Table 4
Results of the MmD technique.
| Object | F1/F2 | λ (Å) | Line | A | M | μ cont | Chromaticity | BW | LC | RW |
|
|
||||||||||
| (a) HE 0047-1756 | B/A | 5100 | C III]a | 0.277 ± 0.003 | 0.231 ± 0.007 | 1.199 ± 0.039 | DE, CML | (1) | 0 | 0 |
| B/A | 7500 | Mg II | 0.258 ± 0.003 | 0.220 ± 0.005 | 1.173 ± 0.030 | - | 1 | 0 | 1 | |
| (b) Q0142-100 | B/A | 5200 | [O VI] | 0.126 ± 0.001 | 0.126 ± 0.001 | 1.00 | DE, IV | - | - | - |
| B/A | 7100 | C III] | 0.131 ± 0.003 | 0.131 ± 0.001 | 1.00 | - | - | - | - | |
| (c) SDSS J0246-0825 | B/A | 5100 | C III] | 0.249 ± 0.003 | 0.315 ± 0.015 | 0.790 ± 0.039 | DE, CML | 1 | 0 | 1 |
| B/A | 7500 | Mg II | 0.260 ± 0.002 | 0.340 ± 0.010 | 0.765 ± 0.023 | - | 1 | 0 | 1 | |
| (d) HE 0435-1223 | B/D | 5150 | C III] | 1.093 ± 0.003 | 1.370 ± 0.030 | 0.798 ± 0.018 | DE, CML | 0 | 0 | 1 |
| B/D | 7500 | Mg II | 1.210 ± 0.002 | 1.470 ± 0.050 | 0.823 ± 0.028 | - | 0 | 1 | 1 | |
| (e) SDSS J0806+2006 | B/A | 4850 | C III]a | 0.780 ± 0.046 | 0.485 ± 0.065 | 1.608 ± 0.235 | - | 0 | 0 | 0 |
| B/A | 7100 | Mg II | 0.755 ± 0.046 | 0.420 ± 0.040 | 1.797 ± 0.203 | - | 0 | 0 | 0 | |
| (f) FBQ 0951+2635 | B/A | 6300 | Mg II | 0.295 ± 0.010 | 0.230 ± 0.020 | 1.283 ± 0.120 | - | 0 | (0) | (0) |
| (g) BRI 0952-0115 | B/A | 6650 | Ly α | 0.295 ± 0.008 | 0.440 ± 0.040 | 0.670 ± 0.064 | - | 0 | 1 | 0 |
| (h) SDSS J1138+0314 | C/B | 5300 | C IV | 0.779 ± 0.035 | 1.100 ± 0.050 | 0.708 ± 0.045 | - | 1 | 1 | 1 |
| C/B | 6550 | C III] | 0.806 ± 0.042 | 1.100 ± 0.050 | 0.733 ± 0.051 | - | 1 | 1 | 1 | |
| (i) J1226-0006 | B/A | 5950 | Mg IIb | 0.456 ± 0.007 | 0.850 ± 0.050 | 0.536 ± 0.033 | DE, LC | (1) | (1) | 0? |
| B/A | 7930 | [O II] | 0.410 ± 0.006 | 0.875 ± 0.075 | 0.464 ± 0.041 | - | 0 | 0 | 0 | |
| (j) SDSS J1335+0118 | B/A | 4890 | C III]c | 0.295 ± 0.003 | 0.250 ± 0.010 | 1.180 ± 0.049 | DE, IV | 0 | 0 | 1 |
| B/A | 7200 | Mg II | 0.321 ± 0.004 | 0.230 ± 0.020 | 1.396 ± 0.123 | - | 1 | 1 | 1 | |
| (k) Q1355-2257 | B/A | 4500 | C III]a | 0.183 ± 0.002 | 0.330 ± 0.020 | 0.550 ± 0.034 | CML, DE, LC | 0 | 0 | (0) |
| B/A | 6630 | Mg II | 0.215 ± 0.004 | 0.340 ± 0.030 | 0.632 ± 0.057 | - | 0 | 1 | 1 | |
| (l) WFI 2033-4723 | C/B | 5070 | C III]a | 0.709 ± 0.022 | 0.900 ± 0.020 | 0.788 ± 0.030 | - | 1 | 0 | 0 |
| C/B | 7450 | Mg II | 0.728 ± 0.040 | 0.900 ± 0.020 | 0.809 ± 0.048 | - | 0 | 0 | 0 | |
| (m) HE 2149-2745 | B/A | 4700 | C IVa | 0.242 ± 0.001 | 0.242 ± 0.001 | 1.00 | DE, LC, IV | - | - | - |
| B/A | 5750 | C III] | 0.245 ± 0.002 | 0.245 ± 0.002 | 1.00 | - | - | - | - | |
