Table 3.
New optical photometry and published IR photometry of the Accident, and other 12 metal-poor T dwarf candidates.
| Name | u′ | g′ | r′ | i′ | z′ | zDES | zPS1 | Y | J | H | K | W1 | W2 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| The Accident | >28.7 | >27.9 | >27.6 | >27.3 | >26.2 | >26.7 | (1)>21.79 | (2)24.5±0.3 | >18.58 | Ks>17.85 | 18.18±0.19 | 16.15±0.08 | |
| W0156 | 24.70±0.24 | 25.42±0.31 | (2)21.94±0.06 | 21.46±0.30 | 18.81±0.42 | 16.06±0.08 | |||||||
| Ross 19B | 25.10±0.33 | 25.80±0.40 | (2)21.86±0.06 | 21.14±0.02 | 18.62±0.20 | 15.81±0.06 | |||||||
| W0505 | 25.24±0.36 | (*)>23.4 | 26.09±0.36 | (2)20.74±0.07 | (2)20.62±0.08 | Ks>18.38 | (**)17.64±0.06 | (**)16.13±0.05 | |||||
| W0523 | 22.10±0.03 | 22.74±0.15 | (2)19.14±0.05 | 17.27±0.06 | 15.91±0.06 | ||||||||
| W0711 | 19.48±0.03 | 20.09±0.12 | 15.09±0.03 | 14.63±0.04 | |||||||||
| W0738 | 24.29±0.19 | 25.23±0.20 | (2)21.37±0.14 | (2)20.73±0.14 | (2)21.44±0.34 | 17.22±0.04 | 15.82±0.04 | ||||||
| W0905 | 24.08±0.09 | 24.97±0.13 | 20.45±0.14 | 18.25±0.16 | 16.46±0.09 | ||||||||
| W1019 | 19.27±0.01 | 20.16±0.08 | (3)16.03±0.10 | (3)15.77±0.13 | (3)Ks 15.73±0.27 | 15.65±0.04 | 14.22±0.04 | ||||||
| Wolf 1130C | 22.64±0.05 | 23.50±0.19 | 19.64±0.09 | 19.57±0.07 | (4),(†)17.16±0.04 | (4)15.14±0.02 | |||||||
| W2014 | 21.52±0.03 | 22.36±0.5 | (5)18.01±0.02 | (5)18.71±0.30 | (5)17.97±0.29 | (4)16.66±0.04 | (4)14.83±0.03 | ||||||
| W2105 | 19.49±0.01 | 20.19±0.02 | (2)17.96±0.03 | (3)16.85±0.14 | (2)15.91±0.03 | (3)15.31±0.15 | (2)14.82±0.01 | (2)13.93±0.02 | |||||
| W2207 | 24.23±0.10 | (*)>23.4 | 25.20±0.12 | >20.36 | >18.98 | Ks>18.38 | (4)18.88±0.27 | (4)16.01±0.07 |
Notes. If not specified otherwise, the reference for the IR photometry will be the same as the one for the object in Table A.1. The optical photometry is in the AB magnitude system (Oke 1974). The JHK photometry uses the MKO filters and is in the Vega magnitude system.
Single-epoch DES 3-σ z-band limit under the AB system, as inferred from the 10-σ limit 22.1 mag (Morganson et al. 2018; Abbott et al. 2021);
From the WISE and DES images we notice that the WISE photometry may be slightly contaminated by a background source.
There are two CatWISE detections with similar proper motion values. We adopted the W1, W2 values of the one with more profile-fit flux measurements with S/N no less than 3 in both bands (column names w1NM and w2NM). (1): Meisner et al. (2023b) (2): Meisner et al. (2023a); (3): 2MASS point source catalogue (Cutri et al. 2003); (4): Profile-fit photometry including motion from CatWISE catalogue (w1mpro_pm and w2mpro_pm column) (Marocco et al. 2021); (5): Best et al. (2021).
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