Table 3.
Multiply imaged systems used to calculate the best-fit model of the foreground mass distribution.
| Image ID | RA | Dec | zspec | zopt | ||||
|---|---|---|---|---|---|---|---|---|
| Best | Fixed center | Faint arcs | Non-cored | NFW | ||||
| 1.1 | 171.81167 | 42.472683 | 2.236 | – | – | – | – | – |
| 1.2 | 171.81128 | 42.473342 | 2.236 | – | – | – | – | – |
| 2.1 | 171.81197 | 42.471372 | – | 2.2 ± 0.1 | 3.4 ± 0.3 (1) | 2.2 ± 0.2 (2) | 1.1 ± 0.5 | 1.9 ± 0.2 |
| 2.2 | 171.80998 | 42.474375 | – | ″ | ″ | ″ | ″ | ″ |
| 2.3 | 171.80819 | 42.475792 | – | ″ | ″ | ″ | ″ | ″ |
| 3.1 | 171.81230 | 42.471500 | – | 2.3 ± 0.1 | 3.4 ± 0.3 (1) | 2.2 ± 0.2 (2) | 1.0 ± 0.4 | 2.0 ± 0.2 |
| 3.2 | 171.81004 | 42.474744 | – | ″ | ″ | ″ | ″ | ″ |
| 3.3 | 171.80872 | 42.475778 | – | ″ | ″ | ″ | ″ | ″ |
| 4.1 | 171.81252 | 42.471500 | – | 2.4 ± 0.1 | 3.4 ± 0.3 (1) | 2.2 ± 0.2 (2) | 1.0 ± 0.4 | 2.0 ± 0.2 |
| 4.2 | 171.80974 | 42.475153 | – | ″ | ″ | ″ | ″ | ″ |
| 4.3 | 171.80925 | 42.475558 | – | ″ | ″ | ″ | ″ | ″ |
| 5.1 | 171.81668 | 42.474678 | – | 2.2 ± 0.4 | 3.6 ± 0.4 | 2.0 ± 0.3 | 1.2 ± 0.6 | 1.8 ± 0.4 |
| 5.2 | 171.81513 | 42.476181 | – | ″ | ″ | ″ | ″ | ″ |
| 5.3 | 171.81402 | 42.478100 | – | ″ | ″ | ″ | ″ | ″ |
| 6.1 | 171.81725 | 42.474458 | – | 2.1 ± 0.3 | 3.5 ± 0.3 | 2.0 ± 0.2 | 1.2 ± 0.5 | 1.7 ± 0.4 |
| 6.2 | 171.81499 | 42.476697 | – | ″ | ″ | ″ | ″ | ″ |
| 6.3 | 171.81440 | 42.477931 | – | ″ | ″ | ″ | ″ | ″ |
| 7.1 | 171.81637 | 42.474692 | – | 2.3 ± 0.3 | 3.0 ± 0.3 | 2.0 ± 0.3 | 1.2 ± 0.5 | 1.8 ± 0.5 |
| 7.2 | 171.81503 | 42.475978 | – | ″ | ″ | ″ | ″ | ″ |
| 8.1 | 171.81590 | 42.478017 | – | 3.5 ± 0.3 | 1.0 ± 0.6 | 3.5 ± 0.4 | 1.8 ± 0.5 | 3.5 ± 0.3 |
| 8.2 | 171.81584 | 42.478325 | – | ″ | ″ | ″ | ″ | ″ |
| 8.3 | 171.81591 | 42.477315 | – | ″ | ″ | ″ | ″ | ″ |
| 9.1 | 171.82636 | 42.481387 | – | ⊘ | ⊘ | 1.5 ± 0.8 | ⊘ | ⊘ |
| 9.2 | 171.82567 | 42.481899 | – | ⊘ | ⊘ | ″ | ⊘ | ⊘ |
Notes. Colors and positions of most images are measured from the HST imaging, expect for system #1 which represents the PdBI CO(4–3) morphology of the Emerald, the bright submm arc. Systems #1 to #8 are the most securely identified from their position, color and morphologies and were used in each of the five models, while system #9 was only considered in one alternative model and ignored in the remaining four (⊘ symbols). Here zopt refers to the redshifts derived from our lens models, and their 1σ confidence intervals, with indices (i) indicating systems that were fitted with a common redshift. Measuring spectroscopic redshifts for other multiply imaged systems would allow us to discriminate between models and to better constrain the foreground dark-matter distribution.
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