Specimen mounting methods for metallography

Miley, D.V.; Calabra, A.E.

doi:10.2172/4370210

Cited by 7 publications

(9 citation statements)

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“…The spectral index values and variations found across the source between data at 0.33 and 1.4 GHz are in reasonable agreement with those found between 0.612 and 1.4 GHz (van Breugels 1982;Jägers 1987), and between 1.4 and 4.1 GHz (Miley 1973). Comparing our results with the 0.074 -0.61 GHz spectral indices of Perley & Erickson (1979), we find that the spectrum flattens at low frequencies, while comparisons with the 0.408-2.7 GHz spectral indices of Riley (1973) and the 2.7-4.8 GHz and 4.8-10.6 GHz spectral indices of Feretti et al (1998) show that the energy spectrum steepens at higher frequencies.…”

Section: Radio Mapssupporting

confidence: 86%

“…The cluster contains two radio galaxies. The radio source 3C 129 is a well studied galaxy in the radio wavelength range as a prototype head-tailed (HT) galaxy with a strongly curved, 15 ′ long (426 kpc), two armed tail (Miley 1973;van Breugel & Jagers 1982;Kassim et al 1993;Fer-etti et al 1998). In an earlier paper (Harris, Krawczynski & Taylor, 2002, called Paper II in the following) we presented evidence for X-ray emission from the inner northern jet of 3C 129.…”

Section: The Cluster 3c 129 and Outline Of The Papermentioning

confidence: 99%

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Thermal and non-thermal plasmas in the galaxy cluster 3C 129

Krawczynski

Harris

Grossman

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We describe new Chandra spectroscopy data of the cluster which harbours the prototypical ‘head–tail’ radio galaxy 3C 129 and the weaker radio galaxy 3C 129.1. We combined the Chandra data with Very Large Array (VLA) radio data taken at 0.33, 5 and 8 GHz (archival data) and 1.4 GHz (new data). We also obtained new H i observations at the Dominion Radio Astrophysical Observatory (DRAO) to measure the neutral hydrogen column density in the direction of the cluster with arcmin angular resolution. The Chandra observation reveals extended X‐ray emission from the radio galaxy 3C 129.1 with a total luminosity of 1.5 × 1041 erg s−1. The X‐ray excess is resolved into an extended central source of ≃2 arcsec (1 kpc) diameter and several point sources with individual luminosities up to 2.1 × 1040 erg s−1. There is no evidence for a correlation between the 3C 129.1 X‐ray and radio morphology. In the case of the radio galaxy 3C 129, the Chandra observation shows, in addition to core and jet X‐ray emission reported in an earlier paper, some evidence for extended, diffuse X‐ray emission from a region east of the radio core. The 12 × 36 arcsec2 (6 kpc × 17 kpc) region lies ‘in front’ of the radio core, in the same direction into which the radio galaxy is moving. We use the radio and X‐ray data to study in detail the pressure balance between the non‐thermal radio plasma and the thermal intracluster medium (ICM) along the tail of 3C 129 which extends over 15 arcmin (427 kpc). Depending on the assumed lower energy cut‐off of the electron energy spectrum, the minimum pressure of the radio plasma lies a factor of between 10 and 40 below the ICM pressure for a large part of the tail. We discuss several possibilities to explain the apparent pressure mismatch.

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Section: Radio Mapssupporting

confidence: 86%

Section: The Cluster 3c 129 and Outline Of The Papermentioning

confidence: 99%

Thermal and non-thermal plasmas in the galaxy cluster 3C 129

Krawczynski

Harris

Grossman

et al. 2003

Monthly Notices of the Royal Astronomical Society

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“…The radio source 3C 129 was identified with an E galaxy by Hill & Longair (1971), and was among the first radio galaxies discovered to have a head-tail structure. Since then it has been studied extensively in the radio by several authors (e.g., Miley 1973, Perley & Erickson 1979, van Breugel 1982, Downes 1984, Feretti et al 1998. Low frequency observations by van Breugel & Jägers (1982) show that the radio tail extends over ∼20 ′ in length (> 0.5 Mpc), making 3C 129 sometimes classified as one of the giant radio galaxies (Ishwara-Chandra & Saikia 1999).…”

