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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/182823

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oai_identifier_str oai:ri.conicet.gov.ar:11336/182823
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling 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/
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application/pdf
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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
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv 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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