Abell 1430: A merging cluster with exceptional diffuse radio emission
- Autores
- Hoeft, M.; Dumba, C.; Drabent, A.; Rajpurohit, K.; Rossetti, M.; Nuza, Sebastian Ernesto; van Weeren, R. J.; Meusinger, H.; Botteon, A.; Brunetti, G.; Shimwell, T. W.; Cassano, R.; Brüggen, M.; Röttgering, H. J. A.; Gastaldello, F.; Lovisari, L.; Yepes, G.; Andrade Santos, F.; Eckert, D.
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Diffuse radio emission has been found in many galaxy clusters, predominantly in massive systems which are in the state of merging. The radio emission can usually be classified as relic or halo emission, which are believed to be related to merger shocks or volume-filling turbulence, respectively. Recent observations have revealed radio bridges for some pairs of very close galaxy clusters. The mechanisms that may allow one to explain the high specific density of relativistic electrons, which are necessary to explain the radio luminosity of these bridge regions, have been poorly explored until now. Aims. When inspecting the first data release of the LOFAR Two-Metre Sky Survey (LoTSS), we discovered diffuse radio emission in the galaxy cluster Abell 1430. Here, we aim to determine the dynamical state of the cluster and characterise the diffuse radio emission. Methods. We analysed the LoTSS data in detail and complemented them with recent Karl G. Jansky Very Large Array observations in the L-band. To study the dynamical state of the cluster, we analysed XMM-Newton data, Chandra data, and Sloan Digital Sky Survey data. Moreover, we compared our results to clusters extracted from THE THREE HUNDRED PROJECT cosmological simulation. Results. We find that Abell 1430 consists of two components, namely A1430-A and A1430-B, with a mass ratio of about 2:1. The massive component shows diffuse radio emission which can be classified as radio halo which shows a low radio power at 1.4 GHz with respect to the mass of the cluster. Most interestingly, there is extended diffuse radio emission in the following dubbed as the 'Pillow' according to its morphology, which is apparently related to A1430-B and which is neither typical halo nor typical relic emission. The origin of this emission is puzzling. We speculate that the two components of Abell 1430 undergo an off-axis merger. In this scenario, A1430-B is moving towards the main cluster component and may have compressed and stirred the medium in the filament between the two cluster components. Conclusions. We have discovered evidence for diffuse radio emission related to the low-density intracluster or intergalactic medium in Abell 1430. To date, only a few examples of emission originating from such regions are known. These discoveries are crucial to constrain possible acceleration mechanisms which may allow us to explain the presence of relativistic electrons in these regions. In particular, our results indicate a spectral index of α144 MHz1.5 GHz = -1.4±0.5 for the Pillow. If upcoming observations confirm a slope as flat as -1.4 or even flatter, this would pose a challenge for the electron acceleration scenarios.
