Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy contributions
We present a detailed examination of the relationship between the magnetic field structures and the variations in Faraday Rotation across PKS1246-410, a radio source in the Centaurus cluster of galaxies, using data from Taylor, Fabian and Allen. We find a significant relationship between the intrins...
| Egile Nagusiak: | , |
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| Formatua: | Journal article |
| Argitaratua: |
2003
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| _version_ | 1826267251025641472 |
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| author | Rudnick, L Blundell, K |
| author_facet | Rudnick, L Blundell, K |
| author_sort | Rudnick, L |
| collection | OXFORD |
| description | We present a detailed examination of the relationship between the magnetic field structures and the variations in Faraday Rotation across PKS1246-410, a radio source in the Centaurus cluster of galaxies, using data from Taylor, Fabian and Allen. We find a significant relationship between the intrinsic position angle of the polarization and the local amount of Faraday Rotation. The most plausible explanation is that most or all of the rotation is local to the source. We suggest that the rotations local to cluster radio galaxies may result from either thermal material mixed with the radio plasma, or from thin skins of warm, ionized gas in pressure balance with the observed galaxy or hot cluster atmospheres. We find that the contribution of any unrelated cluster Rotation Measure variations on scales of 2 - 10 arcsec are less than 25 rad/m^2; the standard, although model dependent, derivation of cluster fields would then lead to an upper limit of approximately 0.4 microGauss on these scales. Inspection of the distributions of Rotation Measure, polarisation angle and total intensity in 3C75, 3C465 and Cygnus A also shows source-related Faraday effects in some locations. Many effects can mask the signatures of locally-dominated RMs, so the detection of even isolated correlations can be important, although difficult to quantify statistically. In order to use radio sources such as shown here to derive {\it cluster-wide} magnetic fields, as is commonly done, one must first remove the local contributions; this is not possible at present. |
| first_indexed | 2024-03-06T20:51:19Z |
| format | Journal article |
| id | oxford-uuid:37acda5f-36f5-4b40-ac7e-8d1e9cc1066a |
| institution | University of Oxford |
| last_indexed | 2024-03-06T20:51:19Z |
| publishDate | 2003 |
| record_format | dspace |
| spelling | oxford-uuid:37acda5f-36f5-4b40-ac7e-8d1e9cc1066a2022-03-26T13:45:25ZLowering Inferred Cluster Magnetic Field Strengths - the radio galaxy contributionsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:37acda5f-36f5-4b40-ac7e-8d1e9cc1066aSymplectic Elements at Oxford2003Rudnick, LBlundell, KWe present a detailed examination of the relationship between the magnetic field structures and the variations in Faraday Rotation across PKS1246-410, a radio source in the Centaurus cluster of galaxies, using data from Taylor, Fabian and Allen. We find a significant relationship between the intrinsic position angle of the polarization and the local amount of Faraday Rotation. The most plausible explanation is that most or all of the rotation is local to the source. We suggest that the rotations local to cluster radio galaxies may result from either thermal material mixed with the radio plasma, or from thin skins of warm, ionized gas in pressure balance with the observed galaxy or hot cluster atmospheres. We find that the contribution of any unrelated cluster Rotation Measure variations on scales of 2 - 10 arcsec are less than 25 rad/m^2; the standard, although model dependent, derivation of cluster fields would then lead to an upper limit of approximately 0.4 microGauss on these scales. Inspection of the distributions of Rotation Measure, polarisation angle and total intensity in 3C75, 3C465 and Cygnus A also shows source-related Faraday effects in some locations. Many effects can mask the signatures of locally-dominated RMs, so the detection of even isolated correlations can be important, although difficult to quantify statistically. In order to use radio sources such as shown here to derive {\it cluster-wide} magnetic fields, as is commonly done, one must first remove the local contributions; this is not possible at present. |
| spellingShingle | Rudnick, L Blundell, K Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy contributions |
| title | Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy
contributions |
| title_full | Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy
contributions |
| title_fullStr | Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy
contributions |
| title_full_unstemmed | Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy
contributions |
| title_short | Lowering Inferred Cluster Magnetic Field Strengths - the radio galaxy
contributions |
| title_sort | lowering inferred cluster magnetic field strengths the radio galaxy contributions |
| work_keys_str_mv | AT rudnickl loweringinferredclustermagneticfieldstrengthstheradiogalaxycontributions AT blundellk loweringinferredclustermagneticfieldstrengthstheradiogalaxycontributions |