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Table 4.

Catalogue of the 99 diffuse cluster radio sources detected in the MGCLS.

(1) (2) (3) (4) (5) (6) (7) (8) (9)
Cluster name RAJ2000 DecJ2000 z Class New? LAS LLS Notes [Refs.]
(deg) (deg) (′) (Mpc)
Abell 13 3.384 −19.501 0.094 cR 3.0 0.32 W of centre; [8, 13, 17, 37]
Abell 22 5.161 −25.722 0.142 cH 2.7 0.41 [8]
Abell 85 10.453 −9.318 0.056 MH ( † ) ✓ 4.0 0.26
Ph (a) 5.6 0.36 SW of centre; [8, 18]
Abell 168 18.791 0.248 0.045 R 12.4 0.66 N of centre; [10]
Abell 209 22.990 −13.576 0.209 H 7.9 1.62 Embedded HT; [17, 19, 20, 41, 42]
Abell 370 39.960 −1.586 0.375 cH ✓ 3.1 0.96 [44]
Abell 521 73.536 −10.244 0.248 R 6.0 1.40 SE of centre; [11, 15, 28, 41]
H 5.3 1.23 [4, 6, 20, 28, 42]
R ✓ 4.0 0.93 NW of centre
Abell 545 (b) 83.102 −11.543 0.154 H 4.7 0.75 [1, 17]
Abell 2645 355.320 −9.028 0.251 cH ✓ 2.7 0.64 Irregular shape; [5]
Abell 2667 357.920 −26.084 0.232 H ( † ) 4.6 1.02 [16]
Abell 2744 3.567 −30.383 0.307 H 7.5 2.04 [8, 13, 17, 21, 32, 42]
R 5.8 1.57 NE of centre; [8, 13, 21, 30, 32, 42]
R 4.6 1.25 SE of centre; [32]
Abell 2751 4.058 −31.389 0.081 cPh ✓ 0.9 0.08 NW of centre; [8] (says relic)
Abell 2811 10.537 −28.536 0.108 H 5.2 0.62 [8]
Abell 2813 10.852 −20.621 0.292 cH ✓ 3.1 0.81
Abell 2895 19.546 −26.973 0.228 cPh ✓ 0.8 0.18 E of centre
Abell 3365 87.050 −21.935 0.093 R ✓ 6.8 0.70 NE of centre; [45]
R ✓ 3.4 0.35 W of centre; [45]
Abell 3376 90.426 −39.985 0.047 R 28.1 1.55 E of centre; [2, 12, 23]
R 18.8 1.04 W of centre; [2, 12, 23]
Abell 3558 201.978 −31.492 0.048 H 4.5 0.25 [7, 39]
Abell 3562 202.783 −31.673 0.050 H 11.5 0.67 [7, 14, 40]
R 8.6 0.50 SW of centre; [40]
Abell 3667 303.140 −56.841 0.056 R 25.8 1.67 SE of centre; [22, 33]
R 35.2 2.28 NW of centre; [22, 33]
Abell 4038 356.880 −28.203 0.030 cMH ✓ 4.5 0.16 Embedded HT
Abell S295 41.400 −53.038 0.300 H 4.0 1.07 [46]
Abell S1063 342.181 −44.529 0.348 H 5.5 1.62 [44]
Abell S1121 351.284 −41.212 0.190 U 2.2 0.42 SE of centre
Bullet 104.658 −55.950 0.297 H 8.5 2.26 [26, 35]
R 3.8 1.01 E of centre; [36]
El Gordo 15.719 −49.250 0.870 H 3.3 1.53 [3, 27]
R 2.0 0.93 NW of centre; [3, 27]
R 1.0 0.46 SE of centre; [3, 27]
R 0.9 0.42 E of centre; [27]
PLCK G200.9−28.2 72.587 −2.949 0.220 R ✓ 5.6 1.19 E of centre
R ✓ 2.7 0.58 SW of centre; [24]
cR ✓ 1.0 0.21 NW of centre
MACS J0257.6−2209 (c) 44.412 −22.163 0.322 U 1.6 0.45 [16]
cR ✓ 1.4 0.39 SW of centre