Fil: Hoeft, M.. Tautenburg Observatory; Alemania
Fil: Dumba, C.. Tautenburg Observatory; Alemania. Mbarara University; Uganda
Fil: Drabent, A.. Tautenburg Observatory; Alemania
Fil: Rajpurohit, K.. Università di Bologna; Italia. Tautenburg Observatory; Alemania. Istituto Nazionale di Astrofisica; Italia
Fil: Rossetti, M.. Istituto Nazionale di Astrofisica; Italia
Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: van Weeren, R. J.. Leiden University; Países Bajos
Fil: Meusinger, H.. Tautenburg Observatory; Alemania
Fil: Botteon, A.. Leiden University; Países Bajos
Fil: Brunetti, G.. Istituto Nazionale di Astrofisica; Italia
Fil: Shimwell, T. W.. Leiden University; Países Bajos. Netherlands Institute for Radio Astronomy; Países Bajos
Fil: Cassano, R.. Istituto Nazionale di Astrofisica; Italia
Fil: Brüggen, M.. Universitat Hamburg; Alemania
Fil: Röttgering, H. J. A.. Leiden University; Países Bajos
Fil: Gastaldello, F.. Istituto Nazionale di Astrofisica; Italia
Fil: Lovisari, L.. Istituto Nazionale di Astrofisica; Italia. Universitat Hamburg; Alemania
Fil: Yepes, G.. Universidad Autónoma de Madrid; España
Fil: Andrade Santos, F.. Istituto Nazionale di Astrofisica; Italia
Fil: Eckert, D.. Universidad de Genova; España - Materia
-
GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1430
RADIATION MECHANISMS: NON-THERMAL
RADIATION MECHANISMS: THERMAL
RADIO CONTINUUM: GENERAL
TECHNIQUES: INTERFEROMETRIC
X-RAYS: GALAXIES: CLUSTERS - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/182823
Ver los metadatos del registro completo
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oai:ri.conicet.gov.ar:11336/182823 |
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CONICET Digital (CONICET) |
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Abell 1430: A merging cluster with exceptional diffuse radio emissionHoeft, M.Dumba, C.Drabent, A.Rajpurohit, K.Rossetti, M.Nuza, Sebastian Ernestovan Weeren, R. J.Meusinger, H.Botteon, A.Brunetti, G.Shimwell, T. W.Cassano, R.Brüggen, M.Röttgering, H. J. A.Gastaldello, F.Lovisari, L.Yepes, G.Andrade Santos, F.Eckert, D.GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1430RADIATION MECHANISMS: NON-THERMALRADIATION MECHANISMS: THERMALRADIO CONTINUUM: GENERALTECHNIQUES: INTERFEROMETRICX-RAYS: GALAXIES: CLUSTERShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Diffuse radio emission has been found in many galaxy clusters, predominantly in massive systems which are in the state of merging. The radio emission can usually be classified as relic or halo emission, which are believed to be related to merger shocks or volume-filling turbulence, respectively. Recent observations have revealed radio bridges for some pairs of very close galaxy clusters. The mechanisms that may allow one to explain the high specific density of relativistic electrons, which are necessary to explain the radio luminosity of these bridge regions, have been poorly explored until now. Aims. When inspecting the first data release of the LOFAR Two-Metre Sky Survey (LoTSS), we discovered diffuse radio emission in the galaxy cluster Abell 1430. Here, we aim to determine the dynamical state of the cluster and characterise the diffuse radio emission. Methods. We analysed the LoTSS data in detail and complemented them with recent Karl G. Jansky Very Large Array observations in the L-band. To study the dynamical state of the cluster, we analysed XMM-Newton data, Chandra data, and Sloan Digital Sky Survey data. Moreover, we compared our results to clusters extracted from THE THREE HUNDRED PROJECT cosmological simulation. Results. We find that Abell 1430 consists of two components, namely A1430-A and A1430-B, with a mass ratio of about 2:1. The massive component shows diffuse radio emission which can be classified as radio halo which shows a low radio power at 1.4 GHz with respect to the mass of the cluster. Most interestingly, there is extended diffuse radio emission in the following dubbed as the 'Pillow' according to its morphology, which is apparently related to A1430-B and which is neither typical halo nor typical relic emission. The origin of this emission is puzzling. We speculate that the two components of Abell 1430 undergo an off-axis