Diffuse Radio Emission from Galaxy Clusters
Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
van Weeren, R. J. [verfasserIn] de Gasperin, F. [verfasserIn] Akamatsu, H. [verfasserIn] Brüggen, M. [verfasserIn] Feretti, L. [verfasserIn] Kang, H. [verfasserIn] Stroe, A. [verfasserIn] Zandanel, F. [verfasserIn] |
|---|
| Format: |
E-Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2019 |
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| Schlagwörter: |
Galaxies: clusters: intracluster medium Gamma rays: galaxies: clusters Radiation mechanisms: non-thermal |
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| Übergeordnetes Werk: |
Enthalten in: Space science reviews - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962, 215(2019), 1 vom: 05. Feb. |
|---|---|
| Übergeordnetes Werk: |
volume:215 ; year:2019 ; number:1 ; day:05 ; month:02 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11214-019-0584-z |
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| Katalog-ID: |
SPR017819741 |
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| 245 | 1 | 0 | |a Diffuse Radio Emission from Galaxy Clusters |
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| 520 | |a Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. | ||
| 650 | 4 | |a Galaxies: clusters: general |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Galaxies: clusters: intracluster medium |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a X-rays: galaxies: clusters |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Gamma rays: galaxies: clusters |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radiation mechanisms: non-thermal |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Acceleration of particles |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Magnetic fields |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Large-scale structure of Universe |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Intergalactic medium |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a de Gasperin, F. |e verfasserin |4 aut | |
| 700 | 1 | |a Akamatsu, H. |e verfasserin |4 aut | |
| 700 | 1 | |a Brüggen, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Feretti, L. |e verfasserin |4 aut | |
| 700 | 1 | |a Kang, H. |e verfasserin |4 aut | |
| 700 | 1 | |a Stroe, A. |e verfasserin |4 aut | |
| 700 | 1 | |a Zandanel, F. |e verfasserin |4 aut | |
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10.1007/s11214-019-0584-z doi (DE-627)SPR017819741 (SPR)s11214-019-0584-z-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl van Weeren, R. J. verfasserin aut Diffuse Radio Emission from Galaxy Clusters 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 de Gasperin, F. verfasserin aut Akamatsu, H. verfasserin aut Brüggen, M. verfasserin aut Feretti, L. verfasserin aut Kang, H. verfasserin aut Stroe, A. verfasserin aut Zandanel, F. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 215(2019), 1 vom: 05. Feb. (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:215 year:2019 number:1 day:05 month:02 https://dx.doi.org/10.1007/s11214-019-0584-z kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 215 2019 1 05 02 |
| spelling |
10.1007/s11214-019-0584-z doi (DE-627)SPR017819741 (SPR)s11214-019-0584-z-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl van Weeren, R. J. verfasserin aut Diffuse Radio Emission from Galaxy Clusters 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 de Gasperin, F. verfasserin aut Akamatsu, H. verfasserin aut Brüggen, M. verfasserin aut Feretti, L. verfasserin aut Kang, H. verfasserin aut Stroe, A. verfasserin aut Zandanel, F. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 215(2019), 1 vom: 05. Feb. (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:215 year:2019 number:1 day:05 month:02 https://dx.doi.org/10.1007/s11214-019-0584-z kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 215 2019 1 05 02 |
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10.1007/s11214-019-0584-z doi (DE-627)SPR017819741 (SPR)s11214-019-0584-z-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl van Weeren, R. J. verfasserin aut Diffuse Radio Emission from Galaxy Clusters 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 de Gasperin, F. verfasserin aut Akamatsu, H. verfasserin aut Brüggen, M. verfasserin aut Feretti, L. verfasserin aut Kang, H. verfasserin aut Stroe, A. verfasserin aut Zandanel, F. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 215(2019), 1 vom: 05. Feb. (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:215 year:2019 number:1 day:05 month:02 https://dx.doi.org/10.1007/s11214-019-0584-z kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 215 2019 1 05 02 |
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10.1007/s11214-019-0584-z doi (DE-627)SPR017819741 (SPR)s11214-019-0584-z-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl van Weeren, R. J. verfasserin aut Diffuse Radio Emission from Galaxy Clusters 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 de Gasperin, F. verfasserin aut Akamatsu, H. verfasserin aut Brüggen, M. verfasserin aut Feretti, L. verfasserin aut Kang, H. verfasserin aut Stroe, A. verfasserin aut Zandanel, F. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 215(2019), 1 vom: 05. Feb. (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:215 year:2019 number:1 day:05 month:02 https://dx.doi.org/10.1007/s11214-019-0584-z kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 215 2019 1 05 02 |
