long-baseline aperture synthesis surveys. Previous, targeted studies showed that kiloparsec-scale radio structures ( KSRs) may be a common feature of Seyfert and LINER galaxies, and the origin of KSRs may be starbursts or active galactic nuclei (AGNs). We report a new Very Large Array survey of a complete sample of Seyfert and LINER galaxies. Out of all of the surveyed radio-quiet sources, we find that 44% (19 out of 43) show extended radio structures at least 1 kpc in total extent that do not match the morphology of the disk or its associated star-forming regions. The detection rate is a lower limit owing to the combined effects of projection and resolution. The infrared colors of the KSR host galaxies are unremarkable compared to other Seyfert galaxies, and the large-scale outflows orient randomly with respect to the host galaxy axes. The KSR Seyfert galaxies instead stand out by deviating significantly from the far-infrared-radio correlation for star-forming galaxies, with tendency toward radio excess, and they are more likely to have a relatively luminous, compact radio source in the nucleus; these results argue that KSRs are powered by the AGNs rather than starbursts. The high detection rate indicates that Seyfert galaxies generate radio outflows over a significant fraction of their lifetime, which is much longer than the dynamical timescale of an AGNpowered jet but is comparable instead to the buoyancy timescale. The likely explanation is that the KSRs originate from jet plasma that has been decelerated by interaction with the nuclear interstellar medium ( ISM ). Based on a simple ram pressure argument, the kinetic power of the jet on kiloparsec scales is about 3 orders of magnitude weaker than the power of the jet on 10-100 pc scales. This result is consistent with the interaction model, in which case virtually all of the jet power must be lost to the ISM within the inner kiloparsec.

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“…The structures are generally aligned with the minor axis of the host galaxy, rather than that of the nuclear radio source, and can be interpreted as plasma -perhaps a relic of previous cycles of activity -which has lost its bulk kinetic energy and is now drifting out of the plane of the host along the local density gradient (e.g. the features in Mrk 6: Kukula et al 1996).…”

Section: Comparison With Compact Steep-spectrum Sourcesmentioning

confidence: 99%

The radio properties of radio-quiet quasars

Kukula

Dunlop

Hughes

et al. 1998

Monthly Notices of the Royal Astronomical Society

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127

173

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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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Unusual radio and optical structures in the Seyfert galaxy Markarian 6

Cited by 36 publications

References 0 publications

Heavy and Complex X‐Ray Absorption toward the Nucleus of Markarian 6

Heavy and Complex X‐Ray Absorption toward the Nucleus of Markarian 6

A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei

The radio properties of radio-quiet quasars

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