Table 6.
Lens masses ML and distances DL for best fitting solutions assuming different distances to the source or lens mass distribution.
| Parameter | GF+ | GF− |
|---|---|---|
| Gblend [mag] |
 |
 |
| Mass function ∝M−1.00, 14.5 kpc < DS < 23.0 kpc | ||
| ML [M⊙] |
 |
 |
| DL [kpc] |
 |
 |
| GMS [mag] | < 10.76 (B2.5V) | 10.95 (B5V) |
| Mass function ∝M−3.00, 14.5 kpc < DS < 23.0 kpc | ||
| ML [M⊙] |
 |
 |
| DL [kpc] |
 |
 |
| GMS [mag] | 17.81 (F6V) | 21.89 (K8V) |
| Mass function ∝M−1.75, 6.4 kpc < DS < 9.8 kpc (B − J distance) | ||
| ML [M⊙] |
 |
 |
| DL [kpc] |
 |
 |
| GMS [mag] | -0.39 (B7V) | 13.13 (A0V) |
Notes. Gblend is the limit for the brightness of the lens, GMS is the brightness of the lens if it was a MS star of mass similar to ML located at the median distance DL. We assumed that extinction changes with the distance (see Sect. 5). The absolute magnitude in the G-band was taken from PM, we provide the spectral type of the object used for calculations in brackets.
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