merger. In this scenario, A1430-B is moving towards the main cluster component and may have compressed and stirred the medium in the filament between the two cluster components. Conclusions. We have discovered evidence for diffuse radio emission related to the low-density intracluster or intergalactic medium in Abell 1430. To date, only a few examples of emission originating from such regions are known. These discoveries are crucial to constrain possible acceleration mechanisms which may allow us to explain the presence of relativistic electrons in these regions. In particular, our results indicate a spectral index of α144 MHz1.5 GHz = -1.4±0.5 for the Pillow. If upcoming observations confirm a slope as flat as -1.4 or even flatter, this would pose a challenge for the electron acceleration scenarios.Fil: Hoeft, M.. Tautenburg Observatory; AlemaniaFil: Dumba, C.. Tautenburg Observatory; Alemania. Mbarara University; UgandaFil: Drabent, A.. Tautenburg Observatory; AlemaniaFil: Rajpurohit, K.. Università di Bologna; Italia. Tautenburg Observatory; Alemania. Istituto Nazionale di Astrofisica; ItaliaFil: Rossetti, M.. Istituto Nazionale di Astrofisica; ItaliaFil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: van Weeren, R. J.. Leiden University; Países BajosFil: Meusinger, H.. Tautenburg Observatory; AlemaniaFil: Botteon, A.. Leiden University; Países BajosFil: Brunetti, G.. Istituto Nazionale di Astrofisica; ItaliaFil: Shimwell, T. W.. Leiden University; Países Bajos. Netherlands Institute for Radio Astronomy; Países BajosFil: Cassano, R.. Istituto Nazionale di Astrofisica; ItaliaFil: Brüggen, M.. Universitat Hamburg; AlemaniaFil: Röttgering, H. J. A.. Leiden University; Países BajosFil: Gastaldello, F.. Istituto Nazionale di Astrofisica; ItaliaFil: Lovisari, L.. Istituto Nazionale di Astrofisica; Italia. Universitat Hamburg; AlemaniaFil: Yepes, G.. Universidad Autónoma de Madrid; EspañaFil: Andrade Santos, F.. Istituto Nazionale di Astrofisica; ItaliaFil: Eckert, D.. Universidad de Genova; EspañaEDP Sciences2021-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/182823Hoeft, M.; Dumba, C.; Drabent, A.; Rajpurohit, K.; Rossetti, M.; et al.; Abell 1430: A merging cluster with exceptional diffuse radio emission; EDP Sciences; Astronomy and Astrophysics; 654; A68; 10-2021; 1-130004-63611432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202039725info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039725info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2010.10331info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:36:15Zoai:ri.conicet.gov.ar:11336/182823instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:36:15.673CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
title |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
spellingShingle |
Abell 1430: A merging cluster with exceptional diffuse radio emission Hoeft, M. GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1430 RADIATION MECHANISMS: NON-THERMAL RADIATION MECHANISMS: THERMAL RADIO CONTINUUM: GENERAL TECHNIQUES: INTERFEROMETRIC X-RAYS: GALAXIES: CLUSTERS |
title_short |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
title_full |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
title_fullStr |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
title_full_unstemmed |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
title_sort |
Abell 1430: A merging cluster with exceptional diffuse radio emission |
dc.creator.none.fl_str_mv |
Hoeft, M. Dumba, C. Drabent, A. Rajpurohit, K. Rossetti, M. Nuza, Sebastian Ernesto van Weeren, R. J. Meusinger, H. Botteon, A. Brunetti, G. Shimwell, T. W. Cassano, R. Brüggen, M. Röttgering, H. J. A. Gastaldello, F. Lovisari, L. Yepes, G. Andrade Santos, F. Eckert, D. |
author |
Hoeft, M. |
author_facet |
Hoeft, M. Dumba, C. Drabent, A. Rajpurohit, K. Rossetti, M. Nuza, Sebastian Ernesto van Weeren, R. J. Meusinger, H. Botteon, A. Brunetti, G. Shimwell, T. W. Cassano, R. Brüggen, M. Röttgering, H. J. A. Gastaldello, F. Lovisari, L. Yepes, G. Andrade Santos, F. Eckert, D. |
author_role |
author |
author2 |
