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Table C.9

PACS flux densities for the DUNES_DB stars with d ≤ 15 pc and 15 pc <d ≤ 20 pc.

HIP HD PACS100 S100 χ100 PACS160 S160 χ160 Status
(mJy) (mJy) (mJy) (mJy)
FGK stars (d ≤ 15 pc)
1599 1581 33.23 ± 2.35 30.08 ± 0.19 1.34 29.03 ± 3.46 11.75 ± 0.07 4.99 Dubious
3765 4628 19.43 ± 1.93 15.84 ± 0.36 1.83 <3.38 6.19 ± 0.14 No excess
7751 10360 11.95 ± 1.70 12.39 ± 0.21 −0.26 <5.00 4.84 ± 0.08 No excess
10361 10.66 ± 1.68 14.90 ± 0.26 −2.49 <5.00 5.82 ± 0.10 No excess
7918 10307 14.33 ± 1.75 16.21 ± 0.25 −1.06 10.35 ± 3.17 6.33 ± 0.10 1.27 No excess
7981 10476 20.18 ± 1.91 20.05 ± 0.21 0.07 7.87 ± 2.05 7.83 ± 0.08 0.02 No excess
10644 13974 23.45 ± 2.07 20.75 ± 0.30 1.29 6.59 ± 3.60 8.11 ± 0.12 −0.42 No excess
12114 16160 15.29 ± 1.74 17.26 ± 0.24 −1.12 5.91 ± 3.32 6.74 ± 0.09 −0.25 No excess
12843 17206 20.94 ± 2.08 19.10 ± 0.22 0.88 7.52 ± 3.18 7.46 ± 0.09 0.02 No excess
14879 20010 40.72 ± 2.70 38.77 ± 1.48 0.63 24.90 ± 3.58 15.14 ± 0.58 2.69 No excess
15457 20630 24.78 ± 2.02 19.85 ± 0.24 2.43 12.14 ± 2.52 7.75 ± 0.09 1.74 No excess
15510* 20794 48.62 ± 2.64 40.60 ± 0.34 3.01 27.12 ± 2.33 15.86 ± 0.13 4.82 Excess
16852* 22484 67.30 ± 3.64 28.09 ± 0.34 10.71 33.35 ± 3.19 10.97 ± 0.13 7.01 Excess
22449 30652 65.99 ± 3.67 58.79 ± 0.29 1.95 22.97 ± 0.12 No excess
23693 33262 33.97 ± 2.33 17.49 ± 0.42 6.97 9.39 ± 2.84 6.83 ± 0.17 0.90 Excess
27072 38393 49.21 ± 2.95 43.99 ± 0.29 1.76 19.67 ± 3.13 17.18 ± 0.11 0.80 No excess
37279 61421 867.50 ± 43.38 733.50 ± 8.48 3.03 355.75 ± 17.88 286.50 ± 3.31 3.81 Dubious
47080 82885 10.12 ± 1.87 13.56 ± 0.21 −1.83 8.30 ± 3.16 5.30 ± 0.08 0.94 No excess
56997 101501 15.43 ± 1.71 14.83 ± 0.14 0.35 12.69 ± 3.51 5.79 ± 0.05 1.97 No excess
57443 102365 16.22 ± 1.96 19.83 ± 0.17 −1.84 < 3.85 7.74 ± 0.07 No excess
57757 102870 68.43 ± 3.80 48.38 ± 0.23 5.26 40.67 ± 3.83 18.90 ± 0.09 5.68 Excess
59199 105452 27.10 ± 2.16 21.65 ± 0.34 2.49 25.40 ± 3.29 8.46 ± 0.13 5.14 Dubious
61317 109358 31.43 ± 2.34 30.76 ± 0.30 0.28 9.52 ± 3.46 12.02 ± 0.12 −0.72 No excess
61941 110379J 85.77 ± 4.59 71.92 ± 0.86 2.97 49.43 ± 3.86 28.10 ± 0.34 5.50 Dubious
64394 114710 23.74 ± 1.98 28.55 ± 0.25 −2.41 13.50 ± 3.26 11.15 ± 0.10 0.72 No excess
64924* 115617 211.56 ± 10.74 23.67 ± 1.10 17.40 161.27 ± 8.74 9.24 ± 0.43 17.37 Excess
70497 126660 36.36 ± 2.46 30.16 ± 0.33 2.50 15.57 ± 3.17 11.78 ± 0.13 1.20 No excess
72659 131156 57.51 ± 7.46 27.42 ± 0.55 4.02 42.14 ± 8.58 10.71 ± 0.21 3.66 Dubious
73695 133640 32.17 ± 2.15 24.01 ± 0.25 3.77 30.83 ± 2.94 9.38 ± 0.10 7.30 Dubious
77257 141004 33.11 ± 2.35 25.19 ± 0.42 3.32 20.23 ± 3.12 9.84 ± 0.16 3.33 Dubious
78072 142860 30.71 ± 2.26 35.81 ± 0.20 −2.25 24.40 ± 3.91 13.99 ± 0.08 2.66 No excess
80686 147584 17.31 ± 1.75 15.45 ± 0.28 1.05 < 3.92 6.03 ± 0.11 No excess
89937 170153 57.97 ± 3.27 55.98 ± 0.31 0.61 32.41 ± 3.72 21.87 ± 0.12 2.83 No excess
93017 176051 18.73 ± 1.79 13.38 ± 0.26 2.95 < 5.02 5.23 ± 0.10 No excess
99825 192310 11.79 ± 1.87 14.17 ± 0.16 −1.27 8.32 ± 3.35 5.53 ± 0.06 0.83 No excess
102485 197692 27.11 ± 2.35 23.05 ± 0.20 1.72 9.13 ± 3.09 9.00 ± 0.08 0.04 No excess
105858 203608 30.87 ± 2.23 28.59 ± 0.46 1.00 14.85 ± 3.34 11.17 ± 0.18 1.10 No excess
109176 210027 34.70 ± 2.38 34.35 ± 0.51 0.14 16.90 ± 3.39 13.42 ± 0.20 1.03 No excess
113283 216803 12.21 ± 1.57 12.48 ± 0.25 −0.17 12.69 ± 1.73 4.87 ± 0.10 4.51 Excess
116771 222368 42.11 ± 2.66 29.19 ± 0.44 4.79 21.75 ± 3.33 11.40 ± 0.17 3.10 Excess
FGK stars (15 pc <d ≤ 20 pc)
5862 7570 24.36 ± 2.03 13.83 ± 0.14 5.16 7.33 ± 3.29 5.40 ± 0.06 0.59 Excess
17651 23754 26.70 ± 2.16 21.10 ± 0.53 2.52 8.22 ± 3.23 8.24 ± 0.21 −0.01 No excess
36366 58946 22.24 ± 1.92 18.79 ± 0.32 1.77 18.78 ± 3.47 7.34 ± 0.12 3.30 Dubious
44248 76943 34.66 ± 2.29 28.35 ± 0.59 2.67 22.61 ± 3.38 11.07 ± 0.23 3.40 Dubious
46509 81997 19.15 ± 1.91 16.06 ± 0.13 1.62 9.20 ± 3.36 6.27 ± 0.05 0.87 No excess
48113 84737 9.56 ± 1.56 13.94 ± 0.14 −2.80 9.77 ± 3.35 5.44 ± 0.06 1.29 No excess
61174* 109085 252.00 ± 16.00 16.00 ± 0.43 14.75 231.00 ± 13.00 6.25 ± 0.17 17.29 Excess
64241 114378J 26.01 ± 2.02 21.70 ± 0.14 2.13 16.09 ± 3.09 8.48 ± 0.05 2.47 No excess
67153 119756 19.70 ± 1.88 19.51 ± 0.20 0.10 5.72 ± 2.84 7.62 ± 0.08 −0.67 No excess
71284 128167 39.45 ± 2.57 16.13 ± 0.09 9.06 18.40 ± 3.13 6.30 ± 0.04 3.87 Excess
75312 137107J 12.01 ± 1.86 14.53 ± 0.25 −1.34 4.69 ± 3.45 5.68 ± 0.10 −0.29 No excess
77760 142373 22.41 ± 1.99 23.38 ± 0.16 −0.49 17.09 ± 3.25 9.13 ± 0.06 2.45 No excess
88745* 165908 87.00 ± 10.00 15.69 ± 0.75 7.11 80.00 ± 15.00 6.13 ± 0.29 4.92 Excess
104858 202275 25.12 ± 2.00 20.14 ± 0.19 2.48 5.26 ± 3.61 7.87 ± 0.07 −0.72 No excess
112447 215648 26.32 ± 2.19 27.73 ± 0.29 −0.64 16.19 ± 3.19 10.83 ± 0.11 1.68 No excess

