Table 2.
Excerpt of the MGCLS compact source catalogue at 1.28 GHz.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Src. name | RAJ2000 | DecJ2000 | ΔRA | ΔDec |
 |
ΔStot |
 |
ΔIpeak | smax | smin | sp.a. | Field |
| MKTCS | (deg) | (deg) | (deg) | (deg) | (mJy) | (mJy) | (mJy b−1) | (mJy b−1) | (″) | (″) | (°) | |
| J001059.77−190940.3 | 2.7491 | −19.1612 | 0.0000 | 0.0000 | 0.695 | 0.020 | 0.669 | 0.011 | 7.6 | 7.5 | 6 | Abell_13 |
| J001059.94−190654.9 | 2.7498 | −19.1153 | 0.0001 | 0.0002 | 0.113 | 0.028 | 0.081 | 0.013 | 9.8 | 7.8 | 21 | Abell_13 |
| J001059.14−195204.2 | 2.7464 | −19.8679 | 0.0002 | 0.0003 | 0.106 | 0.027 | 0.056 | 0.010 | 14.2 | 7.3 | 143 | Abell_13 |
| J001059.23−194540.7 | 2.7468 | −19.7613 | 0.0002 | 0.0003 | 0.077 | 0.024 | 0.045 | 0.010 | 11.1 | 8.4 | 153 | Abell_13 |
| J001059.50−192405.3 | 2.7479 | −19.4015 | 0.0001 | 0.0001 | 0.050 | 0.012 | 0.060 | 0.007 | 8.0 | 5.8 | 179 | Abell_13 |
| J002318.34−254121.6 | 5.8264 | −25.6894 | 0.0001 | 0.0002 | 0.053 | 0.016 | 0.061 | 0.010 | 7.4 | 6.5 | 10 | Abell_22 |
| J002317.08−253627.2 | 5.8212 | −25.6076 | 0.0000 | 0.0000 | 0.939 | 0.021 | 0.827 | 0.011 | 8.3 | 7.6 | 36 | Abell_22 |
| J002318.08−253621.5 | 5.8253 | −25.6060 | 0.0002 | 0.0001 | 0.073 | 0.021 | 0.067 | 0.011 | 8.5 | 7.1 | 62 | Abell_22 |
| J002317.47−252111.6 | 5.8228 | −25.3532 | 0.0001 | 0.0001 | 0.242 | 0.030 | 0.198 | 0.015 | 8.6 | 7.8 | 143 | Abell_22 |
| J002317.15−261532.9 | 5.8215 | −26.2592 | 0.0003 | 0.0001 | 0.573 | 0.095 | 0.156 | 0.021 | 19.6 | 10.3 | 80 | Abell_22 |
Notes. The full catalogue, which includes all cluster fields, is available online at https://doi.org/10.48479/7epd-w356. Columns: (1) MGCLS source ID using the IAU designation of the form MKTCS JHHMMSS.ss±DDMMSS.s, where the decimals are truncated; (2)–(5) J2000 RA and Dec, and associated 1σ uncertainty, respectively; (6) and (7) Total integrated Stokes-I flux density and associated 1σ uncertainty at the reference frequency, respectively; (8) and (9) Peak Stokes-I brightness and associated 1σ uncertainty, respectively; (10) and (12) Source size: FWHM of the major and minor axes of the source, and source p.a.; (13) Cluster field of the source. All uncertainties are statistical only and are determined from the images as per Condon (1997).
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