New giant radio sources and underluminous radio halos in two galaxy clusters

被引：37
作者：
Cuciti, V. [1 ,2 ]
Brunetti, G. [2 ]
van Weeren, R. [3 ]
Bonafede, A. [2 ]
Dallacasa, D. [1 ,2 ]
Cassano, R. [2 ]
Venturi, T. [2 ]
Kale, R. [4 ]
机构：
[1] Univ Bologna, Dipartimento Fis & Astron, Via P Gobetti 93-2, I-40129 Bologna, Italy
[2] INAF, Ist Radioastron, Via P Gobetti 101, I-40129 Bologna, Italy
[3] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[4] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Post Bag 3, Pune 411007, Maharashtra, India
来源：
ASTRONOMY & ASTROPHYSICS | 2018年 / 609卷
关键词：
galaxies:; clusters:; individual:; Abell; 1451; Zwcl; 0634.1+4750; galaxies: clusters: intracluster medium; radiation mechanisms: non-thermal; GAMMA-RAY EMISSION; DIFFUSIVE SHOCK ACCELERATION; LARGE-SCALE STRUCTURE; SUNYAEV-ZELDOVICH; COMA CLUSTER; LOW-FREQUENCY; COSMIC-RAYS; ABELL CLUSTERS; SEED ELECTRONS; SKY SURVEY;
D O I：
10.1051/0004-6361/201731174
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Aims. The aim of this work is to analyse the radio properties of the massive and dynamically disturbed clusters Abell 1451 and Zwcl 0634.1+4750, especially focusing on the possible presence of diffuse emission. Methods. We present new Giant Metrewave Radio Telescope (GMRT) 320 MHz and Jansky Very Large Array (JVLA) 1.5 GHz observations of these two clusters. Results. We found that both Abell 1451 and Zwcl 0634.1+4750 host a radio halo with a typical spectrum (alpha similar to 1-1.3). Similarly to a few other cases reported in the recent literature, these radio halos are significantly fainter in radio luminosity with respect to the current radio power-mass correlations and they are smaller than classical giant radio halos. These underluminous sources might contribute to elucidating the complex mechanisms of formation and evolution of radio halos. Furthermore, we detected a candidate radio relic at large distance from the cluster centre in Abell 1451 and a peculiar head-tail (HT) radio galaxy in Zwcl 0634.1+4750, which might be interacting with a shock front.
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