Overview of the observed emission lines in the X-shooter and SINFONI spectra. For non-detections, upper limits are given (see Section 3.1 for details).
| Instrument . | Image(s)a . | Feature . | |$\lambda _\text{vac} \, (\mathring{\rm A})^b$| . | |$\Delta v \, (\mathrm{km\, s^{-1}})^c$| . | |$\mathrm{Flux} \, (10^{-18} \, \mathrm{erg \, s^{-1} \, cm^{-2}})^d$| . | |$\mathrm{EW} \, (\mathring{\rm A})^e$| . |
|---|---|---|---|---|---|---|
| X-shooter | 1 | Lyα | 1215.67 | 156 ± 52 | 440.4 ± 5.9 | 143.3 ± 12.9 |
| |${\rm C\, \small {IV}}$| | 1548.19 | 104 ± 53 | 12.7 ± 3.1 | 11.9 ± 3.2 | ||
| |${\rm C\, \small {IV}}$| | 1550.77 | 104 ± 53 | 6.18 ± 3.48 | 5.78 ± 3.34 | ||
| |${\rm He\, \small {II}}$| | 1640.42 | … | <6.11 | <6.21 | ||
| [|${\rm C\, \small {III}}$|] | 1906.68 | … | <26.7 | <35.2 | ||
| |${\rm C\, \small {III}}$|] | 1908.73 | … | <46.0f | <25.4f | ||
| |${\rm Mg\, \small {II}}$| | 2796.35 | 52 ± 54 | 5.00 ± 1.49 | 16.2 ± 5.1 | ||
| SINFONI | 2 and 3 | [|${\rm O\, \small {II}}$|] | 3727.09 | 0 ± 13 | 60.5 ± 4.5 | … |
| [|${\rm O\, \small {II}}$|] | 3729.88 | 0 ± 13 | 71.4 ± 4.5 | … | ||
| [|${\rm Ne\, \small {III}}$|] | 3869.85 | 0 ± 13 | 60.4 ± 12.6 | … |
| Instrument . | Image(s)a . | Feature . | |$\lambda _\text{vac} \, (\mathring{\rm A})^b$| . | |$\Delta v \, (\mathrm{km\, s^{-1}})^c$| . | |$\mathrm{Flux} \, (10^{-18} \, \mathrm{erg \, s^{-1} \, cm^{-2}})^d$| . | |$\mathrm{EW} \, (\mathring{\rm A})^e$| . |
|---|---|---|---|---|---|---|
| X-shooter | 1 | Lyα | 1215.67 | 156 ± 52 | 440.4 ± 5.9 | 143.3 ± 12.9 |
| |${\rm C\, \small {IV}}$| | 1548.19 | 104 ± 53 | 12.7 ± 3.1 | 11.9 ± 3.2 | ||
| |${\rm C\, \small {IV}}$| | 1550.77 | 104 ± 53 | 6.18 ± 3.48 | 5.78 ± 3.34 | ||
| |${\rm He\, \small {II}}$| | 1640.42 | … | <6.11 | <6.21 | ||
| [|${\rm C\, \small {III}}$|] | 1906.68 | … | <26.7 | <35.2 | ||
| |${\rm C\, \small {III}}$|] | 1908.73 | … | <46.0f | <25.4f | ||
| |${\rm Mg\, \small {II}}$| | 2796.35 | 52 ± 54 | 5.00 ± 1.49 | 16.2 ± 5.1 | ||
| SINFONI | 2 and 3 | [|${\rm O\, \small {II}}$|] | 3727.09 | 0 ± 13 | 60.5 ± 4.5 | … |
| [|${\rm O\, \small {II}}$|] | 3729.88 | 0 ± 13 | 71.4 ± 4.5 | … | ||
| [|${\rm Ne\, \small {III}}$|] | 3869.85 | 0 ± 13 | 60.4 ± 12.6 | … |
Lensed image(s) from which the spectroscopic measurements were taken (see Sections 2.1 and 2.2 for details).
Vacuum rest-frame wavelength.
Velocity offset with respect to the systemic redshift as measured by the relevant instrument (X-shooter: zsys = 4.8737; SINFONI: zsys = 4.8754). Uncertainty in the velocity offsets includes the uncertainty in determining the systemic redshift (see Section 3).
Observed fluxes, uncorrected for the lensing magnification factor of |$\mu = 29_{-11}^{+9}$| of image 1, observed by X-shooter (Section 2.1), and |$\mu = 21_{-8}^{+12}$| and |$\mu = 138_{-74}^{+7}$| of image 2 and 3, respectively, observed collectively by SINFONI (Section 2.2).
Rest-frame equivalent width (EW; positive values indicating a feature is observed in emission). Note that EWs are independent of lensing magnification.
Upper limits inferred under the assumption of a minimum ratio of F1907/F1909 ≈ 1.39 for |$n_\mathrm{ e} \le 10^3 \, \mathrm{cm^{-3}}$| (see Section 3.1).