Notes. The uncertainties σ(PACSν(λ)) for PACS100 and PACS160 are the statistical plus systematic, combined quadratically; values of 5% of the fluxes for the systematic uncertainties (calibration) were considered at both wavelengths (Balog et al. 2014). PACS fluxes for HIP 61174 are from Duchêne et al. (2014). PACS fluxes for HIP 88745 are from Kennedy et al. (2012). HIP 7751 has been treated as a single source in the statistical analysis of the sample. HIP 72659 is a binary (G7-8V+K5V); however, the SED is best fitted with the G8 photosphere only. HIP 73695 is a W UMa eclipsing binary (F5V+G9V); however, the SED is best fitted with the G9 photosphere only. S100 and S160 values for HIP 88745 (F7V+K4V) are from a composite model so as to include both components of the binary. PACS70 fluxes for HIP 15510 (100.0 ± 5.0 mJy, Kennedy et al. 2012), HIP 61174 (230.0 ± 13.0 mJy, Duchêne et al. 2014), HIP 64924 (198.0 ± 3.0 mJy, Wyatt et al. 2012), and HIP 88745 (93.0 ± 10.0 mJy, Kennedy et al. 2012) have also been used in this work. In addition to the PACS data, SPIRE flux densities have been included in the SEDs of these sources: HIP 61174: 100.0 ± 10.0 (250 μm), <100.0 (350 μm), <10.0 mJy (500 μm) (Duchêne et al. 2014). HIP 64294: 129.0 ± 21.0 (250 μm), 55.0 ± 17.0 (350 μm), 20.0 ± 12.0 mJy (500 μm) (Wyatt et al. 2012). HIP 88745: 44.0 ± 6.0 (250 μm), 22.0 ± 7.0 (350 μm) (Kennedy et al. 2012).

(*)

denotes that the source is extended.

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