Table 4
Circumstellar emission for the follow-up targets of Absil et al. (2013).
| HD | Name | Type | K | Baseline | fcse(%) JouFLU |
|
|
fcse(%) FLUOR | Δfcse(%) |
|
|
|||||||||
| 9826 | υ And | F9V | 2.84 | S1-S2 | 3.62 ± 0.61 | 1.26 | 4.42 | 0.53 ± 0.17 | 3.09 ± 0.63 |
| 40136 | η Lep | F2V | 2.91 | S1-S2 | 0.45 ± 0.47 | 2.03 | 1.8 | 0.89 ± 0.21 | 0.44 ± 0.52 |
| 102647 | β Leo | A3Va | 1.91 | S1-S2 | 1.09 ± 0.52 | 0.90 | 1.44 | 0.94 ± 0.26 | 0.15 ± 0.59 |
| 131156 | ξ boo | G7V | 1.97 | S1-S2 | −0.32 ± 0.42 | 1.40 | 1.29 | 0.74 ± 0.20 | −1.06 ± 0.47 |
| 142091 | κ CrB | K1IV | 2.49 | S1-S2, E1-E2 | 3.4 ± 0.52 | 1.85 | 6.54 | 1.18 ± 0.20 | 2.22 ± 0.56 |
| 142860 | γ Ser | F6IV | 2.62 | E1-E2 | 1.09 ± 0.78 | 1.02 | 1.17 | −0.06 ± 0.27 | 1.15 ± 0.94 |
| 173667 | 110 Her | F6V | 3.05 | S1-S2 | 2.34 ± 0.37 | 10.66 | 9.24 | 0.94 ± 0.25 | 1.40 ± 0.44 |
| 177724 | ζ Aql | A0Vn | 2.9 | E1-E2 | 1.23 ± 0.38 | 1.32 | 2.45 | 1.69 ± 0.27 | −0.46 ± 0.47 |
| 185144 | σ Dra | G9V | 2.81 | S1-S2 | −1.11 ± 1.0 | 1.88 | 1.78 | 0.15 ± 0.17 | −1.26 ± 1.01 |
| 187642 | α Aql | A7V | 0.22 | S1-S2 | 6.11 ± 0.74 | 2.76 | 27.33 | 3.07 ± 0.24 | 3.05 ± 0.78 |
| 203280 | α Cep | A7IV | 1.96 | E1-E2 | −0.14 ± 0.78 | 0.74 | 0.64 | 0.87 ± 0.18 | −1.01 ± 0.8 |
Notes. The highlighted boxes in the sixth column correspond to statistically significant excesses: red boxes indicate that the excess is statistically significant, and also consistent with the circumstellar dust model of Eq. (1). We highlight in yellow the excess of HD 173667 because it is likely due to binarity. We also report the FLUOR excess levels reported by Absil et al. (2013) (Col. 9), and the change in circumstellar emission Δfcse = fcse, JouFLU−fcse, FLUOR (Col. 10), the difference between the results obtained here, and those published by Absil et al. (2013). We find discrepant results for four stars, which are highlighted in the last column. See text for details.
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