Dumba, C. Drabent, A. Rajpurohit, K. Rossetti, M. Nuza, Sebastian Ernesto van Weeren, R. J. Meusinger, H. Botteon, A. Brunetti, G. Shimwell, T. W. Cassano, R. Brüggen, M. Röttgering, H. J. A. Gastaldello, F. Lovisari, L. Yepes, G. Andrade Santos, F. Eckert, D. |
author2_role |
author author author author author author author author author author author author author author author author author author |
dc.subject.none.fl_str_mv |
GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1430 RADIATION MECHANISMS: NON-THERMAL RADIATION MECHANISMS: THERMAL RADIO CONTINUUM: GENERAL TECHNIQUES: INTERFEROMETRIC X-RAYS: GALAXIES: CLUSTERS |
topic |
GALAXIES: CLUSTERS: INDIVIDUAL: ABELL 1430 RADIATION MECHANISMS: NON-THERMAL RADIATION MECHANISMS: THERMAL RADIO CONTINUUM: GENERAL TECHNIQUES: INTERFEROMETRIC X-RAYS: GALAXIES: CLUSTERS |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Context. Diffuse radio emission has been found in many galaxy clusters, predominantly in massive systems which are in the state of merging. The radio emission can usually be classified as relic or halo emission, which are believed to be related to merger shocks or volume-filling turbulence, respectively. Recent observations have revealed radio bridges for some pairs of very close galaxy clusters. The mechanisms that may allow one to explain the high specific density of relativistic electrons, which are necessary to explain the radio luminosity of these bridge regions, have been poorly explored until now. Aims. When inspecting the first data release of the LOFAR Two-Metre Sky Survey (LoTSS), we discovered diffuse radio emission in the galaxy cluster Abell 1430. Here, we aim to determine the dynamical state of the cluster and characterise the diffuse radio emission. Methods. We analysed the LoTSS data in detail and complemented them with recent Karl G. Jansky Very Large Array observations in the L-band. To study the dynamical state of the cluster, we analysed XMM-Newton data, Chandra data, and Sloan Digital Sky Survey data. Moreover, we compared our results to clusters extracted from THE THREE HUNDRED PROJECT cosmological simulation. Results. We find that Abell 1430 consists of two components, namely A1430-A and A1430-B, with a mass ratio of about 2:1. The massive component shows diffuse radio emission which can be classified as radio halo which shows a low radio power at 1.4 GHz with respect to the mass of the cluster. Most interestingly, there is extended diffuse radio emission in the following dubbed as the 'Pillow' according to its morphology, which is apparently related to A1430-B and which is neither typical halo nor typical relic emission. The origin of this emission is puzzling. We speculate that the two components of Abell 1430 undergo an off-axis merger. In this scenario, A1430-B is moving towards the main cluster component and may have compressed and stirred the medium in the filament between the two cluster components. Conclusions. We have discovered evidence for diffuse radio emission related to the low-density intracluster or intergalactic medium in Abell 1430. To date, only a few examples of emission originating from such regions are known. These discoveries are crucial to constrain possible acceleration mechanisms which may allow us to explain the presence of relativistic electrons in these regions. In particular, our results indicate a spectral index of α144 MHz1.5 GHz = -1.4±0.5 for the Pillow. If upcoming observations confirm a slope as flat as -1.4 or even flatter, this would pose a challenge for the electron acceleration scenarios. Fil: Hoeft, M.. Tautenburg Observatory; Alemania Fil: Dumba, C.. Tautenburg Observatory; Alemania. Mbarara University; Uganda Fil: Drabent, A.. Tautenburg Observatory; Alemania Fil: Rajpurohit, K.. Università di Bologna; Italia. Tautenburg Observatory; Alemania. Istituto Nazionale di Astrofisica; Italia Fil: Rossetti, M.. Istituto Nazionale di Astrofisica; Italia Fil: Nuza, Sebastian Ernesto. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: van Weeren, R. J.. Leiden University; Países Bajos Fil: Meusinger, H.. Tautenburg Observatory; Alemania Fil: Botteon, A.. Leiden University; Países Bajos Fil: Brunetti, G.. Istituto Nazionale di Astrofisica; Italia Fil: Shimwell, T. W.. Leiden University; Países Bajos. Netherlands Institute for Radio Astronomy; Países Bajos Fil: Cassano, R.. Istituto Nazionale di Astrofisica; Italia Fil: Brüggen, M.. Universitat Hamburg; Alemania Fil: Röttgering, H. J. A.. Leiden University; Países Bajos Fil: Gastaldello, F.. Istituto Nazionale di Astrofisica; Italia Fil: Lovisari, L.. Istituto Nazionale di Astrofisica; Italia. Universitat Hamburg; Alemania Fil: Yepes, G.. Universidad Autónoma de Madrid; España Fil: Andrade Santos, F.. Istituto Nazionale di Astrofisica; Italia Fil: Eckert, D.. Universidad de Genova; España |