MACS J0417.5−1154 64.394 −11.909 0.443 H ( † ) 4.9 1.68 [9, 31, 34]
cR ✓ 1.0 0.34 N of centre
cR ✓ 1.0 0.34 NW of centre
RXC J0510.7−0801 77.685 −8.020 0.220 cH ( † ) ✓ 4.9 1.04
cR ✓ 3.0 0.64 N of centre; possible WAT
RXC J0520.7−1328 (d) 80.200 −13.502 0.336 cR 4.2 1.21 SE of centre; [29]
U 7.1 2.05 SE of centre; bubble?; [29]
RXC J1314.4−2525 198.599 −25.256 0.244 H 4.7 1.08 [38, 48]
R 4.7 1.08 W of centre; [38, 48]
R 2.7 0.62 E of centre; [38, 48]
RXC J2351.0−1954 357.770 −19.913 0.248 cR 9.8 2.28 W of centre; [8]
cR 5.5 1.28 E of centre; [8]
cH ✓ 4.0 0.93 [8]
J0027.3−5015 6.839 −50.251 0.145 cMH ✓ 2.5 0.38
J0145.0−5300 26.260 −53.014 0.117 H ✓ 4.9 0.62
J0145.2−6033 26.320 −60.565 0.181 cMH ✓ 1.9 0.35
J0216.3−4816 34.080 −48.273 0.163 cMH ✓ 1.4 0.24
J0217.2−5244 34.303 −52.747 0.343 cR ✓ 1.5 0.44 N of centre
J0225.9−4154 36.478 −41.910 0.220 H ✓ 2.4 0.51
J0232.2−4420 38.070 −44.348 0.284 H 5.8 1.49 [25]
cR ✓ 3.3 0.85 S of centre
cR ✓ 1.8 0.46 E of centre
J0303.7−7752 45.943 −77.869 0.274 H ✓ 3.8 0.95
J0314.3−4525 48.583 −45.424 0.072 cMH ✓ 2.4 0.20
J0342.8−5338 55.725 −53.635 0.060 MH ( † ) ✓ 5.2 0.36
J0351.1−8212 57.787 −82.217 0.061 U ✓ See Sect. 6.2.2
J0352.4−7401 58.123 −74.031 0.127 R ✓ 15.6 2.13 SE of centre
H ✓ 10.7 1.46
cR ✓ 6.8 0.93 NW of centre
R ✓ 3.9 0.53 NNW of centre
R ✓ 5.0 0.68 N of centre
J0431.4−6126 67.850 −61.444 0.059 R ✓ 9.7 0.66 SE of centre
U ✓ Confused tail
J0510.2−4519 77.558 −45.321 0.200 cMH ✓ 1.3 0.26
J0516.6−5430 79.158 −54.514 0.295 H ✓ 5.7 1.51
R ✓ 5.7 1.51 N of centre
cR ✓ 2.3 0.61 S of centre
J0528.9−3927 82.235 −39.463 0.284 H 4.0 1.06 [46]
J0627.2−5428 96.810 −54.470 0.051 R ✓ 5.4 0.32 W of centre
J0631.3−5610 97.836 −56.172 0.054 cR ✓ 7.7 0.49 W of centre
J0637.3−4828 99.329 −48.478 0.203 U ✓ 7.6 1.52
cR ✓ 2.0 0.40 NW of centre
J0638.7−5358 99.694 −53.972 0.227 H ( † ) 6.4 1.40 [43]
J0645.4−5413 101.372 −54.219 0.164 H ✓ 7.7 1.30
R ✓ 3.5 0.59 SW of centre
J0745.1−5404 116.290 −54.079 0.074 U ✓ 4.2 0.35 S of centre
J0820.9−5704 125.248 −57.080 0.061 U ✓ S of centre
J1130.0−4213 172.523 −42.230 0.155 cR ✓ 2.1 0.34 NE of centre
J1423.7−5412 215.930 −54.203 0.300 U ✓ N of centre
J1539.5−8335 234.891 −83.592 0.073 MH ✓ 2.8 0.23
cR ✓ 2.2 0.18 W of centre
J1601.7−7544 240.445 −75.746 0.153 H ✓ 5.9 0.94
J1840.6−7709 280.155 −77.156 0.019 cMH ✓ 2.5 0.06
J2023.4−5535 305.852 −55.592 0.232 H 4.7 1.04 [47]
R 2.9 0.64 [47]

