The Polarised Bent Jet of 3C 43

Mantovani, F.; Junor, W.; Saikia, D. J.; Salter, C. J.

doi:10.1071/as02059

Cited by 2 publications

(3 citation statements)

References 7 publications

(8 reference statements)

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“…VLBI observations were reported by Nan et al (1991), Spencer et al (1991), andFanti et al (2002). Polarimetric VLBI observations were performed by Mantovani et al (2003) at 8.4 GHz. These , 2, 4, 8, 16, 32, 64,128, 256, 512, 1024 mJy/beam.…”

Section: Comments On Individual Sourcesmentioning

confidence: 99%

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Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Mantovani

Rossetti

Junor

et al. 2013

A&A

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Aims. We report new Very Large Array (VLA) polarimetric observations of compact steep-spectrum (CSS) sources at 8.4, 15, and 23 GHz. Methods. Using multi-frequency VLA observations we have derived sub-arcsecond resolution images of the total intensity, polarisation, and rotation measure (RM) distributions.Results. We present multi-frequency VLA polarisation observations of CSS sources. About half of the sources are point-like even at the resolution of ∼0.1 × 0.1 arcsec. The remaining sources have double or triple structure. Low values for the percentage of polarised emission in CSS sources is confirmed. On the average, quasars are more polarised than galaxies. A wide range of RM values have been measured. There are clear indications of very large RMs up to ≈5585 rad m −2 . CSS galaxies are characterized by RM values that are larger than CSS quasars. The majority of the objects show very large values of RM. Conclusions. The available data on sub-arcsecond-scale rest-frame RM estimates for CSS sources show that these have a wide range of values extending up to ∼36 000 rad m −2 . RM estimates indicate an overall density of the magneto-ionic medium larger than classical radio sources.

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Section: Comments On Individual Sourcesmentioning

confidence: 99%

“…VLBI observations were reported by Nan et al (1991), Spencer et al (1991), and Fanti et al (2002). Polarimetric VLBI observations were performed by Mantovani et al (2003) at 8.4 GHz. These authors detected polarised emission along the jet with polarisation percentages up to 12%.…”

Section: +233 (3c 43) -mentioning

confidence: 99%

Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Mantovani

Rossetti

Junor

et al. 2013

A&A

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“…Results for the first two CSS quasars observed in our ongoing program, B0548 + 165 and B1524 − 136, are available in Mantovani et al (2002), while those for 3C 43 (B0127 + 233) are to be found in Mantovani et al (2003). The results for 3C 147 (B0538 + 498) were presented by Rossetti et al (2009).…”

Section: Introductionmentioning

confidence: 99%

Radio polarimetry of 3C 119, 3C 318, and 3C 343 at milliarcsecond resolution

Mantovani¹,

Rossetti²,

Junor

et al. 2010

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Aims. We report new Very Long Baseline Array (VLBA) polarimetric observations of the compact steep-spectrum (CSS) sources 3C 119, 3C 318, and 3C 343 at 5 and 8.4 GHz. Methods. We analysed our VLBA observations and derived milliarcsecond-resolution images of the total intensity, polarisation, and rotation measure (RM) distributions. Results. The CSS source 3C 119, associated with a possible quasar, has source rest-frame RM values up to ∼10 200 rad m −2 in a region that coincides with a change in the direction of the inner jet. This component is located ∼325 pc from the core, which is a variable source with a peaked radio spectrum. For 3C 318, which is associated with a galaxy, a rest-frame RM of ∼3030 rad m −2 was estimated for the brightest component contributing almost all of the polarised emission. Two more extended components were detected, that contain "wiggles" in the jet towards the southern side of the source. The CSS source 3C 343 contains two peaks of emission and a curved jet embedded in more diffuse emission. It exhibits complex field directions close to the emission peaks, which are indicative of rest-frame RM values in excess of ≈6000 rad m −2 . The locations of the cores in 3C 318 and 3C 343 are unclear. Conclusions. The available data about mas-scale rest-frame RM estimates for CSS sources show that these have a wide range of values extending up to ∼40 000 rad m −2 in the central region of OQ172, and may be located at projected distances from the core of up to ∼1600 pc, as in 3C 43 where this feature has a rest-frame RM of ∼14 000 rad m −2 . The RM estimates for the cores of coredominated radio sources indicate that in addition to responding to an overall density gradient of the magneto-ionic medium, geometry, orientation, and modes of fuelling may also play a significant role. In addition to these effects, the high values of RM in CSS sources are possibly caused by dense clouds of gas interacting with the radio jets. The observed distortions in the radio structures of many CSS sources are consistent with this interpretation.

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The Polarised Bent Jet of 3C 43

Cited by 2 publications

References 7 publications

Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Radio polarimetry of compact steep spectrum sources at sub-arcsecond resolution

Radio polarimetry of 3C 119, 3C 318, and 3C 343 at milliarcsecond resolution

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