description |
Context. Diffuse radio emission has been found in many galaxy clusters, predominantly in massive systems which are in the state of merging. The radio emission can usually be classified as relic or halo emission, which are believed to be related to merger shocks or volume-filling turbulence, respectively. Recent observations have revealed radio bridges for some pairs of very close galaxy clusters. The mechanisms that may allow one to explain the high specific density of relativistic electrons, which are necessary to explain the radio luminosity of these bridge regions, have been poorly explored until now. Aims. When inspecting the first data release of the LOFAR Two-Metre Sky Survey (LoTSS), we discovered diffuse radio emission in the galaxy cluster Abell 1430. Here, we aim to determine the dynamical state of the cluster and characterise the diffuse radio emission. Methods. We analysed the LoTSS data in detail and complemented them with recent Karl G. Jansky Very Large Array observations in the L-band. To study the dynamical state of the cluster, we analysed XMM-Newton data, Chandra data, and Sloan Digital Sky Survey data. Moreover, we compared our results to clusters extracted from THE THREE HUNDRED PROJECT cosmological simulation. Results. We find that Abell 1430 consists of two components, namely A1430-A and A1430-B, with a mass ratio of about 2:1. The massive component shows diffuse radio emission which can be classified as radio halo which shows a low radio power at 1.4 GHz with respect to the mass of the cluster. Most interestingly, there is extended diffuse radio emission in the following dubbed as the 'Pillow' according to its morphology, which is apparently related to A1430-B and which is neither typical halo nor typical relic emission. The origin of this emission is puzzling. We speculate that the two components of Abell 1430 undergo an off-axis merger. In this scenario, A1430-B is moving towards the main cluster component and may have compressed and stirred the medium in the filament between the two cluster components. Conclusions. We have discovered evidence for diffuse radio emission related to the low-density intracluster or intergalactic medium in Abell 1430. To date, only a few examples of emission originating from such regions are known. These discoveries are crucial to constrain possible acceleration mechanisms which may allow us to explain the presence of relativistic electrons in these regions. In particular, our results indicate a spectral index of α144 MHz1.5 GHz = -1.4±0.5 for the Pillow. If upcoming observations confirm a slope as flat as -1.4 or even flatter, this would pose a challenge for the electron acceleration scenarios. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-10 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/182823 Hoeft, M.; Dumba, C.; Drabent, A.; Rajpurohit, K.; Rossetti, M.; et al.; Abell 1430: A merging cluster with exceptional diffuse radio emission; EDP Sciences; Astronomy and Astrophysics; 654; A68; 10-2021; 1-13 0004-6361 1432-0746 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/182823 |
identifier_str_mv |
Hoeft, M.; Dumba, C.; Drabent, A.; Rajpurohit, K.; Rossetti, M.; et al.; Abell 1430: A merging cluster with exceptional diffuse radio emission; EDP Sciences; Astronomy and Astrophysics; 654; A68; 10-2021; 1-13 0004-6361 1432-0746 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202039725 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039725 info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2010.10331 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
EDP Sciences |
publisher.none.fl_str_mv |
EDP Sciences |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |