Table A.3.
Astrometry of sources in the field of PKS 1830−211.
| Reference | Instrument | Position relative to image A (−RA, −Dec offsets, mas) (a) | |
|---|---|---|---|
| Image B | Others | ||
| Lehár et al. (2000) | HST (K,H,I) | (653, 721) ±1 | lens G: (501, 445) ±80 |
| Courbin et al. (2002) | HST & Gemini | (654, 725) ±2 | lens G: (519, 511) ±80 |
| (V,I,K) | SP: (285, 722) ±40 | ||
| Winn et al. (2002) | HST (V,I) | lens G: (328, 486) ±4 | |
| Meylan et al. (2005) | VLT (J,H,Ks) | (649, 724) ±1 | lens G: (498, 456) ±4 |
| star P: (333, 504) ±2 | |||
| Jin et al. (2003) | VLBA (43 GHz) | (642.092, 728.086) ±0.2(systematics) (b) | |
| This work | ALMA | (641.946 ±0.042, 728.082 ±0.033) | C: (500.1 ±2.1, 459.6 ±1.6) |
Notes.
Jin et al. (2003) observed time changes in the separation between images A and B of up to 0.2 mas within eight months, most likely produced by intrinsic changes in the brightness distribution of the background quasar which is enhanced by the lens magnification. The given relative position corresponds to the nominal reference at the first epoch of their observations.
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