Table A.4.
Pair candidates with existing ALLWISE channel W1/W2 photometry.
| Prime QSO | RA/Decl. (2000.0) | g′ | r′ | i′ | z′ | J | H | K | W1 | W2 | ID |
|---|---|---|---|---|---|---|---|---|---|---|---|
| CFHQSJ0227-0605 | 36.9473 −06.0495 | >25.56 | 24.26±0.17 | 21.64±0.05 | 20.11±0.04 | 18.91±0.06 | 18.65±0.06 | 18.84±0.13 | 19.67±0.10 | 20.38±0.33 | L0 |
| HSCJ0859+0022 | 134.7528 +00.3927 | >24.90 | 23.30±0.10 | 20.88±0.04 | 19.29±0.03 | 18.05±0.06 | 17.82±0.06 | >17.72 | 18.67±0.05 | 19.26±0.16 | L0 |
| PSOJ037.9706-28.8389 | 38.0071 −28.8519 | >25.02 | >24.59 | 23.27±0.21 | 21.75±0.08 | 20.27±0.12 | 19.99±0.14 | 19.70±0.23 | 20.29±0.15 | – | M9 |
| PSOJ055.4244-00.8035 | 55.4110 −00.8079 | >23.72 | >23.52 | >23.25 | 21.71±0.19 | 20.08±0.24 | >20.26 | >19.21 | 20.04±0.15 | 19.95±0.30 | QSO |
| PSOJ075.9356-07.5061 | 75.9660 −07.4760 | >25.59 | >25.11 | 22.03±0.07 | 20.43±0.04 | 19.27±0.07 | 18.95±0.07 | 18.97±0.28 | 19.64±0.11 | >19.93 | L3 |
| PSOJ135.8704-13.8336 | 135.8657 −13.8220 | >25.08 | 23.44±0.11 | 21.13±0.04 | 19.43±0.03 | 17.91±0.05 | 17.62±0.05 | 17.86±0.08 | 18.29±0.04 | 18.78±0.10 | L3 |
| PSOJ340.2041-18.6621 | 340.2045 −18.6680 | >25.36 | >24.87 | 22.09±0.06 | 20.53±0.04 | 19.08±0.06 | 18.81±0.07 | 19.14±0.15 | 19.65±0.12 | 19.77±0.26 | L1 |
| SDSSJ0005-0006 | 1.4755 −00.0968 | >25.06 | 23.76±0.18 | 21.40±0.05 | 19.67±0.03 | 18.14±0.05 | 17.94±0.06 | 17.88±0.08 | 18.67±0.06 | 18.79±0.11 | M9 |
| ULASJ0148+0600 | 27.1558 +06.0265 | >25.46 | >24.89 | >23.92 | 22.41±0.13 | 21.06±0.18 | 20.93±0.27 | >19.28 | 19.90±0.14 | >19.89 | QSO/Gal |
Notes. Magnitudes are not corrected for foreground AV, all in the AB system. The ID column gives the best-fitting Le PHARE spectral template. The object marked in boldface had a QSO template as best-fit Le PHARE output, which is inconsistent with our GMOS spectrum; we therefore provide the next best-fit template, a low-redshift galaxy, as potential identification.
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