High-resolution radio observations of Markarian 3

Kukula, M. J.; Ghosh, T.; Pedlar, A.; Schilizzi, R. T.; Miley, G. K.; Bruyn, A. G. de; Saikia, D. J.

doi:10.1093/mnras/264.4.893

Cited by 48 publications

(60 citation statements)

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“…At a distance of 15 kpc the structure would subtend an angle of no such huge and very well collimated molecular struc-1@ .5, tures are seen in our Galaxy. Highly collimated, parsecscale structures are seen in the nuclei of other galaxies (e.g., Kukula et al 1993) but are usually the result of relativistic, synchrotron jets. Only in rare cases (e.g., NGC 1068 ; Gallimore et al 1996) is molecular emission associated with such jets and then not with the structure observed in III Zw 35.…”

Section: Discussionmentioning

confidence: 99%

Global VLBI Observations of the Compact OH Megamaser Emission from III Zw 35 and IRAS 17208−0014

Diamond

Lonsdale

et al. 1999

ApJ

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We have performed global VLBI observations of the OH megamaser galaxies III Zw 35 and IRAS 17208[0014. We detect strong and compact 1667 MHz OH emission from each galaxy, but, apart from one weak detection of a single 1665 MHz OH feature in III Zw 35, no 1665, 1720 MHz, or continuum emission are detected, which indicates that they occur on size scales greater thanWe surmise that 0A .1. the OH emission consists of two components. One is di †use, has unsaturated masers pumped by farinfrared radiation, and is readily explained by the classical OH megamaser model. The second is compact, consists of saturated masers, is responsible for up to 65% of the 1667 MHz Ñux density, is not associated with any compact continuum emission, and may be pumped by a combination of collisional and radiative processes. One component in III Zw 35 exhibits a well-deÐned velocity gradient of 32^4 km s~1 pc~1 along a 5.5 pc line of masers. This indicates strong rotation of a molecular cloud with an enclosed mass density of D6 ] 104 pc~3. M _

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Section: Discussionmentioning

confidence: 99%

Global VLBI Observations of the Compact OH Megamaser Emission from III Zw 35 and IRAS 17208−0014

Diamond

Lonsdale

et al. 1999

ApJ

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“…The HST images point out that the NLR of Mrk 3 exhibit a series of emission-line knots, which show an S-shaped morphology. Radio observations reveal the presence of a pair of jet knots, whose position angle is consistent with that of the NLR (Kukula et al 1993(Kukula et al , 1999. Based on the spectroscopic study carried out with HST, Capetti et al (1999) argue that the NLR is a highdensity shell that was shock heated by the jet.…”

Section: Introductionmentioning

confidence: 67%

“…The high-resolution 18 cm EVN and Merlin radio images of Mrk 3 (see the intensity levels in Figure 4) reveal jets with an S-shaped structure and a remarkable hotspot on the western side (Kukula et al 1993(Kukula et al , 1999. These authors suggest that the S-shaped morphology of the radio jet may either be due to a change in the jet axis or from the jet interacting with the rotating interstellar medium.…”

Section: Comparing the X-ray And Radio Morphologymentioning

confidence: 98%

Probing the Hot X-Ray Gas in the Narrow-line Region of Mrk 3

Bogdán

Kraft

Evans

et al. 2017

ApJ

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We study the prototypical Seyfert 2 galaxy, Markarian 3, based on imaging and high-resolution spectroscopy observations taken by the Chandra X-ray Observatory. We construct a deconvolved X-ray image, which reveals the S-shaped morphology of the hot gas in the narrow line region (NLR). While this morphology is similar to the radio and [O III] emission, the distribution of the X-ray gas is broader than that obtained at these other wavelengths. By mapping the density and temperature distribution of the hot gas in the NLR, we demonstrate the presence of shocks towards the west (M = 2.5 +1.0 −0.6 ) and east (M = 1.5 +1.0 −0.5 ). Moreover, we compute the flux ratios between the [O III] and 0.5 − 2 keV band X-ray luminosity and show that it is non-uniform in the NLR with the western side of the NLR being more highly ionized. In addition, based on the Chandra grating data we investigate the line ratios of the Si XIII triplet, which are not consistent with pure photoionization. Based on these results, we suggest that in the NLR of Mrk 3 both photoionization and collisional ionization act as excitation mechanisms. We conclude that the canonical picture, in which photoionization is solely responsible for exciting the interstellar medium in the NLR of Seyfert galaxies, may be overly simplistic. Given that weak and small-scale radio jets are commonly detected in Seyfert galaxies, it is possible that shock heating plays a non-negligible role in the NLR of these galaxies.

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“…• (Kukula et al 1993). Embedded in the jets are compact components, the western end terminating in a bright lobe containing a hotspot.…”

Section: Mrkmentioning

confidence: 99%

Optical colour maps of Seyfert galaxies

Kotilainen

Ward²

1996

Vistas in Astronomy

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Abstract. We present optical broad band colour maps of nine Seyfert galaxies. In the bands used, the contribution from emission lines to the total flux is relatively small, and hence the images predominantly trace the continuum distribution. The ratios of these images are sensitive to gradients in the stellar populations, and to reddening by dust. We detect ringlike, clumpy or elongated morphological features in several galaxies, which are blue in the B − I index (V − I for NGC 7469). For NGC 7469 there is good spatial agreement with the molecular millimeter CO and radio continuum structure indicating the presence of star forming regions around its Seyfert nucleus. The blue elongations and/or double structures seen in the colour maps of NGC 1068, NGC 3227, NGC 4151, Mrk 3 and Mrk 573 are roughly parallel to their extended radio and NLR emission and probably arise from scattering of nuclear light by extranuclear "mirrors". In Mrk 78 and Mrk 348, the structure is not well resolved, possibly because the scattering mirrors are either less efficient and/or further away from the nucleus than in the previous galaxies. In NGC 1667, we detect double red maxima, again possibly related to obscuring material. The colours of the blue maxima are not well determined due to contamination from the underlying bulge, but they are generally consistent with those expected from scattering off dust or electrons. Our findings thus give further support to the current unified models of AGN.

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High-resolution radio observations of Markarian 3

Cited by 48 publications

References 0 publications

Global VLBI Observations of the Compact OH Megamaser Emission from III Zw 35 and IRAS 17208−0014

Global VLBI Observations of the Compact OH Megamaser Emission from III Zw 35 and IRAS 17208−0014

Probing the Hot X-Ray Gas in the Narrow-line Region of Mrk 3

Optical colour maps of Seyfert galaxies

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