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10.1007/s11214-019-0584-z doi (DE-627)SPR017819741 (SPR)s11214-019-0584-z-e DE-627 ger DE-627 rakwb eng 600 ASE 39.00 bkl van Weeren, R. J. verfasserin aut Diffuse Radio Emission from Galaxy Clusters 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 de Gasperin, F. verfasserin aut Akamatsu, H. verfasserin aut Brüggen, M. verfasserin aut Feretti, L. verfasserin aut Kang, H. verfasserin aut Stroe, A. verfasserin aut Zandanel, F. verfasserin aut Enthalten in Space science reviews Dordrecht [u.a.] : Springer Science + Business Media B.V, 1962 215(2019), 1 vom: 05. Feb. (DE-627)315621222 (DE-600)2017804-9 1572-9672 nnns volume:215 year:2019 number:1 day:05 month:02 https://dx.doi.org/10.1007/s11214-019-0584-z kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 215 2019 1 05 02 |
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van Weeren, R. J. @@aut@@ de Gasperin, F. @@aut@@ Akamatsu, H. @@aut@@ Brüggen, M. @@aut@@ Feretti, L. @@aut@@ Kang, H. @@aut@@ Stroe, A. @@aut@@ Zandanel, F. @@aut@@ |
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J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Diffuse Radio Emission from Galaxy Clusters</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2019</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). 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van Weeren, R. J. |
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van Weeren, R. J. ddc 600 bkl 39.00 misc Galaxies: clusters: general misc Galaxies: clusters: intracluster medium misc X-rays: galaxies: clusters misc Gamma rays: galaxies: clusters misc Radiation mechanisms: non-thermal misc Acceleration of particles misc Magnetic fields misc Large-scale structure of Universe misc Intergalactic medium Diffuse Radio Emission from Galaxy Clusters |
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600 ASE 39.00 bkl Diffuse Radio Emission from Galaxy Clusters Galaxies: clusters: general (dpeaa)DE-He213 Galaxies: clusters: intracluster medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Gamma rays: galaxies: clusters (dpeaa)DE-He213 Radiation mechanisms: non-thermal (dpeaa)DE-He213 Acceleration of particles (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Large-scale structure of Universe (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 |
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ddc 600 bkl 39.00 misc Galaxies: clusters: general misc Galaxies: clusters: intracluster medium misc X-rays: galaxies: clusters misc Gamma rays: galaxies: clusters misc Radiation mechanisms: non-thermal misc Acceleration of particles misc Magnetic fields misc Large-scale structure of Universe misc Intergalactic medium |
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ddc 600 bkl 39.00 misc Galaxies: clusters: general misc Galaxies: clusters: intracluster medium misc X-rays: galaxies: clusters misc Gamma rays: galaxies: clusters misc Radiation mechanisms: non-thermal misc Acceleration of particles misc Magnetic fields misc Large-scale structure of Universe misc Intergalactic medium |
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ddc 600 bkl 39.00 misc Galaxies: clusters: general misc Galaxies: clusters: intracluster medium misc X-rays: galaxies: clusters misc Gamma rays: galaxies: clusters misc Radiation mechanisms: non-thermal misc Acceleration of particles misc Magnetic fields misc Large-scale structure of Universe misc Intergalactic medium |
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Diffuse Radio Emission from Galaxy Clusters |
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Diffuse Radio Emission from Galaxy Clusters |
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van Weeren, R. J. |
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Space science reviews |
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van Weeren, R. J. de Gasperin, F. Akamatsu, H. Brüggen, M. Feretti, L. Kang, H. Stroe, A. Zandanel, F. |
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diffuse radio emission from galaxy clusters |
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Diffuse Radio Emission from Galaxy Clusters |
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Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. |
| abstractGer |
Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. |
| abstract_unstemmed |
Abstract In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos, mini-halos, and possible “intermediate” sources. Halos are generally positioned at cluster center and their brightness approximately follows the distribution of the thermal ICM. Cluster radio shocks (relics) are polarized sources mostly found in the cluster’s periphery. They trace merger induced shock waves. Revived fossil plasma sources are characterized by their radio steep-spectra and often irregular morphologies. In this review we give an overview of the properties of diffuse cluster radio sources, with an emphasis on recent observational results. We discuss the resulting implications for the underlying physical acceleration processes that operate in the ICM, the role of relativistic fossil plasma, and the properties of ICM shocks and magnetic fields. We also compile an updated list of diffuse cluster radio sources which will be available on-line (http://galaxyclusters.com). We end this review with a discussion on the detection of diffuse radio emission from the cosmic web. |
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Diffuse Radio Emission from Galaxy Clusters |
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de Gasperin, F. Akamatsu, H. Brüggen, M. Feretti, L. Kang, H. Stroe, A. Zandanel, F. |
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| score |
7.4022417 |