Table 5
Details of radio point sources and the thermal noise levels for the AMI observations of the cluster sample.
| A | B | C | D | E | F | G |
|
|
||||||
| A2034 | 13 | 32.5 | 0.08 | 0.08 | 0.025 | 10 |
| A1413 | 21 | 47.7 | 0.09 | 0.12 | 0.023 | 12 |
| A990 | 20 | 56.3 | 0.11 | 0.10 | 0.029 | 8 |
| A2409 | 14 | 49.2 | 0.11 | 0.10 | 0.032 | 11 |
| A1914 | 15 | 31.8 | 0.12 | 0.10 | 0.032 | 11 |
| A2218 | 10 | 31.9 | 0.11 | 0.15 | 0.031 | 12 |
| A773 | 9 | 13.6 | 0.12 | 0.12 | 0.033 | 6 |
| MACS J1149+2223 | 15 | 45.2 | 0.09 | 0.14 | 0.028 | 17 |
| RXJ0748+5941 | 15 | 17.1 | 0.07 | 0.06 | 0.025 | 12 |
| PLCKESZ G139.59+24.18 | 14 | 13.2 | 0.09 | 0.06 | 0.028 | 11 |
| PLCKESZ G121.11+57.01 | 19 | 25.4 | 0.07 | 0.06 | 0.035 | 10 |
Notes. Columns are: (A) Cluster name; (B) number of LA sources detected at S/N ≥ 3.5σLA; (C) total source flux (mJy beam-1); (D) σSA (mJy beam-1); (E) σLA (mJy beam-1); (F) σLA (mJy beam-1) for deep LA pointings towards cluster centres (see description of AMI data in Sect. 4); and (G) S/N of SZ decrement detection. σSA and σLA refer to the thermal noise levels reached in the LA and SA maps. S/N is calculated by dividing the peak flux values by σSA.
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