Table 1
Observed (S1–4) and model-predicted (future: SX, past: SY) positions of SN Refsdal, the centre of Sp1149 (SC), and four star-forming clumps for comparison (F1–4).
| Cl. | RA | Dec | μ a | F O ii b | F Mg ii c |
| (J2000) | (J2000) | (10-18 erg s-1cm-2) | |||
|
|
|||||
| S1 | 177.39821 | 22.39563 | 13.5 |
39.1 ± 1.7 | 2.6 ± 0.6 |
| S2 | 177.39771 | 22.39579 | 12.4 |
29.2 ± 1.0 | 2.3 ± 1.0 |
| S3 | 177.39737 | 22.39554 | 13.4 |
20.4 ± 0.9 | 1.6 ± 1.1 |
| S4 | 177.39780 | 22.39517 | 5.7 |
16.3 ± 1.2 | 1.8 ± 1.3 |
| SX | 177.40012 | 22.39670 | 4.8 |
15.0 ± 1.9 | 1.6 ± 0.8 |
| SY | 177.40382 | 22.40205 | 4.0 |
15.2 ± 1.7 | 1.5 ± 1.2 |
| SC | 177.39702 | 22.39599 | 7.0 |
56.8 ± 1.1 | – |
| F1 | 177.39744 | 22.39641 | 11.7 |
25.8 ± 1.5 | – |
| F2 | 177.39883 | 22.39769 | 8.5 |
26.7 ± 1.9 | 2.9 ± 1.4 |
| F3 | 177.39975 | 22.39656 | 9.4 |
19.6 ± 1.6 | 2.1 ± 1.0 |
| F4 | 177.40313 | 22.40257 | 3.9 |
30.5 ± 1.8 | 0.2 ± 0.5 |
Notes. The emission line fluxes are determined in an 0.6′′-radius aperture, and are not corrected for magnification.
emission line flux of Mg iiλ 2796 Å corrected for stellar absorption (see Guseva et al. 2013).
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