| (n) SDSS J0924+0219 | A/B | 4800 | C III] | 0.304 ± 0.019 | 0.39 ± 0.01 | 0.779 ± 0.053 | - | 0 | 0 | 0 |
| 7050 | Mg II | 0.296 ± 0.023 | 0.38 ± 0.01 | 0.779 ± 0.063 | - | 0 | 0 | 0 | ||
| (o) J1131-1231 | B/C | 4650 | Mg II | 0.334 ± 0.012 | 1.30 ± 0.07 | 0.257 ± 0.016 | d | 1 | 1 | 1 |
| 8050 | H β | 0.344 ± 0.030 | 1.30 ± 0.07 | 0.265 ± 0.026 | - | 1 | 1 | 1 | ||
| A/B | 4650 | Mg II | 0.630 ± 0.050 | 2.15 ± 0.05 | 0.293 ± 0.024 | d | 0 | 1 | 0 | |
| 8050 | H β | 0.630 ± 0.050 | 2.15 ± 0.05 | 0.293 ± 0.024 | - | 1 | 0 | 1 | ||
| (p) H1413+117 | AB/D | 5500 | C IV | 0.775 ± 0.010 | 0.40 ± 0.04 | 1.940 ± 0.220 | CML | 0 | 1 | 0 |
| 17200 | H β | 0.630 ± 0.010 | 0.43 ± 0.02 | 1.480 ± 0.080 | - | 0 | 0 | 0 | ||
| (q) HE 2149-2745 | A/B | 5750 | C III] | 0.214 ± 0.003 | 0.27 ± 0.02 | 0.785 ± 0.025 | CML, (DE, IV) | 0 | (1) | 0 |
| (r) Q2237+0305 | A/D | 4150 | C IV | 0.425 ± 0.002 | 1.00 |
0.425 ± 0.085 | e | 1 | 1 | 1 |
| 5150 | C III] | 0.429 ± 0.002 | 1.00 |
0.429 ± 0.085 | - | 1 | 1 | 1 | ||
| 7550 | Mg II | 0.438 ± 0.003 | 1.00 |
0.438 ± 0.088 | - | 1 | 1 | 1 | ||
Notes. See Sect. 4.3 and Appendices C and D for details. Columns #1 and #2 give the object name and the image pair used for the decomposition, Cols. #5–#7 give the continuum flux ratio A, the macro-magnification ratio M, and the micro-magnification μcont of the continuum. These quantities are given at the approximate wavelength (observed frame) given in Col. #3, which corresponds to the center of the emission line given in Col. #4 (see Sect. 4.1). Column #8 lists the possible origins of the chromatic changes of A, namely differential extinction (DE), chromatic microlensing (CML), contamination by the lens (LC), or intrinsic variability (IV). The last 3 columns indicate if microlensing of the broad line is seen in the blue wing (BW), line core (LC; [–500: +500] km s-1), or red wing (RW). The value 0 is used when there is no microlensing and 1 when it is present. The value is in parentheses when the signal is weak or depends strongly on the exact value of M.
The noisy decomposition around C III] might hide a faint broad component similar to the one observed in Mg II. There is a narrow component in the red wing superimposed to the broad one.
Spectra already corrected for chromatic effects induced by the host galaxy (see Sluse et al. 2007).
Spectra already corrected for differential extinction between A & D (see Sluse et al. 2011).
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