Notes. Several of the 62 MGCLS clusters in this catalogue are host to more than one diffuse cluster source. Columns: (1) Cluster name; (2) and (3) NED cluster position: J2000 RA and Dec; (4) Cluster redshift; (5) Diffuse source classification – mini-halo (MH), halo (H), relic (R), phoenix (Ph), candidate (c), unknown/unclear (U); see Sect. 6 for further details. Elongated halos/halo candidates with embedded bright AGN sources are indicated by ( † ); (6) Indicates whether or not the diffuse source is a new detection; (7) Largest angular size in arcminutes; (8) Largest physical linear size at the cluster redshift in Mpc; (9) Notes on the detection with references, in square brackets, to previous studies. HT – head-tail galaxy; WAT – wide-angle tail galaxy.

(a)

Mixed classification in the literature (see Sect. 6.1.1).

(b)

Diffuse emission from the Hα region in the Orion Nebula is also detected in this field.

(c)

MACS J0257.6−2209 has a published detection of a giant radio halo (Giacintucci et al. 2017) but in the higher-quality MGCLS data, the reported giant halo looks like the blending of other sources.

(d)

Diffuse emission in RXC J0520.7−1328 is complex and difficult to classify (see Sect. 6.1.2).

References. [1] Bacchi et al. (2003); [2] Bagchi et al. (2006); [3] Botteon et al. (2016); [4] Brunetti et al. (2008); [5] Cassano et al. (2013); [6] Dallacasa et al. (2009); [7] Di Gennaro et al. (2018b); [8] Duchesne et al. (2021a); [9] Dwarakanath et al. (2011); [10] Dwarakanath et al. (2018); [11] Ferrari et al. (2006); [12] George et al. (2015); [13] George et al. (2017); [14] Giacintucci et al. (2005); [15] Giacintucci et al. (2008); [16] Giacintucci et al. (2017); [17] Giovannini et al. (1999); [18] Giovannini & Feretti (2000); [19] Giovannini et al. (2006); [20] Giovannini et al. (2009); [21] Govoni et al. (2001); [22] Hindson et al. (2014); [23] Kale et al. (2012); [24] Kale et al. (2017); [25] Kale et al. (2019); [26] Liang et al. (2000); [27] Lindner et al. (2014); [28] Macario et al. (2013); [29] Macario et al. (2014); [30] Orrù et al. (2007); [31] Parekh et al. (2017); [32] Pearce et al. (2017); [33] Rottgering et al. (1997); [34] Sandhu et al. (2018); [35] Shimwell et al. (2014); [36] Shimwell et al. (2015); [37] Slee et al. (2001); [38] Stuardi et al. (2019); [39] Venturi et al. (2000); [40] Venturi et al. (2003); [41] Venturi et al. (2007); [42] Venturi et al. (2013); [43] Wilber et al. (2020); [44] Xie et al. (2020); [45] van Weeren et al. (2011b); [46] Knowles et al. (2021); [47] HyeongHan et al. (2020); [48] Feretti et al. (2005). We note that after our review of the literature, detections of diffuse emission in some of the clusters above are published by Duchesne et al. (2021b), Brüggen et al. (2021) and Duchesne et al. (2021c).

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