Overview of the observed emission lines in the X-shooter and SINFONI spectra. For non-detections, upper limits are given (see Section 3.1 for details).
| Instrument . | Image(s)a . | Feature . | |$\lambda _\text{vac} \, (\mathring{\rm A})^b$| . | |$\Delta v \, (\mathrm{km\, s^{-1}})^c$| . | |$\mathrm{Flux} \, (10^{-18} \, \mathrm{erg \, s^{-1} \, cm^{-2}})^d$| . | |$\mathrm{EW} \, (\mathring{\rm A})^e$| . |
|---|---|---|---|---|---|---|
| X-shooter | 1 | Lyα | 1215.67 | 156 ± 52 | 440.4 ± 5.9 | 143.3 ± 12.9 |
| |${\rm C\, \small {IV}}$| | 1548.19 | 104 ± 53 | 12.7 ± 3.1 | 11.9 ± 3.2 | ||
| |${\rm C\, \small {IV}}$| | 1550.77 | 104 ± 53 | 6.18 ± 3.48 | 5.78 ± 3.34 | ||
| |${\rm He\, \small {II}}$| | 1640.42 | … | <6.11 | <6.21 | ||
| [|${\rm C\, \small {III}}$|] | 1906.68 | … | <26.7 | <35.2 | ||
| |${\rm C\, \small {III}}$|] | 1908.73 | … | <46.0f | <25.4f | ||
| |${\rm Mg\, \small {II}}$| | 2796.35 | 52 ± 54 | 5.00 ± 1.49 | 16.2 ± 5.1 | ||
| SINFONI | 2 and 3 | [|${\rm O\, \small {II}}$|] | 3727.09 | 0 ± 13 | 60.5 ± 4.5 | … |
| [|${\rm O\, \small {II}}$|] | 3729.88 | 0 ± 13 | 71.4 ± 4.5 | … | ||
| [|${\rm Ne\, \small {III}}$|] | 3869.85 | 0 ± 13 | 60.4 ± 12.6 | … |
| Instrument . | Image(s)a . | Feature . | |$\lambda _\text{vac} \, (\mathring{\rm A})^b$| . | |$\Delta v \, (\mathrm{km\, s^{-1}})^c$| . | |$\mathrm{Flux} \, (10^{-18} \, \mathrm{erg \, s^{-1} \, cm^{-2}})^d$| . | |$\mathrm{EW} \, (\mathring{\rm A})^e$| . |
|---|---|---|---|---|---|---|
| X-shooter | 1 | Lyα | 1215.67 | 156 ± 52 | 440.4 ± 5.9 | 143.3 ± 12.9 |
| |${\rm C\, \small {IV}}$| | 1548.19 | 104 ± 53 | 12.7 ± 3.1 | 11.9 ± 3.2 | ||
| |${\rm C\, \small {IV}}$| | 1550.77 | 104 ± 53 | 6.18 ± 3.48 | 5.78 ± 3.34 | ||
| |${\rm He\, \small {II}}$| | 1640.42 | … | <6.11 | <6.21 | ||
| [|${\rm C\, \small {III}}$|] | 1906.68 | … | <26.7 | <35.2 | ||
| |${\rm C\, \small {III}}$|] | 1908.73 | … | <46.0f | <25.4f | ||
| |${\rm Mg\, \small {II}}$| | 2796.35 | 52 ± 54 | 5.00 ± 1.49 | 16.2 ± 5.1 | ||
| SINFONI | 2 and 3 | [|${\rm O\, \small {II}}$|] | 3727.09 | 0 ± 13 | 60.5 ± 4.5 | … |
| [|${\rm O\, \small {II}}$|] | 3729.88 | 0 ± 13 | 71.4 ± 4.5 | … | ||
| [|${\rm Ne\, \small {III}}$|] | 3869.85 | 0 ± 13 | 60.4 ± 12.6 | … |
Lensed image(s) from which the spectroscopic measurements were taken (see Sections 2.1 and 2.2 for details).
Vacuum rest-frame wavelength.
Velocity offset with respect to the systemic redshift as measured by the relevant instrument (X-shooter: zsys = 4.8737; SINFONI: zsys = 4.8754). Uncertainty in the velocity offsets includes the uncertainty in determining the systemic redshift (see Section 3).
Observed fluxes, uncorrected for the lensing magnification factor of |$\mu = 29_{-11}^{+9}$| of image 1, observed by X-shooter (Section 2.1), and |$\mu = 21_{-8}^{+12}$| and |$\mu = 138_{-74}^{+7}$| of image 2 and 3, respectively, observed collectively by SINFONI (Section 2.2).
Rest-frame equivalent width (EW; positive values indicating a feature is observed in emission). Note that EWs are independent of lensing magnification.
Upper limits inferred under the assumption of a minimum ratio of F1907/F1909 ≈ 1.39 for |$n_\mathrm{ e} \le 10^3 \, \mathrm{cm^{-3}}$| (see Section 3.1).
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