Section: C 129 Cluster Peripherymentioning

confidence: 99%

Magnetic fields in the 3C 129 cluster

Taylor

Govoni

Allen

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We present multifrequency VLA observations of the two radio galaxies 3C 129 and 3C 129.1 embedded in a luminous X‐ray cluster. These radio observations reveal a substantial difference in the Faraday Rotation Measures (RMs) toward 3C 129.1 at the cluster centre and 3C 129 at the cluster periphery. After deriving the density profile from available X‐ray data, we find that the RM structure of both radio galaxies can be fitted by a tangled cluster magnetic field with strength 6 μG extending at least 3 core radii (450 kpc) from the cluster centre. The magnetic field makes up a small contribution to the total pressure (5 per cent) in the central regions of the cluster. The radio morphology of 3C 129.1 appears disturbed on the southern side, perhaps by the higher pressure environment. In contrast with earlier claims for the presence of a moderately strong cooling flow in the 3C 129 cluster, our analysis of the X‐ray data places a limit on the mass deposition rate from any such flow of < 1.2 M⊙ yr−1.

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“…While strength and orientation of the magnetic field component in the plane of the sky are directly given by the intensity of the polarised emission and its angle, respectively, the component along the line-of-sight can be estimated from the Faraday rotation measure 𝑅𝑀 = 0.81 ∫ 𝐿 0 𝑛 𝑒 (𝑠)B(𝑠) • 𝑑s (e.g., , where 𝑅𝑀 is the rotation measure in rad m −2 , s is the coordinate along the line of sight, 𝐿 is the distance from the source to us in parsec, 𝑛 𝑒 is the electron density along the line-of-sight in particles per cm 3 and B is the magnetic vector field with the field strength measured in units of μG. Such polarization studies of HT galaxies are still rare but Miley (1973) already found significant linear polarisation along the jet with a steady rising in the degree of polarization. However, no correction for Faraday rotation was applied to the data.…”

Section: Introductionmentioning

confidence: 99%

Two striking head-tail galaxies in the galaxy cluster IIZW108: insights into transition to turbulence, magnetic fields and particle re-acceleration

Müller,

Pfrommer,

Ignesti

et al. 2021

Preprint

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We present deep JVLA observations at 1.4 GHz and 2.7 GHz (full polarization), as well as optical OmegaWINGS/WINGS and X-ray observations of two extended radio galaxies in the IIZW108 galaxy cluster at 𝑧 = 0.04889. They show a bent tail morphology in agreement with a radio lobed galaxy falling into the cluster potential. Both galaxies are found to possess properties comparable with narrow-angle tail galaxies in the literature even though they are part of a low mass cluster. We find a spectral index steepening and an increase in fractional polarization through the galaxy jets and an ordered magnetic field component mostly aligned with the jet direction. This is likely caused by either shear due to the velocity difference of the intracluster medium and the jet fluid and/or magnetic draping of the intracluster medium across the galaxy jets. We find clear evidence that one source is showing two active galactic nuclei (AGN) outbursts from which we expect the AGN has never turned off completely. We show that pure standard electron cooling cannot explain the jet length. We demonstrate therefore that these galaxies can be used as a laboratory to study gentle re-acceleration of relativistic electrons in galaxy jets via transition from laminar to turbulent motion.

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Specimen mounting methods for metallography

Cited by 7 publications

References 0 publications

Thermal and non-thermal plasmas in the galaxy cluster 3C 129

Thermal and non-thermal plasmas in the galaxy cluster 3C 129

Magnetic fields in the 3C 129 cluster

Two striking head-tail galaxies in the galaxy cluster IIZW108: insights into transition to turbulence, magnetic fields and particle re-acceleration

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