Table 2
Status of SPOTS exploratory observations.
| Integr. | Bin. | Candidates and bkgd. obj. | Follow-up | |||
| Target | Epoch | time (s) | res.? | (hypothetical masses) | needed? | obtained? |
|
|
||||||
| ESO Program 088.C-0291(A) | ||||||
| δ Cap | 2011-10-06 | 1320 | – | |||
| IK Peg | 2011-10-10 | 1938 | 2 × 7 MJup planet at large separation | ■ | □ | |
| 1 × 7 MJup planet near IWA (4.9 σ) | ||||||
| HIP 12545 | 2011-10-31 | 2040 | – | |||
| TYC 5907 1244 1 | 2011-11-05 | 1224 | – | |||
| HIP 16853 | 2011-11-09 | 1596 | 1 × star | |||
| HIP 9892 | 2011-12-03 | 960 | 1 × background galaxy | |||
| EM Cha | 2011-12-15 | 1428 | 1 × confirmed background star | |||
| TYC 8569 3597 1 | 2011-12-17 | 1200 | crowded field | ■ | ||
| AF Lep | 2011-12-20 | 1596 | – | |||
| Alhena | 2011-12-22 | 1320 | ■ | 2 × brown dwarf | ■ | ■ |
| HIP 25709 | 2011-12-22 | 2520 | – | |||
| 26 Gem | 2012-01-13 | 1638 | 1 × high-mass brown dwarf at IWA | ■ | ■ | |
| HIP 76629 | 2012-07-20 | 1672 | crowded field | ■ | ||
| ESO program 090.C-0416(B) | ||||||
| V1136 Tau | 2012-11-21 | 1560 | ■ | 1 × star | ||
| TYC 6386 0896 1 | 2012-11-26 | 1224 | – | |||
| XZ Pic | 2013-01-03 | 960 | – | |||
| UX For | 2013-01-05 | 2280 | ■ | – | ||
| TYC 8104 0991 1 | 2013-01-07 | 1200 | – | |||
| HIP 47760 | 2013-01-24 | 1224 | – | |||
| TYC 6604 0118 1 | 2013-01-26 | 1224 | – | |||
| GS Leo | 2013-02-10 | 1560 | 1 × 12 MJup planet near IWA | ■ | ■ | |
| TYC 9399 2452 1 | 2013-03-03 | 1224 | 1 × 10 MJup planet | ■ | ||
| HS Lup | 2013-04-30 | 1596 | 3 × 6–11 MJup planet | ■ | ||
| HIP 78416 | 2013-05-11 | 720 | 1 × foreground star | ■ | ||
| 4 × 5–11 MJup planet | ||||||
| 3 × background galaxy | ||||||
| CS Gru | 2013-06-26 | 720 | – | |||
| BS Ind | 2013-06-28 | 1560 | 2 × 3–9 MJup planet | ■ | ||
Notes. A black square in the column “Bin. res.?” indicates that the target binary has been resolved in our images. In the last two columns, a black square indicates that follow-up observations were deemed necessary, and were successfully executed, respectively. The empty square for the target IK Peg marks a follow-up observations that was executed, but turned out to be insufficiently sensitive to re-detect the candidate sources. The acronym IWA stands for inner working angle, which, in this particular context, refers to the minimum angular separation from the star at which there is sufficient field rotation to perform LOCI ADI processing. Note that detections near the IWA suffer from increased false alarm probability due to small-number statistics (Mawet et al. 2014). Background galaxies are identified by their visibly extended morphology that is inconsistent with the stellar PSF observed in the unsaturated calibration frames. None of the targets with reliable follow-up observations have yielded any comoving companions.
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